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SB1. Blue companion? Giant eclipsing binary. Amp. =>0.2V. Period close to SB. Also classified as ellipsoidal var. AP PscAlpheratz represents the head of [X/Andromeda]. It is approximately 100 [G/light year]s distant and 160 times more [G/luminous] than our [G/Sun]. Alpha CV 2.02 - 2.06V, 0.9636 or 0.966222d. Some spectral lines vary same period, others half period, some nonvariable. ALPHERATZAmp. 0.07V. 6.6 A6IV, 6.9 A8IV, 456y, a = 0.924". Combined mag. and colors. Delta Sct, amp. 0.03V, 0.10101d. CaphCombined mag., color. Primary F4III, comp. B, F3III. Companion 9.44V, +0.34(B-V), -0.14(U-B), G5Ve. Suspected occultation double. AB, CPM, combined mag., color. Component B, 8.2 F3/5 IV, HD 662. C, 14v at 20". Beta C 2.80 - 2.87V, 0.1517495d. ALGENIBAB 6.7 G3III, 7.5 F2IV, 368y, a = 0.564". ADS 161C, 10.37V, K0, at 18", physical. 4.78 - 4.86V. CPM. Lb? 5.06 - 5.16V. AD CetLb 4.26 - 4.46V. AE CetComponent A is SB. ADS 191B, 7.3v dA7 at 12". Period apsidal motion, 3y. Possible radio binary. Ell 6.0 - 6.03V, 0.841678d. UU Psc6.8 B8V, 7.1 B9V, 1600y, a = 1.260". Combined mag., colors. CPM. Fixed sep. 6.47 - 6.52V. EB 5.96 - 6.11B, 6.07 - 6.24V, O9III+O9III, 3.523487d. Spontaneous var. in period. Polarization indicates circumstellar envelope possibly related to mass exchange. AO CasDelta Sct?, 4.49 - 4.55V. CPM. Companion F3V. ADS 254B, 9.5 - 12v. Component B, 12.87v at 63", optical. 3.46 - 3.56V. Deneb Kaitos SheB9.5, A2. SRc 5.0 - 6.9v, 6.6 - 7.7p, 158.9d. T CetOptical. BY Dra, amp. 0.032V, 0.037B, 7.655d. BE CetADS 328B, 8.0 at 0.2". However, ADS 328 appeared single in 1953. ADS 328A, E?, 5.56 - 5.62V. Amp. 0.07V. Suspected double probably single. 2.75 - 2.81V. A* 2.38 K0III, 10.538y, a = 0.072". ANKAAAmp. 0.36V. SR 4.65 - 5.42V, 49d, replaced by cycles 70 - 85d. TV PscLb 4.7 - 4.90V. 7.2 G1V, 7.2 G1V, 5.625y, a = 0.134". Combined mag. and colors. ADS 412AB, CPM. ADS 409B 13.3v at 3" CPM with A. Delta Sct 5.18 - 5.22V, 0.0689797d. GN AndOptical. Delta Sct? Amp. 0.04y, 0.174?d. BB Phe5.5 B7.5V, 5.8 B8.5V, 640y, a = 0.586". Combined mag. and colors. Components 14 and 13 solar masses. Optical. CPM with HR 127 of which both are close binaries. Also CPM with HR 136. Faint companion at 14". CD 4.9 A2V, 5.6 A7V, 44.43y, a = 0.385". Combined mag., colors. D-C = 1.17V. Alpha Cyg, 4.22 - 4.30B, 0.09028d. ADS 449A is triple occultation system, 6.2, 6.9v, sep. 0.031"; third component 8.8v at 0.196". ADS 449B, 9.7v at 27.5". AB are CPM. Suspect eclipsing because invisible at time of occultation. ADS 455AB, CPM. B, 10.4v K0V. C, 12.3v at 60". Short period binary. Both components A-type. Sep. 0.099". CPM with HR 126 and 127. Delta Sct 6.06 - 6.15V, 0.04931 and 0.0604d. AB 5.6 F7V, 6.3 G0V, 6.92y, a = 0.23". Combined mag., colors, spectrum. ADS 490A?, Delta Sct?, 5.18 - 5.22V. Amp. 0.06B. Delta Sct, 43.0 minutes. BG Cet3.59 - 3.68V. AB 103000?y. Component B spectrum A6V or Am(A3/F0/F2), RV +11.9k/s. Component C, 11.4v, F3 at 55" optical. Beta CMa, amp. 0.035V, 0.096d. Different cycles show different amplitudes, from 0.002 to 0.036V. Doubt has been expressed that this is due to interference between different periods. RV also shows amplitude changing from a few to 25k/s. Line profiles also vary. AG Psc6.3 G7V, 6.4 G8V, 25.00y, a = 0.670". Combined mag., colors. Companion optical. AB CPM. Component C, 15.2v at 48" optical. 5.83 - 5.89V. Binary. D is 8.5v K2IV-V, vsini <54k/s. All components probably optical. Cst 2.20 - 2.27V. SHEDIRCst 6.68V. Z SclSuspected visual double is probably single. Resolved by speckle interferometry 1983.93, sep. 0.145", but unresolved 1981.68, 1983.94. CPM. Alpha C, 5.69 - 5.78V, 3.952d. A0, A9. Diphda is a slightly reddish star a little over 50 [G/light year]s away. It is approximately 40 times more [G/luminous] than our [G/Sun]. 1.96 - 2.11V. DIPHDAHigh velocity star, possible runaway. Physical pair. ADS 624A, EA 5.71 - 6.12B, 4.467224d, i 87.95d. Amp. of primary 0.40V, secondary 0.12V. YZ CasCPM. Companion F8. Gamma Cas, 4.50 - 4.62V, amp. 0.3:R, 1.1679d. AB CPM. Primary F5III, secondary F6IV. Lb?, 5.32 - 5.45V. Delta Sct? 5.99 - 6.03V, 0.1040d. XX PscAB CPM. Companions probably optical. Component A of visual system, EB 3.92 - 4.14V, 17.7695d. AB 3.45 G3V, 7.51 K4Ve, 480y, a = 11.994". Combined mag., colors. Component B, vsini =<25k/s. Companions C-H optical. A possible invisible companion with period about 40y. Component B, 7.51V, +1.39(B-V), +1.03(U-B). AchirdThe two companions probably optical. CPM. CPM with HR 230. 5.33 - 5.39V. Alpha CV 6.10 - 6.14V, 2.156d. Also var. K-line, same period. GO And5.15 - 5.24V. 6.04 - 6.11V. Delta Sct 6.34 - 6.37V, 0.1360d; sinusoidal components 0.0526 and 0.0396d. V526 CasDelta Sct 5.20 - 5.25V, 0.055d. AZ PheDelta Sct 5.17 - 5.27V, 0.110d. Optical. Combined mag. and color. Fixed sep. AB CPM. Component B, dG4. Primary F4IV, secondary G0V. AB optical. AB 6.23 A1V, 6.89 A4V, 360.4y, a = 0.700". Combined mag., colors. Lb? 5.60 - 5.80V. BQ TucAB 6.02 G6IV, 6.41 K6IV, 164.68y, a = 1.014". Resolved by speckle interferometry 1983.94, sep. 0.68". Combined mag., colors. AB CPM. IRAS observations confirm IR excess and yield simple blackbody temperature of 6750 +/- 100K. ADS 782A, Gamma Cas 1.6 - 3.0v. Spectrum and color vary. Expanding circumstellar shell. High-velocity variable mass loss. Variable hydrogen emission, 0.7d. Variable SiIV, CIV, polarization. Variable X-ray source. H alpha indicates rotating disk-like envelope. AB 6.0 B8V, 6.6 B9V, 83.4y, a = 0.252". Total mass, 6 solar. Primary is a mercury-manganese star. All components optical. ADS 805, 790y. Possible periodicities: 19.4, 16.7, 0.95, 0.49d. Visual binary with HR 282. Color for blended images. Lb 5.95 - 6.12V. WW Psc6.7 A3n, 8.0, 450y, a = 0.816". Suspected occultation double, 5.2, 5.2v, sep. 0.25". AB binary. Component B, G8V. Amp. 0.10V. CC TucVisual pair optical. CPM with HR 311. Third component optical. CPM with HR 310. CPM with HR 314. Faint companions probably optical. CPM with HR 313. AB optical. A* 5.15 G5Vp, 21.43y, a = 0.186", mag. diff 2V, sep. 1.4". Subdwarf with five visual and one astrometric components. MarfakMag. and color blend of close pair 4.2, 4.2v. C, 11.5v at 57". Companions probably optical. Delta Sct? 5.8 A2IV, 6.2 A4IV, 28.5y, a = 0.209". Combined mag., colors. Dheneb4.6 B6IV, 5.5 B9V, 371.6y, a = 0.447". Combined mag., colors. Masses 16 and 10 solar. Resolved by speckle interferometry 1983.93, sep. 0.64". Suspected visual double is probably single. MIRACHAB 4.2, 7.0v close binary; vsini of B 87k/s. C, 7.0 F7V at 6.6" CPM. Primary component of visual system. EA 3.92 - 4.42V, 1.6697664d, i 84.7d. Delta Sct? MarfakCst? 5.50 - 5.60V. RU CasL?, 7.1 - 9.0p. Unresolved by speckle interferometry: probably single. AB CPM. Component B, 10.25V, +0.79(B-V), +0.29(U-B), G1V. Delta Sct? 5.93 - 5.98V, 0.05d. AI SclB CPM, 9.11V, +0.92(B-V), +0.25(U-B). CPM with HR 362 at 24". ADS 996A is close occultation double, 6.3, 6.3v, 0.05":. Component B, HR 362 is SB; C, 12.2 is 1" from B. CPM with HR 361. SRb?, amp. 0.15V. Alpha CV?, 5.94 - 5.98V. Mag. 7.38V and colors from Nicolet. However, HD gives 6.38ptm, 7.38ptg. Abt and Biggs RV Bibliography quotes 6.20V; and AGK3 has 7.7ptg. CPM. Component B, G7V. Component C is faint diffuse nebula, NGC 450. RS, 5.35 - 5.58V. AY CetQuadruple system consisting of two close CPM pairs separated by 320": CPD -69d45, components AB, 5.1, 7.3, 5" and CPD -69d44, components CD. AB, 1222.4y, a = 7.64"; CD 7.8 G5, 8.2, 86.2y, a = 1.12". ADS 1073, quintuple system: A = NGC 457 #136; B, 12.3v at 49"; C = NGC 457 #131 = HD 7902, 6.99V, +0.42(B-V), -0.38(U-B), B5Ia at 134", vsini =<25k/s; D, 10.19V, +0.29(B-V), -0.47(U-B) at 179"; E, 10.63V, +0.28(B-V), -0.52(U-B) at 170". BC 7.4, 7.6, 21.5y, a = 0.136". Combined spectrum A1V. AdhilAB 7.1, 7.3v, binary, combined mag. and color. Components C, 12.8v at 46" and D, 10.50v at 249" probably optical. CPM. ADS 1129B, 13.5v, 3" CPM with A. Component C optical, 9.18V, +0.66 (B-V), +0.34(U-B), Am. Delta Sct 6.20 - 6.22V, 0.070d. AV CetProbably optical. Unresolved by speckle interferometry 1981.69. EA? 2.68 - 2.76V, 759d. Ruchbah6.6 F3V, 6.8 F4V, 16.14y, a = 0.1884". Combined mag. and color. AB binary, B 11.7v at 2"; CD 10.4, 10.4 sep. 4.9" at 120" from A. Optical. Binary. Companion 9.38V, +0.19(B-V), +0.00(U-B), A8V, vsini 48k/s. CPM. SRb 9.1 - 12.8p, 370d. R SclA* 2.0 var. F8Ib, 30.46y, a = 0.038". AB physical; B, 8.20V, +0.49(B-V), +0.16(U-B), F3V, 0.0 color excess, vsini =<60k/s; C, 13v at 43"; D, 14v at 83". Polaris is the star currently aligned with Earth's north [G/Celestial Pole]. It is only the 49th brightest star in the sky. Polaris is actually a double star system, made up of two faint stars that are 465 [G/light year]s away. CDelta 1.92 - 2.07V, 3.969778d. Period increases 53 sec./century. Probably unreddened. POLARISCPM. Component B is BD+7d214, 8.02V, +0.53(B-V), +0.06(U-B), G0. 3.39 - 3.49V. Delta Sct 6.56 - 6.59V, 0.090d. WZ SclDelta Sct 5.90 - 5.92V, 0.131d. VX PscAmp. 0.15V. AW PheCPM. Primary K3.5IIIab, secondary G2V. CPM. ADS 1199B, 8.0 - 11.5v? Unresolved by speckle interferometry 1983.94. Probably optical. Amp. about 0.015u, <0.01v, 0.694d. Alpha CV, amp. 0.012V, 0.6684d. Also long-period variations. KK Andbrightening at rate of about 0.045m/100d. OP AndBoth visual companions probably optical. 6.0 F3V, 7.1, probably combined mag. and color. Alpha CV 6.27 - 6.41V, 36.5d; Sp. and magnetic field var., 22-24y. UII and PmII lines vary in 6.7 hrs. GY And6.8 F5, 7.2, 28.3y, a = 0.19". Possible radio binary. Visual companion optical. Achernar is hot, blue giant star that ranks as the 9th brightest star in the sky. It is approximately 125 [G/light year]s distant and 650 times more [G/luminous] than our [G/Sun]. EB or Ell, amp. 0.02V. H alpha var. emission and possible high-velocity mass loss. Expanding circumstellar shell. ACHERNARCPM. Component B, 11.53V, +0.65(B-V), +0.04(U-B). Alpha CV, 5.55 - 5.64V, 3.1848d. V557 CasCPM. Combined mag., colors. Primary F4IV-V, secondary F8V. EA, amp. 0.3V, 16.77d. Third component mag. diff 4.74v, 110" from A. Component B is K2V, optical. Astrometric binary 20y, a 0.12", mag. diff 3-4v. Companion 25% solar mass. AB CPM; B is F2III; C optical. Binary with HR 487, q.v. Gamma Cas 4.03 - 4.11V, 19.5d. Amp. varies in per. 127d. Possible mass loss. Expanding circumstellar shell. 6.4 A2, 7.8 F0, 573.52y, a = 1.07". Torcularis SepteComponent A, astrometric binary unresolved by speckle interferometry. AB 5.4 F1V, 8.6 G9V, 1192.2y, a = 4.652". C 15.0v at 15", D 11.5v at 142". Spectrum of secondary also classified K1V. Delta Sct 6.54 - 6.59V, about 0.2d. VY PscCPM. Component C 8.4v at 21", D 10.2v at 137". Binary. Component B 7.3v A6V, P.A. 166d; RV, 1.8k/s, variable. Confusion in literature as to which component is HD 11154, which 11155. Probably combined mag. and color. CPM. Companion, dG1 is HD 11131. E? 5.46 - 5.68y. V436 PerSecond visual component optical. Baten KaitosDelta Sct, 5.90 - 5.94V, 0.037312d; also possibly 0.1662, 0.038351 and 0.043013d. BD PheSeginVisual companions probably optical. MetallahBinary with HR 546, q.v. Combined mag. HR 545/6, 3.88V; colors also combined. Sp. var. 38 min. Delta Sct, 5.73 - 5.81V, 0.090336d; also possibly 0.1996 or 0.1663d and 0.09417 or 0.10396d. BK CetDelta Sct? SharatanSR 4.3 - 4.5V, 30d. ADS 1534B not CPM with HR 557, component A. ADS 1534AP, CPM, 11.9v at 18". EA? 6.42 - 6.84p, 47.9?d. RR Ari6.76 F7, 6.76 G0, 170.3y, a = 1.05". Alternate orbit 158.4y, a = 1.00". Masses 1.34 and 1.29 solar. Combined mag. and colors. 6.00 - 6.30V. CPM. Optical. ADS 1563B, 7.40V, +0.58(B-V), +0.07(U-B), dG1, CPM; vsini =<25k/s. ADS 1563B; Cst? 7.30 - 740V. Eta2 HyiAB 4.71 A4V, 6.41 F2V, 60.44y, a = 0.653". Perturbation periods of 26 or 39y suspected. C, 13.6v, 24" CPM; D, 13.0v 48" optical. Additional unseen companion suspected. ADS 1598B. B-A varies 1.5 - 3.0v. ADS 1582AB, 8.5, 11.0v, sep. 2.3" at 188" from the bright component D. C, 9.2v at 31" from A. SR? 5.40 - 5.61V. AR CetADS 1625AB, CPM. Binary with HR 596, q.v. Alpha CV? ADS 1621. Uncertain which component varies. B-A from 4.5 - 6.0v. CPM with HR 604. ALMAAKAB 5.90 F8IV, 7.27 F9V, 288.0y, a = 1.256"; or 309.03y, a = 1.34". Other published periods have ranged from 247 to 925y. Combined mag., colors. Suspected occultation double. ADS 1634AB CPM. B, G5V; C at 83" optical. Alpha CV?, 4.68 - 4.73V, 1.89d. SR 6.20 - 6.38V, about 20d. WZ PscHamal, the brightest star in [X/Aries], lies 67 [G/light year]s away and is 70 times more [G/luminous] than our [G/Sun]. HAMALAmp. 0.065V. Sp. var., H alpha profile var. V472 PerSR?, amp. 0.08V. B, mag. diff 6.9v at 5.6". CPM with HR 629. CPM with HR 628. Resolved by speckle interferometry 1983.93, sep. 0.07". Binary. Companion F6V. Amp. 0.075V pulsating? TZ TriPossible nearby star on basis of spectroscopic parallax. 6.6 F3V, 7.08 F6V, 144.7y, a = 0.908". Combined mag., colors. Suspected occultation double, sep. 0.012". E?, 4.35 - 4.38V. AB binary; B, dG4; C, 11.5v at 173". 19.35y, a 0.17" or 18.614y, e 0.616, a 0.158", 10.82AU, i 130.1d. Alternate orbit 19.35y, a = 0.17". Speckle interferometric sep. 0.17", 1983.93. Possible nearby star on basis of spectroscopic parallax. Probably optical. 5.52 - 5.58V. Companion G2V? Mira is a pulsating, variable, red giant star which changes in brightness from [G/magnitude] 3 to magnitude 9 over the course of 331 days. It is approximately 135 [G/light year]s distant. AP var. M7IIIe, var. dBe, 400y, a = 0.85". The faint companion was first predicted in 1920 by Joy on the basis of a slightly displaced blue secondary spectrum. First seen by Aitken in 1923. Visible only when Mira is faint. Light variations on scale of hours superimposed by variations of 10-15 min. and rare flares of 2 min. duration. Components B, 13v at 73" and C, optical. Two variables: Mira and VZ Cet. Mira, ADS 1778A, M 2.0 - 10.1v, 331.96d; var. CO emission from circumstellar envelope. Speckle interferometry indicates large abrupt variation of diameter as a function of wavelength. Hydrogen lines vary on time scale of 1-2 days. Mira was discovered to be variable by Fabricius in 1596, the first such variable discovered. ADS 1778P, Ne "Novoides" class, VZ Cet, 9.5 - 12.0v, dBe. MIRAAmp. 0.05U, 1.31d. Fixed. Amp. 0.05V. Sp. and H alpha profile var. V474 PerCDelta, amp. 0.123V, 7.572d. V440 PerAmp. at 0.58 micrometers about 0.15m. AB 4.64 A3Vp, 6.89 F5, 840y, a = 2.27". A* 4.64 A5p, 52.4y, a = 0.113". Unresolved by speckle interferometry. ABxC 4.51 A5p, 8.40 G7V, probably physical, 6.706" periastron for parabolic orbit. vsini of C =<50k/s. ADS 1860A, Alpha CV, 4.45 - 4.53V, 1.74050d. Also magnetic and Sp. period. AB CPM. Alpha CV 5.71 - 5.88V, 2.997814d. Irregular magnetic var., 15.9d. AB CetCompanion A3IV. ADS 1878A, spectrum variable, shell star. Amp. 0.11V, 0.09R. TZ HorADS 1904AB binary; B, 11v. Suspected occultation double. Delta Sct 6.11 - 6.15V, 0.080d. UU AriDelta Sct? 6.49 - 6.51V, 0.05d, pulsating. TY ForCompanions optical. Companion 7.83V, +0.20(B-V), +0.15(U-B), A7V or A3Vm; vsini 167k/s. Probably optical. Companion, A5, optical. Lb?, 5.39 - 5.53V. Optical. Visual companion 11.7v dM6 at 165", CPM. A* 5.84 K3V, 60y, a = 0.257".. Mass of invisible companion 0.12 solar. Companion at 2" probably about 5v fainter. Unresolved by speckle interferometry. Binary. Companion 9.08V, +0.56(B-V), +0.19(U-B), F7V. Proper motion from AGK3. Earlier McCormick determination, +.022",-.013". M 5.4 - 12.6v, 266.43d. R TriSep. 0.021". CPM with HR 765. HR 764 formerly misidentified as the SB = HR 765. Data for HR 764 and 765 have frequently been interchanged. CPM with HR 764. B 12v, 8" optical; AC CPM; D, mag. diff 5.97v at 40" from A. Beta C 4.05 - 4.10V, 0.16113668d. Per. changed 1965, then increased about 0.7 sec./century. 5.6 F6V, 5.6 F6V, 2.67y, a = 0.108". Combined mag., colors. CPM. Optical. 0.906y, a = 0.057". ADS 2046. Delta Sct?. Uncertain which component varies. AB fixed. AB 6.2, 12.2v, 19" about 6y. Occultations indicate A is triple system, 7.0v A1, at 0.06", and 8.0v at 0.2". Aa resolved by speckle interferometry, sep. 0.045" 1981.68, 0.040" 1981.69. Delta Sct? AB 4.13 F7V, 9.87 M1V, 2720y, a = 22.289". C probably optical. AB CPM. AB binary, combined mag., colors. CPM with BD+2d418, 10.2v M6 at 840". KaffaljidhmaDelta Sct 5.18 - 5.22V, 0.0355d with overtones of 0.046 and 0.061d. UV AriOccultation binary. Combined mag., color. Delta Sct? Binary. Combined mag., color. EA 6.18 - 7.72V, 1.1952473d. Period varies irregularly. i 82.14d. May have two dark companions with orbital periods 23 and 105y. RZ CasAB binary. 7.1 F5, 7.1 F8, 28.5y, a = 0.279". Amp. 0.038V. V480 PerSuspected occultation double, 6.8, 6.8v, sep. 0.2". CDelta 5.78 - 6.16V, 1.949319d, possibly changing. RV varies in same period. SU CasAlpha CV, 5.82 - 5.89V. VZ AriSRb 7.0 - 8.63p, 80d. Secondary cycle 746d. Z EriComponent B, B9V, CPM, vsini 149k/s. MiramAB CPM. B 8.8v, A0Vp at 3.2", RV -21k/s, probably optical; C 10.72V, +0.60(B-V), +0.60(U-B), F8V at 25". A is close SB pair with computed sep. 0.00004". Optical system. Delta Sct? AB CPM, B, 13v at 12"; C, optical. AB, 7.2, 9.2v sep. 0.2" possibly optical; AC binary. Primary G6III, secondary G4V. AngetenarA* 4.06 G4III+A4V, 4.150y, a = 0.050". Speckle interferometric sep. 0.080" 1981.67. Circumstellar material surrounding the pair? Visual companions 10.7v at 51" possibly physical; 11.8v at 4" possibly optical. EA, 3.94 - 4.07V. AB 5.9 F4V, 6.5 F6V, 31.37y, a = 0.258". Nearly equal components, 3.7, 4.3 solar. Component C, 9.7v at 14", CPM? Delta Sct? Component B, 15v, possibly spurious. SRb 5.62 - 6.01V, 30d. Rho1 Fl 44M 4.7 - 14.3v, 401.5d, JD2412800-28900; later 407.6d. R HorAlpha CV 5.03 - 5.14V, 2.88422d, same for RV and line-intensities. Also var. magnetic field and H-lines. Rotating spotted star. LT PerAzhaGorgonea SecundaBinary. Companion F7IV. Binary with HR 888. Mag. and colors for combined light. Uncertain if HR 887 or 888 is the variable suspect. CPM with HR 891. CPM with HR 890. MenkarBinary with HR 898. Uncertain which component var. Combined mag. HR 897/8, 2.91V; combined colors, +0.125(B-V), +0.13(U-B). ACAMARLb? 6.11 - 6.29V. CV EriADS 2348B probably optical. Lb? 2.45 - 2.54V. Spectrum var. MENKARSKYLAB observations indicate cool star with hot companion. Components Aa, 14.65y, a = 0.159". Physical nature of B, 11m at 57", uncertain. Close to error box of X-ray source 3U0305+53. CPM. ADS 2312B, 8.5 - 11.0v. SRb 3.30 - 4.0V, about 50d with possibly slow var. in mean brightness in 1100d period. Gorgonea TertiaSee HR 927. Algol is an eclipsing variable star, meaning the light from this star appears to brighten and fade as its companion star passes in front of the star and behind it. The star's [G/magnitude] changes in brightness from mag. 2.1 to mag. 3.4, over the course of 2.8 days. Algol is approximately 100 [G/light year]s distant. A* var. B8V, 1.858y, a = 0.011" or 1.862y, a = 0.104". Apparent apsidal period 28.4y or 32y. Resolved by speckle interferometry: sep. 0.086", 2-3v fainter than primary. This may be Algol C. Four visual companions all optical: B, 12.7v at 59"; C, 12.5 at 67"; D, 10.5 at 82"; BC sep. 15"; E, 12.5v at 11" from D. One of the few known galactic radio sources in which the dominant star is normal. 21cm radio source. ADS 2362A is the prototype Algol star, first discovered as variable by Montanari in 1669. The first period determined by Goodricke in 1783, who also interpreted the variations as due to eclipses. The prototype star proves to be a more a complicated system than most of the Algol-type stars, i.e., compact triple system with separation of the components well under 0.1". The components usually designated Algol A, B, C, sometimes A, a, P. Two formerly additionally desig- nated components D and E, inferred on the basis of an apparent 32 year apsidal motion, are now considered spurious. The various Algol components must not be confused with the visual components ADS 2362 B-E, optical companions at much greater distances from A. ADS 2362A, EA 2.12 - 3.40V, 2.86732442d, abrupt period changes. Orbital and rotation periods synchronized. Rotational velocity 65k/s. Radio flares extending to about 1 A.U., not associated with X-ray activity. Radio flare activity appears correlated with period discontinuities, attributed to "starquakes." Mass flow from K to B8 component at rate of 1.8x10E-08 solar masses/year. Possible circumstellar material associated with radio or H alpha emission. ALGOLSep. 0.03". Runaway star from Ori OB1 association at 59k/s. Presumably originated in Ori 1 assoc. Its space vel. is twice that of HR 1712 = AE Aur and opposite that of HR 2688. These three stars and HR 1996 (Mu Col) appear to be receding from an HII shell of about 110000 solar masses expanding at 10k/s. Beta C 6.10 - 6.23V, 0.15275d. Possibly a SN 4.9 million yrs. ago. UW AriInterferometric double, 6.3, 6.3v. Combined mag. and color. Companion optical. Constant light but large H-line variation. Gorgonea QuartaSuspected occultation double. BoteinSuspected occultation double. SX Ari 5.67 - 5.81V, 0.7278925d. Spectral variations (SiII, HeI, same period). Possible 30 min Sp. var. suggesting star spots related to magnetic field. Silicon abundance varies 10 to 100 times solar, and magnesium 0.03 to 10 times solar. SX AriOptical. Space motion same as for Hyades cluster. AB CPM. C, 13.1v at 11" optical. Delta Sct? CPM. 3.9 F8IV, 6.5 G7V, 314y, a = 4.367". Combined mag., colors. ADS 2402B, 7.0 - 9.03v. FornacisAB 6.8 A2V, 7.3 A4V, 330y, a = 0.386". Combined mag., colors. AB 6.6 G2III, 6.9 A7IV, 44.82y, a = 0.443". Combined mag., colors. Component C 9.5v at 3" physical. Amp. 0.06(U-B). Ell 6.16 - 6.28V, 5.543491d. V423 PerSRb 5.52 - 5.95V, about 158d. TW HorComponent B, 8.0 A7m. CPM. Secondary 8.06V. Amp. 0.02V. Fundamental and overtone periods 0.041 and 0.065d. BN HyiADS 2440. B-A varies from 0.2 to 2.0m. Uncertain which component varies. B6, A1. ZibalProbably optical. Gamma Cas, 4.78 - 4.89V. Spectrum var. 4.5y from 1916 to 1931, previously longer cycles, but no changes noted after 1937. R-I also found at -0.03 and -0.05. BK Cam5.6 K1IV, 7.5 G8V, 351.94y, a = 1.077", or 217.20y, a = 0.974". Combined mag., colors. Double discovered by Alvan Clark. CPM with BD-1d474, 9.5v at 11'. ADS 2459B, 7.66V. Doubtful var. Combined light ADS 2459AB, 5.37 - 5.46V. Considered variable by Gould, but never confirmed. CoD-22d1146 C, 11.9v at 251". RW Aur? Amp. 0.10 IR. Binary. AB binary, B is K0V. C, 11v at 40" optical. Lb? 3.57 - 3.72V. Tau4 Eri7.3 - 7.4B. Suspected of being double or triple by Tebbutt in 1893. Components 5.4, 7.9v, sep. 0.15", and 8.4v at 0.67". CPM with HR 1010. Nearby star suspected of variability from discordant photometric observations. CPM with HR 1006. MIRPHAKAB CPM. Binary. AB 6.8 B9V, 7.8 A1V, 259.90y, a = 0.370". Combined mag., colors. H alpha profile var. 7.2, 7.2, sep. 0.1" listed by D. W. Dunham. Probably not occultation double. H alpha profile variable. 550y. AB CPM. Delta Sct. ADS 2552A is close binary, 6.3, 7.7v, sep. 0.010". AB binary; C, 13v at 148". EA, amp. 0.1V, 5.363d. Alpha CV 5.45 - 5.53V, 2.4928d. First helium-weak star found to have periodic variations (1973). V396 PerB CPM, A3V, vsini 100k/s, both components. AB CPM. B, spectral class F2V. Component C, 10.5v at 164". Beta C 6.37 - 6.47V, 0.2101753d, multiple periods, 0.1982, 10.85, 0.01d. KP PerAB 6.8 F3V, 7.6 F9V, 287.7y, a = 1.245". Combined mag., colors. Mass AB, 2.2 solar. C, 10.3v at 92" optical. Ell 5.80 - 5.85V, 0.9171877d. IW PerEll 5.90 - 6.04V, 0.935971d. TU HorAstrometric binary, 25y. Unresolved by speckle interferometry. AB 6.6 A3V, 6.7 A3V, 568.22y, a = 0.650" or 600y, a = 0.719". Combined mag., colors. C, 9.9v at 22" physical. Amp. 0.04V, 0.5d. Hydrogen emission variable. Expanding circumstellar shell. 6.8 F5V, 7.1 F6V, 19.4y, a = 0.225". Combined mag., color. Spectrum variable. 5.88 dG9, 8.83, B-V +0.99, U-B +0.79, K6V, 2101y, a = 8.023". Close radio binary. RS 5.70 - 5.81V, 2.83782d. Min. migrate in period 13y. Brightest of 25 RS CVn binaries known in 1976. Also var. radio emission. Radio flare star with variable polarization. Amp. in red light (6600 A) 0.11 mag. Star spots inferred to be about 1100d cooler than surrounding photosphere. V711 Tau5.23 - 5.32V, amp. 0.11U, 1.93d. EG EriCPM? Position angles disagree by about 40d. Lb 5.04 - 5.17V, 6.7 - 6.85p. BD CamADS 2661A, occultation double?, 7.1, 7.1v, sep. 0.3". Component B, 11.8v at 36" optical. Component D, 8.73V, +0.10(B-V), -0.22(U-B), B8III. Gamma Cas?, 5.55 - 5.58V. Alpha CV? 2.98 - 3.03V, about 1d. Strong variable emission at 1650A, CaII? 5y? Sep. 0.052". vsini of secondary =<50k/s. Binary. Combined mag., colors. Rotational velocity B, 150:k/s. Unresolved by speckle interferometry 1982.16. In interstellar ultraviolet radiation field. Ell 3.79 - 3.85V, 4.419171d, possibly half. AtikRS:, 3.51 - 3.56V, about 10d. RanaSuspected occultation binary, sep. 0.0062". Unresolved by speckle interferometry 1981.69. CelaenoCPM. Sep. 0.062". Occultation of 1972 Mar. 19 indicated mag. diff 3.4, sep. 0.010". ElectraPrimary is SB, 4.6, 6.1v, sep. 0.012". Visual pair 4.4, 8.1v, sep. 69". TaygetaSep. 0.003". Unresolved by speckle interferometry 1981.69. Duplicity questioned. Probably cst. Var. helium lines. MaiaAsteropeSuspected occultation double. Sterope IIB possibly optical. Lc 4.35 - 4.48V, amp. 0.12p. BE CamSuspected double probably single star. Variable hydrogen emission. MeropeCPM. Primary K1IIIab, secondary G3IV. Probably optical. Lb? 4.38 - 4.44V. Binary. B-A varies from 2.8 to 4.3V. Uncertain which component varies. Component A is occultation double, sep. 0.031". B, C, D, 8.1 A0V, 8.1 Am(A5/F0/F2) and 8.7v F2V at 117" to 190". Possibly second occultation companion at 0.001", unresolved by speckle interferometry. vsini of B 155k/s. Numerous photometric determinations yield 6.3 for B component. The HD gives 8.1 for 23629 and the IDS indicates 8.1. Burnham, Double Stars, gave 7.0 vis. ALCYONEDelta Sct 5.8 - 5.91V, variable amp. Primary and beat periods, 0.098299 and 0.39206d. V376 Per11.1v companion at 5" noted by Innes not confirmed. Binary. Old disk population runaway star. A variable comparison star was used when HR 1176 was suspected of variablility. A published period, 22.58d, does not satisfy available SB observations, whereas the SB period does satisfy the photometric equally well. However, more observations are badly needed. V467 PerComponent A SB, 4.1, 5.6, sep. 0.006" and 0.019". B, 6.8v at 0.4". AtlasGamma Cas 4.77 - 5.50V. Var. may be clue to shell episodes. Shell ejection 1936 led to decrease in light 1937-1958. Variable hydrogen emission. Shell spectrum shows phase changes every 17 or 34 yrs. Pleione5.81 A3V, 6.21 A5V, 62.28y, a = 0.430". Resolved by speckle interferometry 1983.93, sep. 0.66". Binary with HR 1190. Suspected occultation double. Old disk population runaway star. Amp. 0.06y?, 2.53d. V766 TauCompanion F4V, optical. AB CPM, B 9.16V B8IV; C, 9.12V at 33" optical; D, 10.35V, +0.713(B-V), +0.20(U-B), at 92" optical; E, 9.90V, A2V, +0.33(B-V), +0.17(U-B), at 120" physical. 2.80 - 2.93V. Companion A0, CPM. CPM? Component A possibly optical counterpart or companion of X-ray source 4U0352+30. Possibly a triple system with a neutron star moving around the optical primary in 22.4 hrs., and either apsidal period 581d or close double moving around a distant component in 581d. Rotational velocity of primary, vsini 306k/s. Component ADS 2859B is normal M1III, not T Tau type as once assumed. Space velocities of X Per and Xi Per indicate the two stars approached to within 17 pc 2 million yrs ago. ADS 2859A, Gamma Cas 6.07 - 7.0V, 580.7?d. Amp. about 0.02U. X-ray period 22.4 hrs. Spectrum variable. Sudden decrease in H alpha emission followed by 450 sec. flare in continuum. Possible neutron star companion pulsating in 13.924 min. Simultaneous X-ray and optical obs. 21 Jan. 1975 showed X-ray var. by factor 2 but no corresponding optical 100 sec. quasi periodic photometric var. may indicate binary with compact companion undergoing mass accretion. X PerAB CPM. Component C, 11.4v at 101" optical. P, 12.5v at 279". Binary with HR 1211. Tau8 EriBeta C?, 5.45 - 5.50V. RV possibly var. 0.13169d. Alpha CV 5.97 - 6.00V, 12.4580 or 12.4564d. Rotation and magnetic field same period, no polarity reversal. Spectrum variable, 12.460d. Maximum intensity Eu at minimum light. DO EriAB combined mag. and color. C, 12.7v at 23". AB CPM. B, 7.39V, -0.03(B-V), -0.52(U-B), B9.5V, vsini 300:k/s. Beta C, 2.88 - 3.00V, 0.216:d. Brightest component on visual triple. Photoelectric and spectroscopic resonant periods found are submultiples of 26.9 hrs or 1.12d. V817 TauDelta Sct 6.50 - 6.58V, 0.052d. V386 PerDelta Sct 6.17 - 6.24V, 0.155879d. DL EriDelta Sct. Slightly variable, possibly same period as SB. Menkib5.54 gG8, 6.29 A7, 415.1y, a = 1.00". 2.88 - 2.96V. ZaurakEA 3.3 - 3.80p, B3V+A, 3.952955d, i 86d. Alpha CV 4.62 - 4.67V, 1.2094d. Tau9 EriComponent B, F8V, optical. Third component mag. diff 6.13v, at 100". Lb?, amp. 0.07V. XY DorA is occultation binary, sep. 0.033", unresolved by speckle interferometry 1981.68. Spectrum binary; vsini of early-type component 160k/s. AB, mag. diff 6.5v, sep. 25.5". Beta C amp. 0.04b, over 1d? AB fixed. Some confusion in literature as to which component is A, which B. SZ CAM is Np = B, 6.94V, +0.41(B-V), -0.53(U-B), O9.5V, vsini 160:k/s. Colors of both components have been described as "yellowish" even though both have B-type spectra. Component Q, 10.39V, +0.58(B-V), -0.26(U-B). Two variables: ADS 2984A = NSV 1458, amp. 0.05V, SB; component B = SZ Cam, Np, EA 7.0 - 7.29B, changing period, abrupt change in 1972 from 2.6984378 to 2.69854365, later to 2.6985439d. SZ CamLb? 4.42 - 4.64V, 25d. Alpha CV 5.15 - 5.22V, 7.227424d. Earlier period 11.94d still frequently quoted. Lines of SiII, SrII, possibly TiII var. GS TauGamma Cas 4.00 - 4.10V, 55?d. Slow var. possibly associated with emission spectrum. MX PerCPM with GC 4949 at 12' = ADS 2995, a triple system 7.3 dK2, 9.0 sep. 1"; C at 234". CPM. B is dG8. ADS 2999, B-A varies from 2.95 to 3.55V. Uncertain which component varies. Delta Sct? Primary of ADS 3006 is occultation binary, sep. 0.05". Visual companion, 9.3v at 4.4", CPM. Delta Sct 5.37 - 5.44V, 0.144923d. Possible other periods 0.126535 and 0.126569d. Light curve composite of 0.1449 and 0.1120d. Amp. B-V 0.035, amp. U-B 0.015. Variations in U-B opposite in phase from B-V. IM TauProbably var., amp. 0.08V. Spectrum var. Delta Sct 4.00 - 4.05V, 0.0815d. Secondary per. 0.1291d. BeidA* 4.13 G0Ib, 0.778y, a = 0.019". AB CPM; B, 11.8v at 15". C , 10.25V, +0.47(B-V), +0.06(U-B), B8. ADS 3071A, 4.1 - 4.24V. B, 13.6v at 8"; C, optical. 6.0 F2V, 6.1 F3V, 7.18y, a = 0.135". Resolved by speckle interferometry 1983.93, sep. 0.09". AB binary; C, 12v at 32" optical. AB binary, B is G2V. CPM with HR 1322. BY, 6.92 - 7.00V. The fainter component of ADS 3085. Amp. 0.06V, 6.8d rotational period traced by large scale star-spot activity. V891 TauCPM with HR 1321. 6.28 - 6.37V. V774 TauSource of weak radio emission. Ell 4.59 - 4.65V, 1.527365d. Radio binary showing radio flare activity. Third component may eclipse primary. b PerBC 9.51 A2, 11.18 M4Ve, 252.1y, a = 6.943". Component B is white dwarf. Component A, CPM. ADS 3093C; UV, min. 11.18V, +1.50 (B-V), 12.16 - 13.85U. X-ray source. KeidDuplicity questioned. Visual primary is speckle-interferometric double, sep. 0.076". Visual companion 10.7v at 166". Amp. 0.020V. EW? or Delta Sct? 4.23 - 4.27V, per. between 0.33 and 1.0d. CPM with HR 1341. Optical. CPM with 1339. 0.07V, 1.569d (light and spectrum). V724 TauAmp. 0.3V. Amp. 0.1V. Hyadum IC, 11.8v at 49". Small amp., possible periods 0.96, 1.93, 8.5, 0.89d, with 8.5 slightly favored (Manfroid and Mathys 1985, A&AS, 59, 429). Optical. Astrometric binary unresolved by speckle interferometry. Amp. 0.01V, 7.29?hrs. V469 PerBinary. Delta Sct 5.56 - 5.59V, 0.054d. V483 TauADS 3146B, 10.5 - >12V. Delta Sct 5.20 - 5.26V, 0.036d or double. V696 TauBinary. Combined mag., colors. Amp. 0.015y, 2.833d. TT RetSecondary F7V, vsini 90k/s. BY, amp. 0.12V, 154d. EK EriVaries several hundredths of a mag. on a time scale of days. EM EriCPM. Companion G0V. B, 13.0v at 36" optical. CPM. Component A suspected occultation double; component B, G2V, strong lithium. Amp. 0.1V. Hyadum IIAB 6.6 F1V, 6.9 F3V, 76.92y, a = 0.500". Combined mag., color. Component C, 12v at 37" optical; D, 8.25V, +0.57(B-V), +0.04(U-B), G0 at 45" CPM. Amp. 0.13V. AB CPM. B is A0. Component A suspected occultation double. ADS 3188B, 9.6 - 11.3v. 5.8 A3V, 5.9 A4V, 51.6y, a = 0.18", or 55.40y, a = 0.20". Optical. Delta Sct? Amp. 0.12V. Kappa1 Tau is occultation double. Together with Kappa2 = HR 1388 they form a multiple system of at least 6 components. Delta Sct? See HR 1387. Delta Sct, 5.26 - 5.29V. AB binary; C, 11v at 77" CPM. A blue straggler. Amp. 0.02U, 57.25d. Also magnetic field period. V776 TauAP 7.2 dF5, 7.2, 13.15y, a = 0.133"; occultation binary. Component B, 12.4v at 126". Speckle interferometric sep. of AP 0.093" 1980.94; 0.094" 1983.93. The visual primary is SB, 4.6, 6.5v, sep. 0.020". Component B, 12.5v at 110". Visual primary is occultation double. Component B, 11.1 at 137". V777 TauAB optical? C, 11v at 4" from B. Primary is SB, 6.2, 7.0v, sep. 0.01". Visual secondary is 10.5v at 161", probably optical. Binary. Components G1V and G5V. AB binary; C, 11.32V at 121" optical. Fourth component 13.3v at 17" from C. Sep. 0.024". Ain6.8 A2, 7.0, 175.7y, a = 1.250". CPM with HR 1412. Not clear if there are one or two occultation companions: mag. diff 3.8v, sep. 0.082", another possible mag. diff 8v, sep. 0.2". CPM with HR 1411. Close occultation binary, 3.5, 5.8v, sep. 0.005". Delta Sct, amp. 0.03V (variable), 0.080d. Possibly also eclipsing. The2 TauAB binary. B, 6.94V, +0.16(B-V), -0.70(U-B), B1IV? vsini =<25k/s. Suspected of being double; probably single. 5.7 F0V, 7.98 G2V, 189.5y, a = 1.01" (alternates 180.0y, a = 1.00"; 170y, a = 1.029"). Combined mass 2.82 solar. Speckle interferometric sep. 1.300" (1980.94). Gamma Cas 5.41 - 5.49V. Expanding circumstellar shell; possibly high velocity mass loss. Equivalent width of H alpha variable. DU EriCPM. Component A of visual pair is occultation double 5.6, 5.6v, sep. 0.02"; component B, 6.7v at 250". Delta Sct? SX Ari 5.73 - 5.82y, 1.374d. Var. helium lines. DZ EriBinary. No change after 113y. CPM. Alpha CV, amp. 0.035V, 0.065U, 3.80d. EH EriLb? 5.10 - 5.13V, amp. 0.20p. DV EriA* 4.27 G8II+B, 28.67y, a = 0.054"(not confirmed). Visual duplicity questioned. Unresolved by speckle interferometry 1983.93. Known as the "red eye of the Bull'" Aldebaran is a red giant star, 40 times Larger than our Sun. It is approximately 68 [G/light year]s distant and ranks as the 13th brightest star in the sky. AB binary. B is 13.5v, dM2 at 31". CD, 122" from A is 11.2, 13.6v sep. 2" also binary but independent of AB. Lb 0.75 - 0.95V. Var. H and K emission. ALDEBARANCPM. Companion 7.84V, +0.54(B-V), +0.04(U-B), F8V. vsini =<25k/s. ADS 3317A, E?, 4.23 - 4.30V. CPM. Companion A7V. Component C optical. Beta C 3.4 - 3.60p, 0.17790414d, changing. Probable interference periods 0.1779 and 0.1735d with beat period of 7.0256d. Possibly also E, 103.9d. Theemim3.8 A0IIIp, 4.3 B9IV, 13.00y, a = 0.212". Combined mag., colors. Companion 10v at 78" optical. Alpha CV 3.26 - 3.30V, amp. 0.10u, 2.943d. AB 5.8 F0V, 7.4 F9V, 26.25y, a = 0.18" or 26.797y, a = 0.157". ABxC 5.6, 7.3, 425.0y, a = 1.38". Component D, 13.2v at at 24" optical. Spectral classes component A, A9V; B, F8V; C, F8V. ADS 3359A, Cep?, 5.05 - 5.10V, 5d? 5.3 - 5.38V. Occultation indicated mag. diff 0.37v, sep. 2.117" (half the visual sep.) and PA 78d in contrast to visual 194d. EA 5.92 - 6.7V, 2.056302d, period possibly variable. HU TauIDS gives AB, 5.3, 11.8v sep. 30". Optical. Component C by Wallenquist. Binary with HR 1479 at 431" and with fainter SB companion, 7.4v at 0.0015". Binary with HR 1478. Sceptrum280.0y, e 0.56, a 0.45", i 51.9d, mag. diff 0.0. AB, CPM. Third component by Wallenquist, mag. diff 6.42, sep. 90". B is 11.9 at 34". Uncertain which of components B,C is the brighter: discordant magnitudes. Component A of triple, SRb 4.8 - 6.6v, about 338d. R DorSeen as double only in 1877 and 1923. SRb 4.28 - 4.36V, 30d. DM EriAB CPM, 4.3, 8.9v sep. 0.1", 28y? C, 7.3A1V at 63" vsini 100k/s, physical. D. W. Dunham gives 4.9, 5.6v sep. 0.1" and 4.9, 6.4 sep. 0.0005". CPM. Comp. A of double, Delta Sct? 7.2 G5V, 7.3 G6V, 552.30y, a = 3.164". Combined mag., colors. Both components also classified G3V. CPM with HR 1506. Alpha CV?, amp. 0.025V. DW EriDelta Sct? In Hyades instability strip. Gamma Cas 5.76 - 5.98V. Equivalent width of H alpha is variable. Amp. 0.09R, 0.05(R-I). DX EriVisual companion probably optical. Delta Sct? Amp. 0.05V. Delta Sct 5.09 - 5.11V, 0.042d. V480 TauCPM. SRb 4.65 - 4.88V, about 30d. Companion optical. CPM with HR 1564. B-V for combined light. CPM with HR 1563. Ell 3.66 - 3.73V, 3.700363d. Pi5 OriAB 4.5, 7.8, 284.0y, a = 0.78". C, 11v at 26" CPM, possibly physical. 4.0 - 4.15p. HassalehOptical group. Cst? 5.72V. R Eri136.0y, e 0.32, a 0.425", i 88d, mag. diff 1.0. Component A suspected occultation double. Two visual companions. Binary. CPM. 6.4 - 6.48V. AB probably optical. B, 8.0v B9; C, 9.8v at 54"; D, by Wallenquist, mag. diff 7.1 at 90". AB 5.94 F3V, 7.28 F9V, 54.62y, a = 0.507". Component C, 8v at 54", optical. ADS 3605A. A* 2.98 var. A8Iap. Five visual and one astrometric components. AB visual binary, B, 14v at 29"; C, 11.26V, +1.83(B-V), +1.31(U-B), at 43"; D, 12.0v at 46". ADS 3605A, EA 2.94 - 3.83V, 9892d. Spectrum var. even outside eclipse. RV and light fluctuations about 110d. Al AnzFixed with HR 1610. Fixed with HR 1609. Colors for combined light. RRc 4.77 - 4.80V, 0.273d. S EriEA 3.70 - 3.97V, 972.164d, i 90d. Variable duration of min. Amp. depends on wavelength, 0.55B, 1.97U. K component amp. 0.05V. HaediBC binary 7.7, 10.7v sep. 0.5"; AxBC binary, B = GC 6148 A1IV?, vsini 53:k/s; D, 9.5 at 130". Probable double, 5.4, 5.4v, sep. 0.4". Optical pair with HR 1623. Gamma Cas, amp. 0.07V, period a few hours? BV CamOptical pair with HR 1622; C, 10.8v at 173" from B; D, 13.3 at 16" from B. RS CVn amp. 0.14V, 82.8d. BM CamHR mag. 6.31 should have been 7.31. A,B,C, CPM; D, optical; E, 12.3v at 132" from A. Alpha CV, 4.65 - 4.69V, amp. 0.03y, 4.6398d. V1032 OriBeta C? Hoedus IIAlpha CV, amp. 0.10U, 0.06B, 0.05V, 0.7325d. BN CamSRb 8.2 - 12.4p, 212d. Mean mag. varies in period 2450d. W OriADS 3738B, amp. 1.8v? Delta Sct 6.28 - 6.39V, 0.1352227d. X Cae5.6 G4V, 5.6 G4V, 1.19y, a = 0.18"; or 2.38y, a = 0.10"; or 5.8y, a = 0.11". Combined mag., colors. Sep. 0.099". Unresolved by speckle interferometry 1983.93. E? 5.1 - 5.6v. About 2d. A is SB, 5.7, 7.7v sep. 0.0004". Visual companions 12.0 at 13", 8.6 at 35". Primary of visual pair is possible occultation double, 6.8, 6.8v, sep. 0.3"; secondary, 9.1v at 111.5" is BD +21d764. 6.73 - 6.82p. 5.78 Am, 6.62 Am, 198.9y, a = 1.04". Mean mass 1.7 solar. Combined mag., colors. CPM with ADS 3712 = GC6270, 9.8, 8 K2 sep. 3" at 348". CursaAB, CPM. BC 8.6 dG7, 9.1, 32.1y, a = 0.217". CPM with component A. ADS 3722B, K0III-IV, RV +72k/s. 2.87d not confirmed. Suspected visual double probably single: unresolved by speckle interferometry. Candidate for becoming a Be star. Beta C 4.22 - 4.34V, 0.701538d. Both spectroscopic and new photometric data suggest period 0.70177d. Small changes in mean brightness (<0.1mag). B, dF5, optical. C observed only once. Binary. Amp. 0.003V, 0.565d. V1085 OriSRb 5.0 - 7.4v, 60:d. RX LepSRb, amp. 0.12:V, 40d. WZ DorCPM companion G8Ve, strong lithium. AB fixed. B, 8.4v, F7V at 7"; C, 11.8 at 182". AB 6.9 A4V, 7.1 A6V, 312y, a = 0.383". Combined mag., colors. C, 13v at 7", may be physical. Alpha CV 2.97 - 3.41V, per. about 2d. CPM. Combined mag., colors. Companion B9V, optical? AC binary. B, 11v F4V at 13" optical. Delta Sct 4.94 - 5.10V, 0.088088d. Form of light curve varies. Also nonradial pulsations of 0.096533 and 0.088243d. KW AurCapella is a bright binary star system whose two stars, only 70 million miles (116 million km) apart, are too close together to be seen as individual points of light with a small telescope. This star system is approximately 45 [G/light year]s distant. AP 0.6 G5III, 1.1 G0III, sep. 0.04", 0.285y, a = 0.054", masses 2.67 and 2.55 solar. Combined mag., colors. Capella is first star for which an orbit was determined from interferometer measures, by Anderson at Mt. Wilson in 1920. Speckle sep. 0.040" 1981.24 and 1981.68; 0.055" 1982.16. CPM with component H, a close binary, 10.0 dM1, 13.7 dM5 sep. 2" at 723" from A, probably physical with A. Other components all faint and distant from A. Amp. 0.03V. Variable helium and X-ray emission. CAPELLAComponent B doubtful, possibly the nebula. C 10.7V at 30". ADS 3843A, Ina 5.78 - 6.08V. Possibly a SN 2.5 million yrs. ago. AE AurThe bright blue giant star, Rigel, represents one of [X/Orion]'s feet. It is an extremely hot star, with a surface temperature over 7,000 degrees hotter than that of our [G/Sun]. As a result, it is over 57,000 times more [G/luminous] than our star. AxBC, CPM. BC binary, 7.6 B8II, 7.6v sep. 0.12". D, 15.4v at 44". BC also classified B5V+B5V. For B, vsini =<39k/s. 0.03 - 0.30V, 25d. Amp. at 0.58 micrometers about 0.06m. RIGELLb?, amp. 0.10V. PU AurCPM. ADS 3872A, E? Possible CPM with HR 1732. EA 6.15 - 6.82V, 6.05 - 6.72B, A0 + A0, 4.134695d, changing period. AR AurB, 13.4v at 29". C, 12.1v at 42" and D, optical. Possible CPM with HR 1728. Alpha CV 5.35 - 5.41V, 2.4660d. Spectrum var. same period. IQ AurFixed. Companion spectral class A. CPM. Companion 9.64V, +0.76(B-V), +0.19(U-B), G1IV-V. Component B optical. Fixed with HR 1754. Fixed with HR 1753. Alpha CV, amp. 0.04V, 2.28704d. Magnetic star. TX LepCPM. Component B optical. Fixed. Secondary 7.17V, -0.12(B-V), -0.63(U-B), B5Vn, B8nnp or B3V, RV -58k/s, vsini 350k/s, optical. AB binary; C, 9.2v K0 at 61" optical. Amp. 0.13:V. AB fixed. Companion A5IV, vsini 124k/s. CPM. Companion F6V. Companion optical. BC 7.8 F8V, 7.9 F8V, 48.0y, a = 0.34". AxBC physical. ADS 4002A is SB triple system, abc with periods 9.2y and 7.989d. Speckle interferometry gives 9.219y, a = 0.036" for for ab x c. Visual components AB, binary, 3.8, 4.8v, sep. 1.650"; C, 9.4v at 115". The total mass of the quintuple system exceeds 50 solar masses, the most massive component being about 17 solar masses. EA + Beta C 3.31 - 3.60V, 3.14 - 3.35B, 7.989268d. Also sinusoidal pulsation period, amp. 0.05V, 0.30197 or 0.30145d. Gamma Cas?, 4.92 - 4.96V, 14.50d? Amp. 0.07R, 0.06(R-I). BELLATRIXALNATHLb? 5.71 - 6.05V. SW Col359.1y, e 0.19, a 0.28", i 50.9d, mag. diff 0.3. ADS 4038A is occultation double. B and C are 10.1v at 305" and 11.8v at 343". ADS 4048A is occultation double, equal magnitudes, discovered during occultation of Feb. 26, 1901 by Innes. The three visual companions: B, 12.39V at 38"; C, 11.55V at 59"; and D, 11.6 at 74" may all be CPM with A; however, B and C may possibly be optical. AB about 6300y. B, 10.3V, vsini 96k/s. C, 12.3v at 83", optical. Ell 4.55 - 4.61V, 4.31 - 4.34B, 2.52596d. Companion F5. AB, 6.9, 7.2v sep. 0.2" binary. C, 6.8v A0. Combined mag. and colors of AB. AB binary, B is A0V; colors for combined light. C, 11.5v at 141". Companion 7.62V, +0.94(B-V), +0.69(U-B), G8III. AB binary; C, 12.0v at 64"; D, 10.5 at 206"; E, 10.5 at 241". ADS 4066B, 7.0 - 11.0v. NIHALCPM. Companion 9.70V, +0.71(B-V), +0.15(U-B), F7V. ADS 4097, cst? 4.67: -4.71V. CI OriSR? 5.9 - 7.1v, 120?d. CK Ori4.49 B5IV, 5.82 B7V, 586y, a = 1.293". Combined mag. and colors. AB fixed. Combined mag., colors. SRc 6.1 - 6.5p, 165d. CE TauCompanion is B7IV, vsini 291k/s, optical. Binary with C = HR 1851. Component B, 14.0v at 33". ADS 4134A, EA 2.14 - 2.26V, 1.94 - 2.13B, 5.732476d. Intrinsic variability also possible. MINTAKAThabitCPM. Gamma Cas, 5.53 - 5.69V. V960 TauCPM. Amp. 0.10y. All components CPM? CD binary, 8.9v A0V, 9.7v sep. 0.8" at 30" from A, physical. ARNEBEA 5.31 - 5.66V, 5.14 - 5.51p, B1V + B7V, 1.4853784d, i 80.9d. A third component has orbital period 119.09d. VV OriSuspected visual double probably single. Unresolved by speckle interferometry. Companion has K-type spectrum. See HR 1879. CPM. Fixed with HR 1887. Fixed with HR 1886. E:+SX Ari 6.54 - 6.58V, 0.94629d superimposed on SX Ari type, 0.9015d. V1046 OriBinary. COPERNICUS spectra and IR photometry yielded no evidence on the companion. ADS 4186AC fixed at 13". C = HR 1895. ADS 4186 and 4188 together appear to form one complex multiple system whose brightest components are ADS 4186C = HR 1895 and ADS 4188A = HR 1897. These two components are double star STF 17 which IDS lists as part of ADS 4188. Thus, the 9 components of ADS 4186 and the 4 of ADS 4188 form one system of at least 12 components. Those of ADS 4186 range from mag. 5.4 to 16.7v, all within 22" of A. ADS 4188 has two other companions in addition to HR 1895: B, 6.5v at 53" and C, 7.6v at 129" from HR 1897. ADS 4186A, EA, 6.72 - 6.75V, 65.43233d. Component E is NSV 2291, amp. 0.41V; component F is NSV 2296, 11.0V; component H is NSV 2292, 15.6V. See HR 1893. Fixed with HR 1896 at 13". No clear evidence for being X-ray source. Temp. 32000d excites nebulosity to 10600d. 5.10 - 5.16V. He II 4686 suggests var. density of infalling material on time scale of days. See HR 1893, 1895. 6.65 - 6.72V. ADS 4188AB fixed at 52". B is 6.38V, -0.05(B-V), -0.93(U-B), B0.5V; vsini 17k/s. See HR 1893. May be X-ray source 3U0527-05. 5.05 - 5.19V. Component B is NSV 2326, 6.38 - 6.44V. CPM. AB fixed. B is B7IV; vsini 50k/s. Component B is NSV 2334, 7.4V. Nair al SaifAB binary, both components B8IV. Combined magnitude and colors. Alpha Cyg 1.64 - 1.74V. ALNILAMGamma Cas 2.90 - 3.03V. Var. shell Sp. Widths H-lines vary in about 10 min. Polarization at H beta changes in tens of minutes, probably due to circumstellar matter. CPM. Combined mag., colors. BC, 10.0, 12.2v, sep. 11.3" at 55" from A, optical. AB 6.0 G5III, 6.3 A2V, 53.2y, a = 0.135". Combined, mag., colors. C, 8.57V, +0.28(B-V), +0.09(U-B), F0V at 12", physical; D, 11.5v at 33". Resolved by speckle interferometry 1983.93, sep. 0.12". Suspected occultation double. CDelta 3.46 - 4.08V, 9.84200d. Period varies. Component B, 9.9v M1 at 99", is BD +53d935, CPM. Component D is F5. Other companions 12.4 and 12.8v. TX PicTriple system: SB and third component 8.5v at 0.32". AB 4.1 O9.5V, 5.1 B0.5V, 170y, a = 0.247". Combined mag. and colors. C, 8.79V, A2V at 11" may be physical; D, 6.62V, -0.20(B-V), B2V, at 13" and E = HR 1932, at 42" CPM with A. A multiple system similar to trapezium. ADS 4241 possibly the most massive visual binary known, 35 solar masses. Gamma Cas 4.40 - 4.59V. Var. hydrogen emission. Lc 6.13 - 6.30V. NO AurExcept B all companions at distances 41" to 129" from A, and 5 of them mag. 8 to 10v. CPM, B is 7.18V, -0.04(B-V), -0.14(U-B), B9.5V, vsini 120k/s. 5.3 B3IV, 5.9 B3V, 95.36y, a = 0.357". Equal components. Combined mag., colors. ADS 4265B, Beta C? 6.2 - 7.0v. See HR 1948. In line of sight of high-velocity interstellar cloud. E?, 4.91 - 4.95V. Gamma Cas?, 2.62 - 2.66V. H alpha variable. Rapid variations in H beta profile. PhaetAlpha CV, amp. 0.03V, 0.04U, 1.099d. V1051 OriCPM. Amp. about 0.04V. V731 TauLb?, amp. 0.15V, 0.08R. WX MenAB 6.5 F5V, 6.9 F6V, 20.10y, a = 0.201". V1197 OriSRa 10.1 - 12.2p, 240.9d. Mean mag. varies in period 1750d. Y TauBC, 9.5, 13.0v, sep. 1.3" at 17" from A, optical. CPM with HR 1982. Delta Sct? CPM. Companion 8.97V, +0.55(B-V), +0.08(U-B), G0IV. Optical. Ell 6.00 - 6.05V, 5.288d. Additional irregular variability. Third component mag. diff 6.29V, 80" from A. Component B optical. Speculation that star may have been a SN 2.5 million yrs. ago. AB binary. C, 7.2v A0 at 75", CPM. Binary. Companion F0. EA 6.02 - 6.43V, 6.1 - 6.5p. 3.4057d. Redder at min. V1031 OriSAIPHAmp. 0.1V. Cycles 35-36d in 1970-1 not confirmed in other seasons. Companion optical. Third component, visual, 11.6v at 15". Reality of the occultation binary, sep. 0.01", has been questioned. High space velocity. Amp. 0.10V. CPM. Combined mag., color. Amp. 0.082. EB 5.12 - 5.29V, 2.933241d. TU CamHigh space velocity. Amp. 0.05U, 2.63?d. Possible new periods of 2.654 and 1.5889d, of which the smaller preferred. V809 TauWeznPossibly triple system. Magnitudes of separate components unknown. A*, 14.25y, a = 0.095". Probably low-mass companion. Optical. Beta C?, amp. <0.02V. AB optical. C, 12v at 45". Ell? 4.85 - 4.92V, 0.03b, 0.640d. EA 6.19 - 6.87V, 8.56898d. Sp. at min., B9V. TZ MenThis huge star, possibly the largest known today, is a irregularly pulsating red supergiant. Its size changes from 550 to 920 times the diameter of our [G/Sun] over the course of 5 1/2 years. At its largest, this star would completely fill our inner solar system and its surface would be extremely close to Jupiter! Betelguese is 650 [G/light year]s distant. Components B-E all 11 to 14.5v at sep. 40" to 174" from A. D 13.5 at 77", optical. Speckle interferometric observations in 1983 November (Karovska et al. 1986, ApJ, 308, 360) show A to be a triple system with closer companion at 0.06" (mag. diff. 3.4 at H alpha) and more distant companion at 0.51" (mag. diff. 4.6 at H alpha). Radio star. Circumstellar shell of gas and dust. The gas shell detached from photosphere at about 5 stellar radii. Diam of optically thin dust shell possibly 1".5. Surrounded by reflection nebula. Gas shell up to 100 R, dust shell from 12 to 250 R. Highly limb darkened. ADS 4506A, SRc 0.40 - 1.3V, 2335d. Also superimposed waves 200-400d. BETELGEUSEAll companions optical. AB binary. C, 14.1v at 13". ADS 4556A, EA 1.89 - 1.98V, 1.93 - 2.02B, A2+A2, 3.9600421d, i 78.5d. MenkalinanRadio star. Lc 4.24 - 4.34V. Radio emission at 2.85cm indicates mass loss. AB binary , combined mag., colors. B is 7.2v G2V. C, 11v at 49" optical. ADS 4566B. Alpha CV 2.62 - 2.70V. Amp. 0.43m at 1400A, 1.3735d. Magnetic field varies 3.618d. AB probably binary. B, 11v at 2". Component C, K0III, optical. 126.0y, e 0.56, a 0.265", i 75.4d, mag. diff 1.4. Delta Sct 5.88 - 5.92V, 0.0611d. V1004 OriDelta Sct 5.93 - 6.36V, amp. 0.38 B, 0.13372, 0.13612 and 0.08261d; amp. var. in 7.7455d. Multiple periods. V474 MonOptical. C, 13.0v at 20" from B. Amp. 0.15p, may be spurious due to companion. Suspected occultation double. BC, 9.0, 10.0v, sep. 0.6", CPM with A. Delta Sct? AB 4.4 A2V, 6.0 F3V, 17.5d, a = 0.276"; ABxP, 18.25y, a = 0.089". Magnitude and colors for combined light. A is alpha CVn var., SB1, 4.45d; B is SB2, 4.78d. Component C, 14v at 18" probably optical. ADS 4617A, Alpha CV 4.10 - 4.18V. Binary. Triple system, SB, sep. 0.0014". Third component found by occulation, 6.5v at 0.060". AB 4.7 G6III, 5.1 G8III, 13.17y, a = 0.19". Combined mag., colors. Component A is SB, 4.9, 6.9v, sep. 0.0013". Speckle interferometric sep. 0.128" 1982.17, 0.086" 1983.93. Component C, 13.0v at 101". PropusOccultation binary, sep. 0.02". H alpha profile var. Confusion as to whether B or C is the brighter, B at 18", C at 84" from A. C is 15v at 21". 5.20 - 5.23V, 80.85d, periodic shell phenomena. Suspected of 0.01m variability. CPM. Companion 10.72V, +0.90(B-V), +0.25(U-B), F7V. Z And 4.82 - 5.06V. H-line var. M-type component irreg. amp. 0.07y. Shell Sp. varies like R CrB. SS LepSep. 0.097". Runaway star from Sco OB1 from which it appears to have been ejected 14 million yrs ago at velocity 150 km/sec. Lb? 6.39 - 6.51V. SW PicSRb 6.0 - 7.58v, 7.1 - 8.9p, 89d, superimposed on oscillations of 875 to 890d. Amp. 0.55V, 0.08(B-V), 0.16(U-B). S LepCPM with HR 2158. Binary 5.9, 9.4v sep. 5", CPM with HR 2157. 7.2 G5, 7.4, 463.5y, a = 2.94". Amp. 0.10V. Component A is itself double, showing variable radial velocity 12.10 to 33.22k/s, and vsini 7.99k/s. One of the three components may be a spotted star. Amp. 0.13V. AB binary, combined mag., colors. C 14.4v at 18". ADS 4751B, 7.0 - 10.0v. AB CPM. B is 6.94V, +0.04(B-V), -0.02(U-B), A0V, vsini 120k/s. Component C, 8.9v at 118". HD erroneously assigned the preceding number, HD 42092, to the fainter following component of ADS 4749. Consequently the data for the two primary components are sometimes interchanged. vsini for component A is 250k/s. ADS 4749A, spectrum variable. Sometimes shows shell features. Binary with HR 2175. Old disk population runaway star. Sep. 0.099". 6.4 F5V, 6.5 F5V, 18.2y, a = 0.203". IUE observations of uv continuum suggest an early-type companion, B9 or A1III-IV. SRc 8.7 - 9.5p, 182d. TV GemAlpha CV, amp. 0.04U, 1.36:d. V653 MonLc? 5.74 - 8.1V, possibly E, per. 32y. BU GemAlpha CV 6.16 - 6.18V, amp. 0.02y, 0.724d. V638 MonEB 4.65 - 4.90V, 1.672541d. Binary. Occultation indicates sep. 0.27". Lb? 4.93 - 5.04V. UW LynAB, 473.7y, a = 1.08". B is 8.8v at 1.4". A is suspected occultation double, 3.4, 5.4v, sep. 0.03". Masses A, 12.4; B, 5.5 solar. The three components are surrounded by a gaseous envelope. ADS 4841A, SRa + EA 3.15 - 3.9v, 232.9d. Deepest min. satisfy SB period 2984d. PropusAB CPM. B is dF0; C 12.3v at 202" optical. D, 11.5v at 120" from A. B and C optical. Aitken and Wallenquist disagree on magnitude difference: Aitken AB 6.0, AC 5.3, AD 4.8; Wallenquist 5.6, 7.6, 7.3, respectively. Separation 25", 76" and 86", respectively. Companion, RV -2k/s, optical. Old disk population runaway star. Suspected occultation double, 6.9, 6.9, sep. 0.1". 6.8 F5, 7.0, 28.1y, a = 0.165". 132.7y, e 0.52, a 0.24", i 55.7d, mag. diff 0.3. E: + Delta Sct: 4.43 - 4.73V. Line widths vary 0.3d. UZ LynAP 6.1 A2IV, 9.0y, a = 0.109". B and C both 8.4v at 63" and 117", both optical. D, 11v at 5" from C. AP resolved by speckle interferometry 1983.93, sep. 0.06". Aa resolved by speckle interferometry 1983.93, but unresolved 1983.94. AB binary. B, 13.0v at 2". C, optical? 13.28V, +0.56(B-V), +0.34(U-B). Optical. 5.4 - 5.47B. AB binary. C, 12.9v at 26". D, 11.0 at 100". AE magnitude difference 6.24V, sep. 70". Amp. 0.04U, 1.0785d. H and K lines vary. V1155 OriAmp. 0.03V. AB optical. B is F8. 6.8 A3V, 7.4 A6V, 120y, a = 0.448". ADS 4971, 6.3 - 6.37V, combined mag. Difference between components varies from 0.2 to 1.5V. Uncertain which component is var. Beta C? FurudAB CPM. C at 56", optical? Gamma Cas 5.46 - 5.64V. FR CMaCPM. Lb 2.76 - 3.02V. Tejat Posterior5.48 - 5.54V. Not var. in U. Lc? 4.75 - 5.70V, 6.6 - 7.2p. Possibly faint visual companion at 50". EA 5.64 - 6.03V, 9.945070d, i 87.8d. Close third body or circumstellar matter needed to account for the light curve, but no spectroscopic evidence available. RR LynB, 10v at 31" optical; C, G8III probably optical. D, 12v at 80". Beta C 1.93 - 2.00V. Prototype star. Multi-periodic: 0.25002246, 0.2513003, 49.17 and 0.23904d, others reported. Beat periods 49.198, 5.442 and 4.900d. Sp. also var. over 0.25d. MurzimBinary with HR 2299. Combined light 4.30V, +0.21(B-V). Component C, 12.2v at 93". See HR 2298. Speckle interferometric double, 6.5, 6.9v, sep. 0.055". ADS 5023B, 7.5 - 9.0v. Lb 8.5 - 9.7p. BL OriCPM companion F0V; however, the companion is optical. IUE observations suggest an early-type companion, about A0. CDelta 5.58 - 6.62V, 27.0205d since 1933. Period has increased from 27.0093 before 1900, with mean value 27.024649d. T MonCanopus is the second brightest star in the sky. It is 116 [G/light year]s away, 30 times the diameter of our [G/Sun] and 1,400 times more [G/luminous]. CANOPUSFixed sep. CDelta 5.02 - 5.82V. Per. changing, 3.728365 before 1950, 3.728115 since. CaII emission on rising branch of light curve. Blue companion suspected. RT AurSep. 0.003". AA' probably combined light and color. This may be the SB pair, 4.3, 6.0v, sep. 0.2". B, 8.5V A1V at 113", vsini 141k/s, is binary with C, 8.9v, sep. 0.2". Component P, 15.1V at 24" optical. Other components faint at 54" to 92". See HR 2356. Amp. 0.055b. AB binary. B is K0V. Component C, 11.4v at 45" optical. Double emission lines of which red component variable intensity. Component B, 9.09V, -0.05(B-V), -0.30(U-B), B9IVe, RV +6k/s, vsini 201k/s. EA 5.79 - 6.54V, 2.52501922d. Per. changes. Rot. line apsides per. about 40,000d. WW AurCompanion F5V, optical. Optical. Quadruple system, AB 6.1 G5, 6.2, 52.9y, a = 0.484". CoD = -50d2440, 9.7, 9.8v sep. 0.5" at 12" from AB, 105.6y, a = 0.535". AB, CD are CPM. R-I also found at -0.02. Beta C 4.33 - 4.36V, 0.2095755d, secondary variations. Effective temperature varies by 1400K and ratio of max. to min. radius by 1.042. Lb? 6.28 - 6.41V. SX ColCompanion 8.70V, -0.08(B-V), -0.40(U-B), A0V, optical? Beta C, 5.64 - 5.72V. Fixed sep. SRb 7.83 - 10.00B, 8.2 - 10.0p, 234d. Mean mag. varies in per. about 3500d. UU AurH alpha emission var. A* 1.93 A0IV, 12.9y, a = 0.038". ALHENAProbably star of largest known mass for primary and secondary components, each about 50 solar masses. 6.04 - 6.08V, irregular variations, possibly transition from O- to WR-type spectrum. Polarization variable. Plaskett's starCPM. Companion 7.65V, +0.32(B-V), +0.02(U-B), F2V. AB binary. C, 11.5v at 21". Discovered by both occultation and speckle interferometry 1978, sep. 0.075"; 1983.93, sep. 0.13". 6.9 G0V, 7.3 G1V, 29.0y, a = 0.295". Combined mag., color. Companion A2V. Beta C? 6.2 - 6.25V, 7.5 hrs., possibly longest period Beta C type. Beta C?, 3.16 - 3.20V. AB binary, 4.8 Oe5, 7.6 B7; C, 9.9v B8V at 17", physical, vsini 141k/s; D, 9.7v A6III at 41", physical, vsini 115k/s; E1 the brighter component of E, B5V at 74", probably optical, vsini 253k/s; E2, A0V, vsini 132k/s. ADS 5322A, Ia? 4.62 - 4.67V. R-I also found at -0.11. S MonBinary. Companion A0. 5.58 - 5.62p. Some spectral lines appear double, indicating separation of about 110k/s and vsini of 90 and 75k/s. CPM. AB 5.37 A2n, 5.95 A2V, 699.0y, a = 1.660"; vsini of B 100k/s. C, 7.1v at 8", physical. Companion 9.22V, +1.13(B-V), +0.91(U-B), K0III-IV. MebsutaCompanion has A-type spectrum. Optical. CPM. Companion orange, optical. Delta Sct? AlzirrSee HR 2485. Color for combined light. Mag. for blended images 5.52V. Sirius, the brightest star in our night sky, is also one of the closest stars to us at only 8.7 [G/light year]s. It is 23 times more [G/luminous] than our [G/Sun] and almost twice its diameter. It has a small companion star that is believed to be a white dwarf. The companion is difficult to see because of its closeness to Sirius. AB -1.46 A1V, 8.49 A1V, 50.090y, a = 7.500" or 49.94y, a = 7.62". D, 14.0v at 32" from A. C, companion to B at 1.4" suspected but not confirmed. B is first white dwarf ever discovered; predicted by Bessel (1844) on basis of orbital motion of Sirius, it was first seen by Alvan Clark in 1862, and its peculiar high temperature, small size and great density established by W. Adams in 1925. Soft X-rays observed from Astronomical Netherlands Satellite (ANS). Sirius B not unusual compared with other dA white dwarfs. Effective temperature about 32000K. SIRIUSGamma Cas 5.13 - 5.44V. Also classified beta C, 5.10 - 5.26V. FT CMa6.81 A1V, 7.01 A2V, 1057.8y, a = 1.536". Combined mag., colors. Beta C, 5.48 - 5.76V. HP CMaAmp. 0.06V. Alpha CV 6.06 - 6.09V, 2.181d. HK CMaGamma Cas 6.15 - 6.27V. A 2-year (1977-78) minimum attributed to a dust cloud. V339 PupSRc 6.6 - 7.3p, about 47d. IS GemComponent B, 13.31V at 27.5", optical. SX Ari, amp. 0.10V. OV GemAB 5.7 G4III comp., 6.9 A2, 480y, a = 0.736". Combined mag. and color. C and D 6.3 and 6.2 pv fainter than AB. 7.1 - 7.28B. AB binary. Optical. CPM. Alpha CV 6.16 - 6.32V, 2.9760d. Magnetic field and rotation same period. Strontium var. V592 Mon7.01 - 7.06?V. Radial velocity possibly variable from +22 to +44k/s. Gamma Cas 3.78 - 3.97V, 3.7 - 3.85B. AB fixed. Space motion almost identical to that of the Sun. Delta Sct 5.94 - 6.14V, primary period 0.115442, secondary 0.154412d. OX AurAB binary. B discordantly classified B9V: or A6:, vsini 158k/s. H alpha variable. 6.52 - 6.57V. From orbit based on IUE data, the star should be eclipsing with period 195.24d. V415 CarDelta Sct 6.037 - 6.054y. About 4 hrs. One of most luminous Delta Sct stars: abs. mag. about 0.0V. V352 AurAB binary. C, 13v at 29" optical. D, 9.5 at 207". AB 4.8 A9Vp, 7.6 G6V, 1943.8y, a = 8.194". Combined mag., colors. ADS 5548A, Lb, amp. 0.22V. Emission var. about 16 yrs. Beta C 4.60 - 4.63B, 0.184557 and 0.19296d, beat per. about 2d. EY CMaLc 3.78 - 3.99V. E? 6.71 - 6.95V, 3.763d, possibly irregular. HeII 4686 var. about 13d; profiles var. in minutes. Suspected SN remnant. Companion is probably a neutron star. EZ CMaComponent B is 9.3v K5 at 44"; D, 9.5 at 130". CPM. Lb 6.25 - 6.37V. NP PupAB fixed. Old disk population runaway star. Beta C 4.36 - 4.40v, 0.08:d. Beta C 6.50 - 6.66V, 0.19d. HH CMa7.1, 7.1v, sep. 0.040". Resolved by speckle interferometry 1983.93, sep. 0.06"; unresolved 1984.93 and 1985.25. SR 5.00 - 5.07V, 6.54 - 6.64p. OV Cep6.9 F8IV-V, 7.1 F8IV-V, 16.74y, a = 0.218". Combined mag., colors. Fixed sep. ADARAAC, mag. diff 6.1v, sep. 32"; AD, mag. diff 6.1v, sep. 60"; AE, mag. diff 6.4v, sep. 50". Component B, M5III; component C, F6V, optical. Component X, K-type spectrum, optical. Gamma Cas 6.48 - 6.60V. Time scale 7d. FU CMaCep?, amp. 0.086V, 0.7282d. Sep. 0.020". Lb? 5.89 - 6.04V. NP GemOld disk population runaway star. AB binary. Lc 3.43 - 3.49V. Beta C 4.96 - 5.01V, 0.19120d, secondary 0.19740d, beat period 6.09d. V637 MonComponent A is suspected occultation double, 4.5, 4.5v, sep. 0.1". B, 10.5v at 87". C, +20d1686, 7.55V, +0.62(B-V), +0. +0.07(U-B), G1V at 96" has high proper motion, 0.100", optical, vsini =<54k/s. Other components fainter. ADS 5742A, CDelta 3.62 - 4.18V, 10.15073d. Period decreasing 3.1s/y. MekbudaAmp. 0.08V. H alpha profile changes in 30 min. or less. MuliphenAmp. 0.53:V. 5.16 - 5.32V. CPM with HR 2668 and third component, 9.2v K2 at 200". See HR 2667. Component B, 10.3v, F5III. ADS 5782A, Beta C 6.42 - 6.53V, 0.267d? or 0.18d. Other indications from 4 to 10.4 hrs. V569 MonAB binary A9V, F6V. CPM with C, 10.0v at 37". Component C, 9v at 18" probably optical. Beta C 5.36 - 5.39V, 0.12377d? FN CMaAmp. 0.026y, 3.275d. V386 CarAB optical. This star and HR 938 form a pair with opposite motion. See HR 938. Amp. 0.04b? Gamma Cas 5.64 - 5.92V. FV CMaAmp. 0.02V, 0.04U. Var. H alpha emission. WezenPossibly the center of SN explosion 0.8 million years ago. AB CPM. 4.3 - 4.36V. Component B, 11.3v, F3V. Beta C? Lb? 5.47 - 5.55V. V-R varies by 0.08m. UY LynAmp. 0.04b? Delta Sct 5.43 - 5.50V, 0.0999081 and 0.07500d, var. amp., beat per. 0.30083d. Sp. var. V571 MonAB 7.18 F8V, 7.23 F8V, 116.50y, a = 0.929". Combined mag., colors. C, 12.5v at 16" optical. Delta Sct? Difference between components B-A varies. SRb 6.63 - 7.01B, about 50d. BQ GemAmp. 0.037V, 2.68d or double. May be SB with double period. Delta Sct type. HN CMaOptical. The fainter component of the double is the variable suspect, 7.5v. Magnetic field var. 36.5d. Companion 9.07V, +0.77(B-V), +0.35(U-B), G1III or G5III, RV -3k/s, optical? Beta C, amp. 0.04V, 0.112d (variability questioned). GY CMaBinary with HR 2736. Combined light with HR 2736 varies, but 2736 is probably the variable. Binary with HR 2735. Combined mag. and colors, 3.63V, +0.91(B-V), +0.60(U-B), +0.48(R-I). 3.56 - 3.62V, blend with 2735. Amp. about 0.07u, 0.04v, 0.02b, 0.04y; 0.936d. QW PupBeta C 6.56 - 6.61V. GG CMaSR 4.80 - 4.96V, 6.40 - 6.70p, 23.7d. VZ Cam31?y. Sep. 0.098". Gamma Cas 4.42 - 4.82V. EW CMaAmp. about 0.04u, 0.01v,b,y. Combining their data with previous observations, Heck et al. (1987, A&AS, 70, 33) derive 0.91889d. OU PupAmp. 0.05V. Primary of vis. double, SRb 2.6 - 6.2v, 140.42d. L2 PupGamma Cas 3.60 - 4.18V, cycles 20 - 22 hrs. Also amp. 0.06V on time scale of 5d reported. Hydrogen emission varies with period 1.3667d (possibly a rotation period). Amp. 0.04y, 1.93d. PR PupCompanion optical. ADS 5961A is dubious occultation double, 4.0, 5.0v, sep. 0.045". B, 10.7v at 10" is CPM. Delta Sct? B, 6.01V, +0.49(B-V), dF0, optical. CPM. Old disk population runaway star. AB 3.55 F0IV, 8.18 K3V, 1200y, a = 6.975". Component A is SB, 3.7, 5.7v, sep. 0.2". WasatEB 4.84 - 5.33V, 4.5 - 4.8p, amp. 0.45V, 4.393407d. Sp. lines vary within about 1 hr. Variable polarization. UW CMaB, 10v at 8" fixed. D, 8.22V, -0.19(B-V), -0.93(U-B), B2V at 85". 3.90 - 3.96p. Possibly same period as SB. Binary with HR 2784. Component C, 10.9v at 74". Binary with HR 2783. Component D, 8.9v A0V at 215". Amp. 0.18V. NV PupEA 5.70 - 6.34V, 1.13593876d. Per. changes, possibly sinusoidally. i 77d. R CMaBeta C amp. 0.02V. 3-hour period not confirmed. Ell, amp. 0.045V, 1d. NW PupAB CPM. C, 12.7v at 42" optical. B optical. Old disk population runaway star. Amp. 0.035b. EA, 6.01 - 6.27V, amp. 0.14b, 24.6d. HQ CMaSuspected occultation double. Delta Sct? 5.80 - 5.84V. Binary with HR 2813. Gamma Cas 6.0 - 6.44V. Probably short period. Hydrogen emission also var. However, light variability questioned. OT GemPropusGamma Cas 5.00 - 5.50V. Emission lines vary in period of about one month or less. FW CMaCompanion is A0V, optical, vsini =<54k/s. AludraCompanion F5V, optical. Red giant of about 9 solar masses. Comp. A of double. Amp. 0.1V. See HR 2842. AB binary: B, 10.1v sep. 1"; C CPM. Gamma Cas 2.84 - 2.92V. GomeisaA is occultation triple, 5.9, 6.4v sep. 0.001" and 7.5v at 0.047". Visual companions B, 9.5v at 43" CPM; C, 10.5v at 146". Optical? CPM. B, 12.5v at 3" CPM. Gamma Cas 5.55 - 5.69V. FY CMaABC fixed. B, 8.1B; C, 8.6 B8V or B9p Hg Mn: at 20". Mag., color for combined light. AB 6.4 F4V, 7.5, 1090.9y, a = 3.684". C, 11.5v M0 at 21" orbital period around AB probably over 10000y. Component D, 12v at 42" optical? CPM. Companion G5V. CPM. Companion F8V. CPM? Suspected occultation double, 5.4, 7.0v, sep. 0.15". Resolved by speckle interferometry 1983.94, sep. 0.18". Ell amp. 0.051u, 0.03v, b, y. 0.6711d. Sp. period revolution about 1.4d. PS PupBinary with HR 2891. Combined colors. CASTORAB binary. Resolved by speckle interferometry 1983.94, sep. 0.24". Rapidly evolving shell. VV Cep type or symbiotic, 4.88 - 5.17V. Var. shell spectrum. KQ PupDelta Sct? 6.5 - 6.55V. Binary with HR 2910. Colors for combined light. Magnitude of blended images 5.09V. 5.5 - 5.60B. Also amp. 0.025 on time scale of 2d reported. OW PupAB fixed; B, 12.2v at 5". C, 9.71V, +0.03(B-V), -0.23(U-B), B9.5V, optical? Amp. at 0.58 micrometers about 0.10m. Companions optical. C is G type, strong lithium. AB, CPM. B, 13.2v at 26". Comp. A of multiple. Delta Sct?, amp. 0.01V, 1.5hr. Amp. 0.01B, 0.16121d. PT PupAmp. 0.02V. Triple system, components all about same mag. and within about 1". Occultation binary, sep. 0.03". Procyon is the 5th brightest star in the sky and also one of the closest. It is only 11.3 [G/light year]s away. It is twice the diameter of our [G/Sun] and 6 times more [G/luminous]. AB .35 F5IV-V, 10.3, 40.65y, a = 4.548". Binary nature first revealed in 1840 by variable proper motion; companion first seen in 1896. Component C, 11.7v at 122" optical. Delta Sct? A 0.09:d period originally attributed to the star beta CMi (HR 2845) may instead apply to Procyon, which had been used as a comparison star. PROCYONUnresolved by speckle interferometry. EW amp. 0.06V, 2.57895d. m PupBinary with HR 2949 at 10". C, 13.8v at 6" optical. Colors for combined light AB. Combined mag. 3.82V. MarkabCDelta 5.54 - 5.76V, 5.6952d. MY PupOptical. SR 5.52 - 5.72V. NZ GemAmp. >0.004y, 0.030u, 1.040d. V390 CarRS 4.13 - 4.29V, 19.423d. SRd? 6.56 - 6.64V, over 27d. Discovered by Gould 1879, variability questioned. Now confirmed by PEP observations, amp. 0.19U, larger in V. R PupAlpha CV 6.43 - 6.48V, 4.285d. Magnetic field same period. BC CamBinary with HR 2980. Colors for combined light. Blended mag. 6.34V. Delta Sct 6.43 - 6.50V, 0.09526d. AZ CMiPollux represents the head of the southern twin in [X/Gemini]. It is a yellowish star, approximately 35 [G/light year]s distant. It is a little over 4 times the diameter of our [G/Sun] and 35 times more [G/luminous]. All the visual companions optical. NSV 3712 is component A, 1.10 - 1.17V, while component E is NSV 3716, 10.5v. POLLUXVar. in red and IR. Amp. 0.24R, 0.20(R-I). D. W. Dunham gives 5.8, 5.8v, sep. 0.1". Amp. 0.07b? Binary with HR 3010. E, amp. 0.41y, 1.660d. Equal components. PV PupBinary with HR 3009. C optical. Some disagreement as to which of B and C is the brighter. H alpha emission var. Amp. 0.03b. Amp. 0.2V. QY PupAmp. 0.18V. Binary. Companion dG3. 2.41d, 0.06V. OX PupSR? Amp. about 0.02V. R-I also found at +0.06 and +0.07. Cst 6.14V. T PupAzmidiskeAmp. 0.5p. Binary, 211.8y, e 0.17, a 0.265", i 59.1d, mag. diff 0.2. Companion B9V, RV -72k/s, optical. Beta C, amp. 0.015u, 0.1182d. QS PupSRb 6.14 - 6.42V, about 35d. BC CMi5.6 F9V, 6.2 G4V, 23.18y, a = 0.58". Combined mag., colors. Masses 0.86 and 0.99 solar. Optical. 6.4 F2, 6.7, 30.8y, a = 0.295". BetaC, Amp. 0.03b, 0.040u with large modulation. Primary period 0.1927d with secondary 0.1680 or 0.2019d. QU PupBinary. Beta C or Ell?, 4.47 - 4.54V, amp. 0.07y. QZ PupBeta C Amp. 0.027V, primary period 0.1160d with secondary either 0.1168 or 0.1323d. V372 CarLocated just inside 3U0750-49 error-box. HeI 4026 varies, 1.3295d. 7.0 F5V, 7.1 F7V, 57.04y, a = 0.44". Combined mag., colors. Amp. 0.42V. PX Pup6.4 - 6.58V. Occultation double. Alpha CV 5.95 - 6.08V, 8.0278d. 1.14d also possible. Length of period varies in cycles 1.8 yrs. Magnetic and spectrum variable 8.0269d; also rotation period. AX CamAmp. 0.03b? Soft X-ray source. Beta C, amp. 0.015V, 0.101d. RS CVn?, amp. 0.06V, 10.163d. AE LynL 6.2 - 7.10V. IR observations of red giant in reflection nebula suggest star is losing mass and becoming a planetary nebula. Circumstellar reflection nebula probably related to a hotter companion. V341 CarComp. A of visual double, EB 4.74 - 5.25p, 1.4544877d, contact binary, equal components. V PupGamma Cas?, 6.48 - 6.63V. Amp. at 0.58 micrometers about 0.10m. FK Com, amp. 0.020V, 0.025B, 0.030U, 0.207878d. V645 MonCPM with HR 3143. CPM with HR 3142. Amp. 0.03B pulsating. Gamma Cas 5.72 - 5.84V, period a few days. H alpha variable. V374 CarAmp. 0.04v, 6.82d. PY PupAmp. 0.07(U-B). Companion B9IIIp. Amp. 0.15V. Fixed sep. Companion 8.77V, +1.30(B-V), +0.07(U-B), M6III, optical. May be Mira-type variable. Amp. >0.022, 2.008d. V336 PupBinary. Combined light and colors. With HR 3207, appears capable of producing most of the observed ionization of Gum Neb. Change in H alpha emission profile between 1974 and 1976 interpreted as change in rate of mass loss. NaosLb 5.97 - 6.04V. Lc? 5.2 - 5.44V. MZ PupB is A0. BC double 8.6, 13.0 sep. 1". Component B, 8.66V, -0.09(B-V), -0.52(U-B), B9IV. Companion not confirmed. Delta Sct 2.68 - 2.78v, 0.14088143d. Companion K0. Beta C, amp. 0.04V, 0.264 or 0.359d? V375 Car6.70 - 6.80p. B, 10.1v G8II at 33" optical. C is K2III. Psi2 Fl 14 CncCompanion A5III, optical. Old disk population runaway star. PQ PupOld disk population runaway star. Components B6V and B9V. See HR 3206. Mag. and colors blended with other companions. C = CoD -46d3848, 7.65V, B6V at 63", physical. D, 9.07V, Am at 94", SB, over 7d?, optical. Low degree of polarization indicates symmetric shell. The brightest O-type star and one of only four WR stars bright enough to have been observed spectroscopically in UV by COPERNICUS. With 3165, appears capable of producing most of the observed ionization of Gum Neb. The brightest and presumably the nearest Wolf-Rayet binary. Radio emission interpreted as coming from circumstellar gas cloud extending farther than the orbital radius of the binary. 1.6 - 1.8V, 154 sec. Sp. var. in about 200 sec. Variability too great to be explained by the 78.5d SB companion. Possibly a third close companion: a collapsed star of less than 2 solar masses. Suhail al MuhlifCombined mag. and color for 3208-9-10, 4.67V, +0.53(B-V). AB 5.63 F7V, 6.02 F9V combined colors (AB), 59.7y, a = 0.884". Component C = HR 3210. TegmenBetaC, Amp. 0.018u, 0.108d. IS VelAlpha CV 5.53 - 5.65V, 4.116d. BM CncSuspected occultation double. Lc 4.4 - 4.5V. NS PupCep 5.50 - 5.86V, 4.22717d. Per. and form of light curve vary. AH VelB, 9.78V, +0.39(B-V), -0.02(U-B), F5IV. Gamma Cas 4.60 - 4.88V. H alpha variable. MX Pup4.60 - 4.71p. OS PupCompanion K5V, RV +7k/s, optical. Amp. 0.03b. E? Amp. 0.062. M 6.2 - 11.8v, 361.43d. R CncCPM. AltarfCPM, A2IV, F2V. Delta Sct 6.29 - 6.33V, 0.0755d. Some intervals of constant brightness. HQ HyaAlsciaukat7.1 A, 7.4, 435y, a = 0.654" or 241.4y, a = 0.569". Companion A2V, optical. AB, sep 0.100", unresolved by speckle interferometry. 7.9 - 8.03B. CPM with HR 3302. CPM with HR 3301. C, 8.5v at 38" from B, binary. E? 1.82 - 1.94V, 3.57 - 3.83p, 785:d. AviorSee HR 3310. Binary with HR 3313. B, K1III optical. SRb 5.41 - 5.75V, about 40d. BP CncDelta Sct? 5.58 - 5.61V, 54.71 min. LM HyaB is 15v at 7", CPM. C and D optical. 3.3 - 3.8V, 358d. Also 0.05d, amp. 0.02V. MuscidaBinary with HR 3328. EA 6.7 - 7.14v, 1.25686d. NO PupDelta Sct, amp. 0.025V, 2.3 hours. CX CncComponent B, CoD-51d3003, 10.2v, B8V, optical. Third component G3V may be physical. Uncertain if double or triple; 6.4, 6.9, sep. 0.25", other possible component 7.0v at 3". Occultation obs. uncertain. E amp. 0.3p, 4.56960d. Equal min. Redder at both minima. VV PyxAB 7.1 A5m, 7.2 late F, 53.0y, a = 0.321". C, 10.5v at 18" binary around AB. EA 6.37 - 6.61V, 2.49955d = SB period. Secondary eclipse amp. 0.06V; primary not yet observed. LO HyaAP 6.6, 6.6v binary. Combined mag. and colors. B, 9.7v at 25" optical. Companion 10.3v, F2V, optical? Delta Sct amp. 0.015V, 0.07:d. GU VelCPM. ADS 6872B, L 9.0 - >12v. H alpha emission var. Occultation pair 6.4, 6.4v, blended mag. and colors. Visual component 10v at 63". Suspected as double by Innes from observation of occultation of April 28, 1898 (references: Astron. Nachr. 150, 423, 1899; MNRAS, 61, 416, 1901; Cape Ann. 2, part 6, 1907). Theta Cnc B is NSV 4117, 11.5v at 58", 59d. AP, 6.4, 6.4v, sep. 0.176", combined mag., color. Components B, 7.7v at 4" binary with AP, C, 9.3v at 19". Components B2III and B2.5V. Equal components reported; however, duplicity not confirmed. Delta Sct? 5.6 - 5.67V. Lc? amp. 0.27B. AB 6.9 A7, 7.0, 136.5y, a = 0.568". Combined mag. and color. VX PyxSKYLAB indicates cool star with hot companion. Old disk population runaway star. 5.8 - 5.89B. MuscidaCPM with HR 3396. See HR 3395. 7.2 G5IV-V, 7.2 G5IV-V, 13.9y, a = 0.160". Combined mag., colors. Alpha CV 5.66 - 5.76V, 5.57d or 11.305d, double wave. Rotation, same period. Spectrum var. Magnetic field 4.606d. HV HyaComponents M1IIIa and G7IIIb. Amp. 0.09V. MuscidaAmp. 0.025y, 2.67d. Spectrum var. same period. HV VelAl Minliar al ShComponents B, 6.60V, +0.01(B-V), +0.03(U-B), A0III at 150", vsini =<40k/s; P, 9.22V, +0.39(B-V), +0.01(U-B) at 134"; and Q, 8.81V, +0.32(B-V), +0.09(U-B), F2V, at 135", vsini 86k/s, form a physical system with A. B is 40 Cnc; Q is +20d2161. ACD a physical group: C, 7.70V, +0.20(B-V), +0.16(U-B), Am, vsini <45k/s. D, 9.39V, +0.41(B-V), +0.03(U-B), F5V at 83". B, 10.37V, +0.59(B-V), +0.11(U-B), G0IV-V at 21", CPM. AB 5.3 G3V, 6.7 K0V, 145.0y, a = 1.700" or 140.0y, a = 1.8884". Combined mag., colors. Amp. 0.05v, 1.43d. 6.5 F3IV, 7.6 F6V, 66.5y, a = 0.527". Combined mag., color. Companion A2V. Amp. 0.02V, 0.26145d. Probable beat phenomena. HW VelOptical. CPM? Companion F0IV. Component A of double. Ell?, 5.17 - 5.27V. Beta C 3.56 - 3.67V, 0.131977d. Beta C?, 5.56 - 5.62V, amp. 0.01b, 0.388d. Possibly the shortest period known for a He-weak star. Component A suspected occultation double. Three visual companions. Asellus BorealisBeta C 4.27 - 4.33V, 0.17d. Beta C 4.3 - 4.33V, amp. 0.04B. V343 CarAP, suspected double, unresolved by speckle interferometry. Visual companion 12.2v at 38" optical. Asellus AustraliUnusually high-velocity interstellar CaII not associated with galactic rotation, but probably part of Vela supernova remnant associated with Pulsar 0833-45 about 3d away. Amp. 0.037b, 0.563d. HX VelAlpha CV 5.58 - 5.71V, 4.2359d. BI CncBinary with HR 3467. Component C 8.0v at 0.5" from B. Alpha CV, 5.49 - 5.56V, 3.376d. KT VelSee HR 3466. Amp. 0.015b, 0.0284d. HY VelBinary. Companion is dF3. Binary with HR 3475. The magnitude difference between HR 3474 and 3475 appears to vary. Binary with HR 3474. Probably NSV 4238. 5.6 - 5.70B. AB 3.8 G5III, 4.7 A8IV or F0V, 15.05y, a = 0.238". Speckle interferometric sep. 0.263-0.272", 1980-3. Combined mag., colors. ABxC, 3.4, 7.8, dF7 at 3" from AB, 890y, a = 4.536". Component D, 12.7v at 19" from A, in hyperbolic orbit about ABC, periastron distance, 29". AB binary with CPM double companion CD at 69". CD 11.0, 13.5v sep. 6". H alpha emission var. Components B8III and B7IV. Component B, RV +24k/s. 6.30 - 6.40V. CPM. Wide CPM pair with HR 3496. See HR 3494. Gamma Cas 4.4 - 4.50V. Variable H alpha. V344 CarAlpha CV, amp. 0.02V, about 6d. KX HyaSep. 0.05", but duplicity doubtful. Delta Sct, 0.087d. HZ VelLb? 6.23 - 6.37V. BO CncCPM. AB binary. Other components optical. ADS 7050. Uncertain which component varies. B-A discordant by over 2.0v. EA 6.02 - 6.66V, 1.6698684d. Also Delta Sct amp. 0.04V with possibly changing period, 0.074 - 0.097d. RS ChaCPM. AB binary. B is K0. SRb 5.6 - 7.5v, 9.3 - 10.9p, 195:d. X CncBinary. Combined mag., colors. Suspected occultation double. 6.1 Am, 6.1, 7.24y, a = 0.1036". Combined mag., color. Binary with HR 3552. Colors for combined light. Blended mag., 6.08V. Levato indicates spectral classes G5III+A0V, both vsini =<50k/s. IDS gives two other components. CD, both 11v sep. 2.5" but does not indicate separation from A or B. Amp. 0.04:V. Multiple periods 1.97, 1.73 and 1.66d found, but subsequently questioned. IY Vel7.0, 7.0v; combined mag., colors. Unresolved by speckle interferometry. Amp. 0.08(B-V). BC 10.8, 11.0, 39.69y, a = 0.68". BC is dM1. BCxA: 817.91y, a = 9.092". Separation rapidly decreasing. ADS 7114Aa, 11.02y, a = 90.354". This is the SB pair. ADS 7114A, S, 3.12 - 3.18V, 0.071d. TalithaADS 7115A is questioned close double. Combined mag., colors, 5.0, 5.0v, sep. 0.1". B is 10.8v at 11", binary. AcubensAB 4.11 F5V, 6.18 G5V, 21.85y, a = 0.619". Combined mag., colors. Companions C - E optical. Masses A, 1.13; B, 0.84 solar. Fixed. B is B9.5V. vsini both components 0k/s. Beta C 4.91 - 4.96V, amp. 0.015b, 0.0208d. V376 CarAB fixed. Delta Sct 5.15 - 5.17V, 0.065d. FZ VelCPM. Companion F3IV. Beta Cep 6.02 - 6.06V, about 7 hrs. with beat phenomenon. IU Vel4.2 A0IV-V, 4.4 A0V, 70.1y, a = 0.27" or 64.29y, a = 0.26". Mag., colors for combined light. Alpha CV 5.33 - 5.49V. Spectral-line intensities vary with period 4.191d. Optical. Amp. 0.03:V. Multiple periods 9.64, 14.4 and 10.7d. IZ VelAB 4.85 F7IV-V, 8.16 K2V, 1067.1y, a = 6.20". C, probably optical. ADS 7203B, 7.5 - 10.0v? AB binary. B is F5V. C, optical. Binary. Triple SB system. Combined mag., colors. Alpha CV 5.22 - 5.27V, 5.0035d. B, optical. Unresolved by speckle interferometry. Young disk population. Lc 2.14 - 2.22V. AlsuhailSRc? 6.2 - 7.7p, 120d. Mean mag. varies in period 1700d. RS CncUnresolved by speckle interferometry. Gamma Cas 4.67 - 4.78V. V345 CarBC, 10.5, 10.8v, sep. 0.3", CPM? Noted by W. Herschel as double, sep. 49", is probably error: single star. AP 7.2 G9V, 7.2 G9V, 2.65y, a = 0.126". Resolved by speckle interferometry 1983.94, sep. 0.17". Combined mag., colors. Amp. 0.07V. GX VelEA 6.11 - 6.58V, 7.750d. Misnamed KM Hya in the 64th Name List of Variable Stars (IBVS 1581) and propagated in IBVS 2015, the KM designation having previously been asigned to a faint star. HR 3655 has now been corrected to KW Hya (IBVS 2681). KW HyaE 3.41 - 3.44V, 3.20 - 3.56p, 0.05R, 6.751154d. V357 CarAB 6.7, 7.2v sep. 0.11". Combined mag., colors of ABC. KL VelDelta Sct? Amp. 0.03V, 3 hrs., but sometimes cst. for 5 hrs. DD UMaHelium var.? AB optical. 6.3 - 8.1p. Binary, combined mag., colors. Balmer lines show quasi periodic var. in cycles of about 35 min. Miaplacidus6.3 - 6.34p. Optical. AB binary. Amp. 0.04b. 5.08 - 5.14V. AB, mag. diff 4.6v, binary. Lb 5.87 - 5.95V. CG UMa2.2 - 2.5:v. TuraisAB 6.50 F3V, 6.74, 389.05y, a = 1.516". Binary. AB CPM. BC, 6.87v F5V, 9.0v K2V, sep. 9", physical. B, 7.04V, +0.35(B-V), +0.03(U-B), vsini =<60k/s. AB 6.1 F4V, 6.1, 3.2y, a = 0.124". CPM. Components B9V and A0V. Close to error box of X-ray source 3U0918-55. AB binary. C, 10.0v at 7", CPM? AB 7.3 A2, 7.4, 58.93y, a = 0.150". Combined mag., colors. Alpha CV 6.51 - 6.53V, 33.97d. KU HyaCPM. 5.72 - 5.76V. AB binary. NSV 4478 is ADS 7351B, 9.5 - 11.5v. Al Minliar al AsThird UHURU Catalogue suggests Kappa Vel as optical counterpart of 3U0918-55, but HR 3717 is much closer. AB combined mag., colors. C, 11.5v at 10.7". All three CPM. Alphard, the "Dragon's Heart" in the [G/constellation] of [X/Draco], has a reddish tint to it. This slightly variable star lies approximately 140 [G/light year]s away. ALPHARDCPM. CPM. 5.87 dF8, 6.53, 116.85y, a = 0.875" or 118.227y, a = 0.880". CPM. AB binary. C, 10.5v at 100", optical. Delta Sct, amp. 0.07B, about 2 hrs. CPM. Amp. 0.025V, pulsating. Optical. Amp. 0.058V, 0.9202d, pulsating. DK UMaSp. var., 7 - 12d. AlterfCPM. Companion 9.54V, +0.44(B-V), +0.03(U-B), F6V. CPM with HR 3781. Suspected occultation double. 4.1 F2IV, 4.6 F0V, 33.99y, a = 0.795". Combined mag., colors. Comp. B, 4.5 - 5.1v. Optical. Spectrum var.? EW 6.4 - 6.92V, 6.7 - 7.22B, 0.648345d, per. probably varies. S AntSuspected double unconfirmed by speckle interferometry. Amp. 0.012y, 40.4d. Possibly rotational modulation from active regions. SU LMiL? 3.10 - 3.16V. N VelBinary. Secondary F0. AB fixed? B is F5. C, at 118". Probably optical. Heis-Argelander Binary? Amp. 0.033y, 18.0d, possibly due to rotational modulation. SV LMiSecondary B8V, vsini 157k/s. CPM. Companion F8V. Discordant magnitudes and colors: Nicolet: A = 7.86V, -0.10(B-V), -0.43(U-B); B = 9.07V, +0.55(B-V), +0.01(U-B). USNO Photoelectric Catalogue: A = 6.36V, +0.01(B-V), +0.03(U-B); B = 9.51V, +0.50(B-V), +0.03(U-B). Component A suspected occultation double. Suspected occultation double; possibly SB. Amp. 0.05V, 2.8519d. Also pulsations of 11.67 min. IM VelCPM. CPM. Lb 5.84 - 5.98V. DR LeoComponent B, 9.9v at 85". Subra4.4 - 4.44B. Companion G8V, RV +14k/s, optical. R-I also found at -0.04. High velocity star. 5.06 - 5.17V, 0.04R. 6.0 A2, 6.1, 10.72y, a = 0.142". Combined mag., colors. Amp. 0.16p. CS UMa5.4 F7V, 5.6 F8V, 18.32y, a = 0.134". Combined mag., colors. E amp. 0.2b. Component A of visual double. IP VelCep amp. 0.1V, period a few days. Ras Elased AustrBinary 7.0, 7.2v, sep. 0.031", resolved by speckle interferometry at 4-meter Mayall telescope, but unresolved 1983.96 at Pic du Midi. Combined mag., colors. 6.5 - 6.59V. CDelta 3.28 - 4.18V, 35.53584d. Period varies. l CarCPM. Delta Sct 3.77 - 3.86V, 0.133d, amp. and form of light curve vary. AB, about 200y. B also A8IV. Comp. B of visual double, Delta Sct 6.08 - 6.12V, 0.08184505d. DG LeoSee HR 3890. 5.30 A3IV, 5.38 A3IV, 105.5y, a = 0.360". Combined mag., colors. Secondary B9. Ras Elased BoreaAB 5.58 A1V, 6.07 A4V, 77.55y, a = 0.383". Combined mag., colors. C, 12.28V at 36" optical. Binary. Cst? 5.23V. SY UMa6.3 - 6.36B. BetaC, Amp. 0.03b, 0.1096d. Binary. Combined mag., colors. Amp. 0.13V. Companion K0III, optical. BetaC, amp. 0.013b, 0.1608d. IV VelCPM companion A0III; however, the companion is optical. Amp. 0.24V. CPM. Amp. 0.10V. Fainter component is BD+32d1968. Probably optical. AC binary. B, 12v at 12" optical. C, 7.0v A0, vsini 50k/s. Suspected occultation double. Delta Sct? 4.47 - 4.52V, about 0.1d. Binary, sep. 0.097", unresolved by speckle interferometry 1982.17. 5.3 K0IV, 6.9 G5V, 232y, a = 0.64". Combined mag., colors. Cst 6.49V. R VelABxC, CPM. C is 13.0v at 28". CPM. Regulus, the heart of [X/Leo], is the star at the base of the "Sickle of Leo". It is approximately 75 [G/light year]s distant. It has a small companion star which lies approximately 4,660 [G/A.U.]'s from Regulus. AB binary, B, 8.13V, +0.86(B-V), +0.51(U-B), K1V. BC, 7.6, 13.1v, 2000y, a = 4.163". REGULUSVisual companions both optical. CPM. M 4.5 - 9.9v, 149.49d. S CarLb? 6.1 - 6.40v. V368 CarCst? 6.25V. U UMaSuspected hard X-ray source. Gamma Cas 5.63 - 5.83V. QY CarAB binary. Both A and B Am stars. vsini both components =<25k/s. B is 7.36V, +0.30(B-V), +0.19(U-B). 7.2 dF2, 7.5, 552.0y, a = 1.299" or 810.5y, a = 1.198". Combined mag. Primary unresolved by speckle interferometry 1982.17. AdhaferaTania BorealisCompanion is M1. 6.9 A5V, 7.0 A5V, 124.0y, a = 0.435". Combined mag., color. Amp. 0.32V, 0.11R. GY VelAlpha Cyg: 5.30 - 5.65V, amp. 0.65U, about 140d. AG AntLc? 3.36 - 3.44V. V337 CarDelta Sct?, 4.77 - 4.83V. See HR 4057. See HR 4057. 6.37 - 6.44P, 0.21R. GZ VelCst? Comparison star was the var. RS SexCPM? Combined mag., colors. Components A1V and A1Vn. E?, 2.99 - 3.33V. Tania AustralisProbably not var. Comparison star was variable. Alpha CV?, 4.91 - 4.99V. AB binary? Spectrum and H alpha vary. Amp. 0.025y, 4.37d. Spectrum var. SS SexB, 13v at 8", optical. SRb? 5.60 - 5.67V, 1 - 2d? DE LeoPossible He var. CPM. 4.40 G8III-IV, 6.12 F8V, 37.92y, a = 0.340". Combined mag., colors. Primary is occultation double, 6.7, 6.7v, sep. 0.02". Alpha CV 5.97 - 6.15V, 7.897d. Magnetic var. 7.9d? and var. Sr, Cr. CX LeoPossible small amp. variations with proposed periods of 3.57, 0.64d rather uncertain (Manfroid and Mathys 1985, A&A, Suppl. 59, 429). Amp. 0.07B, 0.06(B-V), 0.14(U-V), 58.82d. V399 CarAmp. (U-B), 0.13. Triple CPM and common RV system. B = BD+56d1458, 9.94pg; C = BD+57d1266, 8.99pg. 3.79 - 3.83V. Companion F9Ve, strong lithium. Primary is SB. Slight variation with period or half-period of about 8d suspected. AB CPM. B is F6V. C, 9.5v at 64" optical. Optical. B = CPD-60d1944 = HD 91269, 7.54V, -0.08(B-V), -0.57(U-B), B5Vne, shell star. Visual companion optical. 4.4, 4.8v, sep. 0.11"; combined mag., colors. Old disk population runaway star. Alpha Cyg 3.83 - 3.90V. Companion K5, optical. Fixed with HR 4136. Mag. and color for combined light, 5.16V, -0.15(B-V), -0.62(U-B). See HR 4135. Gamma Cas 3.27 - 3.37V. PP CarCPM? Companion spectral class A. Alpha Cyg, amp. 0.1v, 0.05y, cycles 15 - 20d? Irregular var. in H alpha emission profiles indicating chromospheric activity. V369 CarA is SB. Visual companion 8.5v at 2.4"; CPM. ADS 7837A, EA 5.66 - 5.75V, 2.4450566d. TX LeoAmp. 0.08(B-V). Lb 8.1 - 9.7p. Amp. 0.25V. U AntPhi16.7 F4V, 7.5 G0V, 210.1y, a = 0.982". Combined mag., color. Optical. Companion A8III, optical. SRb 7.0 - 9.2p, 7.0 - 9.4B, about 450d. Amp. 0.12V in one cycle in 1971. U Hya4.2 F3IV+F0V, 5.1 A6V, 16.30y, a = 0.340". Possible abs. mag. = -8.0V. Alpha Cyg 5.45 - 5.52V, amp. 0.035y. V370 CarPhi in most cataFixed. Combined mag., colors. Companion A5V. Optical. Probably CPM. B is B8. C, 11.2v at 20" from B. SRb 5.98 - 6.16V, 150d. RX LMiLambda 4200 star. Alpha CV 5.48 - 5.52V, 1.6731d. Magnetic field varies with same period. Relative to HR 4205, delta u = 0.102, delta y = 0.046. V364 CarOne of only four WR stars bright enough to have been observed spectroscopically in UV by COPERNICUS. Companions optical. AB CPM. B is GC 14751, dG0. AB binary. B is K0III. Lb 5.89 - 6.5v. VY UMaSpectrum var., 1.7788d. Discussion of earlier suspected period of 0.7045d given by Walborn (1979, PASP, 91, 442). vsini 202k/s. High speed mass ejection. Sep. 0.03", but duplicity doubtful. Amp. 0.028y, 0.038u, possibly eclipsing. Intervals between minima about 3d. Old disk population runaway star. CPM with HR 4212. CPM with HR 4211. 2.7 G5III, 6.4 G2V, 116.24y, a = 1.437". Secondary also classified F8:V:. Old disk population runaway star. Suspected amp. 0.08V on time scale of 2 hrs. Amp. 0.09 in (B-V). Old disk population runaway star. PraecipuaCPM. Companion 8.75V, +0.58(B-V), +0.01(U-B), G0V, RV = +18k/s. B, optical. Amp. 0.2V. Suspected visual binary unresolved by speckle interferometry. 3.76 - 3.80V. See HR 4259. Appears to be variable over long time scale, especially toward uv (may be constant in V). KQ VelAB 6.1 F2III, 8.0, 128.34y, a = 0.823", or 90y, a = 0.75. Visual primary is SB, sep. 0.001". Lb? 5.69 - 6.03V. VY LeoCst? 7.00B. T CarAmp. 0.02B, 0.150d. IW Vel6.0 - 7.4p. Faint only Feb. 6, 1943. CDelta 5.72 - 7.02V, 38.7681d since 1939. Period varies, earlier 38.753d. U CarAlkesSuspected occultation double. Optical. MERAK1.87 K0III, 4.81 F0V, 44.4y, a = 0.603". Also classified K0II-III + A8V:. Combined mag., colors. Also CPM at 280" with HD 95638 = GC 15179, 7.12V F8; SB, 6.04d. ADS 8035A; B also var. suspect NSV 5071, too close to primary to be certain of variability. DUBHEUnresolved by speckle interferometry. Suspected occultation double. CPM. AB, CPM. 5.6 F4V, 5.7 F4V, 7.40y, a = 0.140". Combined mag., colors. Blue straggler. EA 5.65 - 5.94V, 2.267701d. Chi2 Hya7.2 - 7.37B. Alpha CV, amp. 0.03V, 2.433d. V815 CenAmp. 0.02b. Large spectrum var., 0.8183d (not confirmed). Amp. 0.02V. HR 4340 used as comparison star. Lb? 5.79 - 5.95V. CO UMaDelta Cep? 3.84 - 4.02V. V382 CarAlpha Cyg 5.12 - 5.19V, amp. 0.055y, 15 - 20d cycles. Also var. H alpha profiles indicating chromospheric activity. V371 Car6.7 B9V, 7.1 A1V, 233.0y, a = 0.383". Astrometric binary. Combined mag., colors. Fixed sep. Fixed sep. Component A of double; Cep?, 4.58 - 4.62V. Companion A0, optical. Delta Sct? ZosmaChortAmp. 0.03b, 0.58:d. Lb?, 4.59 - 4.65V. CPM. If secondary is on main sequence, the spectral class is inferred to be F1V. AB CPM. B, 11.5v at 1". C, optical. ADS 8115A, brighter component of the SB system, Alpha CV 6.32 - 6.35B, 5.90513d, two unequal max. Same rotation and magnetic per., related var. EuII and SrII emission. SV CrtPrecedes HR 4369 because 1900 position given in HR, (Harvard Annals, Vol. 50), is erroneously 11.9 instead of 11.8m. AB 4.32 G0V, 4.79 G0V, 59.840y, a = 2.530". Combined colors. Mag. for blend 3.79V. AB, first visual double for which an orbit determined, in 1828 by Savary. Third component astrometric with A, 1.832y, a = 0.055". See HR 4374. Alula AustralisCPM. Alula Borealis6.0 - 6.6V. 4.3 B5VN, 5.0 B6V, 39.18y, a = 0.277". Combined mag., colors. 4.03 F2IV, 6.70 G3V, 192.0y, a = 1.92"; possible subsystem with period about 16y. Combined mag., colors. Combined mass about 3 Suns. Delta Sct? Sep. 0.0034", discovered by occultation. Companion not confirmed. AB 6.51 K0IV, 7.57 K2IV-V, >4000y. Combined mag. 6.16V. C, 9.9v at 90" probably physical. ADS 8175AB, 8.2 dG5, 4500y. Primary SB. Visual companion A3V. Ell:, amp. 0.13V, 39d x 2? EE UMaSR, 3.78 - 3.86V, about 1100d. Gianfar5500y. Circular orbit. Companion, K6IV. Alpha Cyg 6.31 - 6.36V. V809 Cen5.75 F6V, 7.07 G3V, 72.87y, a = 0.813". Combined mag., colors. Possibly wide physical pair with HR 4442. SRd 5.8 - 6.6p. At times shows cycles about 200d. See HR 4441. Alpha Cyg 5.12 - 5.22V, 46.3:d. Omi2 CenCPM with HR 4444. Binary. AB binary. Combined mag., colors. B is B6. C, 9.64V F5 at 63". SRb 5.55 - 5.80V, about 60d. V763 CenAB long period binary. C, 11.17V at 21" optical. Companion B9V, optical. Duplicity doubtful. Lb 5.23 - 5.37V. CPM. AB binary. CPM. Amp. 0.09V. 5.5 G0, 6.3 A0, combined mag., colors. GT MusAmp. 0.13V. Resolved by speckle interferometry 1986.44, sep. 0.03". AC CPM. C, 8.44V, +0.50(B-V), +0.035(U-B), F7V. SRd 4.95 -5.12V, 130:d. Spectrum var. F5-G0Ia-O + B1Iab. At blue edge of instability strip. V810 CenOptical. Amp. 0.08V. Amp. 0.04V? 7.0 - 7.12p RS, amp. 0.03V, 71.7d. DQ LeoLb 4.6 - 4.8V. 6.0 A8V, 8.3 G2V, 122.0y, a = 0.68", 180y, a = 1.00". Combined mag., colors. ADS 8311B, 7.5 - 9.5V. SRb 4.85 - 5.12V, 61d. II HyaRepresenting [X/Leo]'s tail, Denebola lies 40 [G/light year]s away and is approximately 20 times more [G/luminous] than our [G/Sun]. B, 15.7v at 40" physical; C, 13v at 80" optical. Delta Sct?, 2.09 - 2.16V. DENEBOLACompanions optical. ZavijahSuspected occultation double. Combined mag., colors. The reality of the companion, CF UMa, announced by P. van de Kamp (see Low Luminosity Stars, ed. S. S. Kumar, p. 199, 1968) has been questioned (PASP, 96, 557, 1984). Unresolved by speckle interferometry 1980.47. Companion of Groombridge 1830, UV? 8.5-12v. Groombridge 1830Alpha CV, amp. 0.04V, 0.04B, 2.344d. PHADCPM. Combined mag., colors. Binary with HR 4561 = ADS 8347D. AB binary 7.2, 9.0 sep. 0.3". ABxC, 8.4 at 4" also binary. Amp. 0.09B, 0.87d? Uncertain which of components A, B, C of ADS 8347 is the var. DN UMaSee HR 4560. Discovered as double by W. Herschel, sep. 90" but no visual companion subsequently seen at that separation. LV HyaUsed as comparison for HR 4603; uncertain which is the variable. AB, CPM. B, 12.5v at 7". D, 12v at 140". Doubtful if double. Optical. Fixed sep. Old disk population runaway star. Delta Sct amp. 0.02V, 0.04d - 0.08d, possible beat phenomena. DP UMaBinary. Companion A9V. vsini both components =<50k/s. Beta C 4.70 - 4.74V, 0.0889d. See HR 4573. The2 CruUnresolved by speckle interferometry 1982.17. CPM. ADS 8417B, 10.4 - 11.4?v. AB combined mag., colors. C, 8.2v A3 at 9", CPM. CPM with HR 4619, 4621. H alpha varies. CPM with HR 4618, 4619. Gamma Cas 2.51 - 2.65V. Expanding circumstellar shell. AlchibaEA 5.75 - 5.94V, 4.966377d. V788 CenGamma Cas 5.47 - 5.58V, 5.4 - 5.6B. V817 CenMinkarCDelta 5.89 - 6.49V. Period changes 9.66011 to 9.66007d. S MusAmp. 0.28V. Old disk population runaway star. CPM. Binary. Combined mag., colors. Beta C 2.78 - 2.84V, 2.25 - 2.31p, 0.151038d. Expanding circumstellar shell. MEGREZ6.8 F5, 7.9. Old disk population runaway star. Expanding circumstellar shell. Gienah GhurabRS Cvn, amp. 0.19V, 63.15d. DK DraBinary. Companion 8.77V, +0.57(B-V), +0.09(U-B), F7V. Delta Sct amp. 0.04B. SRb? 3.99 - 4.31V, 40d. CPM. Old disk population runaway star. 4.2 - 4.24v. Binary with HR 4678. Binary with HR 4677. Companion G8III, optical. Delta Sct 6.40 - 6.48V, 0.05515028d. Also possible cycles of 0.0713d. The first Delta Sct type star to be discovered in a galactic cluster. FM Com4.9, 5.4, sep. 0.008". Also astrometric and interferometric double, 5.4v sep. 0.124", position angle changed 35d in 1.5yrs. Delta Sct? ZaniahPrimary may be close double 5.8, 5.8v, sep. 0.6". Visual companion 11.6v at 132". Companion F6III optical. CPM. Companion also dF2. I? 3.4 - 4.0v. AC binary. C, 8.55V, +0.52(B-V), +0.01(U-B), F7V. Component B, 12.52v at 35" optical. Binary. Secondary is dK5. ADS 8531B, 8.0 - 9.5V. Delta Sct 5.89 - 6.15V. Multiple periods 0.2085, 0.1529, 0.1259 and 0.1158d. AI CVnE? Amp. 0.067V. Alpha CV 5.18 - 5.20V, >1d. GN ComComponents K3IIIab and F8IV. AB 6.76 A7V, 7.79 F4V, 678.0y, a = 1.30". AB 1.35 B0.5IV, 1.75 B3n or B0.5Vn, q = 0.916". Mag. and colors for blend of HR 4730-31, 0.76V, -0.25(B-V), -1.00(U-B), -0.24(R-I). Masses 14 and 10 solar for hyperbolic orbit with periastron distance 61 AU. Possibly X-ray source 2U1223-62. Acrux is a bright binary star system whose combined light makes Acrux the 14th brightest star in the sky. It is about 400 [G/light system is much larger than our [G/Sun] (14 and 10 solar masses respectively). ACRUXIn stage of rapid evolution after core hydrogen exhaustion. Faint CPM at 542" S. prec. Amp. 0.35V, 0.25p. BL CruDelta Sct 6.20 - 6.23V, 0.05d. Form of light curve varies. FT VirCPM with HR 4752. Component C, 14.7V at 2" from B. CPM with HR 4751. Alpha CV + Delta Sct 5.23 - 5.40V, 5.0633 or 5.0754d and possible pulsation 0.052d. Var. magnetic field UII varies with period 71 min. AI ComCPM. B is K2Ve, lithium strong. ADS 8572A. AlgorabAB 6.5 G0V, 8.6, 161.53y, a = 1.385". I? Amp. 0.30p. GacruxLb? 4.95 - 5.04V. CQ DraAlpha CV + Delta Sct 5.41 - 5.46V, 2.1953d with secondary variations of 1.0256d and 0.9178d. Also Delta Sct amp. about 0.01V, 0.0227d or 0.0274d and 0.2909d. Considerable discordance among observers. CaII and SrII vary in period about 1d; period changes. UU ComCDelta 5.36 - 5.58V, 3.34258d. BG CruDelta Sct? Probable nearby star. Beta CVn amp. 0.05V. KrazRadio star. Gamma Cas 3.82 - 4.10V. H alpha and H beta emission vary period about 30d. H alpha profile changes in 1 min. or less. Binary with HR 4792. Binary with HR 4791. 5.11 - 5.16V. Delta Sct, amp. 0.02B, 0.082d. TU CrvCompanion B4V, optical. Beta C 2.68 - 2.73V, 2.17 - 2.24p, 0.0903d. CPM? Combined mag., colors. Companion B7p. H alpha emission var. 0.1V, 0.15d. FW VirEll? Amp. 0.025V, 0.58:d. FH MusAlpha CV 6.32 - 6.55V, 4900:d. AX CVnAlpha CV? 4.61 - 4.66V. Period about 0.46d: AB 2.9 A0III, 2.9 A0III, 84.50y, a = 0.930". Combined mag., colors. CDelta 5.89 - 6.49V, 7.510211d. Period changes. R MusBinary with HR 4822, q.v. See HR 4822. EA? 4.91 - >7.5V, 5.0 - >7.5p. Faint May 22, 1896. Also amp. 0.04V suspected on time scale 1d. Delta Sct, amp. 0.02U,B,V; 0.056 and 0.042d. GG VirBinary with HR 4825, q.v. Delta Sct? Amp. 0.02V, cycles 0.02 to 0.10d. Gamma Cas 5.24 - 5.45V. BZ CruAmp. 0.07V. 3.7 B2V, 4.0 B3V, 383.12y, a = 1.735". Combined mag., colors. SRb 7.4 - 10.0p, 158.0d, some cycles 250 and 90d. Possible secondary 2000 - 2200d. Y CVnDelta Sct 5.20 - 5.23V, 0.0756d. FM VirProbably optical. CPM? Companion A3p. Comp. B, 8.70 - 8.82V, Ap. Possible spectrum var. Interferometer measures indicate close double or multiple star. Component B, 11.4v, F8V, optical; C, 7.5v, B8. Beta C 1.23 - 1.31V, multiple periods, 0.2365072d, 0.160474d, 0.121383d, 6d, 7 - 8y and others. BecruxAlpha CV 6.29 - 6.39V, 16.31d. Same rotation period. Var. spectral lines and magnetic field. Magnetic and rotation axes nearly aligned. EP VirAmp. 0.05V. Optical. Equal components. Delta Sct? 5.9 - 5.94v. B, optical. Amp. 0.07V. H alpha emission var. Suspected occultation double. CPM with HR 4893. CPM with HR 4892. AB 5.05 G8III, 7.22 F3V, 510y, a = 1.42", or 674.23y, a = 1.897"; masses 2.7 and 1.4 solar. Component C, 9.74V, +0.73(B-V), +0.31(U-B) G3IV-V 29", possibly physical, although a hyperbolic orbit has been computed with periastron about 400 years ago. CDelta 6.23 - 6.92V, 4.68997d. S CruBeta C?, amp. 0.02V, 0.3951d, possible secondary 0.1793d. CPM with HR 4899. CPM with HR 4898. Gamma Cas 4.99 - 5.18V. Mu2 CruCombined mag., color, 6.7, 6.8v, sep. 0.100"; occultation double. Close binary, sep. 0.040", unresolved by speckle interferometry. If companion on main sequence, the inferred spectral type is F6V. Lb 4.7 - 4.8V. Alpha CV 1.76 - 1.79V, 5.0887d. Spectrum variable. Photometric var. due to UV absorption from overabundant metals. ALIOTHCompanion K0III. SRb 5.55 - 6.6V, 7.2 - 7.7p, 50d. TU CVnAuvaCep-like supergiant, 6.61 - 6.69V, amp. 0.32B, 43.96d preferred; 53.33 or 67.80d also possible. LN HyaBinary with HR 4915. Binary with HR 4914. ADS 8706A, Alpha CV 2.84 - 2.98V, 2.78 - 2.81B, 5.46939d. The prototype star. Var. magnetic field with same rotation period. COR CAROLIAB binary? C, 10.4v at 124" optical? CPM. Component A suspected occultation double. CPM. AB CPM. C, 13v at 36" optical. ADS 8732B, 8.0 - 11.0v. BC, 9.5, 9.9v sep. 2". AxBC optical. 6.02 - 6.17V. Miscellaneous magnitude determinations range from 5.93 to 6.132V, probably confirming variability. Also suspect amp. 0.03V on time scale 2 hrs. 5.05 F2V, 7.43 G6V, 109.97y, a = 1.270" or 106.7y, a = 1.281". Combined mag., colors. ADS 8739B, 7.5 - 10.5v. VINDEMIATRIXCPM? Combined mag., colors. Lb? 7.9 - 8.01p, amp. 0.09V. V789 Cen8.1 - 8.20B. Companion K0Ve, high lithium abundance. CPM companion F7V. 5.1 - 5.3v. Period of some hours? AB CPM. BC, 11.9, 12.1 sep. 0.4" in 1901, single in 1958. Companion at 149" from A, noted by John Herschel, small nebula. SRb 5.30 - 6.1v, 58:d. FS ComCPM. vsini of secondary 110k/s. Second brightest Wolf-Rayet star in the sky. E + WR 5.50 - 5.52V, 18.341d; UV, var. 1.5d. A is SB and speckle interferometric binary, third component 9.4v, sep. 7.1". B, 8.00V, +0.20(B-V), -0.09(U-B), CPM. Alpha CV, amp. 0.035V, 1.272d. V824 CenADS 8805BC. Binary? C, 11.2 at 1". A is HR 4971, not CPM. ADS and IDS differ on naming of the components. IDS, adopted here, is the more consistent with FGW Struve's early discovery. AB 5.05 F5V, 5.08 F5V, 25.87y, a = 0.662". Colors, spectrum for combined light. Mag. of blended HR 4968, 4969 is 4.32V. ADS 8804A speckle interferometric sep. 0.43" 1978.40, 0.58" 1981.47. Var. of combined light with HR 4969 not confirmed, but 90d inclination of orbit indicates eclipses possible. DiademAB 5.0 B8V, 5.7 B9V, 27.0y, a = 0.185". Combined mag., colors. C, 8.4v at 2" physical. 4.54 - 4.65V, combined light of 5.2, 5.8, sep. 0.3". Uncertain which component is variable. V831 Cen7.2 A5V, 7.3 A5V, 19.0y, a = 0.118". Combined mag., color. B, 12.5v at 79". Component C at 184" discovered by John Herschel in 1897 not seen 1908 or later. Binary. Component B, 8.2 A0p, Am?, CPM. E? 4.76 - 4.81V. Optical. 6.54 - 6.60p. Delta Sct 6.67 - 6.72V, 0.119153d. Probably long beat period; long intervals const. mag. DK VirFainter component 8.5 - 10.5v. Companion is GC 17977, 8.2v A2, CPM. 4.8 - 4.85V. Delta Sct 4.70 - 4.75V, 0.12168d. Var. amp.? AO CVnAlpha CV, amp. 0.04V, 0.767d. BK CVnAmp. 0.10V. Possibly double. Old disk population runaway star. Amp. 0.10V. Aa = AP 3.0 A2V, 3.0 A2V, sep. 0.0115", 0.056y, a = 0.012". Combined mag., colors AP. Binary with HR 5055. Alcor, HR 5062, at 709", CPM. MIZARSpica is the 16th brightest star in the sky. It is a binary star system that lies 142 [G/light year]s away. The largest of the two stars is almost 11 times more massive than the [G/Sun], while the second star is approximately 7 times the mass of our star. Interferometer indicates visual component A is multiple system. Occultations yield three companions: 3.1v at 0.0025", 4.5 at 0.05" and 7.5 at 0.5". Combined mag. and colors. Visual component B, 12.0v at 148". Ell (Beta C) 0.97 - 1.04V, 4.01454d, and Beta C, 0.1737853d. Period changes. SPICAComp. A is speckle interferometric binary, sep. 0.045". CPM with HR 5054-5. Delta Sct. ALCORAlpha CV, amp. 0.09V, 4.3127d; alternative periods 4.3032, 4.3224d. EZ MusFirst known potassium flare star. CPM with HR 5075. CPM with HR 5074. ADS 8920A, M 3.5 - 10.9v, 388.87d. Period varies; was 500d beginning of 18th century. M8 at minimum. Discovered by Montanari in 1670. R HyaComponent B is CPD -76d769. CPM. Cst 6.6p. S ChaBinary. 4.5 G8III, 4.7 G9III, 78.7y, a = 0.165". Combined mag., colors. Unresolved by speckle interferometry. HX VirAlpha CV 4.91 - 4.99V, 3.7220d, also magnetic field and rotation period. Probable irregular magnetic variable. CW VirAB 6.5 A1, 6.9, 197.7y, a = 0.563". C, 12v at 26" optical. ADS 8954. Uncertain which, if either, A or B varies. HezeOptical. RS 4.94 - 5.01V, 2.6131738d. Probable reflection effect. BH CVnDelta Sct? AB 6.2 F6V, 6.5, 34.969y, a = 0.463". Combined mag., color. Companion 8.5v F6V, CPM. AB binary. B is A7IV. AB 5.01 A7III, 6.91 F0V, 240.0y, a = 1.091" or 220.4y, a = 1.205". Combined mag., colors. Companion B1p, optical. Beta C 2.30 - 2.31V, 0.169608, 0.17696 or 0.2150d. Multi-periodic. Binary. Companion K3III. SRb 5.14 - 6.55V, about 90d. Amp. 1.2V, 0.19(B-V), 0.47(U-B) from another source. Possible type E with very long period. V744 CenLb? Amp. 0.08V. V765 CenAB 6.3 F0IV, 6.3 F2IV, 22.35y, a = 0.208". Combined mag., colors. Masses 7 and 6 solar. AB binary. B is Am. AB combined mag., colors. SRa 5.5 - 9.0v, 90.44d. Amp. 2.04V, 0.32(B-V), 1.09(U-B). Spectrum variable. T CenCPM. Alpha CV 6.24 - 6.26V, 2.449909+/-0.000011d, asymmetric light curve. Spectrum var. CQ UMaVariations in 17 and 24 min., amp. about 0.8B. Third component 9.2v at 0.8" from A. Alpha CV, amp. 0.025V, 2.605d. V827 CenBinary. B = NSV 6401. ADS 9000B. Delta Sct? Amp. 0.02V. Visual companion 11.7v at 44". Primary is occultation triple, companions 8.2v at 0.039" and 8.4 at 0.061". Companion 10.01V, +0.78(B-V). One of the intrinsically most luminous stars in the Galaxy. S Dor? 6.17 - 7.50V. V766 CenAB CPM. CD at 27", 11.9, 13.1v sep. 2", binary. High space velocity. Amp. 0.08V. CPM with +7d2692, 9.4v at 486". Binary, period several centuries. Companion M2. Delta Sct? 4.40 - 4.58V. Alpha CV 5.64 - 5.67V, 1.37996d, amp. 0.03U. Spectrum variable. CR UMaCPM. Beta C?, 3.40 - 3.43V, 3.48 - 3.52R, 0.175d. Alkaid is located at the end of the [G/Big Dipper]'s handle. It is about 93 [G/light year]s distant. ALKAIDSRb 4.16 - 4.26V, 5.79 - 5.87P, 12:d. V806 CenCompanion F2V, optical. Gamma Cas 2.92 - 3.43V, 3.535d. Variable H alpha. Expanding circumstellar shell. R and I mags. decreased by about 0.3m between 1965 and 1983. Variable line profiles. CPM. Companion 7.72V F0Vp. See HR 5210. SR? 4.72 - 4.81V. AW CVnVisual companion, 8.35V, +0.36(B-V), +0.12(U-B), A3Vm, vsini 71k/s. AB 6.3 F2, 6.5, 257.7y, a = 1.268". Mag., colors for combined light. Component E, 8.5v at 66" optical. Companion B8V. Gamma Cas 5.85 - 6.26V. H alpha also variable. V767 CenLb? 4.52 - 4.67V. CU DraExpanding circumstellar shell. ADS 9053, 2613y, a = 4.998". A* 2.68 G0IV. Visual component 8.8v at 113" optical. MufridI 6.1 - 6.6p. Expanding circumstellar shell. SRb 6.4 - 8.6p, 119d. Amp. 0.56V, 0.10(B-V), 0.26(U-B). IUE observations on Aug. 2, 1985 and Oct. 2, 1986 show slight increase in visual mag. and decrease by 0.9 mag. in Mg II 2800. B is G type, optical. Hadar, a bright, hot star, is the 10th brightest star in the sky. It is over 360 [G/light year]s away and has a companion star that is difficult to see with a small telescope. Beta C? Amp. 0.07V, 0.157d, modulation 352d. Line profiles also vary per. 0.157d. HADARAlpha CV, amp. 0.045V, 1.837d. V828 CenA*, 9.897y, a = 0.1075". Unresolved by speckle interferometry 1986.45. Amp. 0.04V. Amp. 0.020B, 0.035d. MenkentThuban is the bright star located halfway between the bowl of the [G/Little Dipper] and the second star of the handle of the [G/Big Dipper]. It is approximately 180 [G/light year]s distant and 135 times more [G/luminous] than our [G/Sun]. 4,800 years ago, Thuban was aligned with Earth's North [G/Celestial Pole], making it our North Star. Alpha CV?, 3.64 - 3.67V. THUBANCompanion K2V. Companion K2. Amp. 0.08V, 1.456d. Suspected occultation binary. Lb? 4.98 - 5.33V. BY BooLb 5.2 - 5.3v, 7.0 - 7.13p. CF BooSRb 4.80 - 5.00V, 80d. ET VirPossible runaway star. EB 5.96 - 6.52V, 1.49009305d. V716 CenOptical companion. Alpha CV 4.98 - 5.05V, 0.52067688d. Same period spectrum var. Si a major source of photometric variability and suggests starspots related to magnetic field. SiII varies out of phase with HeI. Period unusually short for star with peculiar A-type spectrum. CU VirComponent B, M3IV; C, F4V; both optical. Gamma Cas 4.97 - 5.10V. V795 CenDelta Sct amp. >0.05B, over 2 hrs. Companion F5V, optical? I 1240A, M 5.3 - 11.8v, 546.2d. R CenBinary with HR 5329. ADS 9173B. Formerly suspected amp. 0.01V, not confirmed. Binary with HR 5328. ADS 9173A, Delta Sct 4.50 - 4.58V, 0.06682 or 0.076242d. Possible beat period of about 16d. Asellus TertiusLb? 6.37 - 6.52V. FS Vir4.06 - 4.11V. SyrmaArcturus is the fourth brightest star in the sky. It is 25 times the diameter of our [G/Sun] and 115 times more [G/luminous]. It is only 37 [G/light year]s away. High space velocity? H and K emission vary. ARCTURUSAB CPM? B is K0V. Delta Sct 4.73 - 4.78V, amp. 0.025B, about 40 min. Asellus SecondusAlpha CV 5.73 - 5.93V, 9.29477d. Line intensities, rotation and magnetic field same period. Also possible magnetic cycles about 1 hr. CS VirAB CPM. B, 13.3v at 3". Combined mag., colors. Occultation sep. 0.006", mag. diff. 1.4B. Possibly triple star with SB. Optical. AB binary. Component A is close double, sep. 0.2", combined mag. and colors. SX Ari 4.38 - 4.43V, 8.814d for light, He, magnetic field; light and mag. field max. correspond to He min. Sp. from B2V to B7IV in per. 8.8172d. Var. possibly due to rotation of inhomogeneous surface; possibly prolate spheroid. V761 CenBC 7.5 F0V, 7.6 F2V, 39.50y, a = 0.228". Combined mag., colors. Also binary with HR 5386 = ADS 9247A. EA? 5.7 - 6.2p. Beta C 4.54 - 4.58V, 4.36 - 4.43B, 4.10 - 4.14p, 0.17738884d. Binary. Combined mag., colors. Triple system. BC, 7.0v A4V or A1IV, 8.2v sep. 1". vsini of B is 60k/s. CPM. Asellus PrimusABxC, CPM. C, 10.0v at 4". AB binary. Combined mag., colors. Companion G6Ve, optical. Fixed with HR 5414. CDelta 6.43 - 7.21V, 5.493839d. V CenCompanion K1V. Identification of companion questioned. Component C optical. 6.5 A7IV-V, 6.7 A7IV-V, 30.0y, a = 0.210". Combined mag., colors. Primary found double by speckle interferometry, sep. 0.069". Component B, optical. Delta Sct 3.02 - 3.07V, 3.23 - 3.28B, 3.20 - 3.25p, 0.2903137d. Hydrogen and Ca lines vary. SeginusCompanion K0V. Innes catalogue indicated a faint companion at 6" in 1897, not subsequently seen. Gamma Cas 2.30 - 2.41V, 1.83 - 1.95p. H alpha variable, H beta sometimes bright, sometimes dark and double or multiple. Variability shows evidence of mass loss. Amp. 0.07V on time scale 1d suspected. Delta Sct? Amp. 0.02V, over 3 hours. CP Boo5.52 - 5.56V. Delta Sct? AB combined mag., colors. C, 9.2A1V at 19" = CoD -45d9303, CPM? Lb, amp. 0.14V, 7.2 - 7.34p. CH BooS, amp. 0.1:V, 0.20U. Expanding circumstellar shell. AB 79.920y, a = 17.515". B = HR 5460, CPM with Proxima at 2.2d, discovered by Innes in 1915, a flare star, V 645 Cen, 12.4 - 13.4p, 11.10V, +1.88(B-V), +2.05(R-I), M5.5Ve. RIGEL KENTAURUSSee HR 5459. Binary. Companion K5V. Amp. 0.03V. Magnetic var., about 4 months. Pulsation period 6.8 min? Beta C 2.29 - 2.34V, 0.2598466d. Period varies. Possible secondary period 3.145d. Modulation period 10y? Possible nearby star on basis of spectroscopic parallax. Binary with HR 5476. Colors for combined light. Mag. for blend, 4.53V. ADS 9338A, Alpha CV? 4.94 - 5.00V. Binary with HR 5478, q.v. H alpha variable. Rijl al AwwaBeta C, amp. 0.04u, 0.03y, 0.04V, 0.131d with possible secondary periods. BU CirSRb 4.7 - 5.4v, about 30d or 450:d. W BooDelta Sct 6.47 - 6.52V, 0.08d. BP OctBinary. Delta Sct 6.22 - 6.29V, 0.0825 and 0.0837d. Difference in mag. between components of double varies. DL DraBinary, components F0V, G1V. 7.0 F7V, 7.2, 25.95y, a = 0.297". Binary with HR 5505. Colors for combined light. Mag. of blend, 2.37V. IZARSRb 5.93 - 6.15V, 60 - 80d? V768 CenCPM? AB and AE binary. B = Am(A2/A6/A8)s. C and D optical. E 12.5v at 27". ADS 9396AB, Alpha CV. In Innes catalogue, 6.5, 6.5v sep. 0.5" in 1913. Not confirmed. CDelta 5.65 - 6.09V, 5.273268d. AX CirBinary. CPM with HR 5531 at 231". Component A, HR 5531, is the suspected occultation double, 3.4, 3.8, sep. 0.01". CPM with HR 5530. Suspected occultation double. Zuben ElgenubiMergaAB binary, B is G7V. Binary. Combined mag., color. Cst? 7.8p. R ApsAB 4.74 G8V, 6.9 K4V, 151.505y, a = 4.904". Combined mag., colors. Masses 0.89 and 0.74 solar. Perturbation period 2.2y, a = 0.020" suspected; unresolved by speckle interferometry. Component C optical. BY? 4.52 - 4.67V, 10.137d. B, 10.8v at 13", CPM. 6.8 F4IV, 7.5 G1IV, 215.4y, a = 1.09". Combined mag. Gamma Cas 5.02 - 5.44V. Amp. 0.03 on time scale 2d reported. H alpha varies. CPM? Combined mag., colors. KOCABAB 5.79 K4V, 7.93 M2V, q = 20.388" hyperbolic orbit. Component B is dM2. CPM. 2.9 - 2.95B. 6.3 A4V, 6.6 A6V, 339.3y, a = 0.93". Combined mag., colors. AB CPM. B is G8V. CPM. Companion M1. EA 4.92 - 5.90V, 2.32735297d, period may vary. Component A of quadruple system. Contact binary. Zuben ElakribiSR? 6.17 - 6.5p, 40?d. RR UMiAB CPM. Component C, 14v at 32" optical. CPM. Component B F4V. ADS 9447A, Alpha CV 6.33 - 6.41V, 0.6080722 or 0.741285 or 2.8881d. Magnetic field var. 0.7447d?, possibly irregular. BX BooNekkarSRb 3.20 - 3.46V, 20d. BrachiumLb? 6.38 - 6.46V. GM LupBinary with HR 5606. Colors for combined light. Blended mag. 3.88V. vsini for combined light. 5.3 F5V, var. G2V+G2V, 225.0y, a = 3.772". Combined mag., colors. Combined mass 2.1 solar. ADS 9494B, EW 6.5 - 7.10v, 0.2678160d. Period changes with orbital motion. Variation in light curve may be caused by mass transfer between close pair. Reddening at max. due to ADS 9494A. Component A may vary up to 0.09m. i BooSpectrum variable. Amp. 0.09V. Alpha CV 5.76 - 5.81V, 0.8775d. HR Lup4.6 B3V, 4.9 B3V, 72.88y, a = 0.422". Combined mag., colors. CPM. Companion A5. 6.7 A2V, 6.8 A1V, sep. 0.08", 8.0y, a = 0.10". Combined mag., colors. Unresolved by speckle interferometry. Both companions optical. IUE observations show a B8V companion 2.5 mag. fainter than primary. Optical pair with HR 5643. Lb 8.1 - 9.1p. Amp. 0.51V, 0.36(B-V). X TrACPM with HR 5647. See HR 5646. CPM. B is F8. Nearly same proper motion as HR 5646, 5647. Var? Amp. 0.015b. AP 5.1 B9IV, 5.6 B9V, 23.42y, a = 0.116", combined light, colors. Mean mass 5 solar. BC, 10.5, 11.2v sep. 1.9". A physical pair in orbital motion about AP at 58"; possibly quintuple system. ADS 9532A, Alpha CV?, 4.53 - 4.56V. Spectrum variable. Resolved by speckle interferometry 1986.45, sep. 0.51". Lb 5.79 - 6.02V. FL Ser7.1, 7.1v, sep. 0.03"; suspected SB, but duplicity doubtful. Binary. Companion 7.53V, +0.35(R-I), dG6. Component C, A5V, optical. Component B, RV -16k/s. CPM with HR 5664. CPM with the triple star HR 5661. Faint companion of HR 5664, G5V, probably optical. Component A of double, Ell?, amp. 0.08V. Suspected of being double. SKYLAB indicates cool star with hot companion. Companions: B, B9V; C, A-type spectrum. CPM. AB binary. C, 7.17V at 23" CPM. Described by Eratosthenes (ca. 200 B.C.) as brighter than Antares, by Ptolemy (ca. 150 A.D.) as equal to Antares. Zuben ElschemaliEB 5.49 - 6.0B, 2.164175d. Period 1.85 found for secondary min. GG LupAB binary. Some disagreement as to whether B or C, at 127" from A, is the brighter. MQ SerBeta C 3.21 - 3.24V, 0.16547d; 0.14273d also possible. Probable CPM. 5.1 B5, 5.5 F8, 778.54y, a = 2.384" or 269.90y, a = 2.485". Although a period has been derived, spectroscopic evidence indicates that the F8 component is a dwarf much closer to the Sun than the B5 star: probably optical. AB binary. Combined mag., colors. C, 9v at 27" probably optical. Var? Amp. 0.015b. CPM? Pherkad MinorSpectrum variable. AB 5.62 G1V, 5.89 G3V, 41.623y, a = 0.907". B is HR 5728. Colors for combined images. Mag. for blend 4.98V. Masses 0.95 and 0.94 solar. C, 13.4v at 58" optical; D, 11v at 215" probably optical. Blend of 5727/8, 4.94 - 5.02V. Uncertain which component is the variable. Companion K5IV. Gamma Cas 5.43 - 5.61V. If variable, period much longer than 180d. Probably binary with HR 5734, a close binary ADS 9626BC. Delta Sct? AlkaluropsBC 6.98 dG5, 7.63, 260.10y, a = 1.463". Combined mag., colors of BC. Mean mass BC, 0.52 solar. Delta Sct? Amp. 0.03V. Hydrogen and CaII variable. PherkadPossible nearby star on basis of spectroscopic parallax. Zeta1 Fl 32Ed AsichFirst astrometric binary discovered from parallax measurements, by K. Burns, 1931. Alpha CV 3.65 - 3.72V, 18.487d. Magnetic field and rotation same period. Variable H alpha. Amp., light, magnetic field, spectrum vary per. 10.5y. Possible secondary light period of 240d. NusakanB, 8.94V, +0.55(B-V), +0.07(U-B), F6V or G0V, CPM at 11.2". A, doubtful occultation double, mag. and color combined, sep. 0.03". BC 7.8, 8.0, combined F0V 54.3y, a = 0.225" or 57.32y, a = 0.245". This pair binary about component A at 9.3". Companion A5. Combined mag., colors. Companion resolved by speckle interferometry, sep. 0.040" on 1985.5. 3.5 B2IV-V, 3.6 B2IV-V, 147y, a = 0.59". Combined mag., colors. Component A is NSV 7134, 4.12V, amp. 0.7m. However, 1300 UBV observations on 57 nights (1984-6) revealed no variation over 0.06 mag. R-I also found at -0.16. Component B, the rarely seen companion, is NSV 7135, 5.5, 7.8v. Var? Amp. 0.015b. Companion B, K0V; C is optical. ADS 9704 AP, sep. 0.097", unresolved by speckle interferometry. Component B, 11.2v at 42", optical. Zuben ElakrabADS 9701, 3168y, a = 5.8432". Binary with HR 5789, blended mag., colors. Alphekka is the brightest star in [X/Corona Borealis]. It lies approximately 75 [G/light year]s distant and is about 45 times more [G/luminous] than our [G/Sun]. EA 2.21 - 2.32B, 17.359907d. Possibly also intrinsic var. ALPHEKKACPM. Binary with HR 5816. Binary with HR 5815. Combined mag. 5.79V. AB binary, B, 8.5 G8IV-V; C, 11.4 at 135". Companion 10.33V, +0.49(B-V), -0.01(U-B), F5V, CPM. Binary with HR 5833. Is 7.3 - 8.3p. AB 5.2 A1V, 5.3 AIV, 11.07y, a = 0.117". AB combined mag., color. Resolved by speckle interferometry 1986.45, sep. 0.05". Alpha CV 5.33 - 5.36V, 1.59584d. SrII same period. Magnetic field var. Period probably due to rotation of star spots. CPM. 4.08 A0IV, 5.51 A3V, 91.0y, a = 0.74". Combined mag., color. Delta Sct 3.80-3.86V, 0.030d. Mass 1.9 solar. Possibly beat period? CPM with HR 5851. Quintuple system of which E is brightest companion; B, 12.0V at 4"; others at 172" and 208". SR? Amp. 0.2V. ADS 9765B, optical. UNUKALHAIAB binary; C, 9.0 G0 at 51" fixed. Alpha CV 5.50 - 5.51V, 1.30488d. Beat period 4.2283d. BP BooSep. 0.097". AB, CPM. B, 9.72V, +0.84(B-V), +0.68(U-B), K3V, CPM. C, 10.7v at 201". Also CPM with BD+15d2906 at 1642", itself a double, 8.4, 10.5v sep. 6". Component B, K0V. Third component optical. R CB 5.8 - 14.8v. The prototype star, discovered by Pigott in 1795. R CrBComponents white and orange-red. Amp. 0.07V. B, 10.5v at 1.08"; C, 9.1 at 45"; D, 8.7 at 48". Amp. 0.07V. Binary. Delta Sct? CPM. Combined mag., color. Suspected occultation double. Amp. 0.03V on time scale 2 hrs. suspected. 1.45937d. Magnetic field variable 1.45955d (Landstreet et al. 1979, MNRAS, 188, 609). V927 ScoVariable intrinsic polarization observed Aug. 1974. Binary. Companion G8V, optical. Delta Sct 6.20 - 6.23V, about 0.250d. FP SerCompanion F5V, optical. High space velocity. Binary with HR 5926. Mag. and color for combined light, 4.585V, +0.09(B-V), +0.07(U-B). Binary with HR 5925. Suspected occultation double. Old disk population runaway star. Companions optical? Beta C?, 5.84 - 5.87V, 0.2872d. Spectrum var. Balmer emission and metallic absorption vary in period about 30 yrs; H alpha profile varies in period of =<1 min. A potassium flare observed June 21, 1965. Probable mass-transfer between components. CDelta 6.06 - 6.81V, 6.32344d. Possible blue companion. S TrAGamma Cas 4.79 - 4.96V. Variable polarization. R-I also found at -0.13. FX LibSmall amp. in y. 0.492d or 0.976d. Also spectrum var. V913 ScoPrimary is SB, 3.4, 6.4v sep. 0.0003"; third component, ADS 9862B, 12.2v at 50". vsini both A and B =<100k/s. Component B, F4V, optical. Component B, 12.6v at 2", CPM. Possible X-ray source 3U1555+27. AB binary. Companion A5Vp. Possible quadruple system: SB 3.0, 5.0v, sep. 0.00001", 3.3v at 0.1", and 4.9v at 0.186". DschubbaComponent B optical. Delta Sct 4.95 - 5.00V, 0.063d. CL DraAB 5.3 A5V, 5.5 A6V, 26.93y, a = 0.366". C, 7.5v at 11". Combined mag., colors. Companion optical. Alpha CV?, 4.96 - 5.08V. Binary with HR 5978, q.v. CPM with HR 5985 = ADS 9913C, at 14" and with B, 5.9v at 0.5", possibly SB. Lunar occultations and speckle interferometry indicate companions 4.2v at 0.001" from A and 7.6v at 0.129" from C. Occultations by Jupiter and Io in 1971 indicate complex system. Component C occulted by Io revealed the 2.5 mag. fainter companion at 0.1". GraffiasCPM with HR 5984, q.v. Spectrum var., amp. 0.03V, 1.49187d. V929 ScoAB binary, B, 9.2v at 1"; C, 10.4 at 29" fixed; and D, 10.8 at 53" optical. Amp. 0.02(b-y). CPM with HR 6000 at 44". CD, 7.1, 11.7v, sep. 1.3". 6.97 - 7.71V, about 30d, variability attributed to circumstellar dust. Possibly a binary shell star with mass exchange. Considerable confusion between HR 5999 and 6000 particularly as to which is the variable and which the brighter. Originally announced as HR 6000, V856 Sco is really HR 5999, the southern preceding and fainter component C of the bright double. The error stems from interchanged photometric data in Harvard Annals 45, 197, 1901, all other early visual and photographic estimates indicating that the S. prec. component is the fainter. V856 ScoCPM with HR 5999. Component B, 13v at 298". Not the variable. Originally confused with HR 5999. CPM. Components K0.5IIIab and F4III. Optical pair with HR 6009. MarfikOptical pair with HR 6008. Amp. 0.04V. FS SerCPM. Physical pair with HR 6021. Lb? 4.66 - 4.87V. Physical pair with HR 6020. Amp. 0.13V. Alpha CV?, 4.23 - 4.27V, amp. 0.015U, 7.832d, symmetric light curve. ADS 9951A is SB, 4.9, 6.9v, sep. 0.0003". AB, binary. Component B, 6.9v at 1". Components CD at 41" = HR 6026, q.v. HR 6026, q.v. JabbahBinary, companion F3V. A5, F1. Binary. Lb? 5.58 - 5.83V, 7.1 - 7.31p. LQ HerAB binary. C, 10.5v at 78". Sep. 0.090". Companion, 10.73V, +0.58(B-V), +0.08(U-V), F8IV:, CPM. Sep. 0.03". Amp. 0.10V. Yed PriorOptical. CDelta 6.12 - 6.77V, 9.75411d. Period changes. Possibly blue companion. S NorBinary with HR 6063, q.v. A4, A7. Yed PosteriorCompanion, F9V, CPM. Small amp. in V. MgII 4481 appears to vary. B, 8.26V, +0.25(B-V), -0.23(U-B), B9.5V at 20", optical; vsini : 54k/s. The visual primary is triple: SB, 3.3, 5.3v, sep. 0.0005" and 5.5v at 0.49", discovered by occultation. Beta C 2.94 - 3.06B. Multiple periods, 0.2468429, 0.239671, 8.2, and 33.1d. Surrounded by HII region. Primary period varies in period of 23.2y with an amp. of 0.7 sec. Occultations indicate the variable has a 2.2 mag. fainter companion at 0".49. The duplicity had been suspected from occultations as early as 1860. Orbital period probably over 112 yrs. UV observations indicate temperature varies by 2510K and ratio max. to min. radius by 1.095. AlniyatCPM. Lb 6.8 - 7.5p. AT DraCPM. ADS 10010AB, 6700y. 3.85 - 3.90V. Amp. 0.07V. ADS 10022B, 9.58v, optical. Components also classified B9.5V(n) and A1V(n). Sep. 0.098". Binary with HR 6105. Mag. and colors for combined light, 5.41V, +0.59(B-V), +0.12(U-B). Visual companion, 9.76V, +0.87(B-V), +0.43, G7IV:. See HR 6112. Companion 7.46v B9V, CPM, possibly binary with the SB. B, 12.0v at 2" CPM; C optical. Alpha CV, amp. 0.08V, 2.951d, double wave light curve. Also rapid var. 0.15d. KajamGamma Cas 4.18 - 5.0V. Long term variation in emission lines. Variable polarization. R-I also found at +0.09 and +0.11. E, amp. 0.017V, 2.144202d. DQ DraHigh space velocity. SRb 5.0 - 5.38V. V2105 OphComponent B of visual double, 7.0 - >11.0v. Binary. Companion gG7. Gamma Cas 5.29 - 5.41V. QU NorADS 10058A, var. suspect NSV 7713; ADS 10058B, var. suspect NSV 7712, 8.8v, dK2, amp. about 2v. This bright red supergiant star has a diameter of 600 million miles (1,000 million km), making it almost 700 times larger than our [G/Sun]. This star is in its final stages of life. Once it has used up all the fuel in its core, Antares, will explode in a [G/supernova] explosion. What's left of the star will form either a [G/pulsar] or a [G/black hole]. Antares is 135 [G/light year]s away. Var. M1Ib, 5.5 B2.5V, 878y, a = 2.90", masses 15.5 and 7.0 solar. Companion is radio source. SKYLAB confirms cool star, hot companion. ADS 10074A, SRc 0.88 - 1.8V, 1733d. Possibly considerably fainter before 150 A.D.: see HR 5685. ANTARESAB binary. Components A (F5V) and B both optical. Spectrum variable? SRb 4.3 - 6.3v, 5.7 - 7.2p, 89.2d. Also slow var. of about 875d and aperiodic superposed cycles 5 - 15d. g HerVisual companion probably optical. KornephorosAB 4.16 A1V, 5.22 A4V. 129.87y, a = 0.970" or 126.78y, a = 0.95", combined mag., colors. Component C, 11.0v, 120" CPM. MarficAlpha CV, 4.45 - 4.51V, 1.79 or 4.67d. Alpha Cyg? 4.87 - 4.98V. 4.82 - 4.85V. Amp. 0.08V. V918 ScoSep. 0.067". Noted as double by speckle interferometry in 1971-2, unresolved at Mayall 4-meter in 1976. Spectrum double-lined. Resolved by speckle observations 1986.45 (Blazit et al. 1987, A&AS, 71, 57). Companion A2V, CPM; vsini 80k/s. Amp. 0.04: at wavelength 4530; 0.02: at 6585. Rotation period from starspots, 11d. V2133 OphCPM. COPERNICUS observations of CO indicate a SN remnant near Zeta Oph which may have caused Zeta Oph to become a runaway star. Gamma Cas 2.56 - 2.58V. Spectrum var.: UV spectra in 1972 indicated mass outflow probably related to formation of shell. Evidence disappeared in 1974. H alpha in absorption 1971, emission 1973. Rotational period 19.7 hrs. Alpha CV, amp. 0.03U, 0.02B, 0.01V, 1.45876d. V773 HerSep. AB, 0.102". About 6d. Spectrum variable. CPM with HR 6185. Binary with HR 6185, q.v. AB binary, 5.6, 9.0v sep. 1.6". C = HD 150135, O7:, CPM. Binary with HR 6195. Component B is speckle binary, sep. 0.145". Component C, optical. A companion 0.145" from B discovered by speckle interferometry. Binary with HR 6194, q.v. Optical. Amp. 0.05v, 3.76d. LP TrACPM with HR 6209 at 96". CPM with HR 6206. ADS 10157AB, 2.90 F9IV, 5.53 G7V, 34.49y, a = 1.355". ADS 10157A*, 10.5y, a = 0.08". ADS 10157A is var. suspect NSV 7915. Secondary A5V, optical. ADS 10173AB, binary. E?, amp. 0.03V. Companion questioned. Alpha CV, 5.21 - 5.27V, amp. 0.04U, 1.31159d. V776 HerSecondary = GC 22634, 6.47V A8m. Primary, fast rotation, not Am. EB 6.1 - 7.00v, 0.6614261d. Period varies. Contact binary. Temperature discontinuity at interface. All photometric indices variable. Four-color measures by Gronbech and Olsen give +0.129(b-y), +0.184(m1), +0.887(c1), 2.810(beta) from 3 observations. V1010 OphLb 5.83 - 6.03V. V636 HerLong per? CPM with HR 6252 at 346". EB 2.80 - 3.08B, 1.44026907d. Semi-detached system. 6.51 - 6.61V, HeI, NII 4097 var. 3.5d. V919 Sco5.5 - 5.54V. CPM with 6247 at 346". BC 9.0, 9.1, 56.75y, a = 0.267". AxBC physical. ADS 10227A, Alpha CV 4.78 - 4.83V, 3.8567d. K line varies, 3.88d. V637 HerAmp. 0.14V. Component F, 7.3v O6, vsini 125k/s. 6.29 - 6.34V, 2.631? or 6.28 or 6.85d. V900 ScoAmp. 0.09V. Variations in HeI, NII, OII suggest turbulent outer layers. Innes and IDS data on components and number of components appear inconsistent. Probably different cluster components measured. AB, CPM. V823 Her3.6 - 3.64V. Companion F4p. Either runaway, or P Cyg type with extended expanding atmosphere. Amp. 0.07V. Amp. 0.04V. Time scale of 1d suspected. Third component 14v at 20". EB 6.07 - 6.69V, 7.84818d. V861 ScoDelta Sct 6.32 - 6.36V, 0.11505449d. V644 HerCPM. AC, CPM. C, 12.5v at 93". 6.7 A3V, 6.9 A4V, 37.9y, a = 0.181". Combined mag., colors. Lb? 3.14 - 3.20V, 4.1 - 5.0p. Possible nearby star on basis of spectroscopic parallax. Gamma Cas 6.11 - 6.20V, time scale 1d suspected. V828 AraSuspected occultation double. A8, F3, sep. 0.107". Delta Sct?, 4.85 - 4.91V. All companions optical. B is A8V, C is F5V. 7.1 F1V, 7.3, sep. 1.02", 577.85y, a = 1.183". EA 4.22 - 4.28V, 39.4809d. Fixed sep. ADS 10310A, Alpha CV 6.26 - 6.34V, 6.00925d. Spectrum, magnetic field, RV, same period. Rotation 6.0087d. V451 HerE amp. 0.35V, 34.8269:d. V923 ScoBinary. H alpha profile variable. Component B of system with HR 6341. B, 11.0v at 1.5" CPM. ADS 10323B, 10 - 11.3v? Amp. 0.03 or 0.04y. Cycle of 8d in 1984 consistent with var. in Ca II emission. V2213 OphOld disk population runaway star. Optical. CPM. 6.7 - 6.9p. Optical. 6.2 A1V, 8.2 F3V, 137y, a = 0.415". Optical. Binary with HR 6370, q.v., B* 3.2y, a = 0.026"; or 7.4y, a = 0.013", 0.2 solar mass. (Some uncertainty if unseen astrometric companion is A* or B*.) AB 6.2 A9III-IV, 6.2 A9III-IV, 8.159y, a = 0.116". Mean mass 2.7 solar. Alternate orbit, 16.08y, a = 0.167". Combined colors. Speckle interferometry indicates companion 1 mag. fainter than primary at 0.079". However, speckle observations 1986.46 (at 7000 Ang.) give sep. 0.15". AB 3.0 A2V, 3.5 A3V, 88y, a = 0.86". Combined mag., colors. SabikDelta Sct? The visual companion is optical. A companion at 0.168" has been discovered by speckle interferometry. Ellipsoidal binary, 6.118 - 6.195V, 80d orbital period. V829 AraDelta Sct 6.19 - 6.23V. Period analyses of new and existing data by Reed and Welch (1988, AJ, 95, 1510) favor fundamental period of 0.088d with overtones of 0.052, 0.130d, with the fundamental and second values as radial pulsations and the third as nonradial. V620 HerComponent B, 10.42V, +0.52(B-V); component C, 11.40V, +1.55(B-V). Amp. 0.15V. V915 ScoAldhibahEmission lines variable? H alpha width and profile vary. Sep. 0.108". Speckle observations 1986.45 give 0.14". AB, CPM. Binary with HR 6402, q.v. CPM with CoD-26d12036, 6.34v K5V at 700", same parallax. CPM. AB, 3600y, a = 4.68". Component B is HR 6407. Combined colors. Combined mag. 3.08V. Mass A, 14 solar. Other components faint, optical. Circumstellar lines around both A, B. ADS 10418A. Discovered by W. Herschel in 1795. SRc 3.0 - 4.0v. 6-yr. period superimposed by variations 50 - 155d. Surrounded by envelope of 2x10E+05 solar radii, expanding 10k/s, mass loss 3x10E-08 solar masses/y. RASALGETHIADS 10424B, dG4, optical. SarinSep. 0.121". B is dG0, optical. ADS 10428A, EA 5.84 - 6.56V, 1.67734617d. Period changes. i 86.57d. Components 5.3 and 4.6 Suns. U OphAB 5.53 G8V, 8.65 M0V, 693.24y, a = 10.415", or 2205y, a = 23.90". Various published orbits range from 242 to 2205y. Combined mag., colors. Companion is F2V. Amp. 0.04V on time scale 3 hrs. and 0.05 on time scale 1d suspected. Sep. 0.108". Binary with HR 6425. Binary with HR 6424. AB 6.1 K3V, 7.6 K5V, 42.177y, a = 1.734" or 42.09y, a = 1.82", combined mag., colors. Component C, 9.9v M2, 32" physical. D, 12.8v at 15". Amp. 0.04. Binary. Combined mag., colors, sep. 0.200". Binary. ADS 10449A, EA 4.69 - 5.37V, 2.0510270d. i 75.9d. Semi-detached system. Polarization measures indicate light from primary reflected on photosphere of secondary. u HerDelta Sct 6.50 - 6.52V, 0.1874472d, secondary 0.1449461d. V2112 OphAB binary; A3, A6. C, 11.7v at 12" CPM. CPM. SRd? 6.28 - 6.32V, about 170d. VW DraCompanion G5III, optical. Gamma Cas? 5.22 - 5.25V on time scale of fraction of a day. Lb? 4.9 - 5.1v, amp. 0.16p. V656 HerBeta C 3.25 - 3.31V, multi-periodic 0.140531 and others ranging from 0.0464 to 0.1399d. B not CPM; optical. Amp. 0.4V. Possibly CPM and same RV as HR 6462, 50'N. Component B, A7V; C is optical. Recognized as triple system by speckle interferometry: single star G5IV and close pair of which the brighter component is F7V eclipsing, sep. 0.045". E, amp. 0.085V, 2.2299d. Also long period var. outside eclipse, amp. 0.04V, 83.2d; probably the rotation period of the G5IV component. V819 HerAB binary. Combined mag., colors. Component C, 7.6v at 103". Delta Sct? Fixed sep. Companion A6V, optical. Binary with HR 6485, q.v. Another companion with sep. 0.29" seen on 1981.47 (McAlister and Hartkopf). Unresolved on 1985.25 (Bonneau et al.). B, 14.0v at 15"; C, 12.5 at 37". dF7, CPM, sep. 0.100". Measured sep. 0.069" on 1985.5 by speckle interferometry. F0V, CPM. Lb 5.98 - 6.21V. V640 HerCompanion K0III, optical. LesathCompanion K0IV, optical. 2.76 - 2.90V. ADS 10583B, 8.5 - 11.0v. 6.00 G8IV-V, 6.10 G8IV-V, 46.4y, a = 1.02". Combined mag., colors. V949 ScoSep. 0.098". Seen double 1911 and 1923, elongated 1918, single 1957 and 1959, and unresolved by speckle interferometry 1976. MaasymBeta C 1.59 - 1.65V, 0.2137015d, secondary 0.1068518d, beat period 10.1605d. Also possible 0.04V eclipse. X-ray flare observed in vicinity Lambda Sco on 1 June 1975. SHAULAComponent B, B9V; C, B8V. Central star of open cluster NGC 6383, probably older than the rest of the cluster core and might have initiated star formation in the core and beyond. Ell?, 5.68 - 5.71V. RastabanSRb 6.41 - 6.56V, about 12d. V642 HerAlpha CV, amp. 0.041V, 9.74073d. Variability and physical parameters discussed by North (1987, A&AS, 69, 371). V2125 OphComponent B, 7.81V, +0.30(B-V), +0.05(U-B), A8IV, vsini 129k/s. Fixed sep. from A. 1.90 - 1.94V? SargasBinary with HR 6555. ADS 10628B, I, 4.84 - 4.91V. Binary with HR 6554. ADS 10628A, I?, 4.83 - 4.95V. KumaA* 2.08 A5III, 8.5y, a = 0.065". Resolved by speckle interferometry. Delta Sct? RASALHAGUECompanion, 9.53V, +0.36(B-V), -0.02(U-B), F6IV-V, CPM. Measured sep. 0.140" on 1985.5 by speckle interferometry. Delta Sct? Visual companion optical. Delta Sct?, 3.52 - 3.54V. 7.3 F5, 7.6, 101.3y, a = 0.653". Combined mag., colors. Delta Sct? AB 5.34 G0V, 7.95 K3V, 76.00y, a = 1.52". Combined mag., colors. Third component 10v dM1 at 740" CPM. Component B, F4IV CPM. Lb 6.2 - 6.57V. V626 AraBeta C 2.39 - 2.42V, 0.1998303d, 0.205430, 7.3316, 0.189512 and 2.591d. Delta Sct 4.20 - 4.26V, 0.053d. Beta C?, amp. 0.01V. Component B, F4V CPM. Suspected occultation double. AB 5.58 F4V, 11.1, 122.68y, a = 1.004". Component C, 12.8v at 155" CPM. Sep. 0.02", but duplicity uncertain. Visual companion CPM. Sep. 0.111". Possibly close double. CebalraiDelta Sct? CPM with HR 6610. Combined colors. Mag. for blend 5.59V. CPM with HR 6609. Visual companion ADS 10749B, optical. EA 6.18 - 6.36V, 3.894977d. V624 Her7.1 B9, 7.3, 34.00y, a = 0.157". Combined mag., color. CDelta 4.24 - 4.84V, 7.01225d. X Sgr6.27 - 6.39V. Amp. 0.05V on time scale 3 hrs and 0.08 on time scale 1d suspected. V3894 SgrEA 5.66 - 6.18V, 3.169128d. V539 AraBC 10.3 dM4, 10.8, 43.20y, a = 1.360". This close pair forms a wider physical binary with component A. Component B, 9.70V, +0.75(B-V), +0.19(U-B), F5V, binary. Component C mag. diff 5.36v at 70" from A. V826 HerBinary. CPM with HR 6637, not shared with components C,D. DsibanCPM with HR 6636. Companion A0IV. Fixed sep. SX Ari, amp. 0.05V, 1.658d. Spectrum variable. V957 Sco6.9, 6.9v, 160.759y, a = 0.37". Binary. Delta Cep 5.87 - 6.46V, 17.12413d, period varies. Atypical light curve. Possibly SB. Y OphE? Amp. 0.26V. V906 ScoAmp. 0.04V. Possible periods 4.45597, 4.4588d (North 1984, A&AS, 55, 259). V951 ScoGamma Cas 6.65 - 6.94V, 86.7207d, similar to Pleione (HR 1180). Spectrum var. with possible periods 2.5552 and 0.78906d, correlated with RV. V744 HerAB binary. C, 13v at 28" and D, 10v at 95" both optical. Speckle interferometry sep. 0.102". ADS 10875. Not certain which component is the var. suspect. Rapid change in difference between components. AB CPM; C, 12v at 34" optical. Beta C 5.81 - 5.84V, 0.13989183d. Shortest period and lowest luminosity of type. Effective temperature varies by about 1000K. Ratio max. to min. radius 1.031. V2052 OphSRd 5.34 - 5.54V, 68:d. V441 HerGrumiumCompanion F0. Fixed with HR 6693. Possibly 5 yr. period in He 10830 emission. Sep. 0.107". Closed from 0.114" to 0.065" between 1981.5 and 1984.3 (McAlister and Hartkopf). However, speckle observations 1986.44 (Blazit et al. 1987, A&AS, 71, 57) yield 0.085". Possible nearby star on basis of spectroscopic parallax. SRb 5.85 - 6.73V, 7.7 - 8.3p, 120.5d. OP HerSuspected occultation double. Amp. 0.08V. He 10830 variable. ETAMINSRd? 4.38 - 4.48V, 29:d. However, more recent photoelectric observations cast doubt on variability. Alpha CV, amp. 0.008V, 0.719d (Manfroid and Mathys 1985, A&AS, 59, 429). Spectrum variable. V2126 OphGamma Cas 4.55 - 4.85V. Also rapid flares to amp. 1.8m possibly from later type companion. V2048 OphComponent B, 13.7v F? at 7", optical. AC fixed. C, 8.12V, -0.02(B-V), -0.57(U-B), B1V, vsini 130k/s. Alpha CV 6.44 - 6.52V, amp. 0.04U, 0.517468d. V771 HerBinary. ADS 10990B? 8.0 - 10.0v. Binary with 6729. AB 5.24 F2, 5.94 F3, 280.03y, a = 1.494". Component B is HR 6733. Color for combined light. Spectrum for combined light, F4IV. C, 11.28V, +0.78(B-V), +0.33(U-B) at 100", optical? AB CPM. C, 13v at 55" optical. 5.17 - 5.19B. Observations satisfy the SB period. V820 HerADS 11029A is speckle interferometric double, sep. 0.116". Visual companions, 13.5v at 33" and 13.5v at 48". ADS 11029A, CDelta 4.30 - 5.08V, 7.594710d. Period changes. Spectrum and magnetic field variable. One component of SB. Although HR 6742NashBeta C? 6.10 - 6.15V. Period varies from 0.284653 to 0.323d. V986 OphAB 5.7 A5V, 5.7 A5V, 191.23y, a = 1.063". Component B is HR 6750. Color for combined light. Combined mag. 4.95V. AB 4.20 K0V, 5.99 K4V, 88.13y, a = 4.545". B is 6.00V, +1.15(B-V), vsini =<25k/s. Aitken listed 9 additional faint companions within 180". Both companions optical. AB binary. B = HD 165474, 7.45V, +0.30(B-V), +0.17(U-B), A7pCrEu:Sr: or A8p (beta CrB), vsini 12k/s. ADS 11056B. Magnetic star; possible spectrum variable. Component B, B9V, optical? 5.1, 5.9, sep. 0.26", doubtful duplicity. Discordance in designations of components between ADS and IDS. We accept IDS. Component B, in notes to ADS 11076 not assigned letter: doubtful, sep. 0.1" if real. C, 14v at 25" CPM. D = ADS C, 11v at 54" optical. Visual companion is blue. EB 6.43 - 6.88V, 2.24815d. Mass transfer indicated. The var. is probably the 8.85V companion of the visual double. GCVS gives combined light. V3792 SgrAB 5.10 F7V, 8.50 K4V, 55.8y, a = 1.00". Optical. Gamma Cas 3.81 - 3.9B, 4.1 - 4.2p. Binary. Combined mag., colors. Component B is F0IV or F0V. Binary with HR 6782. Primary is speckle binary, sep. 0.106". Component C, 11v at 76". A companion to A at 0.106" discovered by speckle interferometry. Combined light of 6781-2 varies; uncertain which component the variable. Binary with HR 6781. Companion A6V, optical. YildunAB 6.07 F2V, 7.03, 270.0y, a = 1.16". Companion not confirmed. AB visual double, A4V, F0, combined mag., color. Third component found by lunar occultation, 1.3B, 0.9R fainter than B, sep. 0.024". Companion, 11.52V, +0.66(B-V), +0.11(U-B), F8V: Amp. 0.013v, 2.8855d. V4045 Sgr6.5 A, 7.2 F2, 3040y, a = 1.500". SX Ari, amp. 0.05V, 1.67d or 0.83d. V692 CrACPM. Binary with HR 6810. Binary with HR 6809. Faint component C at 221". ADS 11169A is SB, 4.1, 7.0v, sep. 0.011". Closest visual companion is B, 11.5v, B9III at 17"; C is 13.5v at 26"; D, 9.9v, B3; E, 9.4v, B2V, physical, vsini 184k/s. ADS 11169A, EA 3.79 - 3.92V, 180.45d. Also irregular changes in brightness. AB measured sep. 0.102" on 1985.5 by speckle interferometry. ADS 11149B, 8.5 - >11?v. Amp. 0.14B. V669 Her5.29 - 5.37V, correlated with H alpha emission. Companion A3V. Double may be spurious: companion not seen in 1934. Lb 3.08 - 3.12V. B, 9.68V at 39"; CD, 8.7, 10.2v, sep. 16.5". EA 6.0 - 6.9p, 2.4156832d. Period changes. Component A of visual double. RS SgrAmp. 0.10V. Companion A3V, optical? Three faint companions form compact group at about 95". Primary of visual double and a suspected astrometric binary. Optical. Kaus MeridionaliV4028 SgrCDelta 5.40 - 6.10V, 5.77335d. Y SgrADS 11271B, 12.08V, +1.08(B-V), +0.50(U-B). May have close fainter white dwarf companion. Amp. 0.01v, 6.3d. Weak variable magnetic field, 14.6d. V4050 Sgr6.11 - 6.14V. Emission variable 12 to over 22 yrs. KAUS AUSTRALISCompanion is A5:. 6.8 F6III, 7.0 A7IV, 240y, a = 0.59". Combined mag., colors. ADS 11320B, 12.9v at 17", CPM. ADS 11320A, I, 7.9 - 8.7p. AlathfarAB 6.5 A2V, 7.5 A4V, 775y, a = .90". Combined spectrum A5; component B, A8V:. Kaus BorealisOld disk population runaway star. 4.6 - 4.64V. AB physical. B is F5V, vsini =<54k/s. Component P, vsini 80:k/s. ADS 11353A, 4.9 - 5.9v. d Ser4.4, 6.1v, 271.7y, a = 0.392". Alpha CV, amp. 0.04V, 1.71646d. Same rotation period. AB binary with slow orbital motion. Combined mag., colors. B is A5p, vsini 80k/s. C, 7.1v F6V at 90" CPM. Some discordance whether B or C is the brighter. B, 12.6v at 6". Possibly CPM and common RV with HD 170051, 6.9v B5 at 185". Amp. 0.24V. A* 3.57 F7V, 0.768y, a = 0.124". Masses 1.5 and 1.1 Suns. Shortest known period for astrometric binary. Speckle interferometry indicates component A is binary, sep. about 0.1". B, 12v K1V at 149"; C, 13.5v at 10". Amp. 0.10V. Spectrum (Balmer emission lines) variable. V4031 SgrAmp. 0.012v, 2.21d. V432 SctAB, CPM. Primary is speckle binary, sep. 0.149". Component B, 11.8v, A7Vp; C, 12.8v, F5V, optical; D, 12.9v, F8V. A fifth companion at 0.149" from A discovered by speckle interferometry. Binary. CPM companion A0V. CDelta 6.34 - 7.08V, 6.744925d. May have blue companion. U SgrCPM with HR 6953. CPM with HR 6952. 0.945099d, amp. 0.03U. MV SerDelta Sct? Suspected binary probably single star. Companion optical. H-emission var. H-line widths vary in cycles of about 6 yrs. Amp. 0.10V. 6.3 G9III, 6.5 G7III, 210.9y, a = 0.416" or 190.8y, a = 0.418". Combined mag., colors. AB 6.8 G2V, 7.0 G2V, 292y, a = 1.358", or 3083y, a = 6.7811". AB 6.1 K0III, 6.1 G9III, 169.50y, a = 0.243" or 184.6y, a = 0.255". Component C, 8.8v at 26" physical. Hydrogen line widths vary in cycles of about 6 yrs. Amp. at 0.58 micrometers about 0.10m. Primary is speckle binary, sep. 0.141"; both ADS companions optical. Possible binary listed by D. W. Dunham, 6.5, 6.5, sep. 0.1". AB, fixed sep. Alpha CV?, 5.40 - 5.45V. AB 7.2 F9V, 7.3 F9V, sep. 0.13", 12.18y, a = 0.196". Measured sep. 0.141" on 1985.5 by speckle interferometry. Third component 14v, optical. Vega is the westernmost star of the Summer Triangle. It is the fifth brightest star in the sky and is approximately 25 [G/light year]s distant. It is over 2 1/2 times the diameter of the [G/Sun]. Companions in IDS optical. BD=+38d3231, 8.6v, 23' N. prec., may be CPM. Delta Sct -0.02 to +0.07V, 0.19d. VEGAAmp. 0.05V. Optical. Lc 5.80 - 6.35V, 7.3 - 7.8p. XY LyrCompanions probably optical. C at 108" may be brighter than B. Sep. 0.14" by Couteau; 0.175" by McAlister et al. from speckle interferometry. Component B, 10v, gK, optical. AC, CPM? A may be close binary, about 10d orbital period. ADS 11581A, Delta Sct 4.98 - 5.16B, 0.193770d, 0.11636d. Beat period 5.24774d. Other periods 0.095129, 0.186872, 0.838d. This "prototype" Delta Sct star is the least typical of its class. Component B, K0. Amp. 0.07V. Occultation double. SRb 6.05 - 6.58p, about 50d. V3879 SgrListed as double by Innes but probably not. AB fixed, B at 25", 8.05V, -0.05(B-V), -0.25(U-B), B8V, vsini 150k/s. AP, measured sep. 0.145 on 1985.5 by speckle interferometry. Duplicity questionable. 4.1, 4.1v, sep. 0.13", doubtful. Gamma Cas?, 5.00 - 5.05V. Amp. 0.15V. ADS 11640AB, >5600y. Both components close binaries. Speckle interferometry 1985.5 gives sep. Aa = 0.141"; Bb = 0.137". Alpha CV?, 5.04 - 5.05V. AB 5.00 A2n, 6.10 A4n, 1165.6y, a = 2.78". Binary with HR 7052 = B, and CPM with HR 7053-4 at 208". Combined mag. and colors for HR 7051-2 are 6.48V, +0.19(B-V), +0.04(U-B). See HR 7053. Fixed sep. ADS 11670A, I, 5.64 - 5.81V. CPM with HR 7057 = ADS 11639D. Other components optical. Delta Sct? CPM with HR 7056. Alpha CV 6.41 - 6.58V, 10.1353d or 9.975d; also spectrum, magnetic field, RV. V535 HerAB binary, B, Am, F3Vm, or Am(A5/F1/F2), RV +9.2k/s, vsini =<25k/s. C, 11.3v optical. All companions probably optical. Discovered by Pigott in 1795. RVa 4.45 - 8.20V, 140.05d, period varies. Variable He 10830 and Ti emission. Largest intrinsic polarization in UV at minimum light. Light and RV periods differ. R SctGamma Cas 3.4 - 4.3V. Suspected occultation double. 6.69 - 6.82V. Possible nearby star on basis of spectroscopic parallax. B, 12.5v at 23"; C, 8.14V, +1.05(B-V), +0.75(U-B), K0II-III. delta, epsilon in cycles of 3 yrs. Gamma Cas 5.68 - 5.99V, 6.696d; also about 2400d with amp. 0.2m. H alpha profile varies in period about 7d; H gamma, CX DraADS 11726A, SR 9.7 - >10.9p, 148.0d. S SctBinary, companion K3III-IV. B, 10.89V, +1.05(B-V), +0.76(U-B), at 35"; C is G0V. 5.98 - 5.98V. Cycles 7.5d? AB fixed. B is 8.6v, B7v; may be collapsed star; vsini 120k/s. E, 9.9v A8pSr or B9V at 67" optical? F, 9.9v A8-9V or or B9V at 86". A, B, E and F are CPM. ADS 11745A, EB 3.25 - 4.36V, 12.913834d. Period varies. Presumed disk around secondary. Also radio flare activity. Prototype Beta Lyrae type, discovered by Goodricke in 1874. SheliakCW 3.94 - 4.75V, 9.088d. Period changes. EB 6.12 - 6.30V. V822 HerAB fixed, combined mag., colors. C, 11.21V, +1.25(B-V), +1.20(U-B), at 28". Ain al RamiInterferometer measures indicate multiple star. NUNKIB is K3IIIp optical, vsini =<54k/s. C, 11.5v at 139" is receding from A. Alpha CV 5.25 - 5.41V, 3.6733d. Similar period for He-line intensities, magnetic field. V686 CrAC, 11v at 38" optical. SRc? 4.22 - 4.33V. Del2 LyrABC fixed. B, 10.2v at 2". C, 7.69V, -0.08(B-V), -0.28(U-B), variously classified B8V, B9.5IV, A2, F3. Binary with HR 7142. 4.59 - 4.72V. AlyaBinary with HR 7141. V828 HerHigh-velocity star. EW 4.74 - 5.00V, 0.5914264d. AB observed as single round image in 1974. Suspected occultation double, equal components. SRb 3.88 - 5.0V, 46.0d. R LyrHydrogen line widths vary in cycles of about 10 yrs. 6.6 F8V, 6.6 G0, 13.58y, a = 0.131". AB 5.36 G0V, 7.46 K1V, 61.203y, a = 1.24". Combined mag., color. Components C, D, optical. Suspected occultation double. Companion blue star? ADS 11884A, CDelta 5.18 - 5.68V, 4.470916d. Magnetic field. Possible blue companion. FF AqlBinary. B1, B9. Amp. 0.053B. Alpha CV 5.83 - 5.93V. Published periods of 6.05 and 9.78d probably spurious; nor does a more recent 6.5386d satisfy all observations. Period may be years. Abt and Golson found range 5.83 - 5.91V. Two isolated obs. of 5.93 and 5.94V, while other observers report intermediate values with amp. <0.015V. V1286 AqlCPM with HR 7170. Combined mag. 5.82V, -0.03(B-V). CPM with HR 7169. Both companions optical. Deneb el OkabB, 12.1v at 13", optical. SulafatCompanion 9.80V, +0.21(B-V), +0.07(U-B), A5V fixed. 6.9 A1V, 7.2 A3V, 259.07y, a = 0.601". Combined mag. AB CPM. B is G8V. AB 3.2 A2III, 3.4 A2V, 21.138y, a = 0.532". AscellaSuspected occultation double with equal components; combined mag., color. vsini of secondary 150k/s. AB CPM. B, 9.17V, +0.47(B-V), +0.09(U-B). Probable double, 7.1, 7.1v, sep. 0.05". Sep. 0.099". Consistently unresolved by speckle observations at five epochs between 1977.48 and 1981.47 (McAlister and Hartkopf). B, 10v at 44" optical. SRb 6.6 - 8.4v, 10.6 - >12.4p, 353d. Mean mag. varies in cycle of about 2270d. V AqlDelta Sct 6.58 - 6.62V. Period analyses of new and existing data by Reed and Welch (1988, AJ, 95, 1510) imply radial pulsations of 0.099d and 0.060d with no evidence of nonradial pulsations. LT VulEE DraCompanion gK4, optical. See HR 7226. Delta Sct, amp. 0.05V, 0.04B, 0.097d. Polaris AustraliAxBC binary, BC 9.2, 9.8, 138y, a = 0.195". Variable on short time scale with uncertain 0.33772d period. Manfroid and Mathys (1985, A&AS, 59, 429) also give possible 0.48773d period. Magnetic field not detected (Borra and Landstreet 1980, ApJS, 42, 421). Deneb el OkabCompanion A0V. E 5.02 - 5.06B, 1.30227d. Form of light curve possibly variable. Y AqlAmp. 0.2V. V4024 SgrAlfecca MeridianAB binary. Other companions probably optical. Resolved by speckle interferometry 1986.45, sep. 0.08". AB, combined mag., colors, sep. 0.093". Third component 6.0v at 0.4". Albaldah7.0 K3III, 7.2 K2III. Unresolved by speckle interferometry. Probably not double. AB binary, B is G5. Speckle interferometry indicates a fourth companion at 0.089" from A. Amp. 0.05V. V1762 Cyg6.1 A2N, 6.5, 157y, a = 0.56". Alpha CV 5.91 - 5.98V, amp. 0.03U, 0.03c1, 0.05m1, H-beta 0.015, 1.160898d. V471 LyrB, 8.0v at 0.7" CPM. C is G5. Companion optical. Alpha CV 5.06 - 5.16V, 1.73d. V1288 Aql5.5 F8V, 5.7 F9V, 18.75y, a = 0.153". Component A is SB, 6.2, 6.2v, sep. 0.001". Binary with HR 7294. C, 12.7v at 56" optical. Possibly high luminosity evolved helium star. RCB 6.0 - >15.0v. Also pulsations 38.454d, changing amplitude. Observations 1984-86 indicate semiregular pulsations of 33 to 40d, 6.13 - 6.78V, 0.38 - 0.76(B-V), -0.09 to +0.52(U-B). RY SgrB is A0, optical. AladfarBinary. Companion A1V. Suspected occultation double. AB binary. C, 10.1v at 48" from A; D at 50", mag. diff 5.54V. AB CPM, B is 9.07V, +0.14(B-V), -0.05(U-B), F8V or G0IV, optical? Speckle interferometry indicates a fourth companion at 0.051" from A. Delta Cep 5.99 - 6.35, 1.49078 or 1.49107d. Period variable. Also 1178.5 and 2655d. Amp. variable in 1063.5d. If Pop. I, shortest known classical Cepheid in Galaxy. V473 LyrNodus SecundusAB, CPM. AB binary. ADS 12287A, Beta C? 5.4 - 5.46v, 0.6096d. ES VulAB binary. C, 13.7v at 12" optical. EA 6.58 - 9.18V, 3.3806260d. Period varies irregularly. i 90d. Semi-detached system. U SgeNearby star suspected of variability from photometric discordances by different observers. Delta Sct 5.51 - 5.57V. Period analyses of new and existing data by Reed and Welch (1988, AJ, 95, 1510) indicate a possible change in pulsational modes during the last several years, with fundamental period of 0.146d and possible nonradial pulsations of 0.141, 0.183, and 0.091d. V1208 AqlB probably optical. Possible X-ray source 3U1915-05. Old disk population runaway star. CPM. Companion A5V; vsini 129k/s, optical? Arkab PriorComponent B, K2IV, RV -3; component C, G5:III, optical. Sep. 0.036". Questionable occultation double. Delta Sct 3.90 - 3.93V, 0.050d. Spectrum var. 8.115813d. EB 4.34 - 4.44p, 137.939d. Irregularities in light variation. Variable polarization, probably due to circumstellar dust. Arkab PosteriorRukbatOptical. 5.8 A8, 5.8 A6-F0, 10.8y, a = 0.123". Probable occultation double. Speckle interferometry 1985.5 gives sep. 0.081". Chi1 Fl 47AB, CPM. Unresolved by speckle interferometry 1986.46. Component A astrometric binary, A* 3.36 F0IV, 3.422y, a = 0.058"; unresolved by speckle interferometry. Delta Sct? Proper motion slightly variable? H alpha emission variable. Both companions optical. Components B-D are 40" to 90" from A. A new component at 0.181" found by speckle interferometry. Colors of B are +0.31(B-V), +0.16(U-B). Components B, 10.8v at 27"; C, 10.46V, +0.61(B-V), +0.08(U-B), at 73" and P, 14.5v at 26" all optical. Alpha CV, amp. 0.02U, 0.68674d. V1741 CygBinary. B, 8.69V, +0.86(B-V), +0.32(U-B), G1IV-V. AB fixed. C, 7v at 2", binary. ADS 12503A, CDelta 6.08 - 6.86V, 7.02393d. Period changes. U AqlSecondary K0. Anser (rarely usAmp. 0.1B. B, optical. Gamma Cas, amp. 0.12V, 0.8518d. Variation may be due to rotation and inhomogeneous distribution of brightness on disk. V923 AqlAmp. 0.015v, 2.92133d. PW TelLocated at the head of [X/Cygnus] the swan, Albireo is a unique binary star system that lies about 190 [G/light year]s away. One star in this system is a yellow star while the second star is a hotter, blue type star. 7270.2y, a = 62.90". Binary with HR 7418. vsini of B-type component of ADS 12540A 50:k/s. Component C, 11v at 50". Two additional components of A resolved by speckle interferometry: Aa 1981.70, sep. 0.42"; Ap 1978.41, sep. 0.12" and 1979.46, sep. <0.08". ALBIREOSee HR 7417. Unresolved by speckle interferometry 1981.47, sep. <0.03". E, amp. 0.13V, 4.62988d. V4089 SgrRS CVn. Amp. about 0.045V, 108.5707d. Variable H alpha emission. V1817 CygB and C optical. Primary of SB Delta Sct? Amp. 0.015V in about 10d. CPM. ADS 12654. Uncertain which component varies. Visual companion CPM. SRb?, amp. 0.18V, 40:d. V1743 CygFixed. Companion K0III. CDelta 6.78 - 7.51V, 7.990676d. U VulDelta Sct oscillations with periods 94.1 and 115.7 min. QQ TelAlsafiB is B8, optical. V4090 SgrAP, sep. 0.1" unresolved by speckle interferometry at eight epochs between 1976.45 and 1981.70 (McAlister and Hartkopf). AB CPM. B, 13v at 3". C, optical. Sep. 0.200". B, 12v K0Ve at 48" optical. C, 12v at 130". Rotational velocity of A 123k/s, of B 142k/s. ADS 12737A, EB 5.18 - 5.36B, 1.95026827d. i 71.7d. Spectra vary in period 1.950271d. CPM companion B3V. Primary is close double, combined colors. Mag. for blend 5.30V. Component B, 12.6v at 38" optical. C, 8.9 F8V at 46" physical. Amp. 0.09V. 1.188y, a = 0.026". Companions B and C optical. ShamA companion at 0.084" discovered by speckle interferometry. AB binary. EA 5.85 - 6.37V, 7.6407613d. V1143 CygCompanions probably optical. Speckle interferometry 1985.5 gives sep. 0.178". Primary of visual double, EA 5.93 - 6.05V, 2.513294d. Double unresolved in 1961 when period changed sharply. QS AqlSuspected visual double, but may be single. AB, fixed sep. Delta Sct 6.50 - 6.53V, 0.088d. V1276 CygBinary with HR 7504. Third component mag. diff 7.17V, sep. 70" from A. See HR 7503. E? Amp. 0.076V. PS VulLb 6.33 - 6.55V. B-V from +1.57 to 1.62. V1351 CygCDelta 6.44 - 7.22V, 3.8455473d. Period changes. SU CygHigh space velocity. SRb 7.8 - 8.6p, about 40d. V973 CygDelta Sct 6.04 - 6.06V, 0.080d. NZ PavTARAZEDAB 2.91 B9.5III, 6.33 F1V, 827.6y, a = 3.20". ADS 12880A is NSV 12381, 2.85 - 2.89V. Component B is NSV 12380, 6.5 ->8.5v. AB binary. B is 7.16V, +0.02(B-V), -0.07(U-B), B9.5V, vsini 250k/s. Component B, 8.56V, +0.05(B-V), +0.11(U-B), A2V at 39". AB binary. B is dK6. Component C, optical. ADS 12913AB and ADS 12889 (9.2, 9.4 dK5 sep. 3") at 792" are CPM and have same RV and parallax. ADS 12889, 259y, a = 2.27", mean mass 0.6 solar. ADS 12913B, 8.55 - 8.60V; difference between components varies from 1.9 to 3.3p. B, 13v at 3" binary with A. C, 14v at 10" binary with A. D, optical. Suspected visual double probably single image, composite spectrum. Secondary either B6 or A0V. Amp. 0.09p. Amp. 0.12V. 6.1, 11.9v sep. 2" in 1910, 1913, not seen as double in 1926, 1928, 1929. Probably single? AB, >3000y. AB 5.5 A1V, 6.2 A3V, 22.8y, a = 0.146". Masses 4.0, 2.0 solar. C, 8.7v at 8" physical. Speckle interferometry 1985.5 gives sep. 0.180". CPM with HR 7549. CPM with HR 7548. 7.2 F5V, 7.7 F7V, 156.52y, a = 0.624" or 157.21y, a = 0.607". Combined mag., colors. 6.44 - 6.50V. V1765 Cyg5.28 - 5.33V, 2445.2d. Revised period 2300d. Variable magnetic field and spectrum. V3961 SgrOptical. Gamma Cas? 6.33 - 6.52V. V1339 AqlAltair is the southernmost star of the Summer Triangle. The 12th brightest star in the sky, Altair is only 16 [G/light year]s from us. This star rotates extremely fast, once every 6 1/2 hours. For comparison, our [G/Sun] rotates once every 25-30 days. Component B optical. ALTAIRComponent B optical. AC, 13.8 dM4, 22" binary. Delta Sct 6.29 - 6.35V, 0.100d. CN DraDiscovered by Kirch in 1686. M 3.3 - 14.2v. Period changes: 1686-1842, 405.88d; subsequently 408.05d. Variable CO emission from circumstellar envelope and enhancement of shell at minimum light. Total visual absorption of shell = 2 mag. Variable SiO maser source. Appreciable reddening at ascending light. Amp. at 0.58 micrometers about 0.11m. H line widths vary in cycle about 15 yrs. Component B, optical. Lb 5.08 - 5.4v. V1509 CygEA 5.61 - 5.78V, 12.42612d. Period changes. V380 CygDiscovered by Pigott in 1784. CDelta 3.50 - 4.30V, 7.176641d. Period changes. Variable He 10830 in emission and absorption. Speckle interferometry indicates companion at 0.291", probably not the same as the SB or occultation binary. EA 6.48 - 7.51V, 1.18287511d. Period decreases about 0.49s/y. i 80.3d. Contact binary. Masses 2.2 and 1.2 solar, radii both about 2.2. V505 SgrComponent B = A3V. E?, 6.20 - 6.25V, amp. 0.06B, over 80d? Variable polarization. Expanding atmosphere. Alpha CV 5.61 - 5.67V, 224.5d. Also period for spectrum and magnetic field var. Rotation 226d. V1291 AqlI 6.4 - 6.52p. Variability suspected on basis of comparison stars, both of which are either variable or suspected of variability. Optical. BY Dra type predicted, but variability not yet detected. Binary, companion K5III (AJ, 82, 431, 1977). However, Buscombe points out that the companion is F6V and this is more consistent with the magnitude difference between the components, if physical. TylAmp. 0.05B. CPM with HR 7594. CPM with HR 7593. TerebellumOptical. Speckle interferometry 1985.5 gives sep. 0.173". Old disk population runaway star. Beta C? 6.26 - 6.30V, 0.3775d. V819 CygAB binary. B 12v dM3 at 13". ADS 13110A, amp. 0.05V. ALSHAINTerebellumCDelta 5.28 - 6.04V, 8.382173d. Period varies. Spectrum varies, F6Ib-G5Ib. S SgeAB CPM. B, 12v at 7". Other components optical. AB combined mag., colors. Sources differ on spectral class of component B from A7V to F4V. vsini of B, 120k/s. SRb 4.91 - 5.26V, about 80d. NU PavAmp. 0.07V. AB and AC binary. C, 9.0v Am(A2/A8/A8) at 3", physical. Lb? 5.27 - 5.57V, 7.0 - 7.24p. VZ SgeGamma Cas + Beta Cep, amp. 0.07V, 0.20:d. V1746 CygL? 4.45 - 4.61V. V3872 SgrAmp. 0.03V, 14.0d. NT VulSuspected occultation double. 3.52 - 3.65V. Companion 16.4pgM6, CPM. Discovered as double by W. Herschel; companion not rediscovered. SRd 6.18 - 6.55V, 28.49d. V1401 AqlLb?, 4.89 - 4.94V. Optical companion, +0.74(B-V), +0.34(U-B). Amp. 0.08B, about 26d. Mass loss 0.00005 solar masses/y. V1768 CygCPM. B, 13.2v at 12", optical. C, 12.5v at 40". AD CPM. B, 13.7v at 23"; C, 11.6v at 36". 5.36 - 5.41V. Binary. AB CPM. B, 11v dM5, sep. 6.6". Wroclaw contr. no. 16 gives mag. differences but no sep. for four components: AB 5.4v, AC 5.15, and AD 4.0. Possible misidentification? Discovered by John Herschel as simply double. Components C and D apparently first listed by van Albada at Lembang in 1958; only magnitudes and no separations were indicated. Precedes HR 7703: error in HR catalogue. AB binary. B, 8.7v at 13". C, optical. SX Ari 4.91 - 4.97V, 0.07d. Possibly also Gamma Cas type. H-line widths vary in cycles about 15 yrs. V1624 CygAmp. 0.3V, 0.09U, 16.82d. Magnetic var. Discordance as to which component has the peculiar spectrum usually attributed to A. However, on the basis of better spectrograms, Abt gives A = A0V, B = A0Vp(Sr,Cr st.,Ca wk.). S, 5.87 - 5.92V. Binary. AB CPM. Component D of ADS 13554 of which primary is HR 7735. Delta Sct? Delta Sct, 16.478d, amp. 0.07V. NU VulComponent C, 6.99V, -0.14(B-V), -0.58(U-B) B5V, vsini : 25k/s, at 107" fixed. AP probably single star. ADS 13554A, EA 3.77 - 3.88V, 3784.3d. Amp. varies strongly with wavelength. C = NSV 12931, 6.98V. B is K1III, optical, vsini =<54k/s. Delta Sct 4.94 - 4.97V, 0.031d. Lambda Boo-type star in Delta Sct instability strip. V1644 CygAB and AC both binary. C, 9v at 12". AB CPM, 680?y. 4.60 - 4.80V. Sudden brightening in 1982, amp. 0.18V. QR VulDelta Sct? E, amp. 0.367U, 0.142B, 0.052V, 0.031R, 0.010I, 249.099d; duration of primary eclipse <17d. QS VulCPM. See note for HR 7754. ADS 13632B, 14v at 44"; C, 9.6v K5III, at 45" physical, vsini =<54k/s. D, 14.3v at 29" from C. Prima GiediEA 3.90 - 4.14V, 1147.4d. Period varies. Light var. outside eclipse. The K component may be slightly intrinsically variable. V1488 CygIDS notes Alpha1 Cap = HR 7747 (ADS 13632, four components) as one of five components of Alpha2 Cap = HR 7754 = ADS 13645. Hence, we have recorded n = 9 for both. ADS 13645AB optical; BC 11.2, 11.5v, sep. 1.2" binary. Secunda GiediPossible radio source. SD 3 - 6v. Since 18th century, 4.6 - 5.6v. Shell star, Nova 1600. P CygComponent C, photometric spectral class A2IV, vsini 53k/s. Component B, 10.1V at 4.1". For component AB, Rakos and Mermilliod give 6.93V, +0.28(B-V), +0.24(U-B). However, other sources give the following V magnitudes: Comp. 1976 1978 1980 Preferred Gronbech and Oblak Ruffener Olsen AB 6.635 6.610 6.608 6.61 C 7.724 7.706 7.72 Colors converted from the uvby system (Gronbech and Olsen) are AB +0.13(B-V), +0.185(U-B); C +0.165(B-V), +0.14(U-B). AB binary. C, at 34", 11.11V, +0.19(B-V), -0.29(U-B), B7Vp:, vsini 340k/s. D at about 45", 11.17V, +0.19(B-V), -0.32(U-B), B8Vp:, physical, vsini 279k/s. Primary is speckle binary, sep. 0.047". Amp. 0.06V. CPM. AlshatDelta Sct? Complex system with HR 7776, CPM at 205". ADS 13717A is occultation double, 6.2 - 8.3v, sep. 0.8"; also 7.2, 7.2v, sep. 0.05". Component B, 10.2v, A1, binary with A at 0.9". A is astrometric binary. The close occultation pair is questioned; it has not been confirmed by speckle interferometry. Complex system with HR 7775, q.v. Component B, vsini 97k/s. Occultations indicate component A is multiple system: 4.0, 4.3v sep. 0.0002", 4.8v at 0.022" and 6.7v at 0.0001". A also suspected astrometric binary, 3.07 F8V. Possibly also two faint 13v components at 112" discovered by John Herschel. DabihAmp. 0.05V. Variability agrees with spectroscopic period. V1773 CygAB binary. B is dF3. AB 6.33 A2V, 8.87 F6V, 69.86y, a = 0.2766" or 90y, a = 0.214". Component C, 9.2v at 3" also binary with AB. Alpha CV, amp. 0.04V, 8.5304d. Variable spectrum 1.132854d. V1584 CygAB binary. Combined mag., colors. BC, 9.2, 10.2v sep. 17.6". PeacockADS 12214, 18.75y, a = 0.153". EA amp. 0.15V, 5.298036d. DE DraNo physical relation between the radio components and the star. No demonstrable connection between Gamma Cyg and the so-called Gamma Cygni supernova remnant. SadrAB binary. B, 11v at 1.3". C and D optical. ADS 13786B, 8.5 - 11.0V. Discordances as to which component is B, which C. IDS gives B, 13.1v at 17.1". Lb, amp. 0.25B. AC DraCPM. 6.6 K2IV-V, 7.8 K1V, 232.76y, a = 1.225". Amp. 0.04V, pulsating. AB CPM. Probable spectrum variable. 7.1 A3V, 7.4 A5V, 83.72y, a = 0.172". AB binary. B, 8.0v at 0.8". CPM. Secondary, A2V, vsini 75k/s. Omega CygCPM with HR 7830. CPM with HR 7829. AB binary. Also observed as occultation double, 6.6, 7.4v, sep. 0.1". BC 7.5, 7.6v, Am, measured sep. 0.108" on 1985.5 by speckle interferometry, vsini 63k/s. A, optical, with companion, measured sep. 1985.5 Aa = 0.341" by speckle interferometry. B component 8.5v, frequently invisible. Component B, 12.9v A5V at 18", optical. AB, CPM. B, 11.3v at 3". Binary. B is A2. Deneb DulfimDelta Sct amp. 0.03V, 0.11d. CPM. Companion G5V. AB sep. 0.1", no magnitudes cited. Both 2 micron IR and UV sources. Alpha CV 5.16 - 5.22V, 20.2728d. Also period of spectral changes and magnetic field. Var. in K-line profile suggests star spot rotation. Rotation period 20.2754d. AF DraAB 4.0 F5IV, 4.9 F5IV, 26.65y, a = 0.475" or 26.60y, a = 0.480". Speckle interferometry gives sep. 0.58" and with SB data leads to masses 2.2 and 1.8 solar. Combined mag., colors. Components C-E optical. RotanevOptical. Double with HR 7887 at 181". Third component 12.9v at 71". High space velocity. SRb 5.79 - 6.9v, 59.7d. Amp. 0.36V, 0.12(B-V), 0.19(U-B), but varies. EU DelDouble with HR 7885. AB 5.8 B6III, 6.3 B6IV, 200y, a = 0.31". Visual third component 13v at 159". Occultation fourth companion, 9.3V, sep. 0.052". Tau1 Fl 13 and TH alpha varies. AB optical. B, 11.8v at 29". AC CPM, C is K2IV. Both companions optical. AB optical. B, 13v at 7". Companions optical. SualocinB is BD+80d662, 8.71V, +0.63(B-V), +0.00(U-B), F8V, CPM. AB binary. C, 8.5v A0 at 69" CPM. Delta Sct? Binary. AB binary. Deneb is the easternmost star in the Summer Triangle. It is a blue/white supergiant star that is 60,000 times more [G/luminous] than our [G/Sun], although it is only 25 times more massive. It lies 1,600 [G/light year]s away. Alpha Cyg 1.21 - 1.29V. Change in H:H epsilon. No emission recorded before 1944. DENEBGamma Cas 6.40 - 6.68V. V568 CygDelta Sct 4.39 - 4.49V, 0.135547 and 0.154991d. Combined magnitude of two components. AB fixed. CDelta 5.85 - 6.91, 16.386332d. Period changes. X CygSRb 7.6 - 8.9p, 110d or 160 - 180d. Mean mag. varies in period 1100d. Amp. 0.26V, 0.04(B-V), 0.19(U-B). U Del3249y, a = 13.813". Binary with HR 7948. See HR 7947. AB optical. C, 13v at 78" CPM. Gienah CygniAlbaliLb 4.41 - 4.45V. EN AqrADS 14293. Uncertain which component varies. B-A changes by up to 3v. B is BD+57d2241, optical. CastulaAB CPM. B, 10.03V, +1.27(B-V), +0.66(U-B). C, 13v at 14" optical. ADS 14290A, Lb? 4.91 - 4.96V. T CygSee HR 7959. AB 4.85 B5V, 6.07 B7V, 391.30y, a = 0.777". Combined colors. Mag. of blend 4.52V. Component C, 9v K2III-IV at 84", optical; vsini =<54k/s. Resolved by speckle interferometry 1986.45, sep. 0.87". Companion optical. Optical. Alpha Cyg 4.81 - 4.87V, no clear periodicity. Small variations in polarization have been observed, 2.0 to 2.6%. V1661 CygB8V+A3V. CPM. AB 6.4 F5V, 7.22 F8V, 187y, a = 0.855". Mag., colors for combined light. Old disk population runaway star. In Schurig's Atlas this is mistakenly labelled 58 Cyg for 56 Cyg. CDelta 5.44 - 6.06V, 4.435572d. T VulCPM. G8III-IV + G2.5IV. Delta Sct 6.55 - 6.58V, 0.054d. Per. and amp. may vary. EM AqrBeta C 6.2 - 6.43p, 0.20104071d. Sudden period change in 1972. 1924-70 per. increased 0.037s/y. BW VulFixed sep. Binary. Optical. AB fixed sep. B, 11.8v at 36". AB, CPM. H alpha profile variable. Possibly binary star. EB 5.95 - 6.25V, 1.575531d. Also Delta Sct amp. 0.1V, 0.12d. DV AqrBinary. Alpha CV, amp. 0.050V, 2.25d. AO CapAB 6.0 F5IV, 6.3 F7IV, 101.485y, a = 0.647". Combined mag., colors. Component C, 7.2v G0V at 11", CPM. 6.3 A5V, 7.6 F4V, 52.5y, a = 0.27". AB binary. CPM? Companion K0IV. AB CPM. B, 9.38V, +0.22(B-V), +0.04(U-B) A8III, vsini 97k/s. Component C, 12v at 26" optical. ADS 14526A, Gamma Cas 4.49 - 4.88V. Expanding circumstellar shell. Marked evidence of mass loss. Shell spectrum faded between 1973 and 1975. Metallic absorption lines disappeared. V832 CygSep. 0.110". 5.34 - 5.48V, probably eclipsing; same period as SB. V1931 CygAB 6.74 F5, 7.21, 3055y, a = 3.740". CPM with HR 8059. Duplicity of AB uncertain; sep. 0.110"? AB, combined mag., colors. CE optical. AB CPM. 9.1v A2 companion. CDelta 5.57 - 5.96V, 2.499215d. Period varies. DT CygAB 5.22 K5V, 6.04 K7V, 722y, a = 24.65". B is HR 8086. Aa x P, 4.9y, a = 0.014". Astrometric measures indicate 3 invisible companions, periods 6, 7 and 12y. Unresolved by speckle interferometry. Suspected planetary companion not substantiated. Proper motions for HR 8085 and 8086 taken from Luyten LHS. SAO has only one entry (component A?), but appears to give the mean position of A and B. 5.19 - 5.27V, 350 - 400d. V1803 CygSee HR 8085. ADS 14636B, Is, 6.02 - 6.09V. AB binary. B, 7.8v A0V or Am(A2.5/A7V/A9), vsini 80k/s. C, 9.2v K1III at 58" optical, vsini =<54k/s. ADS 14682A, 5.55 - 5.71V. Alternating periods of 1.12912 and 1.19328d. V 389 Cyg may be triple star, with long period about 150d, perhaps 110 or 270d. V389 CygAB binary, B, 11.6v at 2". C, 12.6v at 48" optical. ADS 14702A, Alpha CV 4.58 - 4.77V, 314d, 0 00868d. Magnetic field var. 1786d and 72y. Spectrum var. 72y. Fixed. Companion A4V. Delta Sct 6.41 - 6.48V, 0.097d. EW AqrCompanion B8V. AB fixed. B, 9.6v at 1.2". C, 7.29V, +1.55(B-V), +1.38(U-B), M5III, vsini =<25k/s. 6.5 A7V, 6.5 A7V, 17y, a = 0.11". Combined mag., color. White dwarf companion. 7.0 A7V, 7.0 A7V, 34.44y, a = 0.227". Combined mag., colors. Measured sep. 0.090" on 1985.5 by speckle interferometry. AB binary. B, 7v at 1". Amp. 0.045V. AB 5.2 F7V, 5.3 F7V, 5.70y, a = 0.26". Combined mag., colors. Component C, 9.5v at 48" optical. 6.44 - 6.50V. AB 3.82 F0IV, 6.42 G1V, 49.80y, a = 0.85". Components C, 13v at 29" and P, 12v at 72", both optical. Q, 12v at 90", physical. R, 13v at 90", CPM. Delta Sct 3.65 - 3.84V. 2-3 hrs.? Possibly variable period. Sep. 0.08". May be only single star. Kitalpha7.0 G2IV, 7.2 G2IV, 84.4y, a = 0.61". Combined mag., colors. Companion A7V or G0V. Old disk population runaway star. H alpha profile varies. SRb 7.7 - 9.4p, 320d. T IndAB CPM; 79000?y. Component B, 10.0v G8.5V, probably optical. 4.28 - 4.50V. AB binary. B is K4. Components D and E, 12v at 247" and 149" probably optical. Alpha CV 4.77 - 4.87V, 2.1215d. AB fixed. Ell?, 6.40 - 6.44V, 5.4d? 5.05 - 5.075V, 3.390d. V1809 CygSRb 8.6 - 10.3p, 233.3d. Y PavBinary, sep. 0.130", about 30y. Unresolved by speckle interferometry. Delta Cep 5.77 - 5.96V, 3.332816d. Uncertain which component of ADS 14859 is var. Perhaps Delta Sct type. V1334 CygADS 14858A, Delta Sct?, 2.41 - 2.47V. ALDERAMINAB binary. B is B3V. Variable shell spectrum. AB binary. Component B, G5IV. AB CPM. Companion K0V. Companions optical. Component B of which primary is HR 8193. Component A in system of which B is HR 8189. Other components 11.6, 13.4, 14.6v. ADS 14943A. All companions 10.5m or fainter. SRb 5.43 - 5.97V, about 50d. SX PavDelta Sct? V1934 CygADS 14969A. Companions optical. B 12.06V, +1.13(B-V), 33". C 10.38V, +0.46(B-V), -0.04(U-B), F5V, 54", vsini =<54k/s. Components B and C sometimes interchanged. Delta Sct amp. 0.01V, 0.044d. IK PegAlpha CV?, 5.20 - 5.30V, 0.726d. Amp. 0.06V. Optical. Both companions optical. SadalsuudADS 15032AB, 50y. B, 7.84V, +0.18(B-V), +0.06(U-B), A2.5V, vsini 60:k/s. Third component discovered by speckle interferometry, mag. diff about 4v. Sep. 0.025". Possible circumstellar material. ADS 15032A, Beta C 3.16 - 3.27V, 0.1904881d, modulation period 10.893d. SiIV and CIV vary. Satellite UV obs. indicate temp. varies 1340d, max./min. radius 1.038. AlfirkA* 3.76 K0III, 2.84y, a = 0.052". 6.7 A2V, 7.0 A4V, 173.9y, a = 0.293". Combined mag. A third component is suspected. Component A is SB, 5.0, 6.3v, 0.0047"; component B, 9.5v K1III-IV: at 68", physical, vsini =<54k/s. Gamma Cas 4.44 - 4.72V. Polarization variable. Slight variation in H alpha line width. SRb 6.8 - 8.9p, 131.1d; secondary period 235.3d. W CygCPM. Speckle interferometry indicates mag. diff 3.0, sep. 0.033"; D. W. Dunham gives 5.1, 7.1v, 0.07". AB CPM. B is 7.65V, +0.37(B-V), -0.01(U-B), F2V; vsini 30k/s. Delta Sct? Optical. Cst 6.4p. CP CygNashiraAlpha Cyg 4.69 - 4.78V. H alpha profile var. V337 CepBinary. Companion A3. AC fixed. C, 8.05V, +0.23(B-V), -0.68(U-B), B1.5V at 12", vsini 80k/s. AD also fixed. D, 8.03V, +0.20(B-V), -0.72(U-B), B2IV at 20", vsini 270k/s. In earlier sources C is brighter than D. Unlikely that this system is related to the X-ray source Cep X-4. AB binary. B, 10.5v at 3". Component C, optical. CPM. Suspected occultation double. Amp. 0.010V, 0.02B, 0.064d. CG OctSuspected occultation double. Lb 5.6 - 7.0v. Formerly called DS Peg, now in Cyg. V460 CygSRb 5.9 - 7.1v, 35?d. V1339 Cyg6.4 B9.5V, 6.6 A0V, 27.2y, a = 0.16". ADS 15251 8.3, 8.3, 11.9m at 2' may be member of same system. AzelfafageAB CPM. B is A0. AP, 5.6 11.0v sep. 1.5" binary. Enif represents the nose of [X/Pegasus]. This slightly reddish star is 540 [G/light year]s away and over 5,000 times more [G/luminous] than our [G/Sun]. ADS 15268AB optical. 0.7 - 3.5V. 1.7m flare 1972 Sept. 26-7; fainter than normal following night. ENIFAB 4.78 F4V, 6.09 G2V, 507.5y, a = 4.278". B is HR 8310. Combined colors. Mag. for blend 4.50V. Components C, D, optical. D, at 201" is ADS 15275, 6.9 A5, 13.3v sep. 16". Amp. 0.02V, 24.90d. Var. due to star spots? Period corresponds to period of rotation. Variable H and K emission indicates chromospheric activity. HN PegAB 4.7 F2IV, 5.0 F6IV, 11.558y, a = 0.255". ADS 15281C, 10.8v at 13.8" possibly in hyperbolic orbit about AB or is optical. ADS 15271A, SRc 3.43 - 5.1v, 730d; also a cycle of 4400d. Mean magnitude varies 13.5y. Correspondence between polarization and light. SRb 5.90 - 6.14V, about 25d. AG CapADS 15314A. Component A is SB, 3.2, 5.2v, 0.0018"; B, 15.8v, 69"; C 12.7v, 120". EA (possibly RS CVn type) 2.83 - 3.05V, 1.0227789d. Form of light curve varies. Deneb AlgediSep. 0.102". Alpha Cyg 4.25 - 4.35V, 7.6:d. 5.5 F2, 7.5, 29.0y, a = 0.396"; previous orbits 37.594y, a = 0.433" and 27.508y, a = 0.387". Delta Sct? Both components optical. Alpha CV, amp. 0.01V, 20.70d. Double wave curve. Amplitude var. V1619 CygI, amp. 0.4B. HO Peg6.6 F0IV, 6.7 F0IV, 27.5y, a = 0.240". Combined mag., color. Occultation third component 8.8v at 0.02"; AB, sep. 0.114" by Finsen, 0.090-0.093" by speckle interferometry. AB CPM. B is A1p Sr Si, vsini 60k/s. C, 13.2v at 55". ADS 15405A, Beta C?, 5.68 - 5.71V. Component B Am(A2/A6/F2). Optical. AB CPM. Companion F7V. Delta Sct 6.13 - 6.21V, 0.147825d; also 0.11983 and possibly 0.14129 and 0.2172d. BZ Gru5.1 F0IV, 5.1 F0IV, 6.094y, a = 0.127", or 12.242y, a = 0.160". Combined mag., colors. EA 6.11 - 6.36V, 1.464047d, amp. 0.20 in uvby system. Similar spectral types both components, vsini 70k/s and 50k/s. H alpha profile variable. Identified in BAA* var. M2Iab, B6IIe. Combined mag., colors. Absolute magnitudes based on astrometric and spectroscopic data are -4.0V for red component, -2.3 for the blue. EA 4.80 - 5.36V, 6.65 - 7.46p, 7430d. Also slow oscillations, amp. 0.15, per. 13.7y and amp. 0.03, per. 349d. Red observations indicate Sr amp. 0.4m, 58d. H alpha varies in 118.37d, period stable over 20y interval. This is probably the pulsation period of the red component. Amplitude varies in period 825d or more. The blue companion may be intrinsically variable. VV Cep also magnetic variable. VV CepCompanion HD 208971, 7.0, K5III-IV, probably optical. Component B, 7.2v, at 3.7" variously classified G2V, G2III:, K0III:; C 11.7v at 143". ADS 15562A, EA 6.37 - 6.78V, 0.9450132d. DX AqrSecondary of visual double, 8.6 - 11.0v? Optical pair? Gamma Cas 4.68 - 4.89V, 4.57 - 4.65p. Ell 5.56 - 5.66B, 3.070510d. Identifed as Mu AB CPM. V1942 CygHe 10830 possibly variable. SADALMELIKLb? 5.13 - 5.33V. MO CepAB 4.61 A3m, 6.5 F7V or F3III-IV, 3800y, a = 11.5". Aa, 2.254y, a = 0.073". Component B is HD 209791 = GC 30876, vsini =<25k/s. Component C, 12.7v at 97" optical. AlkurhahSRb 6.08 - 6.36V, 82:d. HT LacAB binary. ALNAIR0.05V, 2.25d. Amp. 0.08V, 2.1727d. V365 LacCompanions optical: B, 11.6v at 20"; C 10.79V, +1.08(B-V), +0.75(U-B). Optical. 6.3 - 7.7:v. Old disk population runaway star. Emission variable in period over 50y. EA 6.08 - 6.77V, RS CVn-type binary, 1.98319204d (period changes). Distortions in light curve possibly due to star spots or to gas streams. Strong radio flare activity. AR LacComponents B and C optical. Delta Sct? BahamPossible nearby star on basis of spectroscopic parallax. B and C optical. D, K0, CPM. Polarization variable in intervals of about a day. AB optical. CPM. Probably single. AB binary. B is F8V. SRb 4.58 - 5.30V, about 55d. Also called BO Oct. B, optical. CPM. Companion A3V. Delta Sct 4.15 - 4.20V, 0.04242 and 0.068073d. Period and amp. vary. AnchaA* 2.85 K3III, 11.5y, a = 0.049". AB binary. AB CPM. B, 10.7v A7V at 6"; C, F6IV, optical. Sep. 0.100". Optical. SadalachbiaAmp. 0.43V. Emission var. period about 8y. IN PegCompanion G0V. B-V for combined light +2.10. Since 1900 no relative motion of components observed. Component A of visual double, SRb 5.41 - 6.70V, about 150d. Visual companion is optical. ADS 15862A, Ell?, 4.53 - 4.56V. CPM. Suspected occultation double. Unresolved by speckle interferometry. AB binary. B, 9.2v at 2.5" in 1832; 0.296" by speckle interferometry on 1985.5. AB 6.6 A0, 6.6, 190y, a = 0.490". Measured sep. 0.121" on 1985.5 by speckle interferometry. Gamma Cas 4.42 - 4.70V. Variable magnitude, RV and emission lines due to slow rotation of line of apsides of rapidly rotating equatorial shell. Spectrum variable 0.087d. Variable polarization. CPM companion F5III, optical. See HR 8544. Colors for combined light. Mag. of blend 5.56V. AB binary. B is K4. Fixed. Binary with HR 8559, speckle interferometric sep. 1.672" (1982.38). B* 4.51, 12v, 25.5y, a = 0.072". Companion optical. B-V for combined light +1.57. Lb? 3.99 - 4.20V. Del2 Gru5.77 F5IV, 7.14 F7IV, 143.0y, a = 0.746" or 140.0y, a = 0.75". Combined mag., colors. B, 13v at 21" optical. AC CPM, C at 41", 6.30V, -0.03(B-V), -0.35(U-B), B7IV, RV -21k/s, vsini 135k/s. ADS 15987A, CDelta 3.48 - 4.34V, 5.366341d. Period varies. Prototype star Delta Cep, discovered by Goodricke in 1784. Blue companion ADS 15987C is also var. and SB. Ell 6.27 - 6.47V, 17.748d, double wave light curve; mean mag. varies. V350 LacCPM. Companion D G2? Photometric data (Oblak 1978, A&AS, 34, 453) give B A2V, 6.22V,; C F2V, 7.71V, +0.38(B-V); D F9V, 7.83V, +0.51(B-V), where MK types are estimated from uvby,beta photometry. ABD physical, C optical. Delta Sct 6.30 - 6.32v, 0.056d. GX PegOptical. Al Kalb al RaiL, 5.8 - 6.8v, period about 1y. AB 6.5 dF2, 7.0 A5, 225.6y, a = 0.78", or 785y, a = 2.042". Combined colors; combined mag. 6.01V. Combined spectrum A9III. AB, CPM. CPM. AB CPM. B is 6.46V, -0.14(B-V), -0.82(U-B), B2V, vsini 40k/s. All companions listed by Worley are more than 22" from A. A new companion at 0.042" discovered by speckle interferometry. ADS 16095A, 4-10y cycles. Emission var. period 16-18y. Probably single. SitulaDelta Sct 6.62 - 6.68V, 0.12477d; also possibly 0.09466 or 0.08646 or 0.07956d and 0.07697d. CC GruMeasured sep. 0.136" on 1985.5 by speckle interferometry. ADS 16130. Uncertain which component varies, B-A 0.5 - 1.8v. ABC CPM. BC 7.3v F6IV, 8.1v sep. 3". Optical. Companion 10.02V, +0.28(B-V), +0.3(U-B), A6III-IV, vsini 141k/s. Optical. AB, 6.4 F8, 7.4 F6, 28.0y, a = 0.17". Speckle interferometric sep. 0.184" on 1985.5153. Occultations indicate third fainter component: sep. 0.129", mag. diff 2.7v 9 Oct. 1973; single 3 Dec. 1973; and 0.065", mag. diff 1.0, 29 Sept. 1974. Possibly variable with high orbital motion? AB 6.26 G3V, 6.81 G8V, 20.93y, a = 0.30". Combined mag., colors. Perhaps invisible companion, period 15.8y. ADS 16173C, 11.6v at 72". Faint CPM, 14.9v at 4.5' N. prec. HomamBinary. B is M1. Primary of visual double, 5.97 - 6.02:V, 6.43 - 6.53p. Variability doubtful. Lc? 2.0 - 2.3V. 6.05 - 6.08V, variability doubtful. B, 9.2A3V, physical, vsini 89k/s. Beta C 5.16 - 5.28V, 0.1930924d. Six secondary periods reported, ranging from 0.095109 to 0.23583d. DD LacAB binary. B9, A7. A* 2.94 G2II-III, 2.23y, a = 0.022". Speckle interferometry measures range from unresolved to sep. 0.059". BC, 10.0, 10.0v sep. 0.2" at 90" from A, physical. ADS 16211A. MatarBC, 7.6, 9.5v sep. 0.15" binary and AxBC binary. Uncertain which component varies. AB binary. B is K2III. C, 12.5v at 11" optical. Fixed sep. CPM, companion G9V. AB binary. B 12v M1 at 12"; C, optical. Delta Sct?, amp. 0.01V, 0.052:d. AB optical. Delta Sct 6.16 - 6.19V, 0.087d. FM Aqr7.0 F2IV, 7.2 F3IV, 26.9y, a = 0.212". Combined mag., color. Old disk population runaway star. AB binary. B is dF5. A is astrometric binary, 4.3y. C is 10.2v at 111". EB 5.91 - 5.98V, 10.075d. Detached main sequence stars. V360 LacBinary, companion F5V. AB binary. B is G2IV. Combined mag., colors. CPM companion M4. Lb 3.70 - 3.80V. AB, CPM. B, 12.2v at 26". Tau1Amp. 0.16V. Out of phase with orbital period. IM PegMag., colors for combined light. Occultation double 6.7, 6.7v sep. 0.2"; speckle interferometry, sep. 0.076". Alpha CV, amp. 0.005V. Possible periods 0.724, 1.27, 3.40, 1.70d. HI AqrAB 5.8 A3VM, 7.8 F6V, 104.5y, a = 0.647", or 102.27y, a = 0.680". Component C, optical. SkatAmp. 0.2:V, 50:d. HR Peg120.0y, e 0.68, a 0.47", i 85d, mag. diff 2.0. ADS 16365B, 7.6v. CPM. Companion G3. CPM with HR 8728. BY 6.44 - 6.49V, 10d. TW PsAAB relative position of component unchanged in a century. Probably physical. B, 11.5v F0 at 27". C, F5IV, optical, vsini =<54k/s. ADS 16381A, Beta C, amp. 0.11B, 0.169170, 0.170770 and 0.181692d. Also EA, amp. 0.04V, 12.096816d. EN LacAmp. 0.06V. Fomalhaut is a bright, white star that lies only 22 [G/light year]s away. Its diameter is twice that of our [G/Sun] and it is 14 times more [G/luminous]. CPM with HR 8721. FOMALHAUTGamma Cas 5.22 - 5.48V, 5.0 - 5.3p; later observations 5.15 - 5.21V. Amp. variable. Periods at different times have varied from 0.7364 in 1951 to between 0.800 and 0.700d; more recent periods were a choice in 1980 between 0.725 and 0.418d; 0.711 in 1981 and then 0.722d. Also indications of long-term changes. Spectrum variable 2.4 - 10.8y. Spectrum also indicates atmospheric quasi-periodic pulsations of about 1d. Strong spectrum and color changes in 1978. EW LacSep. 0.02", but duplicity uncertain. Unresolved by speckle interferometry. AB 7.1 G2V, 7.3 G4V, 26.5y, a = 0.39". Combined mag. ADS 16417AB varies slightly. 6.1 F0V, 7.4 F6V, 270.13y, a = 0.815". Combined mag., colors. Delta Sct? Amp. 0.018V, pulsating. Radio source. One of the most luminous stars in the galaxy. Circumstellar gas shell. Circumstellar features observed in infrared. SRd 4.75 - 5.50V. Spectrum variable. Variable NII emission. Probable nonradial pulsations coupled with mass loss. Phase between V and B-V curves changed between 1980 and 1985, from half phase out of cycle to in phase. Cycles on time scale of about a year. Bimodal radial pulsation inferred (Sheffer and Lambert 1987, PASP, 99, 1277) from analysis of a decade of spectroscopic observations. As opposed to remarks on spectral type, the star appears to be getting bluer (IBVS 3170), implying an increase in temperature of 800 K over the past decade. V509 CasCPM. Gamma Cas?, 6.53 - 6.60V. Suspected occultation double. Separate speckle interferometric measures give sep. 0.05" (Aa) and 0.34" (AB). Ten years of observations reveal steady change in AB position angle of about 10d with decrease in separation from about 0.375" to 0.266". Component B identified as SB2 (see SB remarks), making total number of components at least 4. Gamma Cas 3.58 - 3.65V. Photometric investigations have indicated numerous periods, particularly 0.78823, 1.0815d and 1.5998398d, all doubtful. Form of light curve varies. Probably not an eclipsing binary. Period shell phenomena about 23.5y. Shell features have vanished several times since 1897. H gamma varies in 3.66?d. AB 5.1 A2, 8.8, 76.6y, a = 0.277". ADS 16467B, Delta Sct?, 8.7v. Cst? 5.11V. Fixed. Companion 9.88V, +0.08(B-V), -0.37(U-B), A1V. Amp. 0.02b, 35 min. LN AndAlpha CV, amp. 0.10u, 5.36d. Spectrum variable. V638 CasFum al SamakahLb 2.31 - 2.74V. SCHEATBinary questioned. Companion 9.47V, +0.09(B-V), -0.20(U-B), B9V. The star Markab makes up the southwest corner of the Great Square of [X/Pegasus]. It is 86 [G/light year]s distant. MARKABAB 6.2 F2Vn, 6.3 F2V, 21.84y, a = 0.200" or 22.0y, a = 0.20". Combined mag., colors. Component C, 84 Aqr, 7.6v K0 at 262", optical. Sep. 2.9" observed 1925; single in 1929. CPM. Combined mag., color. Companion F8V. Binary. ADS 16519. Uncertain which component varies, if either. Possible delta Sct type. Amp. 0.08V. Sep. 0.180". ADS 16550A, Lb? 5.0 - 5.16V. GZ PegAmp. 0.22V. AB 4.6 G2III, 6.6 F3V, 150y, a = 0.86". Combined mag., colors. Companion may be collapsed star. C, 8.14V, +0.15(B-V), -0.38(U-B), A, HD 218780. ADS 16556A. Astrometric binary unresolved by speckle interferometry. Amp. 0.02B. Probably optical. AB, CPM. BC, 10.0, 10.5v, K3V, 130y, a = 0.6", mean mass BC 0.35 solar. BC combined, 9.19V, +1.03(B-V), +0.93(U-B), CPM with A. Component C is a close double, equal components, showing orbital motion. Lb 4.9 - 5.25V, 6.5 - 6.8p. High space velocity? E, amp. 0.08V, 0.09B. Close to X-ray source 4U2316+61. V649 CasSuspected occultation double. AB, CPM. B, 13.0v at 8". Alpha CV 6.48 - 6.50V, larger amp. in U = 0.05, 0.617135d, 0.49925d. Other periods previously determined range from 0.44925 to 2.604d. Spectral line strengths vary but not in phase with orbital (SB) period. ET AndEB 6.0 - 6.16p, A7+A, 3.219565d. AN AndAB binary. ADS 16671B, 9.0 - >12?v. AB binary. B is K2V. Component A found double by speckle interferometry. CPM. AB 4.86 K0III, 7.13 F6V, 796.16y, a = 2.991". AB 6.04 F6III, 8.89V, +0.61(B-V), +0.08(U-B), G0V. AB CPM with C, 8.87v A3 at 17". Suspected occultation double. Delta Sct 4.60 - 4.62V, 0.05433d, secondary 0.04895d, beat period 0.4943d. SalmCPM. Amp. 0.14V. 5.6 A2V, 6.4 A7V, 63.16y, a = 0.420". Interferometer double. CPM. Companion A3III, vsini 129k/s. AB optical. Component A suspected occultation double. Alpha CV 4.91 - 4.96V, 0.58525:d. Period changes? Magnetic and spectrum variable, 0.5805d. Probably single star. Amp. 0.012V, 6.97d. HV PegAmp. 0.064v, 2.32d. Spectrum variable, especially SiII and SiIII. CG TucAB, 4.9, 9.3V, 1500y, sep. 1.1". CD, 8.2 A0Vn, 9.8v, sep. 1.6"; vsini of C, 210k/s. Component E, optical. ADS 16795A, EA 4.84 - 4.98V, 6.0663309d; i 90d. AR CasAmp. 0.06V. Alpha CV? 4.36 - 4.39V. Spectrum binary unresolved by speckle interferometry. 7.0 - 7.30p. HW Peg5.6 K4III, 5.7 K5III, 241.20y, a = 0.447". ADS 16836. Uncertain which component varies. Alpha CV 4.70 - 4.75V, about 12.5d. Magnetic variable. Duplicity questionable. Components K2.5IIIb and F9V. Confusion among RS 3.69 - 3.97V, 4.74 - 5.13B, 54.20d. Amp. and cycle length vary in period 3200d. Also 0.25m var. in period about 50d. H and K emission correlated with 56d light period. AB 6.3, 7.2v, 351.22y, a = 0.41". Ellipsoidal var, amp. 0.08B. Period consistent with SB. KS PegOptical. CPM. AlraiAB optical. Amp. 0.05(B-V). Delta Sct? Component B, CPM, A5Vep; however, the companion is optical. Amp. 0.05V. CPM, F6IV and G8V. 11813y, a = 14.21". Companion F2III or F2V, sources discordant; vsini 96k/s. Component A has composite spectrum but star unresolved by interferometer. vsini of G5 component <19:k/s, A0 component =<50k/s. Component B, 14.6v at 25"; C, 13.1v at 62". Lb 6.9 - 7.7p. TX PscADS 17006. Uncertain which component varies. AB binary. B, 11v at 4". C is HD 223340, G type. AC, CPM. AB 6.8 A0, 7.4v, 565.77y, a = 0.74". C, 8.6v at 50" optical. 0.9135 or 1.092d. Amp. 0.03u. V650 CasAB binary. B is cA0. Alpha Cyg 5.34 - 5.45V, =>46d. V566 CasRS CV, amp. 0.04V, 23.25d. OU AndLb? 5.74 - 6.0V. HH PegAlpha CV 5.16 - 5.21V, 3.730d. Variable magnetic field and spectrum. ET AqrAB binary. B, 12v M2 at 5". Delta Sct, amp. 0.01V, 0.06d. HT PegSep. 0.107". Companion F2V; vsini 43k/s. Components also classified A = Am(A1/A8V/F0), B = Am(A1/F1/F0). Possibly wide CPM pair with HR 9052. SRd 4.1 - 6.2v, periods about 110 and 1100d (1946 minimum lasted 320d). Rapid spectral variation from cF5 to M5p. Photoelectric observations since June 1986 indicate an amp. of only about 0.8V and 0.3(B-V). Rho CasLb 5.55 - 5.97V. XZ PscE 6.06-6.30V, B6, B9, 2.445094d. AL SclWide pair with HR 9045. E:/GS 5.9 - 6.3v, 13.4192d. Intrinsic variable which may be eclipsing. V373 CasCst? 6.6p. V CepE?, amp. 0.05V. 4.63 - 4.69V. ADS 17137B, 9.0 - 11.5V. Beta C? 6.4 - 6.46B, 0.310049 or 0.622832d. Spectrum variable. LQ AndAB binary, 5.0v B2III, 7.1v B3V. Binary with HR 9074, q.v. Probably single. Alpha CV 6.32 - 6.42V, 3.73975d, possible cyclical changes. Also magnetic field and spectrum period. Light var. also 2.1 hrs. Widths of hydrogen lines in about 35 min. SiII var. in per. 4.88643d. CG AndAB 5.84 G3V, 8.88 K6V, 26.386y, a = 0.803". A possible new companion found by speckle interferometry. Components C, D probably optical. C is K7V. Lb? 4.35 - 4.41V. YY PscADS 1B, 7.47V, +0.08(B-V), +0.05(U-B), A2Vn, vsini 275k/s, may be shell star. AB binary. C, 10.8m at 99" optical. I? Amp. 0.1B. V639 CasBinary. Amp. 0.02:V, 6.4322d. V567 CasThe [G/constellation] Andromeda is named for the mythical daughter of King [Y/Cepheus] and Queen [Y/Cassiopeia]. To save their kingdom, Andromeda's parents were told they must sacrifice their daughter to the sea monster, [Y/Cetus]. Andromeda was chained to the rocks by the sea to await her fate. Fortunately, [Y/Perseus], riding the winged horse [Y/Pegasus], flew over the kingdom. He saw the princess chained to the rocks and flew down to rescue her. In the sky, Andromeda is shaped like the capital letter "A" with her head at the point of the "A", her belt at the central line of the "A" and her feet at the base of the "A". Her brightest [G/star] is [W/Alpheratz], the star at the top of "A" and one of the stars in the Great Square of [Y/Pegasus]. Andromeda is best seen from October-December. "Must See" objects include: [F/Andromeda Galaxy]; [N/NGC 752], a star [G/cluster]. Antlia is a relatively modern [G/constellation]. It was added to the charts in 1752. This is a faint constellation, with no stars brighter than [G/magnitude] 4.2. Its brightest [G/star] is Alpha Antlia ([S/201405]). Antlia is best seen from April-June. Apus is a faint [G/constellation], with 5 of its 6 brightest stars reddish in color. The brightest [G/star] in Apus is Alpha Apodis ([S/257193]). This constellation is best seen from May-August in the southern hemisphere. The [G/constellation] Aquarius is associated with water in the mythology of many cultures, perhaps because Aquarius rises during autumn in the northern hemisphere - the rainy season for many countries. In Greek mythology, Aquarius caused a great flood that covered the Earth. To the Egyptians, Aquarius poured water into the Nile river each year, causing it to flood. The brightest [G/star] in Aquarius is Sadalsuud [S/145457]. Four stars make up the "Water Jar" of Aquarius: three stars forming a triangle with a fourth star in the center. Stars representing water are pouring from the jar. Aquarius is best seen from September-December. "Must See" objects include: [M/M2], a star [G/cluster]; the [F/Saturn Nebula], a [G/planetary nebula]; [F/Helix Nebula], a [G/planetary nebula]. In Greek mythology, Aquila was the eagle who served Zeus. Aquila carried the god's thunderbolts and delivered messages for him. In Chinese legends, the brightest [G/star] in Aquila, [W/Altair], represented one of two lovers in the tale of the herd boy and the weaving girl. Altair was the hard working herd boy, who fell in love with the weaving girl, a beautiful visitor from the stars. In the sky, three stars form the head of the eagle; Altair is the center star with a fainter star on each side. This [G/constellation] lies along the [G/Milky Way]. Look for dark lanes of dust (areas with fewer stars) in this region. Aquila is best seen from August-October. Ara is a modern [G/constellation] lying just below the curving tail of [Y/Scorpius]. Its brightest star is Beta Arae [S/244725]. Ara is best seen from July-September in the southern hemisphere. In Greek mythology, Aries was a ram with a beautiful golden fleece. This golden ram was identified with Zeus, the king of the gods. In Egyptian mythology, the celestial ram was thought to be Ammon, the Sun god. This faint [G/constellation] was identified with the bright Sun and shiny gold because of its location along the [G/zodiac]. Ancient people noted that when the [G/Sun] was in the constellation of Aries, this marked the beginning of spring and the growing season. Its brightest star is [W/Hamal]. Today, Aries is best seen from October-February. Auriga is a strange [G/constellation], representing a charioteer who is carrying a goat on his shoulder and holding three baby goats in his arms. The brightest [G/star] in Auriga is [W/Capella]. The three baby goats, also known as "The Kids," are represented by three stars forming a narrow triangle, just south of Capella. Auriga is best seen from January-March. "Must see" objects include: three galactic [G/cluster]s, [M/M36], [M/M37], and [M/M38]. Bootes was placed in the sky to guard the great bear, [Y/Ursa Major]. As a result, Bootes can be seen following the bear around the sky once a day. The brightest star in Bootes, [W/Arcturus], can be found by using stars in the [G/Big Dipper] to point the way. If you connect the three stars in the handle of the Dipper, this forms an arc. Follow this arc to Arcturus. Bootes is shaped like an ice cream cone, with Arcturus at the tip of the triangular cone. Two stars finish the cone and there is a small scoop of ice cream on top. Bootes is best seen from June-August. Caelum is a small, faint constellation with no [G/star]s brighter than [G/magnitude] 4.5. Its brightest star is Alpha Caeli [S/216926]. Caelum is best seen from January-February. Camelopardalis was added to the charts in 1690. There are no stars brighter than [G/magnitude] 4.0 in this area of the sky. There is also no easy-to-identify pattern. Its brightest [G/star] is Beta Camelopardalis [S/13351]. This constellation is [G/circumpolar], meaning it is visible year round from most of the northern hemisphere. It is best seen from December-February. Cancer is the faintest of all the [G/constellation]s of the [G/zodiac] and is best viewed under dark skies when the [G/Moon] is not visible. In Greek mythology, Cancer the crab lived in a swamp with the [Y/Hydra]. When [Y/Hercules] came to kill the Hydra, Cancer tried to save his friend by biting Hercules on the foot. Hercules merely killed the crab and brushed it aside. Cancer was given a place in the sky, to honor him for sacrificing his life for a friend. The brightest [G/star] in Cancer is Altarf [S/116569]. This constellation is best seen from March-May. "Must See" objects include: the [F/Praesepe] cluster. The brightest [G/star] in Canes Venatici is [W/Cor Caroli] and it represents one of two hunting dogs in this [G/constellation]. Cor Caroli (the Heart of Charles) was probably named after King Charles I of England, but this bright star is usually associated with the coronation of King Charles II in 1660. The second hunting dog is represented by Beta [S/44230]. This constellation is best seen from May-July. "Must See" objects include: [F/Whirlpool Galaxy]; [M/M3], a globular [G/cluster]; [M/M94], a spiral [G/galaxy]. Canis Major, lying next to the mighty hunter [Y/Orion], is sometimes known as Orion's hunting dog. Its brightest star, [W/Sirius], is also the brightest [G/star] in the night sky and has been worshipped and feared by many cultures. In the past, Sirius (also known as the Dog Star) rose and set with the Sun during the hottest days of summer, causing it to be blamed for the scorching summer heat. As a result, the phrase "Dog Days of Summer" can be associated with this [G/constellation]. Canis Major is best seen in the night sky from February-April. "Must See" objects include: [M/M41], a galactic [G/cluster]; [N/NGC 2362], a galactic [G/cluster]. Canis Minor is the smallest of [Y/Orion]'s two hunting dogs. The brightest [G/star] in this small [G/constellation] is [W/Procyon]. Procyon forms a triangle with two other bright winter stars, [W/Sirius] and [W/Betelgeuse]. Canis Minor is best seen from February-April. Capricornus is one of the older [G/constellation], although its origin as a half goat-half fish is not clear. According to one Greek myth, Capricornus was Aegipan, a half man, half goat whose father was Zeus. Once, while helping his father, Aegipan was pursued by Typhon, the monster god. To avoid Typhon, Aegian ran into a river. When he was waist-deep in the water, he changed the lower part of his body into a fish and swam to safety. Zeus placed Aegipan in the sky, as a way of thanking him for his help. The brightest [G/star] in this constellation is Deneb Algedi [S/164644]. Capricornus is best seen from September-November. Carina, originally part of the ancient [G/constellation] of Argo, the ship, is best seen from the southern hemisphere. Its brightest [G/star] is [W/Canopus], the second brightest star in the night sky. ([W/Sirius] is the brightest.) Carina is best seen from March-May. "Must See" objects include three galactic [G/cluster]s: [N/NGC 2516]; [N/NGC 3532]; [C/C102]. In Greek mythology, Queen Cassiopeia, along with her husband, King [Y/Cepheus] ruled over Ethiopia. Cassiopeia was very beautiful, but boastful and arrogant as well. She once boasted that she was even more beautiful than the sea nymphs. This claim angered the sea nymphs, whose beauty was legendary. They complained to Poseidon, the god of the sea, who sent [Y/Cetus], a sea monster, to destroy Ethiopia. Cassiopeia and Cepheus were forced to sacrifice their daughter, [Y/Andromeda] to save their kingdom. Fortunately, Andromeda was saved by [Y/Perseus] and [Y/Pegasus]. Cassiopeia sits on her throne in the sky, with her brightest stars forming a "W" or "M" shape, depending on the season. The brightest [G/star] is [W/SHEDIR] which lies at the lower right vertex of the "W". Because of her placement in the sky, half the time her royal throne is upside down. The queen must be chained to the chair so she won't fall out. This awkward position is part of her punishment for being so vain. Cassiopeia is a [G/circumpolar] constellation and can be seen most of the year. However, she is best seen from September to December. "Must See" objects include four galactic [G/cluster]s: [M/M103]; [N/NGC 457]; [N/NGC 7789]; [N/NGC 663]. In Greek mythology, Centaurus was the first of the Centaurs, a race of beings with the head, arms and chest of a man and the body of a horse. The brightest [G/star] in this [G/constellation] is Alpha Centauri, [S/252838]. It is also the closest star to our solar system. Alpha Centauri along with Agena [S/252582] make up the "Pointers", two bright stars that point the way to the [G/Southern Cross]. Centaurus is best seen from May-July in the southern hemisphere. "Must See" objects include: [F/Omega Centauri], a globular [G/cluster]; [F/Centaurus A], a peculiar [G/galaxy]. In Greek mythology, King Cepheus ruled over the country of Ethiopia with his beautiful, but vain, wife [Y/Cassiopeia]. Cepheus was forced to sacrifice his daughter [Y/Andromeda] to save his kingdom from [Y/Cetus] the sea monster. As fortune would have it, Andromeda was rescued by [Y/Perseus] and [Y/Pegasus] and the sea monster was killed. Peace was restored to the kingdom. The stars in this [G/constellation] form a box with a triangle sitting on top. The brightest [G/star] in Cepheus is [W/Alderamin]. This constellation is [G/circumpolar] and can be seen most of the year. However, it is best seen from September-December. "Must See" objects include: [N/NGC 188], a galactic [G/cluster]. Cetus, the sea monster, was sent to destroy the kingdom of King [Y/Cepheus] and Queen [Y/Cassiopeia]. But, before he could complete his task, he was killed by [Y/Perseus]. The brightest [G/star] in the [G/constellation] is [W/Diphda]. Cetus is best seen from October-December. "Must See" objects include: [W/Mira], a variable star. Chamaeleon was added to the charts in the early 1600's and is considered a modern [G/constellation]. It is small in size and shaped like an elongated diamond. Its brightest [G/star] is Alpha Chamaeleont [S/256496]. Chamaeleon is [G/circumpolar] and can be seen most of the year from the southern hemisphere. This small, narrow "V"-shaped [G/constellation] lies close to the "Pointers", the two brightest stars of [Y/Centaurus]. Circinus is a modern constellation, added to the charts in the mid 1700's. It contains a few relatively faint [G/star]s, the brightest of which is Alpha Circini [S/252853]. Circinus is best seen from July-September in the southern hemisphere. The brightest [G/star] in this [G/constellation] is Phact [S/196059]. Columba is best seen from January-March in the southern hemisphere. "Must See" objects include: [N/NGC 1851], a globular [G/cluster]. Coma Berenices was named after Berenices II who, along with her king, ruled Egypt around the year 230 BC. With the king at war, Berenices offered to sacrifice her long golden hair to the goddess Aphrodite to insure the safe return of her husband. When the war was over, the king returned safe and sound and Berenice kept her promise. She cut her hair and left the golden tresses on an alter as a gift to the goddess. The next morning, the tresses were gone. Local astronomers convinced the king and queen that the golden tresses had been transported into the sky where they would forever sparkle among the stars. Today, the [G/constellation] consists of a scattering of faint stars, most of which belong to an extremely large galactic [G/cluster] known as the [G/Coma Star Cluster]. The brightest star in this constellation is Diadem [S/100443]. Coma Berenices also contains a wide assortment of galaxies. Unfortunately, most are too faint to be seen with a small telescope. Coma Berenices is best seen from May-July. "Must See" objects include: [M/M53], a globular cluster. Corona Australis is shaped like a "C" and lies just below the "Teapot" of [Y/Sagittarius]. The brightest [G/star] in the [G/constellation] is Alfecca Meridiana [S/210990]. Corona Australis is best seen from August-October. In Greek mythology, the god Bacchus created a beautiful crown which he gave to his mortal wife. Upon her death, he placed the crown in the sky as a tribute to his wife's great kindness and beauty. To the Shawnee Indians, the stars of this [G/constellation] represent celestial sisters. The circle of stars is incomplete because one sister left the sky to marry a human. The stars in Corona Borealis are shaped like the letter "C". Its brightest star is [W/Alphekka]. This constellation is best seen from July-September. In Greek mythology, Corvus was the messenger raven for the god Apollo. One of raven's many tasks included bringing water to the god when he was thirsty. One day, Corvus was about to fill a goblet with water when he noticed a fruit tree in bloom. He decided to wait until the fruit was ripe so that he could have a snack before returning to Apollo. Corvus waited several days for the fruit to ripen. Finally, he ate his fill of the ripe, fresh fruit and started back to Mount Olympus. Along the way, he realized that Apollo might be angry with him for taking so long to fetch the water. Thinking fast, he swooped down and snatched a water serpent from the river. Then, when he returned the goblet of water to Apollo, Corvus explained that the water serpent had attacked him, causing him to be late. Apollo did not believe the raven's story and flung the raven, the goblet and the water serpent into the sky where they would not bother him again. Today, the raven, or Crow (Corvus), the goblet ([Y/Crater]), and the sea serpent ([Y/Hydra]) are all constellations. The brighter stars of Corvus form a lopsided rectangle in the sky. Its brightest [G/star] is Gienah [S/157176]. Corvus is best seen from April-June. In Greek mythology, Crater represented a water goblet which belonged to the god Apollo. [Y/Corvus] the crow used the goblet to gather water for the god when he was thirsty. Crater was caught in the middle of a fight when Corvus tried to lie to Apollo. In a fit of rage, Apollo flung both the crow and the goblet into the sky. To many cultures, Crater represented a cup, bowl, or some other type of container used to hold wine. The brightest star in Crater is Delta Crateris [S/156605]. Crater is best seen from April-June. Even though Crux is the smallest [G/constellation] in the sky, it contains some of the richest starfields of our [G/Milky Way] galaxy. Originally, Crux was part of the constellation [Y/Centaurus]. Today, its brightest stars appear in the shape of a cross. The brightest star in Crux is [W/Acrux], a fine double star system. Crux is best seen from April-June. "Must See" objects include: [F/Jewel Box] cluster; [F/Coal Sack] nebula. Cygnus, which is also known as the Northern Cross, lies along the hazy patch of light that makes up our [G/Milky Way] galaxy. One Greek myth tells how Cygnus represents Zeus, the king of the gods. Zeus once turned himself into a swan to seduce the lovely mortal woman, Leda. Leda then laid an egg and when the egg hatched, the beautiful Helen of Troy was born. Another myth tells that Cygnus was the best friend of Phaethon. Phaethon had discovered that his real father was Apollo, the Sun god. He went to visit Apollo and watched as his father drove the Sun's chariot across the sky once a day, bringing daylight to the world. Phaethon demanded that he be allowed to drive the chariot, and before Apollo could stop him, he grabbed the reins of the chariot and took off. The four fiery horses pulling the chariot went wild and Phaethon lost control. To save Earth from the runaway Sun chariot, Zeus was forced to fling a lightening bolt and killed Phaethon. Phaethon's body plunged to Earth and fell into the river [Y/Eridanus] while the horses safely returned the Sun's chariot to Apollo. Phaethon's friend, Cygnus, searched the river, but he never found his friend. He continued swimming back and forth, diving deep into the river's depths, reminding those who watched him of a swan. For his devotion to his friend, Cygnus was honored with a place in the sky. Today, he can be seen as the swan flying south along the [G/Milky Way]. The [G/star] at the tail of the swan is also the brightest star in the [G/constellation]. Its name is [W/Deneb]. Cygnus is best seen from August-November. "Must See" objects include: [W/Albireo], a double star; the [G/Milky Way]; [F/Cygnus X-1], a black hole. To many cultures, the stars in Delphinus represented a dolphin or porpoise. In one myth, a dolphin rescued a man about to be killed by pirates. The man had jumped overboard and the dolphin helped him back to shore. For his good deed, the dolphin was honored with his own place in the sky. Five stars in the shape of a diamond form the dolphin's body, with two stars trailing off the diamond, forming the dolphin's tail. The brightest [G/star] in Delphinus is Rotanev [S/106316]. This [G/constellation] is best seen from August-October. Dorado was added to the charts in the early 1600's and is considered a modern [G/constellation]. Its brightest [G/star] is Alpha Doradus [S/233564]. Dorado is best seen from December-February from the southern hemisphere. "Must See" objects include: The [F/Large Magellanic Cloud], a [G/galaxy], the [F/Tarantula Nebula], a nebula within the Large Magellanic Cloud. In Greek mythology, Draco was the dragon in charge of guarding the garden of Hera, the queen of the gods. Within the garden, there were trees on which grew golden apples. [Y/Hercules] had to steal these golden apples as one of his 12 labors. Before he could steal them, however, he had to kill Draco. Draco fought a mighty battle, but he was no match for Hercules. After his death, Hera gave Draco an honored place among the stars. Three stars forming the tail of the dragon lie between the [G/Big Dipper] and [G/Little Dipper]. From the tail, Draco curls around the Little Dipper like a backwards "S". Its head is made up of four stars in the shape of a lopsided square. The brightest star in Draco is [W/Etamin] and it, along with the entire constellation, is best seen from July-September. "Must See" objects include: [W/Thuban], a star which was the "North" star 4,800 years ago. The stars of this small [G/constellation] may once have been combined with the stars of [Y/Delphinus] to form a larger constellation. However, the two were divided into individual constellations somewhere around the second century BC. Today, Equuleus lies between Delphinus and the head of [Y/Pegasus]. Its brightest [G/star] is Kitalpha [S/126662]. This constellation is best seen from August-October. Eridanus, the river, meanders all over the sky. In Greek mythology, it was this river that the body of Phaethon plunged into after his foolish ride across the sky in the chariot of the Sun. (You may refer to the constellation [Y/Cygnus] for the entire story of Phaethon.) Eridanus begins with the star Zaurak [S/149283], which lies next to the star [W/Rigel] in the constellation of [Y/Orion]. From there, Eridanus wanders below [Y/Cetus], around [Y/Fornax], above [Y/Horologium] and finally comes to an end between [Y/Phoenix] and [Y/Hydrus]. Its brightest star, [W/Achernar], lies so far south that it can't be seen from Europe, Japan and most of the U.S. This [G/constellation] is best seen from December-February. This small, faint group of stars is a modern [G/constellation] that was added to the charts in the late 1700's. Fornax lies next to [Y/Eridanus] in the sky. Its brightest [G/star] is Fornacis [S/168373]. This constellation is best seen from December-February. The stars in Gemini have been referred to as the "Twins" by many cultures around the world, with each culture offering a different story about the celestial brothers. One Greek myth tells that the twins are sons of Zeus, the king of the gods, and a mortal woman, Leda. The twins are also associated with "St. Elmo's Fire", an electric glow seen around aircraft wings or a ship's rigging during stormy weather. [W/Pollux], the brightest [G/star] in this [G/constellation], and a faint companion star form the head of one twin. The second brightest star in the constellation, [W/Castor], along with a fainter companion, forms the head of the second twin, with the twins standing side by side in the sky. Gemini is best seen from January-April. "Must See" objects include: [M/M35], a galactic cluster. Grus is a modern [G/constellation], added to the charts in the early 1600's. It is also part of a group of constellations known as the Southern Birds. The other birds of the group are the [Y/Phoenix], [Y/Pavo] the peacock, and [Y/Tucana] the toucan. The brightest [G/star] in Grus is [W/Alnair], a hot blue star. The second brightest star, Beta, [S/231258] is a cooler, orange-colored star. Compare the two and try to detect the differences in color. Grus is best seen from September-November in the southern hemisphere. Hercules was the son of Zeus, the king of the gods, and a mortal woman, Alcmene. Even as a young child, Hercules possessed a tremendous strength. When he was 8 months old, he strangled 2 serpents that had been sent to his crib by Hera, the jealous wife of Zeus. Hera's jealousy was to haunt Hercules for most of his life. At one point, she caused him to go insane. During this time of madness, Hercules killed his wife and children. When he awoke from the insanity, he saw the horror of what he had done and was overcome with grief. He left his village and traveled to the Oracle of Delphi for advice. The oracle told him to travel to Tiryns where King Eurystheus would assign Hercules 12 difficult labors. If and when Hercules completed all the labors, he would be freed from his sins and raised to the rank of godhood. For many years, Hercules struggled to complete the 12 labors, each more difficult than the last. Some of his opponents can be found in the sky, including [Y/Leo], the lion; [Y/Hydra], the many-headed serpent; [Y/Cancer], the crab; and [Y/Draco], the dragon. After many years, he successfully completed the 12 labors. When Hercules died, the gods welcomed him to Mount Olympus, where he was granted godhood, just as the Oracle had foreseen. Today, Hercules can be found next to the head of Draco. Four stars make up the "Keystone", or body of the mighty warrior. The brightest [G/star] in the [G/constellation] is Kornephoros [S/84411]. Hercules is best seen from July-September. "Must See" objects include: two globular [G/cluster]s, [M/M13] and [M/M92]. This small, faint group of stars is considered a modern [G/constellation], added to the charts in the 1700's. Its brightest [G/star] is Alpha Horologii [S/216710]. Horologium is best seen from December-February in the southern hemisphere. Hydra is the largest [G/constellation] in the sky. Its stars snake across over one quarter of the heavens. This constellation figures prominently in two Greek myths. In one myth, Hydra was a many-headed monster who lived in a swamp, along with her only companion, [Y/Cancer] the crab. [Y/Hercules] was sent to kill the monster as one of his twelve labors. The two fought a tremendous battle. For every head Hercules chopped off, Hydra grew two more in its place. Finally, Hercules won and the gods placed the body of Hydra in the sky. In another myth, Hydra was an innocent water serpent who was scooped out of a river by [Y/Corvus] the crow. The brightest [G/star] in Hydra is [W/Alphard]. Because Hydra is such a long constellation, various parts of it can be seen beginning in March and stretching through August. "Must See" objects include: [M/M48], a galactic [G/cluster]; [M/M68], a globular cluster; [M/M83], a spiral [G/galaxy]. This modern [G/constellation] was added to the charts in the early 1600's. Its brightest [G/star] is Beta Hydri [S/255670]. This star is the closest bright star to the south [G/celestial pole], even though it is over 12^ away. Hydrus is a [G/circumpolar] constellation and can be seen most of the year in the southern hemisphere. However, it is best seen from December-January. Indus is a rather small, faint [G/constellation] which lies next to the brighter constellation of [Y/Grus]. Its brightest [G/star] is Alpha Indi [S/230300]. Indus is best seen from September-November in the southern hemisphere. Lacerta is a relatively modern [G/constellation], added to the charts in 1690. It is a small, faint group of stars not far from the constellation of [Y/Cygnus]. The brightest [G/star] in Lacerta is Alpha Lacertae [S/34542]. The lizard's head is made up of four stars in the shape of a diamond. A trail of faint stars coming off the diamond forms the lizard's body. Lacerta is best seen from September-November. In Greek mythology, Leo is associated with the Nemean lion, a fierce creature who came from the Moon. [Y/Hercules] was given the difficult task of killing the ferocious beast. The lion's hide was so tough, no weapon could pierce through it. Arrows that Hercules flung at the beast merely bounced off its chest. Abandoning his useless weapons, Hercules trapped the lion and used his own incredible strength to strangle the creature. The lion's body was then placed in the sky by Hera, the queen of the gods and an enemy of Hercules. The [G/constellation] of Leo has long been associated with the [G/Sun] and hot summer days because, for 4,000 years, the Sun rose in this area of sky on the Summer [G/Solstice], the first day of summer in the northern hemisphere. Today, because of the [G/precession] of the Earth, Leo rises with the Sun in late July and early August. In the sky, the head, mane and chest of the lion are represented by a pattern of stars in the shape of a sickle or backwards question mark. The [G/star] at the handle of the sickle, or the "period" of the question mark, represents the heart of the lion. This star, called [W/Regulus], is the brightest star in Leo. The lion's hindquarters are represented by a small triangle containing [W/Denebola], a bright star whose name means the "Tail of the Lion". Leo is best seen from March-June. "Must See" objects include: two spiral galaxies, [M/M65] and [M/M66]. Leo Minor was added to the charts in 1690. It is a small, faint [G/constellation] that lies between the scoop of the [G/Big Dipper] and the sickle of [Y/Leo]. Its brightest [G/star] is Praecipua [S/62297]. Leo Minor is best seen from March-May. This little hare lives a rather hectic life, positioned in the sky next to a big dog, [Y/Canis Major], and just below the feet of the mighty hunter, [Y/Orion]. Its brightest star is [W/Arneb]. Lepus is best seen from January-March. Of all the [G/constellation]s of the [G/zodiac], Libra is the only one that does not represent a living being. However, the name of its brightest star, Zuben Elschemali [S/140430] (which means the northern claw) indicates that this area of sky was once part of the constellation of [Y/Scorpius]. Libra is best seen from June-July. Lupus is one of the original 48 [G/constellation]s placed in the sky by the ancient astronomer, Ptolemy. It contains several bright [G/star]s, but no easy-to-identify pattern. Its brightest star is Alpha Lupi [S/225128]. Lupus is best seen from June-July. The faint [G/constellation] of Lynx was added to the charts in 1690. Its brightest [G/star] is Alpha Lyncis [S/61414]. Lynx is best seen from February-April. "Must See" objects include: [N/NGC 2419], a globular [G/cluster] In Greek mythology, Lyra represented a beautiful lyre which had been fashioned from an empty tortoise shell. Orpheus, the son of Apollo, inherited the lyre from his father. When Orpheus played the lyre, his music was so beautiful it was said to charm anyone who heard it. Orpheus fell in love and married the beautiful Eurydice. The two lovers were extremely happy, but soon after their marriage, Eurydice was poisoned by a snake and died. Orpheus' grief was overwhelming. He took his lyre to the edge of the Underworld, where all mortal souls go when they die. There, he played his music. The Lord of the Underworld was so touched by the mournful sounds, that he allowed Eurydice to return to the land of the living. There was one stipulation, however. Orpheus could not look at Eurydice until they had completely left the boundaries of the Underworld. As the two lovers made there way back to the surface, Orpheus tried his best not to look at his wife, but the temptation was too great. Just as they neared the boundary between the two worlds, he glanced in her direction. Even a glance was too much and Eurydice was pulled back into the Underworld, never to return. For the rest of his life, Orpheus grieved over the loss of his wife, playing mournful, beautiful music on his lyre. After his death, the gods immortalized his music by raising the lyre into the stars. In one Chinese legend, Lyra's brightest [G/star], [W/Vega], represents one of two lovers from the tale of the Herd Boy and the Weaving Girl. Vega was the Weaving Girl, who wove beautiful tapestries among the stars. An interesting note about Vega: due to the [G/precession] of Earth's rotation, Vega was the "north" star 12,000 years ago, and will be again in another 12,000 years. Lyra is best seen from June-September. "Must See" objects include: the [F/Ring Nebula], a planetary nebula; Epsilon Lyra ([S/67310]), a double/double star; [M/M56], a globular cluster. This small group of stars holds the record for being the faintest of all the [G/constellation]s in the sky. None of the [G/star]s within this group are brighter than [G/magnitude] 5. In fact, its brightest star, Alpha Mensae ([S/256274]) is only magnitude 5.1. Mensa is a [G/circumpolar] constellation and can be seen year round from the southern hemisphere. "Must See" objects include: a small portion of the [F/Large Magellanic Cloud] that extends into this constellation. Microscopium is a faint, modern [G/constellation], added to the charts in the 1750's. Its brightest star, Gamma Microscopii [S/212636] is only [G/magnitude] 4.7. Microscopium is best seen from September-October in the southern hemisphere. Monoceros was added to the charts in the mid 1600's. Although faint, this [G/constellation] is rather easy to find. Simply form a triangle with three bright neighboring stars, [W/Betelgeuse], [W/Sirius], and [W/Procyon]. The area inside the triangle is Monoceros. The light from the brightest [G/star], Beta Monocerotis [S/133316], is actually the combined light from three different stars, one of the best triple star systems in the sky. Monoceros is best seen from February-March. "Must See" objects include: the [F/Rosette Nebula]; [N/NGC 2264], a Christmas-Tree-shaped cluster and nebula; [M/M50], a galactic cluster. This [G/constellation] was first listed on the charts in the early 1600's as a Bee. It was transformed to a fly in the mid 1700's. Musca lies between [Y/Crux] and the south [G/celestial pole]. Its brightest [G/star] is Alpha Muscae [S/251974]. Musca is a circumpolar constellation and can be seen year round in the southern hemisphere. However, it is best seen at sunset during May-June. "Must See" objects include: two globular [G/cluster]s, [N/NGC 4833] and [N/NGC 4372]. Norma is a faint [G/constellation] that was added to the charts during the 1750's. It is best seen during July-August from the southern hemisphere. Its brightest [G/star] is Gamma Normae [S/243643]. "Must See" objects include: two galactic [G/cluster]s, [N/NGC 6067] and [N/NGC 6087]. The only claim to fame for this [G/constellation] is that it lies in the vicinity of the south [G/celestial pole]. In fact, one of its fainter [G/star]s, Sigma [S/258857], can be considered the South Star. Its brightest star is Nu Octantis [S/257948]. Octans is a [G/circumpolar] constellation and can be seen year round from the southern hemisphere. The legend most often connected with Ophiuchus involves a man named Asclepius, who eventually became the god of medicine. Asclepius once killed a snake that had crawled into his hut. Another snake entered the hut, carrying a strange herb in its mouth. It placed the herb in the mouth of the dead snake. Much to Asclepius' surprise, the first snake came back to life. Asclepius retrieved the strange, life-giving herb from the snake and began using it on humans. The healing power of this herb was great and news of Asclepius traveled quickly. He brought so many people back from the dead that Hades, the lord of the Underworld, complained to Zeus. Hades argued that if Asclepius kept bringing humans back from the dead, they would be essentially immortal. Only gods were supposed to be immortal. Hades convinced Zeus that if he allowed Asclepius to continue, the gods would lose their status among the humans. Zeus admired the skill and healing powers of Asclepius, but was forced to agree with Hades. He flung a lightning bolt and struck down the healer. To honor his skills, Zeus raised his body into the sky. Today, the symbol for medicine is a staff with a serpent wrapped around it, in honor of the snake who first found the healing herb. Ophiuchus is seen in the sky next to the constellation of [Y/Serpens], the serpent, or snake. The brightest [G/star] in Ophiuchus is [W/Rasalhague]. The [G/constellation] is best seen from July-August. "Must See" objects include: [F/Barnard's Star], the second closest star in the night sky; a wide variety of globular [G/cluster]s, including [M/M9]; [M/M10]; [M/M12]; [M/M14]; [M/M19]; [M/M62]. Orion has been associated with a mighty hunter in many cultures around the world. In Greek mythology, the hunter played a part in many different stories. In one story, Orion fell in love with Artemis, the goddess of the hunt. So great was their love for one another, that each began neglecting their duties so they could spend time together. Warned by her brother, Apollo, to return to her duties, Artemis refused and the animals under her care began to suffer. The Moon, without Artemis to guide it, was unable to rise. Apollo grew angry. One day, when Orion went for a swim in the ocean, Apollo surrounded the hunter with a cloak of light. Apollo then went to Artemis and challenged her that she couldn't hit the center of the patch of light with one of her arrows. Artemis accepted the challenge and her aim was true. The arrow pierced the very center of the patch of light and struck and killed Orion. When his body washed up on shore, with her arrow in his chest, Artemis realized what she had done. She gently placed Orion's body in the sky, where it would stand out among the other stars and where she could visit it every night as she drove her Moon chariot through the sky. In another myth, Orion boasted to Artemis that his skills as a warrior were so great, he could hunt down and kill all the animals on Earth. Artemis and Gaea, the Earth goddess, were alarmed by this claim. To protect her creatures, Gaea sent [Y/Scorpius], the scorpion, to kill Orion with a deadly sting. Orion fought and killed the scorpion, but before it died, Scorpius managed to prick the mighty giant once with its stinger. The scorpion's poison was so strong, Orion died instantly. The two enemies were placed at opposite points in the sky, so that as one rises in the east, the other sets in the west. This placement insures that the two rivals never get close enough to fight. Another story has Orion forever chasing the [F/Pleiades], the seven sisters. The ancient Egyptians worshipped Orion as the Sun god. In the sky, Orion forms an easy-to-identify pattern. The red supergiant [G/star], [W/Betelgeuse] forms one of Orion's shoulders. [W/Rigel], the brightest star in Orion, represents one of Orion's feet. Between Betelgeuse and Rigel lie the belt stars, three evenly-spaced stars of equal brightness. Hanging off of his belt is Orion's sword. Orion is best seen from January-March. "Must See" objects include: the [F/Great Orion Nebula]. This [G/constellation] was added to the charts in the early 1600's and represents a peacock, the favorite bird of Hera, the Queen of the Gods. Its brightest [G/star] is the Peacock Star, [S/13060], which lies closer to the constellation of [Y/Indus] than the majority of its own star group. Pavo is best seen from September-October in the southern hemisphere. "Must See" objects include: [N/NGC 6752], a globular cluster. In Greek mythology, Pegasus was the beautiful flying horse born from the blood of Medusa, the hideous Gorgon killed by [Y/Perseus]. With Perseus on his back, Pegasus flew around the country. Together, the two rescued the princess [Y/Andromeda] from [Y/Cetus], the sea monster sent to destroy her parent's kingdom. In the sky, the body of the flying horse is represented by four stars forming the "Great Square of Pegasus." The brightest star in the [G/constellation] is [W/Enif], which means "the nose" of the horse. Pegasus is best seen from September-November. "Must See" objects include: [M/M15], a globular cluster. Perseus was the heroic son of Zeus and the mortal woman Danae. At the request of his mother, Perseus set out to kill the hideous Gorgon, Medusa. Medusa and her two sisters had once bragged that they were more beautiful than the goddess Athene. Their boast angered Athene, who turned the three sisters into hideous monsters with hissing, writhing snakes for hair. So ugly were they, that anyone looking at the sisters was instantly turned to stone. To help prepare for the dangerous task ahead, Perseus asked Hermes, the messenger god, and the goddess Athene for advise. Hermes gave Perseus a pair of winged sandals, which allowed him to silently creep up on the sleeping Gorgon. Athene gave him a shiny shield which he could use as a mirror. With the shield, he was able to slice off Medusa's head by watching her reflection. Because he didn't actually look at her, he wasn't turned to stone. Then, with his eyes closed, he grabbed the Gorgon's head and placed it in a special bag. A few drops of blood spilled out of the bag. From the drops, [Y/Pegasus] the flying horse was born. Perseus jumped onto the back of the horse and flew off to show Athene and Hermes his prize. Along the way, he saw a beautiful maiden chained to a giant rock by the sea. As he flew down to investigate, he saw a sea monster about to attack. The maiden [Y/Andromeda] was to be sacrificed to [Y/Cetus], the sea monster to save the kingdom of King [Y/Cepheus] and Queen [Y/Cassiopeia]. As Perseus swooped down out of the sky, he closed his eyes and pulled the Gorgon's head out of the bag. When the sea monster attacked, it saw the head and was instantly turned to stone. Perseus married Andromeda and they lived happily ever after. The brightest star in the constellation is [W/Mirphak], but the most famous star is [W/Algol], the second brightest star which is sometimes known as the Demon Star. It is also associated with the head of Medusa. Algol is an [G/eclipsing binary] star system whose brightness changes noticeably over a three day period. Perseus is best seen from October-December. "Must See" objects include: [M/M34], a galactic cluster; [N/NGC 869] and [N/NGC 884], two side by side galactic clusters; [N/NGC 1275], a galaxy that is an unusually strong radio source. Stories of the legendary Phoenix can be found in civilizations as far back as the ancient Egyptians and early Romans. However, the [G/constellation] wasn't added to the charts until the early 1600's. The Phoenix was a mythical bird that lived for several hundred years at a time. When it was ready to die, it would build a nest and lie down inside. The Sun's rays then ignited the nest and the Phoenix would burn with the flames. From the ashes of the nest, a tiny worm emerged. This worm grew into a new Phoenix and the cycle repeated itself. In the sky, the Phoenix has its wings extended, with each wing shaped like a triangle. The brightest [G/star] in this [G/constellation], [W/Ankaa], is the only bright star in the entire group. Phoenix is best seen from October-November in the southern hemisphere. Originally, this [G/constellation] represented a Painter's Easel. Over time, the "Easel" was dropped and today it is known merely as the Painter. This faint, narrow group of [G/star]s lies between the bright star [W/Canopus] and the constellation of [Y/Dorado]. Its brightest star is Alpha Pictoris [S/249647]. "Must See" objects include: Beta Pictoris [S/234134], an excellent candidate for extra solar system planets. Pisces is made up of two fish who, according to Greek mythology, represent the goddess Aphrodite and her son. The two were being pursued by the terrible monster god, Typhon (who also chased after [Y/Capricornus]). To escape from Typhon, Aphrodite and her son jumped into a river and turned themselves into fish. They tied their tails together with a long rope so they would not be separated and swam to safety. In the sky, Pisces is a faint [G/constellation] extending over a large area of sky. It is therefore sometimes difficult to locate. The most identifiable part of the constellation is the "Circlet", five faint stars forming a pentagon. The brightest star in Pisces is Alpherg, [S/92484]. Pisces is best seen from October-December. "Must See" objects include: Zeta Piscium [S/109739], a fine double star with color. This small, faint [G/constellation] contains only one bright [G/star], [W/Fomalhaut]. This star, sometimes called the Solitary One, is only 22 [G/light year]s away and is the 18th brightest star in the night sky. Data from the [G/IRAS] satellite shows a cloud of cool material surrounding this star, which could be the beginning of a planetary system. Piscus Austrinus is best seen from October-November. Puppis was originally part of the large [G/constellation] of Argo, the southern sailing ship. In the mid 1700's, Argo was divided into several smaller constellations, most retaining the nautical theme. In the sky, Puppis represents the stern of a ship. A small section of the constellation lies to the left of [W/Sirius], with the majority of stars lying below [Y/Canis Major]. Its brightest [G/star] is Naos, [S/198752]. Puppis is best seen from March-April. "Must See" objects include four galactic clusters: [M/M46]; [M/M47]; [M/M93]; [N/NGC 2477]. Originally part of the [G/constellation] of Argo, the sailing ship, Pyxis represents a compass. Its three brightest [G/star]s form a simple line in the sky. The brightest star in this group is Alpha Pyxidis, [S/199546]. Pyxis is best seen from March-April. Reticulum is considered a modern [G/constellation]. It is sometimes known as a net, although today it is most often associated with a reticle (a set of crosshairs found in some eyepieces to aid in the centering of objects in a telescope). It is a compact group of stars lying just north of the [F/Large Magellanic Cloud]. The stars within the group form a rather lopsided "W". The brightest [G/star] in Reticulum is Alpha Reticuli, [S/248969]. Reticulum is best seen from December-January in the southern hemisphere. From Cupid to Hercules, this tiny arrow has been associated with many heroes around the world. Lying between the bright stars [W/Altair] and [W/Albireo], Sagitta consists of four main stars: two stars form the arrow's shaft and two stars, side by side, represent the arrow's fletchings (feathers designed to balance the arrow in flight). The brightest [G/star] in this [G/constellation] is Gamma Sagittae, [S/105500]. Sagitta is best seen from August-October. The beautiful [G/constellation] of Sagittarius lies directly between our [G/solar system] and the center of the [G/Milky Way]. The brighter [G/star]s, the ones that make up the constellation, are fairly close to us. The stars at the center of our galaxy are 30,000 [G/light year]s distant and are too far away to be [G/resolve]d into individual points of light by the naked eye. Instead, the light from these distant stars blends together and appears as large, glowing clouds. In addition to the star clouds, there are also dust clouds visible in this area. These dust clouds are so thick that they actually block some of the light from the galactic center. In Greek mythology, Sagittarius was a Centaur, a creature with the head, chest and arms of a man and the body of a horse. In the sky, the centaur is holding a large bow and arrow, although seeing that figure in the sky requires a great deal of imagination. For observers in the northern hemisphere, there is an easy-to-identify pattern known as the "Teapot," complete with a spout, lid and curved handle. For observers in the southern hemisphere, the Teapot is upside down. The brightest star in the constellation is [W/Kaus Australis]. Sagittarius is best seen from July-August. "Must See" objects include: [M/M7], a galactic cluster which holds the record for being the southernmost Messier object; three diffuse nebulae ([F/Lagoon Nebula]; the [F/Swan Nebula]; and the [F/Trifid Nebula]); three galactic clusters ([M/M21]; [M/M23]; [M/M25]); several globular clusters ([M/M22]; [M/M28]; [M/M54]; [M/M55]). From Greece and Egypt, to the Americas, cultures around the world have identified this distinct group of stars with a scorpion. In Greek mythology, Scorpius is connected with the [G/constellation] of [Y/Orion] the hunter. Orion once boasted that his hunting skills were so remarkable, he could easily hunt and kill all of the animals on Earth. This boast alarmed the earth goddess, Gaea, whose job it was to protect all creatures. To insure the safety of her animals, she sent a scorpion to kill the mighty hunter. Orion and Scorpius fought a fearsome battle, but in the end, Orion was victorious. However, just before the scorpion died, he lashed out and stung the hunter with his tail. Poisoned by the sting, Orion died instantly. Both were given honored places in the sky, although they were placed far apart from one another. As one rises above the horizon, the other sets. This way, they can never see each other and start fighting again. To the ancient Chinese, this constellation represented a dragon. For observers in the northern hemisphere, Scorpius can be found lying lengthwise across the southern summer sky. Observers in the southern hemisphere can find Scorpius high overhead during winter. The brightest star in the constellation is [W/Antares]. Scorpius is best seen from July-August. "Must See" objects include: three galactic clusters ([F/Butterfly Cluster], [M/M7], [N/NGC 6124]); and two globular clusters ([M/M4]; [M/M80]; the [G/Milky Way]. Sculptor is a faint [G/constellation] that lies just to the east of the bright star [W/Fomalhaut]. Its original name was the "Sculptor's Workshop," but over the years it has been shortened to the "Sculptor." Its brightest star, Alpha Sculptoris [S/166716], is only a [G/magnitude] 4.3 [G/star]. The rest of the stars in the constellation are even fainter. As a result, Sculptor is sometimes difficult to locate. It is best seen from November-December. "Must See" objects include: two galaxies (the [F/Sculptor Galaxy] and [N/NGC 55]. Scutum is considered a modern [G/constellation], added to the charts in 1690. This small group of stars lies along the path of the [G/Milky Way], just north of [Y/Sagittarius]. Its brightest [G/star] is Alpha Scuti ([S/142408]). Scutum is best seen from August-October. "Must See" objects include: two galactic clusters (the [F/Wild Duck Cluster] and [M/M26]. In Greek mythology, the [G/constellation] of Serpens is associated with the story of Asclepius, the god of Medicine. Asclepius once killed a snake that had entered his hut. Soon after, another snake entered the hut carrying a strange herb in its mouth. The second snake placed the herb in the mouth of its dead friend who immediately came back to life. Asclepius was amazed. He took the herb from the snake and used its healing powers on humans. Serpens represents the snake with the healing herb, while the constellation of [Y/Ophiuchus] represents the god of medicine. The brightest [G/star] in Serpens is [W/Unukalhai]. This constellation is best seen from July-August. "Must See" objects include: [M/M5], a globular cluster; the [F/Eagle Nebula]. Sextans is considered a modern [G/constellation], added to the charts in 1690. Until that time, the stars in this group had been part of the constellation of [Y/Hydra]. The brightest [G/star] in Sextant, Alpha Sextanis [S/137366] is only [G/magnitude] 4.5. The rest of the stars in the constellation are even fainter, making Sextans rather difficult to locate. Sextans is best seen from April-June. The ancient Egyptians associated this [G/constellation] with their Bull-god over 4,000 years ago, making Taurus one of the oldest constellations in the sky. As you may imagine, with 4,000 years of history, there are many stories surrounding this heavenly bull. In Greek mythology alone, there are at least two stories about the bull, both with Zeus, the king of the gods, as the main character. In one story, Zeus fell in love with the maiden Europa. To lure her away from her father's servants, Zeus changed himself into a beautiful white bull with golden horns. Europa climbed onto his back and before she realized what was happening, Zeus waded into the water and began swimming across the ocean. Europa couldn't jump off his back because the water was too deep. He took her to a distant island where he turned back into his original form and they had many children together. Another story tells of Zeus falling in love with the maiden Io. To protect Io from the wrath of his wife, Hera, Zeus turned her into a white cow. Io escaped. Zeus then changed himself into a white bull and roamed the countryside until he found her. The two lovers were happy for a while, until Zeus was forced to return to Hera. In the sky, the face of the bull forms a distinct "V" shaped pattern. Almost every [G/star] in the "V" belongs to the [F/Hyades], a beautiful galactic [G/cluster]. The brightest star in the "V", [W/Aldebaran], is also the brightest star in the constellation. It is known as the red "eye of the bull." While this star appears to lie within the cluster, Aldebaran is actually two times closer to our solar system than the rest of the stars in the cluster. Another distinct star group in Taurus is the [F/Pleiades] (sometimes called the Seven Sisters). Because of its shape in the sky, this compact group of bright stars is sometimes mistaken for the [G/Little Dipper]. Each of these two clusters are surrounded by their own stories and legends. Taurus is best seen from October-December. "Must See" objects include: the [F/Hyades]; the [F/Pleiades]; [M/M1], a supernova remnant. Telescopium is a modern [G/constellation], placed in the sky in the mid 1700's in honor of the invention of the telescope. Its brightest [G/star] is Alpha Telescopii, [S/229023]. This small, faint constellation can be found just to the south of [Y/Corona Australis]. Telescopium is best seen from August-September in the southern hemisphere. This small [G/constellation] is shaped like its namesake. Three stars form a small, narrow triangle in the sky, with a fourth star lying close to the triangle's narrow base. This constellation lies between the larger constellations of [Y/Andromeda] and [Y/Aries]. Its brightest [G/star] is Beta Trianguli, [S/55306]. Triangulum is best seen from October-December. "Must See" objects include: the [F/Pinwheel Galaxy]. This [G/constellation] was first added to the charts in the early 1600's. Its three brightest stars form an equilateral triangle. The brightest [G/star] is Alpha Trianguli Australe, [S/253700]. This group of stars is a [G/circumpolar] constellation and can be seen year round from the southern hemisphere. "Must See" objects include: [N/NGC 6025], a galactic cluster. Tucana is the faintest [G/constellation] in the group known as the "Southern Birds". Other "southern birds" include [Y/Grus], [Y/Pavo], and [Y/Phoenix]. Though the stars within Tucana are fairly faint, this constellation is easy to locate because the [F/Small Magellanic Cloud] lies within its boundaries and is easily visible to the [G/naked eye]. The brightest star in Tucana is Alpha Tucanae, [S/255193]. "Must See" objects include: The [F/Small Magellanic Cloud]; two globular clusters, [F/47 Tucanae] and [N/NGC 362]; Beta Tucanae, [S/248201] a sextuple star system. Ursa Major contains the most famous seven stars in the northern hemisphere. Known as the [G/Big Dipper], the Plough, or the Chariot, these seven stars represent just a small portion of the great bear. Indian tribes in North America associated the bowl of the dipper as the main body of the bear with the stars of its handle representing hunters chasing the bear around the sky. Look closely at the middle [G/star] and you can see that the second hunter is carrying a cooking pot (a faint second star) on his back. That second star in the handle is [W/Mizar]/Alcor, a visual double star system. In Greek mythology, the Great Bear represents the maiden, Callisto. Zeus, the king of the gods, fell in love with the beautiful maiden. His jealous wife, Hera, turned Callisto into a bear, so the maiden would no longer catch the eye of her husband. As Callisto wandered the forests as a bear, she came across a young hunter whom she recognized as her son. When she rose up on her hind legs to greet the young man, the hunter was scared. He did not know this mighty beast was his mother. He took aim at the bear with his spear. Just before he threw the deadly weapon, Zeus saw the confrontation and intervened. He turned the son into a bear, then picked up both mother and son by their tails and placed them in the sky. Today, Callisto's son, [Y/Ursa Minor] follows his mother around the sky. The brightest star in this constellation is [W/Alioth], the first star in the handle of the dipper as it is seen coming off the scoop. Alioth is just a little brighter than its second brightest star, [W/Dubhe], the first star in the dipper's scoop, across from where the handle attaches to the scoop. Ursa Major is a [G/circumpolar] constellation for many in the northern hemisphere, but it is best seen high in the sky from April-June. "Must See" objects include: two spiral galaxies, [M/M81] and [M/M82]. This [G/constellation] contains the most famous star in the northern hemisphere, [W/Polaris], or the North Star. Many people believe that the North Star is the brightest star in the sky. This is not the case. In fact, Polaris ranks about 50th on the list of bright stars. The reason Polaris is mentioned frequently is because of its location in the sky. It lines up almost directly with Earth's north celestial pole. Polaris appears to remain fixed in the sky as the rest of the stars rotate around it. In Greek mythology, Ursa Minor is associated with the son of Callisto. Callisto was a beautiful maiden turned into a bear by the jealous Hera. As a bear, Callisto was forced to wander the forests where she was almost killed by her hunter son. Zeus saw what was about to take place and turned the son into a bear before he could kill his mother. Zeus then raised them both to the sky. In the sky, the little bear is hanging from Polaris by his tail. The little bear is also known as the Little Dipper, but this group of stars is not as bright as the [G/Big Dipper] and is more difficult to find. Polaris marks the end of the handle of the dipper. Two stars at the front of the scoop are the only other stars easily visible from most urban areas. Ursa Minor is a [G/circumpolar] constellation and can be seen year round from most of the northern hemisphere. Vela was once part of the constellation of Argo, the large sailing ship of the southern skies. During the 1750's, Argo was divided into four separate constellations, although these new constellations retained the nautical theme. Other segments of the sailing ship include [Y/Carina] the keel, [Y/Puppis] the stern, and [Y/Pyxis] the compass. The brightest star in Vela is Gamma Velorum, [S/219501]. Vela is best seen from March-April in the southern hemisphere. It is difficult to choose just one story to describe this [G/constellation] because, throughout recorded history, Virgo has been associated with many different Earth goddesses and female heroines. One of the earliest stories surrounding Virgo comes from the ancient Babylonians. Ishtar was their Earth goddess who was very much in love with her husband. When he died, he passed to the Underworld, where all mortals go when they die. Ishtar could not bear to be without her husband, so she followed him into the Underworld. As she descended into the land of the dead, cold and darkness fell upon the land above. Ishtar found her husband and begged the Queen of the Underworld to return him to the land of the living. She refused, so Ishtar remained with her husband. Meanwhile, in the land above, the cold and dark continued. Plants would not grow, no baby animals were born. The world was dying. The other gods were alarmed by the prolonged winter. They sent a messenger to the Underworld, asking the Queen to grant Ishtar's request. Since the gods above had more power than the Queen of the Underworld, she reluctantly granted Ishtar's wish. As soon as Ishtar returned to the surface with her husband, the air began to warm and plants began to grow. Spring had returned to the land. Every year, Ishtar returns to the Underworld to thank the Queen for returning her husband to her. While she is away, winter falls on the land. When she returns to the surface, so does spring. In the sky, one can use the handle of the [G/Big Dipper] to find Virgo. Simply follow the curve of the handle away from the dipper. The line from the handle will arc to [W/Arcturus] then speed on to [W/Spica], the brightest star in Virgo. Virgo is best seen from April-June. "Must See" objects include: the [F/Sombrero Galaxy]; [M/M49], an elliptical galaxy. Volans is a modern [G/constellation], added to the charts in the early 1600's. Its brightest star is Gamma Volantis, [S/256374]. Volans is a [G/circumpolar] constellation and can be seen year round from the southern hemisphere. Vulpecula is considered a modern [G/constellation], added to the charts in 1690. It can be found lying just below and a little to the east of the bright star [W/Albireo]. The brightest star in this constellation is Anser, [S/87261]. "Must See" objects include: the [F/Dumbbell] nebula. Accretion DiskA disk of material that has been trapped by a [G/black hole], but hasn't yet been pulled inside. ApolloThe name given to the U.S. manned space program designed to land humans on the [G/Moon]. The program was a success, with twelve Apollo astronauts actually walking on the Moon. The first moon landing, Apollo 11, occurred on July, 20, 1969. The last landing, Apollo 17, was on December 11, 1972. Asteroid BeltThe asteroid belt lies between the [G/orbit]s of [P/Mars] and [P/Jupiter] and contains over 100,000 asteroids, most smaller than half a mile (1 km). AsteroidsSmall, rocky objects. Most asteroids, but not all, can be found in the [G/asteroid belt]. Trojan asteroids travel in orbit around [P/Jupiter], in front of or trailing the planet. Amor asteroids cross the orbit of [P/Mars] and Apollo asteroids cross the orbit of Earth. A.U.An A.U., or Astronomical Unit, represents the average distance between [G/Earth] and the [G/Sun], and is equal to 93 million miles or 150 million kilometers. Averted VisionWhen looking through a telescope, focus your eye on the edge of the [G/field of view] and use your peripheral vision to scan the central area. This technique is best used to detect faint objects such as a [G/nebula] or a [G/galaxy]. BayerIn 1901, an astronomer named Bayer first used the Greek alphabet to classify the brightness of [G/star]s in a [G/constellation]. The brightest star was designated "Alpha", the second brightest "Beta" and so on. For example, the fifth brightest star in the constellation of [Y/Lyra] is designated Epsilon Lyra. Big DipperSeven stars in the [G/constellation] of [Y/Ursa Major] that form a dipper. Three stars form the handle of the dipper, while four stars form the scoop. The two stars in the front of the dipper's scoop are known as the "Pointer" stars, because they point to [W/Polaris], the North Star. Black HoleA black hole is a bizarre object of incredible mass, yet no volume. Its gravity is so strong that nothing, not even light, can escape its pull. A black hole is sometimes formed after the death of a supermassive star. Black holes are also found in the center of some galaxies. Blue Moon"Blue Moon" refers to the second Full Moon, [g/Moon, Full] within one calendar month. A "Blue Moon" occurs once every 2 1/2 to 3 years. CassiniA 17th century French astronomer who discovered the large gap in the rings of [P/Saturn]. Cassini DivisionName given to the 3,100 mile wide (5,000 km) dark division in [P/Saturn]'s rings. This division in the rings contains small fragments of dark material. CCDA CCD (Charge-Coupled Device) is an electronic camera that includes a silicon chip covered with a series of sensors. These sensors collect and record individual photons of light that fall onto the silicon chip. The photons are counted and entered into a computer program that converts the numbers into an image. CCD cameras are much more sensitive than standard film, producing digital images that can be enhanced to bring out subtle details. Celestial PoleTwo points in the sky, one aligned with the North pole of Earth, the other aligned with the South pole of Earth. All the stars in the sky appear to rotate around these celestial poles. Although no star lines up precisely with these points, the "north star", [W/Polaris], does come extremely close. CircumpolarCircumpolar stars or [G/constellation]s can be seen year round, never setting below the horizon for most of the world. Circumpolar objects are usually defined as any star or constellation that lies within 20 degrees of either the north or south [G/celestial pole]. ClumpyThe best way to describe [P/Neptune]'s main ring. For some reason, the main ring around Neptune is not uniform in appearance. Instead, material is clumped together at three different locations throughout the ring. ClusterA large grouping of [G/star]s. Two different types include galactic, or open, clusters (loose grouping of young stars formed from the same diffuse [G/nebula]) and globular clusters (compact sphere of thousands of stars, older and more distant than galactic clusters). Coma Star ClusteCovering an area ten times greater than that of a full [G/Moon], this galactic [G/cluster] in the [G/constellation] of [Y/Coma Berenices] is too large to observe through a telescope. Instead, use binoculars to scan the cluster. This cluster is approximately 250 [G/light year]s away. CometsA small body of ice and rock in an [G/elliptical] [G/orbit] around the Sun. When comets approach the Sun, they heat up and melt, leaving behind a long tail of ice and dust. ConstellationA group of stars that ancient people formed into an imaginary pattern. Finding a constellation requires a good imagination and the ability to play a stellar version of connect-the-dots. There were 48 original constellations, first mapped out by the ancient astronomer Ptolemy. Today there are 88 "official" constellations. CraterCircular impression found on most rocky bodies in the solar system. Craters are formed when [G/meteors] slam into the surface of a [G/moon] or [G/planet]. Deep Sky ObjectsFaint objects beyond our [G/solar system]. EarthThe origin of Earth's name is unknown. Our planet is the only planet in the solar system capable of supporting liquid water. In fact, 70% of Earth's surface is covered by water. Earth is one of the most geologically active planets; volcanoes, earthquakes, hurricanes, floods, fires and severe storms are constantly resurfacing the planet, changing its appearance. Earth is also the only planet in the solar system known to support life. The diameter of Earth at the equator is 7,926 miles (12,756 km). The mass of the Earth is 13.17 trillion trillion pounds (5.974 trillion trillion kg). Earth SatellitesObjects in [G/orbit] around Earth, natural (the [G/Moon]) or man-made (space stations, weather satellites, etc.) Earth YearsA year on Earth is equal to 365.2422 days. Eclipsing BinaryA binary [G/star] system refers to two stars in [G/orbit] around a common point. When one star eclipses, or passes in front of the other, as seen from Earth, the star in front blocks the light from the second star. As a result, the overall brightness of the system decreases. EllipticalThe [G/orbit]s of most objects are elliptical, or egg-shaped. EquinoxTwo days during the year when the amount of time the Sun is above the horizon equals the amount of time it is below the horizon, hence a day of equal daylight and darkness. The equinox occurs in March when the [G/Sun] appears to cross over Earth's equator and begin its trek into the northern skies. In the northern hemisphere, this marks the first day of spring. In September, the Sun crosses back over the equator and begins its travels in the southern skies, marking the first day of fall in the northern hemisphere. Extra Solar SystPlanets orbiting stars other than our Sun. Field of ViewThe area of sky seen through a pair of binoculars or a telescope. The more magnification used, the smaller the field of view. Galactic CenterThe center of a [G/galaxy]. Spiral galaxies have a distinct, large sphere of stars at their galactic center. GalaxyAn extremely large grouping of objects containing stars, nebulae, clusters, black holes, and much more. Different types include spiral (pinwheel shaped) galaxies, elliptical (egg-shaped) galaxies, and irregular galaxies. GalileoGalileo Galilie, 1564-1642, was an Italian astronomer and physicist. He was also the first person to use a telescope to study the sky. Galileo discovered many things with his telescope, including the four largest moons of [P/Jupiter] and [G/crater]s on the Moon. Galileo spacecraGalileo launched on Oct. 18, 1989 to study [P/Jupiter] and its moons. It is the first spacecraft to go into orbit around a gas giant planet. Galileo released a probe that plunged into the [G/jovian] atmosphere. Information from Galileo has incredibly expanded our knowledge of the jovian system. GanymedeLargest [G/moon] in the solar system. At 3,270 miles (5,276 km) in diameter, it is larger than the planets [P/Mercury] at 3,024 miles, (4,878 km) and [P/Pluto] at 1,400 miles (2,300 km). Ganymede orbits the planet [P/Jupiter]. HighlandsHeavily cratered regions found on the [G/Moon]'s southern hemisphere. The highlands are over four billion years old, the oldest surfaces found on the Moon. Hubble TelescopeThe Hubble Space Telescope was launched on board the space shuttle in 1990 and placed in low Earth orbit. From its vantage point in space, above Earth's turbulent atmosphere, its 93.6 inch (2.4 meter) objective mirror has revealed an incredible amount of information about our universe. InfraredElectromagnetic radiation that lies just beyond the visible portion of light. Longer than the red wavelengths, this type of radiation can be detected as heat. Int'l Space StatWhen completed, this space station will be 290 feet (79.9 m) in length, 356 feet (108 m) at its widest point and will orbit at an altitude of 220 nautical miles (407 km) above the Earth. IRASThe Infrared Astronomical Satellite (IRAS) was launched on January 25, 1983 to study [G/infrared] sources in deep space. JovianAnything relating to [P/Jupiter]. LanderSpacecraft designed to land gently on the surface of a planet or moon and send back pictures and scientific data from the surface. Light YearThe distance a beam of light travels in one year: 5.9 trillion miles (9.5 trillion km). LimbThe natural curved edge of a [G/planet] or [G/moon], as seen from [G/Earth]. Little DipperSeven [G/star]s in the [G/constellation] of [Y/Ursa Minor] form a dipper: three stars form the handle of the dipper, while four stars form the scoop. The Little Dipper is smaller and much fainter than the [G/Big Dipper]. [W/Polaris], the North Star, represents the last star in the dipper's handle. Local GroupA group of about 20 nearby galaxies, including our own [G/Milky Way] and the [F/Andromeda Galaxy]. LuminosityHow bright an object appears, not just in the visible wavelengths of light, but over its entire spectrum. LuminousHow luminous a star appears is determined by its luminosity, the amount of energy the star emits across its entire spectrum, including infrared, visible, ultraviolet, microwave, x-ray, and all other wavelengths of electromagnetic radiation. Lunar EclipseWhen the Moon passes through Earth's shadow. A lunar eclipse can only occur when the Moon is full, and Earth lies between the Sun and the Moon. A total lunar eclipse occurs when the entire Moon passes through the umbra (dark shadow). A partial eclipse occurs when only a portion of the Moon passes through the umbra. A penumbral eclipse occurs when the moon only passed through an area of reduced sunlight called the penumbral shadow. In a penumbral eclipse the brightness of the moon i s reduced but no dark shadow appears on the surface. MagellanSpacecraft designed to complete a radar mapping mission of [P/Venus]. Launched May 4, 1989 by the U.S., Magellan was a complete success, revealing strange features on the surface of Venus (domes, lava tubes, possible fault lines) as it mapped the entire planet. MagnitudeA scale used to compare the brightness of celestial objects. The brighter the object, the smaller its magnitude rating. In fact, [P/Venus] at its brightest in our skies, has a rating of magnitude -4.5. The bright star, [W/Betelgeuse] is magnitude 0.5. The faintest objects that can be seen with the [G/naked eye] are magnitude 5.5. MariaPronounced MAR-ee-uh, these large, dark smooth regions found in the northern and central regions of the [G/Moon], were formed when huge [G/meteors] slammed into the Moon's surface and cracked its crust. Lava from the Moon's then liquid central core seeped up through the cracks, filling in the original [G/crater]s, leaving a smooth dark surface. Samples brought back by the [G/Apollo] astronauts indicate the maria to be almost three billion years old, much younger than the heavily cratered [G/highlands] to the south. Mariner 10Spacecraft launched on Nov. 3, 1973 by U.S. to study the planets [P/Venus] and [P/Mercury]. This was the first dual-planet mission, using the gravity of Venus to propel itself on to Mercury. Mariner 10 flew by Venus on Feb. 5, 1974, continuing on to take the first closeup pictures of Mercury on Mar. 29, 1974. It flew by Mercury two additional times. Mariner ValleyRift valley on [P/Mars] over 3,000 miles (4,800 km) long and 4 miles (6.4 km) deep. On Earth, this valley would stretch from New York to Los Angeles. Mars Global SurvThe first of several spacecraft in the Mars Surveyor program, Mars Global Surveyor was launched on November 7, 1996 by the US and arrived at [P/Mars] on September 17, 1997. In orbit around Mars, the spacecraft is studying the atmosphere and photographing the planet. The spacecraft will also act as communication support for future missions. MessierCharles Messier was a famous eighteenth century French astronomer and author of the Messier catalog of faint objects. Messier created his catalog to avoid confusion between known deep sky nebulae and faint, new comets, his main interest. Messier contributed 103 objects to his list. An additional 7 objects have been added over the years, for a total of 110 objects. MeteorsSmall pieces of rocks and dust which enter Earth's atmosphere at great speeds. Friction between the dust and the atmosphere causes the rock to heat up, leaving behind a bright streak of light. Most burn up before they hit the ground. The larger rocks do hit the ground, forming [G/crater]s. Milky WayOur home galaxy. Its spiral arms can be seen as glowing clouds of distant stars, stretching across the sky from August through October. The center of the Milky Way is located in the area just behind the [G/constellation] of [Y/Sagittarius]. The bright, individual stars we see in the sky also belong to the Milky Way. These stars lie within the same spiral arm as our [G/solar system] and are our celestial neighbors. MirThe Russian space station Mir, was launched on February 19, 1986. Since then, several modules have been added to the space station, providing a home to over sixty crew members from over a dozen countries. The space station orbits the Earth at an average distance of 242 miles (390 km). MoonThe common name for [G/Earth]'s only natural [G/satellite]. A moon also refers to a natural satellite orbiting around any [G/planet]. Moon, First QuarThe Moon is in its First Quarter. A First Quarter Moon occurs when the western half of the Earth-facing side of the Moon is illuminated by sunlight. The Sun's light falls on the Moon's surface at an angle. In the southern [G/highlands], it illuminates some of the crater walls and central mountain peaks, but leaves the floors of some craters in darkness. The northernmost [G/maria] is Mare Frigoris. Just below that, cut off by the [G/terminator], is the beginning of Mare Imbrium. The Sea of Serenity and Sea of Tranquility are also visible towards the center of the Moon. In the sky, a First Quarter moon is visible before sunset and can be seen during the early evening hours. Moon, FullThe Moon is Full. A Full Moon occurs when the entire Earth-facing side of the Moon is illuminated by sunlight. Through a telescope, this is the worst time to observe the Moon. With the [G/Sun] shining straight onto the Moon, there are no shadows or sense of depth. The lunar surface is all but washed out. A Full Moon rises as the Sun sets and sets as the Sun rises. A [G/lunar eclipse] can only occur during a Full Moon. Moon, NewThe Moon is New. A New Moon is not visible from Earth. A New Moon occurs when the entire far-side of the Moon is illuminated by sunlight. As a result, the Earth-facing side is in darkness and not visible. With the Moon's light out of the way, this phase is the best time to look for those faint [G/deep sky objects] that the Moon's light normally washes out. The exact moment of New Moon has significance in several religions around the world and it is the only time a [G/solar eclipse] can occur. Moon, Third QuarThe Moon is in its Third Quarter. A Third Quarter Moon occurs when the eastern half of the Earth-facing side of the Moon is illuminated by sunlight. The small, heavily cratered area you see near one end of the Moon is the [G/highlands] at the south pole. Near the north pole is the narrow band of Mare Frigoris. Below that is Mare Imbrium, or the Sea of Rains. Located almost in the middle, is the large crater Copernicus - 58 miles (93 km) wide and 2.2 miles (3.7 km) deep. Curving along the [G/limb] is the largest [G/maria] on the moon, Oceanus Procellarum, the Ocean of Storms. In the sky, a Third Quarter moon is visible after midnight and can be seen during the early morning hours. It can even be seen after the Sun rises in the morning sky. Observe along the [G/terminator] to see the most detail. Moon, Waning CreThe Moon is a Waning Crescent. A Waning Crescent Moon occurs when the Moon is between Third Quarter [G/Moon, Third Quarter] phase and New Moon [G/Moon, New]. It looks like a banana, or a "smile" that is shrinking or "waning" as less and less of its Earth-facing side is illuminated by sunlight. Oceanus Procellarum (Ocean of Storms) is the largest [G/maria] on the Moon and is visible near the [G/limb]. A Waning Crescent Moon can be seen in the early morning skies in the east. Moon, Waning GibThe Moon is Waning Gibbous. A Waning Gibbous occurs when the Moon has passed its Full Moon phase, [G/Moon, Full], but has not yet reached Third Quarter, [G/Moon, Third Quarter]. Less and less of the Earth-facing side of the Moon is illuminated by sunlight. It is best to observe a gibbous moon along its [G/terminator], where the Sun casts shadows on the lunar surface. The heavily cratered [G/highlands] at the south pole are a good observing target. [G/Maria] - Mare Vaporum, near the Moon's center, Mare Imbrium, and Oceanus Procellarum, near the [G/limb] - cover a vast majority of the remaining visible surface. A Waning Gibbous Moon can be found, rising well after sunset in the eastern sky. Moon, Waxing CreThe Moon is Waxing Crescent. A Waxing Crescent Moon occurs when the Moon is between its New Moon phase, [G/Moon, New], and First Quarter, [G/Moon, First Quarter]. It looks like a banana, or a "smile" that is growing larger as more and more of the Earth-facing side of the Moon is illuminated by sunlight. Mare Crisium, the Sea of Crises, is visible near the [G/limb] as a distinct dark, round feature. Another [G/maria], the Sea of Fertility, is visible as a dark "blob" below (or above, depending on your orientation) near the nice, round Mare Crisium. A Waxing Crescent Moon can be seen in the early evening skies in the west. Moon, Waxing GibThe Moon is Waxing Gibbous. A Waxing Gibbous Moon occurs when more than half of the Earth-facing side of the Moon is visible, but the Moon is not yet full. Details within the Sea of Tranquility, Sea of Serenity and Sea of Rains begin to fade as more and more of the lunar surface is illuminated by the Sun. In the southern hemisphere, details within the heavily cratered [G/highlands] can still be seen along the [G/terminator]. A Waxing Gibbous Moon can be seen in the eastern evening sky as the Sun goes down. Naked EyeObserving without any optical aid (i.e., binoculars or a telescope). NebulaAn interstellar cloud of gas and dust. Different types include Diffuse nebulae (where stars are forming), Supernova Remnants (cloud of debris from a supernova explosion), and Reflection Nebula (light from bright stars reflecting off of a nearby cloud). NGCNew Galactic Catalog. William Herschel (the discoverer of [P/Uranus]) and his son, John Herschel, observed and recorded nearly 5,000 [G/deep sky objects]. Astronomer J. Dreyer added to their list and the entire work was published in 1888 as the New Galactic Catalog. Today the list includes over 15,000 objects, which are referred to by their NGC numbers (i.e., the [F/Great Orion Nebula] is also known as [N/NGC 1976]). NucleusThe center of a galaxy. Olympus MonsLocated on [P/Mars], Olympus Mons rises 15 miles (24 km) above the surrounding Martian surface, making it the tallest mountain in the solar system. This giant, extinct volcano is almost three times higher than Mount Everest. OrbitThe path a celestial object (satellite, moon, planet, star) travels around another celestial object. Most objects follow an elliptical (egg-shaped) orbit. OrbiterSpacecraft designed to orbit a planet or moon, taking pictures and gathering scientific data from space. PathfinderThe name of a spacecraft launched on Dec. 3, 1996 by U.S. that bounce-landed on [P/Mars], on July 4, 1997. Pathfinder contained a small rover which was able to travel several meters from the lander, studying rock samples and taking photos. Pioneer 10Spacecraft designed to study [P/Jupiter]. Launched on March 2, 1971 by the U.S., Pioneer 10 was the first spacecraft to pass through the [G/asteroid belt] and obtained the first closeup pictures of Jupiter on Dec. 3, 1973. Pioneer 11Spacecraft designed to study [P/Jupiter] and [P/Saturn]. Pioneer 11 was launched on April 5, 1973 by the U.S. It flew by Jupiter on Dec. 2, 1974 and Saturn on Sept. 1, 1979. PlanetA large body orbiting a star. Planet is the Greek word for wanderer. This name is appropriate because planets appear to wander through the sky as they orbit around the [G/Sun], while the stars remain fixed. Planetary NebulaA sphere of gas surrounding an older sun-like star, formed when the dying star shrugs off its outer atmosphere. These objects have nothing to do with [G/planet]s. PrecessionThe slow wobble of Earth's rotational axis. Similar to the way a spinning top wobbles slowly on a table, Earth's poles wobble, or precess, as it spins on its axis. Precession causes the poles to slowly circle, thus pointing to different areas of the sky over the 25,000 years it takes to complete one wobble. ProtostarsFound in diffuse [G/nebula]e, protostars are dark "globules" of gas and dust drawn together by gravity to form a sphere. As the gravitational collapse continues, the temperature and pressure at the core of the sphere increases to the point where nuclear fusion begins. When that happens, the protostar becomes a full-fledged star. PulsarA neutron star (a tiny, massive star produced after a supernova explosion) which rotates incredibly fast, emitting a series of radio pulses. QuasarQuasi-stellar objects which lie at great distances and produce tremendous amounts of energy. RaysWhen a [G/crater] is formed, material from the explosion is flung away from the point of impact, forming streaks across the lunar surface. These streaks, called rays, can be seen extending away from some of the larger lunar craters. ResolveThe act of separating into individual components. For example, a telescope's ability to separate a multiple star system into its individual components, or the ability of the human eye to separate the light from a car into two separate headlights. RetrogradeTraveling in the opposite direction of the majority of planets and moons. RilleA long, narrow crack in the [G/Moon]'s surface. Ring SystemBand of small particles orbiting a [G/planet]. Particles range in size from a grain of sand to the size of a house. White, icy particles are found in [P/Saturn]'s ring system. The rings around [P/Jupiter], [P/Uranus], and [P/Neptune] are made of extremely dark material. SarosA period of 18 years 11.33 days in which the pattern of lunar and solar eclipses repeat. A Saros number defines a particular eclipse configuration within that period. SatelliteAn object, natural or manmade, in [G/orbit] around a planet. Solar EclipseWhen the [G/Moon] moves between the [G/Sun] and Earth. A solar eclipse can only occur during the New Moon phase. There are three types of solar eclipses: a total eclipse (when the Moon completely covers the Sun); a partial solar eclipse (when the Moon only covers a portion of the Sun); and an annular solar eclipse (if the eclipse occurs when the Moon is at its farthest point in its orbit, its disk isn't large enough to completely cover the Sun, so a ring of sunlight appears around the Moon). Solar SystemA [G/star] and anything in [G/orbit] around it. Our solar system consists of nine [G/planet]s orbiting around the [G/Sun]. It also includes [G/meteors], [G/comets], and [G/asteroids]. SolsticeThe solstice marks two days of the year: the day the [G/Sun] reaches its northernmost point in our sky (in June) and the day the Sun reaches its southernmost point in the sky (in December). The June solstice marks the beginning of summer in the northern hemisphere and the longest day. For those in the southern hemisphere, it marks the first day of winter and the shortest day of the year. In December, the positions are reversed. The solstice marks the first day of winter in the northern hemisphere and summer in the south. Southern CrossFour bright [G/star]s which form a distinct cross in the southern sky. The stars are located in the [G/constellation] of [Y/Crux]. SpectroscopeAn instrument designed to observe a star's spectrum, or individual wavelengths of light. A star's spectrum can reveal its temperature, star type, and composition. StarA huge ball of hydrogen gas with nuclear reactions occurring in its core. Our Sun is a star. The color of a star depends on its temperature: a red star indicates a relatively cool surface; a yellow star is a medium type star, like our Sun; and a blue star is a super hot star that burns its fuel extremely fast. SunThe Sun is a star at the center of our solar system. The main difference between our Sun and the stars visible at night is distance. On average, Earth is only 93 million miles (150 million km) from the Sun. The next nearest star, Alpha Centauri [S/252838], is 4.2 [G/light year]s, or 25 trillion miles (40 trillion km) away. SupernovaThe most powerful explosion in the universe, occurring at the death of a supermassive [G/star]. A supernova blast is so powerful, one dying star can easily outshine an entire galaxy of stars. Leftover debris forms a cloud of material expanding away from the point of explosion. If the dying star was massive enough, a [G/pulsar] or a [G/black hole] may form after the explosion. TerminatorThe dividing line between the sunlight and darkness on the Moon. TitanLargest [G/moon] of [P/Saturn], Titan is the only moon with an atmosphere. Titan's methane atmosphere contains a thick layer of clouds which hide its surface from cameras. Titan may have lakes of liquid methane on its surface. TritonLargest [G/moon] of [P/Neptune], Triton is one of the coldest places in the solar system. [G/Voyager 2] measured temperatures of -391^F (-235^C) at the surface of the moon. The spacecraft also discovered active geysers erupting on Triton, spewing nitrogen and dust several miles into space. Venera 14Launched on Nov. 4, 1981, by what was then called the USSR, this spacecraft landed on [P/Venus] March 3, 1982. The spacecraft transmitted information about the atmosphere while descending to the surface. After touching down, it took a soil sample of the surface. It operated for almost an hour before shutting down. Virgo ClusterAn enormous group of galaxies covering a large portion of the sky, including the [G/constellation]s of [Y/Virgo], [Y/Coma Berenices], [Y/Canes Venatici] and [Y/Corvus]. Over 3,000 galaxies have been photographed in this region. Voyager 1Launched on September 5, 1977, Voyager 1 was one of two spacecraft designed to tour the larger planets of the solar system. Voyager 1 flew by [P/Jupiter] in 1979 and [P/Saturn] in 1980. Voyager 2Launched on August 20, 1977, Voyager 2 was one of two spacecraft designed to tour the larger planets of the solar system. Voyager 2 flew by [P/Jupiter] in 1976, [P/Saturn] in 1981, [P/Uranus] in 1986; and [P/Neptune] in 1989. ZodiacThe path the [G/Sun] appears to travel through the stars every year. Long ago, this path was divided into the twelve constellations we know today as the zodiac. This spiral [G/galaxy] is situated perfectly edge-on with respect to the [G/Milky Way]. Since the spiral arms of the galaxy are extremely thin, they almost disappear when observing them from the side, or edge-on. The only real evidence of this galaxy's spiral structure is the dark dust lanes lying between our view and the galaxy's [G/nucleus]. Through a small telescope, its nucleus appears as a faint, tiny oval patch of light. A challenging object for a small telescope, this [G/planetary nebula] is extremely small and faint in our skies. Attempt to observe this planetary nebula only on extremely dark nights. Use a low-power eyepiece for the brightest image possible and observe using [G/averted vision]. Through a 8-inch (203 mm) or larger telescope look for a small, faint, slightly elongated cloud. PHL909: This [G/quasar] is 1.5 billion [G/light year]s from Earth. Because of its tremendous distance, this quasar is visible only to the largest telescopes on Earth. Because of its orientation in the sky, this [G/galaxy] has been difficult to classify. From our point of view, we see the galaxy from the side, or edge-on. Very little detail can be made out from this angle. Astronomers believe this is either a barred spiral galaxy or a flattened irregular galaxy. It is about 8 million [G/light year]s away and 70,000 light years across. Through a small telescope, look for a narrow, faint streak of light in the [G/field of view]. Only the largest telescopes can begin to [G/resolve] individual [G/star]s within this galaxy. 47 Tucanae: This globular [G/cluster] is one of the best in the sky, second only to [F/Omega Centauri]. This glowing sphere of over 100,000 [G/star]s is 16,000 [G/light year]s away and almost 210 light years in diameter. It can be found just to the west of the [F/Small Mag. Cloud]. Through a small telescope, the cluster can be seen as a bright, round patch of light. 4-inch (100mm) telescopes and larger can [G/resolve] individual stars around the cluster's edge. Experiment with different magnifications by observing this cluster through a variety of eyepieces. This galactic [G/cluster] contains approximately 35 stars. This [G/galaxy] is a extremely faint edge-on spiral. This small elliptical [G/galaxy] is an extremely faint companion to the giant [F/Andromeda Galaxy], placing it at a distance of 2.2 million [G/light year]s. It is 4,400 light years in diameter. This small elliptical [G/galaxy] is an extremely faint companion to the giant [F/Andromeda Galaxy]. Although it is slightly brighter than another companion galaxy, [C/C17], it is still very faint in our skies. This galaxy is 2.2 million [G/light year]s away and 2,300 light years in diameter. This elliptical [G/galaxy] is a companion to the great [F/Andromeda Galaxy]. It is 2.2 million [G/light year]s away and 5,400 light years in diameter. M110 was not listed in [G/Messier]'s original catalog, but was added in 1967. Currently, this galaxy is the last object in the catalog. Through a small telescope, look for a fuzzy, star-like object very near the much larger Andromeda Galaxy. This small elliptical [G/galaxy] appears to be in [G/orbit] around the great [F/Andromeda Galaxy]. It is approximately the same distance from us as its larger companion, over 2.2 million [G/light year]s, and is 2,400 light years in diameter. It can be seen as a fuzzy [G/star] just to the south of the larger galaxy. Through a small telescope, its great distance and small size make it impossible to [G/resolve] any stars within the galaxy itself. A giant [G/black hole], with a mass equal to 3 million stars like our Sun, is believed to lie at the center of this galaxy. Andromeda Galaxy: The Andromeda galaxy is the closest spiral [G/galaxy] to the [G/Milky Way]. It is 2.2 million [G/light year]s away, 180,000 light years in diameter, and contains over 300 billion stars. The galaxy is so bright that it can be seen with the [G/naked eye] on extremely dark nights. Through a telescope, it appears faint, fuzzy, and cigar-shaped with a brighter central region. It is best seen through wide angle eyepieces. This large scattered [G/cluster] of 15 to 20 [G/star]s forms a W-shape. This galactic [G/cluster] is 5,000 [G/light year]s away. Studies of individual stars within this cluster show it to be the oldest galactic-type cluster in our skies, with an estimated age of 12-14 billion years. For comparison, our [G/solar system] is thought to be 4.5 billion years old. Through a small telescope, this cluster is faint and the [G/star]s within the cluster are difficult to [G/resolve] into individual points. This [G/planetary nebula] appears as a faint star-like object through a small telescope. This spiral [G/galaxy] is large but extremely faint. It is approximately 6-8 million [G/light year]s distant. Through a small telescope, use a low-power, wide angle eyepiece and [G/averted vision] to detect a long, narrow patch of light. Sculptor Galaxy: This edge-on spiral [G/galaxy] is approximately 7.5 million [G/light year]s away. Through a small telescope it appears as a faint, pale streak of light, with a slight brightening towards its center. Even though it is faint, the Sculptor Galaxy is best viewed through low-power, wide angle eyepieces. PG0052+251: This [G/quasar] is 1.5 billion [G/light year]s away and lies in the center of a spiral [G/galaxy]. Because of its tremendous distance, this quasar is all but invisible except to the largest telescopes on Earth. The [G/star]s within this globular [G/cluster] are rather loosely packed. Small Mag. Cloud: At 190,000 [G/light year]s, the Small Magellanic Cloud is an irregular galaxy. It is the second closest galaxy to the [G/Milky Way]. Its nearby neighbor in the sky, the [F/Large Mag. Cloud], is the closest galaxy to our own. The Small Cloud has a diameter of 16,000 light years and contains its own [G/star]s, [G/cluster]s, and [G/nebula]e. Lying on the fringes of the Small Cloud is a globular cluster within our own galaxy, [N/NGC 362]. Use low-power, wide angle eyepieces for observing the galaxy in general. For more detailed studies of areas within the galaxy, use medium to high power. This spiral [G/galaxy] is very large but its low surface brightness makes it difficult to detect. Use a low-power eyepiece for the brightest image possible. Then, observe using [G/averted vision]. This globular [G/cluster] can be found on the northern fringes of the [F/Small Mag. Cloud]. At a distance of 29,000 [G/light year]s, this cluster is still in our [G/Milky Way], but it is almost twice as far away as its globular cluster neighbor, [C/C106]. Through a small telescope, it appears as a round, hazy patch of light against the mottled backdrop of star clouds of the Small Magellanic Cloud. This extremely dim irregular [G/galaxy] is relatively close to our [G/Milky Way], making it a member of our [G/Local Group] of galaxies. Its distance is approximately 1.8 million [G/light year]s and it is 9,000 light years in diameter. Its low surface brightness makes this galaxy a definite challenge for a small telescope. This galactic [G/cluster] is 9,300 [G/light year]s away and 30 light years in diameter. Because of its great distance, this cluster is difficult to [G/resolve] into individual stars. However, there is one bright [G/star] near the edge of the cluster that should stand out from the hazy cloud. If this bright star is a true member of the cluster, and really is 9,300 light years away, the star must be 275,000 times brighter, or more [G/luminous] than our [G/Sun]. This cluster is best seen using medium-power eyepieces. This galactic [G/cluster] is a compact group of approximately 50 [G/star]s. Galactic clusters are best observed using low-power, wide angle eyepieces. With the cluster centered in the field of view, experiment with different eyepieces to determine which provides the best image. This galactic [G/cluster] is 8,000 [G/light year]s away and 15 light years in diameter. This cluster is small and wedge-shaped, with few [G/star]s. It is best seen through low-power eyepieces. Pinwheel Galaxy: Long exposure photographs of this [G/galaxy] show a beautiful, face-on spiral galaxy in all its splendor. However, through a small telescope this galaxy is a challenge. With little change in brightness over its entire length, there is little contrast for the eye to pick up on. Instead, it appears as a large, dim cloud that can be easily passed over. When observing the Pinwheel Galaxy, use low-power, wide angle eyepieces and slowly scan the entire field of view, looking for any glimpse of the dim distant galaxy. It is possible to [G/resolve] individual [G/star]s within the galaxy using 12-inch (300cm) or larger telescopes. This spiral [G/galaxy] is one of the more difficult [G/Messier] objects to locate with a small telescope. It is believed to be 20 million [G/light year]s away and 80,000 light years in diameter. Under extremely dark skies, using a low-power eyepiece, it may be possible to detect a faint, round hazy patch of light. Larger telescopes, which gather more light, have a better chance of seeing this elusive galaxy. Little Dumbbell: This planetary nebula is one of the more difficult [G/Messier] object to locate in a small telescope. This planetary nebula appears similar in structure to the brighter and easier [M/M27] planetary nebula, but fainter and somewhat smaller. This small, compact galactic [G/cluster] lies close to the bright cluster [N/NGC 663]. It contains approximately 50 stars. This compact galactic [G/cluster] lies close to the bright cluster [N/NGC 663]. It contains approximately 50 [G/star]s. This galactic [G/cluster] is 2,600 [G/light year]s away. The cluster is rather sparse, containing few [G/star]s and is best seen through low-power, wide angle eyepieces. This loosely grouped galactic [G/cluster] is 1,300 [G/light year]s away, 17 light years in diameter and contains over 60 stars. It is best seen through wide angle eyepieces. This galactic [G/cluster] is one of two clusters forming the beautiful Double Cluster of [Y/Perseus]. Of the two, this cluster is closer, younger, and contains more [G/star]s. NGC 869 is about 7,000 [G/light year]s away, 70 light years in diameter, and 6.4 million years old. It contains approximately 400 stars, although less than half of those are visible in a small telescope. NGC 869 is best seen through a low-power, wide angle eyepiece. Double Cluster: This entry represents a beautiful pair of galactic [G/cluster]s. The two clusters, [N/NGC 869] and [N/NGC 884] can be seen at the same time through a low-power, wide angle eyepiece. Details about each cluster can be found under its individual entry. This galactic [G/cluster] is one of two clusters forming the beautiful Double Cluster of [Y/Perseus]. It is 8,150 [G/light year]s away, 70 light years in diameter, and is approximately 11.5 million years old. This cluster contains approximately 300 stars, although less than half of those are visible in a small telescope. NGC 884 is best seen through a low-power, wide angle eyepiece. This edge-on spiral [G/galaxy] has a distinct, dark dust band running through its disk. The galaxy is approximately 20 million [G/light year]s away and 120,000 light years in diameter. Through a small telescope, look for an extremely faint, narrow streak of light only under the best observing conditions: dark skies, calm air and no [G/Moon]. PG1012+008: This [G/quasar] is 1.6 billion [G/light year]s away. Because of its tremendous distance, it is visible only through the largest telescopes. This galactic [G/cluster] is 1,500 [G/light year]s away. Its central core of stars is about 4 light years in diameter with a few additional stars extending out to a total diameter of 18 light years. There are approximately 60 stars easily visible within the cluster. M34 is best seen using low-power, wide angle eyepieces. This compact spiral [G/galaxy] is between 30-60 million [G/light year]s away, its distance being rather difficult to determine. This galaxy is unusual for several reasons, the first being its appearance. Long exposure astrophotographs show this galaxy to have three spiral arms (most spiral galaxies have two). Second, it is an extremely strong radio source. Thirdly, early observations of this galaxy, which showed it moving through the universe at a rate of 620 miles per second relative to our own galaxy, helped introduce the theory of the expanding universe. Through a small telescope, look for an extremely faint, irregular patch of light. It is best seen using a low-power eyepiece. Through a small telescope, this barred spiral [G/galaxy] is extremely faint. Look for a small, narrow slash of light when using a low-power eyepiece and [G/averted vision]. Its faint spiral arms can only be detected on [G/CCD] images and long exposure photographs. The [G/star]s within this globular [G/cluster] are tightly compressed, making it difficult to [G/resolve]. Look for a tiny, fuzzy, round patch through a small telescope. The bigger the telescope, the brighter the image. This galactic [G/cluster] lies just 3 degrees southwest of the brightest [G/star] in [G/Perseus], [W/Mirphak]. This rich cluster contains approximately 150 stars. This extremely faint peculiar [G/galaxy] emits an unusually high amount of radio energy and x-rays. Astronomers are not sure exactly why this system is so active. One theory suggests that the tremendous energy being released may be a result of the interaction between two colliding galaxies. The problem with this theory is that it is difficult to make out a second galaxy within the large cloud. Through a small telescope, this galaxy is extremely small and faint. This distant spiral [G/galaxy] is an extremely strong radio source. This galaxy is the brightest of a group of 18 galaxies belonging to the [Y/Fornax] Galaxy Cluster. Although classified as a spiral, very little structure can be seen. Look for a small, faint, hazy sphere. This irregular-shaped galactic [G/cluster] contains approximately 50 [G/star]s. This barred spiral [G/galaxy] is one of 18 galaxies belonging to the [Y/Fornax] Galaxy Cluster. This diffuse [G/nebula] surrounds the 4th [G/magnitude] [G/star] Atik [S/56673]. This face-on spiral [G/galaxy] is approximately 25,000 [G/light year]s away. Its dim spiral arms and small [G/nucleus] make it a difficult object for small telescopes. Through an 8-inch (203 mm) telescope, a large faint cloud with a slightly brighter center can be detected. Pleiades: This galactic [G/cluster] is almost too large to enjoy through a telescope. With the [G/naked eye] it is possible to see between six and eight [G/star]s, which form a pattern resembling a little dipper. Through a small telescope, it is revealed that these six to eight [G/star]s are embedded in a cluster of 50-100 stars. The Pleiades are only 410 [G/light year]s away and 7 light years in diameter. Because of its relative closeness and size, it may be difficult to see all of the stars of this cluster at one time in a telescope. To do so requires the use of low-power, wide angle eyepieces. The Pleiades (also known as the Seven Sisters) are connected with many myths and legends around the world. One of the more interesting stories can be found not only in a Greek myth but in Japanese, Australian, African, and American legends as well. The story involves six sisters and a missing seventh sister. She is either hiding or has come down to Earth to be with the man she loves. From these stories, it would seem that one of the stars in the cluster was once much brighter and has since faded from view. How many sisters can you see with the naked eye on a dark, clear night? California Nebula: This very faint, very large diffuse [G/nebula] is shaped like the state of California, hence its nickname of the California Nebula. PKS0405-12: This [G/quasar] is over 1 billion [G/light year]s away. Because of its tremendous distance, this quasar is only visible through the largest telescopes. This irregular-shaped galactic [G/cluster] contains approximately 30 [G/star]s. This planetary [G/nebula] appears as a tiny, pale blue sphere. This galactic [G/cluster] contains approximately 80 [G/star]s. Hyades: This enormous galactic [G/cluster] has a distinct V-shape which makes it relatively easy to locate in the sky. The brightest star in the V is [W/Aldebaran], which doesn't even belong to the cluster. Aldebaran lies at a distance of 68 [G/light year]s while the Hyades are 130 light years away. With the exception of a group of stars in [Y/Ursa Major], the Hyades cluster is the closest galactic cluster to our [G/solar system]. Because this group covers such a large area of the sky, it is almost impossible to view the group in its entirety through a telescope. It is best to observe the Hyades with a low-power, wide angle eyepiece or a pair of binoculars. There are approximately 100 [G/star]s within this loosely grouped galactic [G/cluster]. This galactic [G/cluster] contains approximately 40 [G/star]s. The light from the nearby bright [G/star] [W/Rigel] illuminates the gases within this [G/nebula], making it visible to us on Earth. This galactic [G/cluster] contains approximately 50 [G/star]s. This globular [G/cluster] is a strong source of x-rays, which is unusual for a globular cluster. Through a small telescope, this cluster appears as a faint, round cloud. Larger telescopes are able to [G/resolve] individual stars around the edge of the cluster. Flaming Star Nebula: This diffuse [G/nebula] contains a bright [G/star] just inside its boundaries. This star is not directly associated with the nebula. Instead, it appears to be passing through the area. The nebula is approximately 1,600 [G/light year]s distant and 9 light years in diameter. This galactic [G/cluster] contains approximately 45 [G/star]s. This galactic [G/cluster] contains approximately 40 [G/star]s, some of which form the shape of a crescent. Large Mag. Cloud: The Large Magellanic Cloud [G/galaxy] is one of the closest galaxies to our own [G/Milky Way]. It is 169,000 [G/light year]s away and has a diameter of at least 50,000 light years. For many years, it was designated as an irregular galaxy, a galaxy with no uniform structure. Today, there are indications that the galaxy might be more like a barred-spiral, a spiral galaxy with a bar-shape at its core instead of the traditional spherical bulge. This galaxy is easily seen with the [G/naked eye]. Through a small telescope, one can begin to resolve individual stars, star clusters and nebulae within the hazy cloud. More detail is seen with low-power, wide angle eyepieces. This globular [G/cluster] is approximately 50,000 [G/light year]s away. The small, compact sphere of 50,000 to 100,000 [G/star]s appears as a fuzzy, star-like object in a small telescope. Through a large telescope, 4-inches (102mm) or larger, a few stars can be [G/resolve]d around the edge of the cluster. This galactic [G/cluster] contains approximately 35 [G/star]s. This [G/cluster] is 4,200 [G/light year]s away, 25 light years in diameter and contains 100 stars. M38 is the largest and dimmest of three galactic clusters in [Y/Auriga]. (See [M/M36] and [M/M37].) Crab Nebula: This faint, hazy cloud is all that remains of a star that died in a [G/supernova] explosion on July 4th, 1054 AD. According to ancient Chinese records, it was on that day a new star appeared in the sky, a star so bright, it could be seen even when the [G/Sun] was high in the sky. This guest star was visible for over a year until it faded from sight. From the description and location given in the ancient records, astronomers were able to connect the Crab Nebula with this spectacular event. Through the years the nebula has decreased dramatically in brightness. In the early 1700's, its faint hazy appearance in a telescope prompted Charles [G/Messier] to begin his famous catalog of objects. This cloud is also home to the first [G/pulsar] ever discovered. The faint cloud is still expanding away from the point of the explosion at an astounding rate of 600 miles per second. The cloud is approximately 6,300 [G/light year]s distant. Through a small telescope, the Crab Nebula appears as an extremely small, faint cloud. The cloud's irregular shape can be [G/resolve]d through larger telescopes. Great Orion Nebula: The Orion Nebula is one of the most famous diffuse [G/nebula]e in our skies. It is visible to the [G/naked eye] as the second star in [Y/Orion]'s sword. This nebula is 1600 to 1900 [G/light year]s away and 30 light years in diameter. The brighter, central region is about 6 light years across. Through a small telescope, details within the faint, wispy clouds of this nebula can be seen. Imbedded within the nebula are four young stars which form the Trapezium. These stars were born from the gas and dust within this cloud. Experiment with different eyepieces to explore the vast regions of this nebula. Wide-angle eyepieces are needed to observe the entire nebula, while high-power eyepieces show more details of specific areas within the nebula. Larger telescopes are able to [G/resolve] more details of the cloud structure. This small diffuse [G/nebula] lies just to the north of the [F/Great Orion Nebula]. Originally, this small nebula may have been a part of the larger dust cloud. This diffuse [G/nebula] is a detached segment of the [F/Great Orion Nebula]. This [G/cluster] is 4,100 [G/light year]s away, 14 light years in diameter, and contains over 60 stars. It is the smallest and brightest of three galactic clusters in [Y/Auriga]. See [M/M37] and [M/M38]. This diffuse nebula surrounds the star [W/Alnilam], the middle star of [G/Orion]'s belt. The brightness of the central star may make viewing the nebula difficult. PKS0537-441: This [G/quasar] is over 1 billion [G/light year]s away. Because of its tremendous distance, this quasar is only visible through the largest telescopes. Tarantula Nebula: Located within the [F/Large Mag. Cloud], the Tarantula Nebula is the largest diffuse [G/nebula] ever discovered. It is 169,000 [G/light year]s away, yet is still bright enough to be seen with the [G/naked eye]. This nebula is over 800 light years in diameter. If this nebula was the same distance from us as the [F/Great Orion Nebula], a famous diffuse nebula in our own galaxy, the Tarantula Nebula would cover over 30^ of the sky and be bright enough to cast shadows. Low-power eyepieces are recommended for viewing the entire nebula. To see more detail within the nebula, use medium-power eyepieces. This diffuse nebula lies just to the east of the bright star [W/Alnitak], the easternmost star in [Y/Orion]'s belt. The brightness of Alnitak may make viewing the nebula difficult. Horsehead Nebula: The Horsehead Nebula is a dark cloud that lies within a diffuse [G/nebula] just to the south of the bright star [W/Alnitak], the easternmost star in [Y/Orion]'s belt. The Horsehead Nebula can only be seen because it lies in front of some very bright [G/star]s. The light from these stars provides a bright background for the dark cloud. The Horsehead Nebula is best seen using long exposure astrophotography. This diffuse [G/nebula] is approximately 1,600 [G/light year]s away and a little over 2 light years in diameter. Though not as impressive as its brilliant neighbor, the [F/Great Orion Nebula], this nebula is easy to locate with a small telescope, resembling a faint comet through a low-power eyepiece. This [G/cluster] is 4,600 [G/light year]s distant, 25 light years in diameter, and contains 150 stars. It is the most distant of three galactic clusters in [Y/Auriga](see [M/M36] and [M/M38]). This faint, compact galactic [G/cluster] lies just off of the larger galactic cluster [M/M35]. It contains approximately 100 [G/star]s. This galactic [G/cluster] is 2,200 [G/light year]s away and 30 light years in diameter. The stars within this cluster appear to line up in rows, forming chains of lights. This cluster is best seen using low-power eyepieces. This galactic [G/cluster] contains approximately 100 [G/star]s. Rosette Nebula: The Rosette Nebula is 2,600 [G/light year]s away and 55 light years in diameter. Within this diffuse [G/nebula], long exposure astrophotographs reveal dark clumps of matter, called globules. Astronomers believe these globules are [G/protostars] that will eventually ignite and become stars. Details of this diffuse nebula are hard to resolve with a small telescope. With a low-power wide angle eyepiece, look for a faint cloud surrounding the star cluster [N/NGC 2244]. Large telescopes bring out more of the ring-like structure of this nebula, while long exposure astrophotography can [G/resolve] intricate detail within the gas cloud. This galactic [G/cluster] lies in the center of the [F/Rosette Nebula]. Some astronomers believe that the intense radiation released by newly formed stars in this cluster has cleared the surrounding area of gas and dust, giving the Rosette Nebula its ring-like appearance. The remaining gas glows because it is being heated by these young stars. Hubble's Variable Nebula: This unusual [G/nebula] varies not only its brightness, but its appearance as well. While its general triangular shape remains constant, dark features within the triangle disappear and reappear at unpredicted intervals. Astronomers are not sure of the cause of this variability. This nebula is believed to be 2,600 [G/light year]s away and 7 light years long. Cone Nebula: NGC 2264 is a combination of a galactic [G/cluster] and a [G/nebula]. The galactic cluster is the most noticeable of the two. About twenty of the cluster's brightest stars form a nice Christmas tree pattern. The nebula, sometimes called the Cone Nebula, lies on one side of the base of the Christmas tree and is difficult to resolve with a small telescope. NGC 2264 lies about 2,600 light years away and is about 20 light years across. This compact galactic [G/cluster] contains approximately 100 [G/star]s. This galactic [G/cluster] is located just south of the bright star [W/Sirius]. M41 is 2,350 [G/light year]s away and 20 light years in diameter. It is bright enough to be seen with the [G/naked eye] on a dark night. Through a small telescope, individual [G/star]s within the cluster can be seen. This galactic [G/cluster] contains approximately 80 [G/star]s. This galactic [G/cluster] can be found by drawing a straight line between the bright stars [W/Sirius] and [W/Procyon], with M50 lying about half way between. This cluster is about 2,900 [G/light year]s away and 9 light years in diameter. There are almost 200 stars in this cluster, although a small telescope will be able to [G/resolve] less than half that number. M50 is best seen using low-power, wide angle eyepieces. This galactic [G/cluster] contains approximately 100 [G/star]s. This galactic [G/cluster] contains approximately 30 [G/star]s. This large galactic [G/cluster] contains about 50 [G/star]s but may be difficult to distinguish from the surrounding background stars. This unusual galactic [G/cluster] appears to surround the [G/star] Tau Canis Majoris ([S/173446]). This cluster is 4,600 [G/light year]s away and 8 light years in diameter. At first glance, it may appear as a faint cloud surrounding the brighter star. Let your eye adapt to the view and you will be able to [G/resolve] individual stars from within the cluster. Larger telescopes are able to see more individual stars. Eskimo Nebula: The distance to this [G/planetary nebula] is difficult to determine, with estimates ranging from 1,360 to 3,600 [G/light year]s. Through a small telescope, look for a fuzzy star-like object. [G/CCD] images and long exposure astrophotographs reveal a bright central region with darker markings which, to some, resembles a face. Surrounding the central region is a halo of material which looks a bit like the fuzzy hood of a parka, hence the name Eskimo Nebula. This large, bright galactic [G/cluster] may be too big to fit within the [G/field of view] of your telescope. M47 is approximately 1,540 [G/light year]s away, although other estimates place the cluster at a much greater distance. The stars within this group are widely scattered, so it is best to use a low-power, wide angle eyepiece when viewing M47 through a telescope. Larger telescopes can [G/resolve] more stars within the cluster. This spiral [G/galaxy] is approximately 8 million [G/light year]s distant and 37,000 light years in diameter. [G/CCD] images and long exposure astrophotographs reveal clusters of stars within the compact spiral arms. Through a small telescope, use [G/averted vision] to detect a faint oval-shaped cloud. The larger the telescope, the brighter the image and the more details you can [G/resolve] within the galaxy. This rather strange globular [G/cluster] is one of the most distant clusters in our sky. Most globular clusters are found within a halo surrounding our galaxy, a halo that extends approximately 65,000 [G/light year]s from the galactic center. This cluster, however, lies at a distance of 182,000 light years, in a region otherwise devoid of clusters. In some ways it seems that it is trying to escape from the [G/Milky Way]. Through a telescope, this cluster can be seen as an extremely faint, round, fuzzy patch of light. This faint, compact galactic [G/cluster] contains approximately 100 [G/star]s. This galactic [G/cluster] contains approximately 80 [G/star]s. This [G/planetary nebula] is best seen through large telescopes (8-inches (203mm) or larger). NGC 2438 appears to belong to the galactic [G/cluster] [M/M46], but astronomers have determined that it is moving away from us at a much faster rate than the cluster. It is also believed that the planetary nebula is closer to us than M46. Current estimates indicate its distance to be 3,300 light years with an approximate diameter of 1 light year. This planetary nebula appears embedded within the galactic cluster. Through a large telescope, look for a star surrounded by a hazy glow near the cluster's perimeter. Estimates as to the distance to this galactic [G/cluster] range from 3,200 to 5,400 [G/light year]s. At 5,400 light years, the diameter of the cluster would be about 30 light years. [G/Star]s within this cluster form a circular pattern in the sky. Observers with larger telescopes may be able to [G/resolve] a tiny [G/planetary nebula], [N/NGC 2438], lying just inside the cluster, near its border. This cluster is best seen with low-power, wide angle eyepieces. This compact galactic [G/cluster] has a distinct wedge-shape appearance. It lies at a distance of 3,400 [G/light year]s and is 18 light years in diameter. M93 is best seen through low-power eyepieces. Although not as bright as [M/M46], which is also in the [G/constellation] of [Y/Puppis], this galactic [G/cluster] contains many more stars. These stars are evenly distributed throughout the group, making for a very rich starfield. This galactic [G/cluster] is 1,200 [G/light year]s away and 20 light years in diameter. It is bright enough to be seen with the [G/naked eye]. Through a small telescope, you should be able to pick out a bright red giant [G/star] near the center of the cluster. The star will not be brilliant red, but your eye should notice a hint of reddish color. This cluster is best seen through low-power, wide angle eyepieces. This galactic [G/cluster] contains approximately 75 [G/star]s and appears rather irregular in shape. This galactic [G/cluster] contains approximately 60 [G/star]s. This galactic [G/cluster] is 1,700 [G/light year]s away and 20 light years in diameter. The 80 or so stars within this cluster appear in a slightly triangular shape. M48 is best seen using low-power, wide angle eyepieces. Praesepe: The Praesepe [G/cluster] is one of the largest and brightest open clusters that can be seen from Earth. [G/Star]s within this cluster are grouped together in twos and threes. This cluster, which is also known as the Beehive, lies at a distance of 525 [G/light year]s and is 13 light years in diameter. It is best seen through low-power, wide angle eyepieces. This galactic [G/cluster] contains approximately 10 bright [G/star]s scattered over a large area of space. This cluster is best observed using a low-power, wide angle eyepiece. This galactic [G/cluster] is over 2,500 [G/light year]s away from us and 12 light years in diameter. The [G/star]s in this cluster are more compact than its neighbor, the [F/Praesepe] cluster. It is believed to be one of the oldest galactic clusters in our sky. This extremely small, extremely faint spiral [G/galaxy] is difficult to detect with a small telescope. Even with larger telescopes, a dark observing night and the use of [G/averted vision] are a must to detect this galaxy. This extremely rich globular [G/cluster] has a tightly packed central region. This [G/planetary nebula] is extremely small and faint. Through a small telescope, look for a slightly fuzzy, star-like object. This spiral [G/galaxy] has several dark lanes cutting through its spiral arms. These dark lanes give the galaxy an extremely mottled appearance. Through a small telescope, look for a small, mottled, oval shaped cloud. This spiral [G/galaxy] is one of the brightest in a group of galaxies located in [Y/Ursa Major]. It is 7 million [G/light year]s away and approximately 36,000 light years in diameter. The orientation of this galaxy in the sky allows us to see almost all of its spiral arms and large central bulge. Long exposure photographs show incredible detail within this distant galaxy. Through a small telescope, however, expect to see an oval-shaped hazy cloud. Lying close to M81 is [M/M82], another galaxy. This unusual [G/galaxy] appears as a pale narrow streak in the sky. Once thought to be an edge-on spiral galaxy, long exposure photographs of M82 show no indication of spiral structure. It is a strong radio source and there is evidence within its central region of a massive explosion that took place over 1.5 million years ago. This galaxy is 16,000 [G/light year]s away, over twice as far as [M/M81], its companion in the sky. Though a low-power, wide angle eyepiece it may be possible to see both M81 and M82 in the same [G/field of view]. Spindle Galaxy: This extremely flattened, elliptical [G/galaxy] is approximately 27 million [G/light year]s away, and 30,000 light year in diameter. Through a small telescope, look for a tiny, elongated patch of light. It is thought that a [G/black hole], whose mass equals 2 million stars like our Sun, lies at the center of this galaxy. This [G/planetary nebula] is approximately 2,500 [G/light year]s away and 0.5 light years in diameter. This cloud contains one of the brightest central stars of any planetary nebula, making it somewhat easy to detect. In a small telescope, look for a fuzzy, star-like object. This [G/planetary nebula] appears as a star-like object through a small telescope. PG1011-040: This [G/quasar] is over 1 billion [G/light year]s away. Because of its tremendous distance, this quasar is only visible through the largest telescopes. The [G/star]s within this globular [G/cluster] are not as compact as they are within most other globular clusters. Through a small telescope, look for a large, fuzzy patch. Ghost of Jupiter: This [G/planetary nebula] is somewhere between 2,000 and 3,000 [G/light year]s distant. Through a small telescope, look for a fuzzy star-like object. Larger telescopes can begin to make out its spherical nature. This loosely-grouped galactic [G/cluster] is 750 [G/light year]s away and surrounds the [G/star] Theta Carinae ([S/251083]). The cluster is bright enough to be seen with the [G/naked eye] on a dark night. Through a telescope, it is best seen using low-power, wide angle eyepieces. Eta Carinae Nebula: The nature of this extremely unusual [G/nebula] has puzzled astronomers for centuries. In 1843, the [G/star] at the center of the nebula, a star that is 100 times more massive and 4 million times brighter than our [G/Sun], underwent a tremendous explosion which lasted for 20 years. Somehow, the star survived. Since then, it has produced unusual readings and fluctuations which astronomers are still trying to decipher. The star and nebula are 7,500 [G/light year]s away. Through a small telescope, look for a large, faint, wispy cloud. This barred spiral [G/galaxy] is approximately 29 million [G/light year]s away. Long exposure astrophotographs of this galaxy show a faint ring surrounding a rectangular streak (the barred central region of the galaxy). It is extremely faint and difficult to see with a small telescope. This galaxy is best observed on extremely dark nights. Use a low-power eyepiece for the brightest image possible and [G/averted vision] when looking through the telescope. With a larger telescope (8-inches (203mm) or larger) this galaxy appears as a faint round cloud. The barred structure is only visible on long exposure photographs or [G/CCD] images. Another galaxy, [M/M96], lies nearby. Larger and slightly brighter than its nearby neighbor [M/M95], this spiral [G/galaxy] is approximately 29 million [G/light year]s away. It has a large oval-shaped [G/nucleus] and tightly-wound spiral arms. While brighter than M95, it is still extremely faint and difficult to see through a small telescope. Observe this galaxy on a dark night using low-power eyepieces and [G/averted vision]. This elliptical [G/galaxy] is approximately 32 million light years away. It is believed to have a giant black hole at its core. The mass of this giant [G/black hole] is equal to 100 million stars like our Sun. This elliptical [G/galaxy] was not an original entry in [G/Messier]'s catalog, but was added to the list in 1947. It is about 32 million [G/light year]s away and is extremely small and faint in the sky. As a result, is difficult to see in a small telescope. Look for a faint, fuzzy star-like object. Larger telescopes can begin to make out a slight irregularity to its round shape. A giant [G/black hole], with a mass equal to 50 million solar masses, is believed to lie at the center of this galaxy. This galactic [G/cluster] is one of the best open clusters in the sky. It is roughly 1,300 [G/light year]s away and 25 light years in diameter. The [G/star]s within this cluster are scattered loosely over a large area of the sky. As a result, it appears elongated in shape and is best seen through low-power, wide angle eyepieces. This edge-on spiral [G/galaxy] is approximately 25 million [G/light year]s away. It was not an original entry in [G/Messier]'s catalog, but was added to the list in 1960. It is extremely faint in our skies and is therefore difficult to see with a small telescope. Observe M108 on a dark night, using a low-power eyepiece for the brightest image possible. Use [G/averted vision] to detect a narrow streak of light. Larger telescopes can detect irregular mottling within the cloudy patch. Owl Nebula: The distance to this [G/planetary nebula] has proven rather difficult to pinpoint. Estimates range from 1,600 to 10,000 [G/light year]s. A standard value of 3,000 light years has been used often, giving the nebula a diameter of approximately 3 light years. At [G/magnitude] 12, this planetary nebula is so faint, it is almost impossible to observe through a small telescope. A 4-inch (102mm) telescope can begin to make out a faint, tiny, round patch of light. The larger the telescope, the brighter the image. M65 is one of a pair of bright spiral [G/galaxy]s that lie relatively close together in the [G/constellation] of [Y/Leo]. In fact, M65 and its companion, [M/M66] can be seen in the same [G/field of view] of a small telescope using a low-power, wide angle eyepiece. Even though they look close together, the two galaxies are separated by more than 180,000 [G/light year]s. M65 is 29 million light years away and has a diameter of 60,000 light years. Through a telescope, it appears as a faint elongated patch of light. This extremely small, extremely faint spiral [G/galaxy] is difficult to detect with a small telescope. Even with larger telescopes, a dark observing night and the use of [G/averted vision] are a must to detect this galaxy. M66 is one of a pair of spiral [G/galaxy]s that lie relatively close together in the [G/constellation] of [Y/Leo]. This galaxy is brighter and more compact than its companion, [M/M65]. M66 is 29 million [G/light year]s away, with a diameter of 50,000 light years. Through a small telescope, the galaxy appears as a faint elongated patch of light. Through larger telescopes, details within its broad spiral arms become visible. M66, along with its companion, M65, can be seen in the same [G/field of view] of a small telescope using a low-power, wide angle eyepiece. This galactic [G/cluster] is a loose grouping of approximately 60 [G/star]s. This diffuse [G/nebula] surrounds the star Lambda Centauri, [S/223603], forming a faint, wispy cloud around the bright star. The star lies at a distance of 160 [G/light year]s and is 275 times more [G/luminous] than our [G/Sun]. This barred spiral [G/galaxy] was not listed in [G/Messier]'s original catalog, but was added in 1960. It is extremely small and faint in our skies and therefore difficult to see with a small telescope. Observe this galaxy on a dark night, using a low-power eyepiece to achieve the brightest image possible. Use [G/averted vision] to detect a faint, small, oval-shaped patch of light. Ring-Tail Galaxy: This entry represents one of two antennae in an unusual galactic system. [G/CCD] images and long exposure astrophotographs reveal two lobes of material, each a possible galactic [G/nucleus]. Sweeping off each lobe is a long filament of material. This system is 90 million [G/light year]s away and 100,000 light years across. It is extremely faint and will be difficult to detect in a small telescope. This entry represents the second of the two antennae in an unusual galactic system. [G/CCD] images and long exposure astrophotographs reveal two lobes of material, each a possible galactic [G/nucleus]. Sweeping off each lobe is a long filament of material. This system is 90 million [G/light year]s away and 100,000 light years across. It is extremely faint and will be difficult to detect in a small telescope. This spiral [G/galaxy] is positioned nearly edge-on in the sky and estimates give its distance as 35 million [G/light year]s. Through a small telescope, it is extremely difficult to see. Observe this galaxy on a dark night and use low-power eyepieces and [G/averted vision] to see a faint, narrow streak. Larger telescopes can detect mottling within the streak (the spiral arms) and possible brightening towards the center (the galaxy's [G/nucleus]). This spiral [G/galaxy] is positioned almost edge-on in relationship to Earth. As a result, it appears as a highly elongated oval patch in the sky. It is extremely faint and may be difficult to see through a small telescope. Utilizing [G/averted vision] is a must to detect this galaxy. PG1216+069: This [G/quasar] is over 1 billion [G/light year]s away. Because of its tremendous distance, this quasar is only visible through the largest telescopes. This extremely narrow, edge-on [G/galaxy] can be seen as a faint streak through a small telescope. This spiral [G/galaxy] is 45 to 50 million [G/light year]s away, although it is moving farther away from us all the time at the tremendous rate of 1,490 miles (2,400km) per second. Long exposure astrophotographs of this galaxy show two distinct spiral arms with smaller tendrils spraying off one side of the round [G/nucleus]. Through a small telescope, however, this galaxy is extremely faint and difficult to see. Observe on a dark night using a low-power eyepiece and [G/averted vision]. Through larger telescopes, look for an oval patch of light that brightens towards the center. This spiral [G/galaxy] was not an original entry in [G/Messier]'s catalog, but was added to his list in 1947. It is 25 million [G/light year]s away and appears to be receding at a rate of approximately 300 miles per second. Long exposure photographs and [G/CCD] images of this galaxy show a rather elongated [G/nucleus] and faint spiral arms. Through a small telescope, observe M106 on a dark night using a low-power eyepiece to achieve the brightest image possible. Use [G/averted vision] to detect a faint, cigar-shaped streak of light. The nucleus appears brighter towards the middle of the cigar shape. It is believed that a [G/black hole], whose mass is equal to 40 million stars like our Sun, lies at the center of this galaxy. This elliptical [G/galaxy] is 90 million [G/light year]s away. It is believed to have a enormous [G/black hole] at its core, a black hole whose mass is equal to 400 million stars like our Sun. This spiral [G/galaxy] is just one of over 3,000 distant galaxies in the [G/Virgo Cluster] and is believed to be 65-70 million [G/light year]s away. Through a small telescope, detecting this faint galaxy is a challenge. Use a low-power eyepiece and [G/averted vision] to make out a small faint patch of light. Through a larger telescope, 8-inches (203mm) or larger, this galaxy appears as a faint, round cloud with a slight brightening towards its center. Long exposure astrophotographs are needed to see any details within its spiral arms. In 1660, a German astronomer identified a [G/nebula] at this location. Later, Charles [G/Messier] found no evidence of a nebula, yet he included the entry in his catalog anyway. A faint double star system, with its two stars fairly close together, may have been mistaken for the mysterious missing nebula. This [G/galaxy] is the largest spiral-type galaxy in the [G/Virgo Cluster]. Although the largest in this region, it appears small and extremely faint through a small telescope. Observe this galaxy on extremely dark nights using a low-power eyepiece and [G/averted vision]. Larger telescopes show more details within the slightly oval-shaped patch of light, including a brighter central region. This elliptical [G/galaxy] is one of 3,000 galaxies within the [G/Virgo Cluster], which lies at a distance of 50-70 million [G/light year]s. A giant [G/black hole], with a mass equal to 300 million stars like our Sun, is believed to lie at the center of this galaxy. This galaxy lies fairly close to another elliptical galaxy, [M/M86]. Both are faint, and difficult to see through a small telescope. It is best to view this object on extremely dark nights, using a low-power eyepiece and [G/averted vision]. This elliptical [G/galaxy] is one of 3,000 galaxies within the [G/Virgo Cluster], which lies at a distance of 65-70 million [G/light year]s. It is best to view this galaxy on extremely dark nights, using a low-power eyepiece and [G/averted vision]. The stars in this [G/cluster] are rather loosely spaced, which is a little unusual for a globular cluster. It is the fainter of two nice clusters in the [G/constellation] of [Y/Musca]. This elliptical [G/galaxy] lies fairly close to another elliptical galaxy, [M/M84]. Unlike its nearby companion, and several other galaxies in this region of space, M86 is not an actual member of the [G/Virgo Cluster] of galaxies. At a distance of 20 million [G/light year]s, it is much closer than the large group. This galaxy is extremely faint and is best seen through large telescopes, using low-power eyepieces and [G/averted vision]. This irregular [G/galaxy] is an extremely faint, rectangular patch that is difficult to see even under the best observing conditions. 3C273: This Quasar is billions of light years away. This elliptical [G/galaxy] is 70 million [G/light year]s away and about 50,000 light years in diameter. Through a small telescope, M49 resembles a globular [G/cluster], with a round, hazy appearance. Because of its enormous distance, it is not possible to resolve stars within this galaxy, even with larger telescopes. This elliptical [G/galaxy] is one of the largest in the [G/Virgo Cluster] of galaxies. The total mass of this system is calculated to be an incredible 790 billion times the mass of our [G/Sun]. At its core, there is an incredibly massive [G/black hole], equal to 3 billion stars like our Sun. Long exposure astrophotographs show this galaxy is surrounded by an unusually large number of globular [G/cluster]s, almost 1,000. For comparison, just over 100 globulars are known to surround our [G/Milky Way]. Even though this galaxy is so large, it appears small and faint in our skies. After all, it is over 50 million [G/light year]s away. Through a small telescope, it is best to observe on an extremely dark night. Use a low-power eyepiece for the brightest image possible, and use [G/averted vision]. Larger telescopes reveal a round, hazy patch of light. This spiral [G/galaxy] is found within the [G/Virgo Cluster] of galaxies. Long exposure astrophotgraphs reveal this galaxy to be a tiny version of the [G/Andromeda Galaxy]. Through a small telescope, it is extremely faint and difficult to see, and best observed on extremely dark nights. Observe with a low-power eyepiece for the brightest image possible and use [G/averted vision]. Larger telescopes reveal an elongated, hazy patch of light. M91 is considered [G/Messier]'s mystery object. In 1781, he recorded an object resembling a "nebula without stars" at this location. Since then, no one has been able to locate anything resembling Messier's description at these coordinates. Astronomers debate whether Messier recorded a comet that has long since moved along, or if he inaccurately recorded the coordinates of a nearby faint galaxy. Either way, there isn't much to look at here! This elliptical [G/galaxy] is one of over 3,000 galaxies within the [G/Virgo Cluster]. Through a small telescope, it is extremely faint and difficult to see. Through a large telescope, 4-inch (102mm) or larger, this galaxy appears as a small, slightly oval-shaped patch of light. The larger the telescope, the brighter the image. This faint spiral [G/galaxy] is a challenge for a small telescope, requiring extremely dark nights and the use of [G/averted vision] to begin to detect a small, fuzzy, oval-shaped patch. The larger the telescope, the brighter the image and the easier it will be to observe. This edge-on spiral [G/galaxy] is approximately 20 million [G/light year]s away and 90,000 light years in diameter. Through a small telescope, look for a long narrow streak that brightens towards the center. This spiral [G/galaxy] is one of over 3,000 galaxies found in the [G/Virgo Cluster]. It is over 65 million [G/light year]s away. Through a small telescope, it is extremely faint and difficult to see. This galaxy is best observed on a dark night, using a low-power eyepiece for the brightest image possible. Also, use [G/averted vision]. Through a larger telescope, look for an oval-shaped hazy patch with a slight brightening towards the [G/galactic center]. This barred spiral [G/galaxy] belongs to a vast group of galaxies called the [G/Virgo Cluster]. Galaxies within this super cluster are believed to be 65-70 million [G/light year]s away. Through a small telescope, detecting this faint galaxy is a challenge. Use a low-power eyepiece and [G/averted vision] to make out a small faint patch of light. Through large telescopes, 8-inches (203mm) or larger, look for a small, faint, oval-shaped patch which is the galaxy's central region. Its spiral arms form a much fainter, mottled cloud around the central oval. This globular [G/cluster] is 46,000 [G/light year]s away and 100 light years in diameter. Look for a faint, round hazy patch of light. Larger telescopes are needed to [G/resolve] individual stars within the cluster. M68 is best seen using medium power eyepieces. Sombrero Galaxy: This spiral [G/galaxy] is situated in our skies so we see it almost exactly edge-on. It is about 30 million [G/light year]s away and 82,000 light years across. This galaxy gets its name from a dark lane that runs across the enormous center of the galaxy, appearing to cut the galaxy in two, and causing the top portion to look something like a sombrero. An extremely large [G/black hole] is located at the center of this galaxy, a black hole whose mass is equal to 1 billion stars like our Sun. At least a 6-inch (150mm) telescope is required to [G/resolve] this dark lane. Through a small telescope, look for a faint, elongated patch of light with a brighter central region. This elliptical [G/galaxy] belongs to the [G/Virgo Cluster]. Through a small telescope, detecting this faint galaxy is a challenge. Use a low-power eyepiece and [G/averted vision] to make out a small, faint patch of light. Through a large telescope, 8-inches (203mm) or larger, look for an extremely faint oval cloud, with a slight brightening towards the center. This edge-on spiral [G/galaxy] is faint and difficult to see. When observing, look for a long, faint, narrow streak. Large telescopes may begin to [G/resolve] mottling within the galaxy which represents dust in the spiral arms. This galactic [G/cluster] is a fairly compact grouping of approximately 20 [G/star]s. This elliptical [G/galaxy] is just one of over 3,000 distant galaxies in the [G/Virgo Cluster] and is believed to be 65-70 million [G/light year]s away. It is one of the largest elliptical galaxies known, second only to [M/M49] in size and mass. Through a small telescope, look for a hazy oval patch of light, resembling a fuzzy star. The image through a larger telescope is brighter, but at its vast distance, it is not possible to [G/resolve] any individual [G/star]s. This elliptical [G/galaxy] is extremely small and faint, making it difficult to detect with a small telescope. Even with larger telescopes, a dark observing night and the use of [G/averted vision] are a must to detect this galaxy. This spiral [G/galaxy] is 20 million [G/light year]s away and about 33,000 light years in diameter. Because the spiral arms of this galaxy are wound very tightly around its large central core, it is difficult to see any spiral structure through a small telescope. Instead, look for a small, round hazy patch. Coal Sack: From as far back as the 1500's, people have noted this dark, starless patch of sky known as the Coal Sack. The Coal Sack is a dark [G/nebula], an extremely large cloud of gas and dust that does not contain any stars. If it did contain stars, or if there were stars close to it, those stars would illuminate the cloud, thus making it visible. Instead, we see nothing. This dark nebula lies 550 [G/light year]s away and is about 65 light years in diameter. Look for the Coal Sack just to the east of [W/Acrux]. Jewel Box: This magnificent galactic [G/cluster] surrounds the tenth brightest [G/star] in the [G/constellation] of [Y/Crux]. The cluster is 7,700 [G/light year]s away. There is a central knot of stars within the cluster that is about 25 light years in diameter. Stars on the outer fringes make the entire cluster about 50 light years in diameter. The [G/luminosity] of the brightest star in the cluster is 80,000 times that of our [G/Sun]. That star, along with two other bright stars in the cluster form a triangle. The Jewel Box is best seen with low-power, wide field eyepieces. Black Eye Nebula: A dark spiral arm cuts a swath through a portion of the bright central region of this galaxy, earning it the nickname "Black Eye". This galaxy is approximately 12 million [G/light year]s away. At least a 4-inch (102mm) telescope is required to detect the "Black Eye" appearance. Using a medium-power eyepiece can aid in bringing out the contrast between the dark spiral arm and the bright central region. This globular [G/cluster] is one of two nice clusters in [Y/Musca]. It is brighter and more compact than its neighbor, [C/C108], although, through a small telescope it will appear rather faint. Look for an increase of brightness towards the center of the cluster. This elliptical [G/galaxy] is the brightest galaxy within the Coma Cluster, a group containing over 1,000 galaxies. The Coma Cluster is approximately 400 million [G/light year]s away and members stretch across 20 million light years of space. This edge-on spiral [G/galaxy] appears as a faint, narrow streak when observing on a dark night and using a low-power eyepiece and [G/averted vision]. Some mottling within the narrow cloud may be detected with larger telescopes. This spiral [G/galaxy] has tightly bound spiral arms and a compact [G/nucleus]. It appears as an extremely small, faint, oval-shaped patch of light only under the best observing conditions. This globular [G/cluster] is 65,000 [G/light year]s away and over 100 light years in diameter. The total [G/luminosity] of M53 is 200,000 times that of our [G/Sun]. Through a small telescope, this cluster is easily seen as a faint, round patch of light. Larger telescopes are able to resolve individual stars around the edge of the cluster. Sunflower Galaxy: This spiral [G/galaxy] is approximately 35 million [G/light year]s away and 90,000 light years in diameter. Its central oval-shaped region is brighter on one side than the other, giving it a rather unusual, lopsided appearance. Through a small telescope, use a low-power eyepiece and [G/averted vision] to detect a small faint patch of light. 4-inch (102mm) or larger telescopes are needed to begin to detect the faint nebulosity of the spiral arms. Centaurus A: This peculiar [G/galaxy] is approximately 15 million [G/light year]s away and 100,000 light years in diameter. Through large telescopes, this galaxy appears as a glowing sphere with a thick, dark band dividing it into two sections. Its strange appearance has puzzled astronomers for many years. This galaxy is also an unusually strong source for natural radio emissions. Astronomers believe that this galaxy is undergoing a series of extremely powerful explosions within its core, although the reason for these explosions is not completely understood. Through a small telescope, look for a faint, hazy patch with a slight darkening through its center. Centaurus A is best seen using medium-power eyepieces. Omega Centauri: This globular [G/cluster] is 17,000 [G/light year]s away and 150 light years in diameter. The cluster can be seen as a hazy, faint [G/star] with the [G/naked eye]. Through a small telescope, look for a round hazy patch of light. Larger telescopes are able to resolve individual stars within the cluster. The stars in this cluster are extremely close together, with an average distance between stars of only 0.1 light years. For comparison, the distance between the [G/Sun] and its closest neighbor, Alpha Centauri ([S/252838]) is 4.2 light years. Whirlpool Galaxy: This spiral [G/galaxy] is 35 million [G/light year]s away and over 100,000 light years in diameter. A giant [G/black hole], with a mass equal to one million stars like our Sun, is believed to lie at the center of this galaxy. Through a small telescope, look for a dim, hazy patch of light with a brighter central region. Because of the galaxy's face-on orientation in the sky, its spiral or pinwheel shape is clearly visible in photographs and larger telescopes. The giant galaxy has a small companion nearby, which can also be seen through larger telescopes. This spiral [G/galaxy] is 10 million [G/light year]s away and about 30,000 light years in diameter. While this is the 25th brightest galaxy in the sky, it is extremely faint in small telescopes. Larger telescopes are required to show the slight brightening at the central core. This spiral [G/galaxy] appears as a faint, tiny, hazy oval through a small telescope when observing under dark skies and using [G/averted vision]. [G/CCD] images and long exposure astrophotographs reveal this galaxy's beautiful spiral structure. This globular [G/cluster] is 35,000 [G/light year]s away and over 220 light years in diameter. Through a small telescope, look for a faint, round hazy patch of light. Larger telescopes are able to resolve [G/star]s around the edge of the cluster. M3 is best seen through medium or high power eyepieces. This globular [G/cluster] appears as a tiny, fuzzy, round patch through a small telescope. Larger telescopes can begin to [G/resolve] stars around the cluster's border. This spiral [G/galaxy] is 15 million [G/light year]s away and 90,000 light years in diameter. Long exposure photographs taken through large telescopes reveal a galaxy with a bright, tiny [G/nucleus] and an impressive array of spiral arms. Within its spiral arms are distinct clumps of stars. Unfortunately, this incredible detail can only be detected on sensitive photographic film and CCD cameras. Through a small telescope, the human eye can only detect a very small, faint patch of light under the best observing conditions. PG1435-067: This [G/quasar] is over 1 billion [G/light year]s away. Because of its tremendous distance, this quasar is only visible through the largest telescopes. This globular [G/cluster] is approximately 100,000 [G/light year]s away. Measurements of this cluster show it to be moving almost 170 miles (273 km) per second away from our galaxy, fast enough to escape the gravitational tug of our [G/Milky Way] and become an intergalactic traveler. However, you won't be able to see any movement when looking through a telescope. Instead, look for a fuzzy, stationary, "star-like" object. This galactic [G/cluster] contains approximately 80 [G/star]s which form a nice compact group. Observe this cluster with a low-power, wide angle eyepiece. There is some controversy about the identity of this object. In correspondence Messier admitted that it might be a duplicate of M101, as it appears in some catalogs. Other scholars have examined his observations, and believe that NGC 5866 is actual M102. This is consistent with other journal entries and correspondence. Enjoy the object and join the argument that has been going on for 300 years. The [G/star]s in this globular [G/cluster] are more loosely packed than stars in most other globular clusters. This globular [G/cluster] is about 30,000 [G/light year]s away and 100 light years in diameter. Through a small telescope, look for a faint, round hazy patch. With a 4-inch (100mm) or larger telescope, it is possible to [G/resolve] individual [G/star]s around the edge of the cluster. This globular [G/cluster] contains 50,000 to 100,000 [G/star]s. This galactic [G/cluster] contains approximately 30 stars that are brighter than [G/magnitude] 7. It is located just north of the northernmost star in the triangle of [Y/Triangulum Australe]. This small, compact globular [G/cluster] is 3,600 [G/light year]s away and about 50 light years in diameter. Through a small telescope, it appears as a round, hazy patch of light that is slightly brighter towards the center. Larger telescopes are able to [G/resolve] stars on the fringes of the cluster. M80 is best seen using medium- to high-power. This rich galactic [G/cluster] contains over 100 [G/star]s. This globular [G/cluster] is located just to the west of the bright [G/star], [W/Antares] and is an easy target for a small telescope. Even though estimates of its distance range from 6,200 to 10,000 [G/light year]s, it is possible to [G/resolve] stars around the edges of this cluster with only a 4-inch (100mm) telescope and a high-power eyepiece. M4 is best seen using medium- to high-power eyepieces. This galactic [G/cluster] is 1,600 [G/light year]s away. It contains approximately 100 [G/star]s and is best viewed through low-power, wide angle eyepieces. The [G/star]s within this globular [G/cluster] are rather loosely packed. However, its faintness makes it difficult to [G/resolve] into individual stars, even with larger telescopes. Through a small telescope, look for a faint, fuzzy, "star-like" object. This globular [G/cluster] is 10,000 [G/light year]s away and 50 light years in diameter. Its huge sphere of 50,000 to 100,000 stars was not an original entry in [G/Messier]'s catalog, but was added to his list in 1947. Through a small telescope, look for a fuzzy, "star-like" object. Larger telescopes can begin to [G/resolve] individual [G/star]s around the edge of the cluster. This galactic [G/cluster] contains approximately 30 [G/star]s which may be difficult to distinguish from the background stars of the [G/Milky Way]. M13 is the closest and brightest of two globular clusters in [Y/Hercules]. This [G/cluster] is 22,000 [G/light year]s away and 160 light years in diameter. The [G/star]s within its huge sphere are not as compact as they are in the neighboring cluster, [M/M92]. Through a small telescope, look for a round, hazy patch of light. Stars within the cluster may be [G/resolve]d using medium or high power eyepieces. To some observers, M13 looks like a pile of sugar crystals spilled on a black table. Larger telescopes are able to resolve more stars within the cluster. This globular [G/cluster] is approximately 20,000 [G/light year]s away and lies about 2,000 light years from [M/M10], a nearby cluster. The [G/star]s within M12 are loosely-grouped together, allowing a larger telescope (at least 6-inches or 152mm in diameter) to resolve stars within the cluster. Smaller telescopes can see a faint, irregular glow. This galactic [G/cluster] is 5,700 [G/light year]s away and only 8 light years in diameter. It is a small, intense cluster, with several bright [G/star]s gathered into a tight group. To some, this cluster looks like a compact version of the [F/Pleiades]. This globular [G/cluster] is approximately 20,000 [G/light year]s away and lies about 2,000 light years from its neighboring cluster, [M/M12], although the two clusters appear fairly close together in our skies. M10 is perhaps the most distinct of all the globular clusters in [Y/Ophiuchus]. It is compact, containing between 50 and 100 thousand [G/star]s, and appears as a round, hazy patch through a small telescope. Larger telescopes (at least 6-inches or 152mm in diameter) are needed to [G/resolve] stars within the cluster. M62 lies on the border of [Y/Ophiuchus] and [Y/Scorpius]. The distance of this [G/cluster] is about 26,000 [G/light year]s, although there is some uncertainty in this measurement. This cluster appears irregular in shape, unlike the traditional spherical shape of most globular clusters. The stars within the cluster are packed tightly together. Through a small telescope, M62 appears as a faint, hazy patch of light. Larger telescopes (at least 6-inches or 152mm in diameter) are needed to [G/resolve] any stars around the edge of the cluster. This globular [G/cluster] is believed to be imbedded in the central bulge of our [G/Milky Way] galaxy. There are large amounts of dust in this region of space which block some of the light from the cluster. Since astronomers aren't sure how much light is being blocked, it is difficult to determine the cluster's absolute brightness, an important factor used when determining distances of celestial objects. As a result, the distance of M19 is uncertain. Values range from 20,000 to 30,000 [G/light year]s. This globular cluster has an unusual oval shape, a hint of which can be [G/resolve]d through a small telescope. Individual [G/star]s within the cluster can be resolved with larger telescopes. Bug Nebula: This [G/nebula] has an unusual, elongated shape, making its classification somewhat difficult. Some refer to it as a diffuse nebula, most refer to it as a [G/planetary nebula]. Observing this nebula through a small telescope requires an extremely dark night, a low-power eyepiece (for the brightest image possible) and the use of [G/averted vision]. M92 is one of two beautiful globular clusters in [Y/Hercules]. This [G/cluster] is fainter and more compact than its counterpart, [M/M13]. M92 is 37,000 [G/light year]s away. Through a small telescope, look for a round, hazy patch of light. Stars around the edge of the cluster may be [G/resolve]d using a medium power eyepiece. Larger telescopes are able to resolve more stars within the cluster. This globular [G/cluster] was discovered by Charles [G/Messier] in 1764. It is 26,000 [G/light year]s away and 60 light years in diameter. It is very compact and appears as a tiny, round, hazy glow in the sky through a small telescope. Large telescopes (at least 6-inches or 152mm in diameter) are needed to [G/resolve] [G/star]s around the edge of the cluster. This loosely-packed globular [G/cluster] is rather faint in our skies. Through a small telescope, look for an extremely faint, fuzzy object. A neighboring globular cluster, [C/C86], provides a much brighter target. This globular [G/cluster] was discovered by Charles [G/Messier] in 1764, the same year he discovered several other globular clusters in [Y/Ophiuchus]. The [G/star]s within this cluster are packed tightly together, forming a compact, glowing sphere in the sky. M14 is thought to be 65,000 to 70,000 [G/light year]s away. Through a small telescope, it appears as a small, round, hazy patch of light. Large telescopes (at least 6-inches or 152mm in diameter) are needed to [G/resolve] any stars around the edge of the cluster. Butterfly Cluster: This galactic [G/cluster] is about 2,000 [G/light year]s away and 20 light years in diameter. To some, the loose scattering of stars within this cluster resemble the shape of a butterfly with its wings spread open in flight. This cluster is best seen using wide angle eyepieces. At a distance of 8,200 [G/light year]s, this is the closest globular [G/cluster] to our [G/galaxy]. The [G/star]s within this cluster are loosely scattered over a diameter of 50 light years, making it one of the easiest globulars to [G/resolve] into individual stars. This beautiful galactic [G/cluster] is 800 [G/light year]s distant. It is very loosely packed and covers almost one degree of the sky. (The full [G/Moon] covers only half a degree.) It contains 80-100 [G/star]s brighter than [G/magnitude] 10, although just a fraction of these stars are visible through a small telescope. The brighter stars that are visible will offer quite a view. M7 is best seen through low-power, wide angle eyepieces. This galactic [G/cluster] is 2,000 [G/light year]s away and 15 light years across. The [G/star]s within this cluster are loosely scattered and it may be difficult to separate the stars of the cluster from the fainter background stars of the [G/Milky Way]. M23 is best seen using a low-power, wide angle eyepiece. Cats Eye Nebula:This [G/planetary nebula] is approximately 3,200 [G/light year]s away and 0.3 light years in diameter. In 1864, it was the first of its kind to be observed using a [G/spectroscope], thus determining that planetary nebulae were gaseous objects instead of closely-packed spheres of [G/star]s. Through a small telescope, look for a fuzzy, star-like object. Larger telescopes using medium-power can begin to [G/resolve] some nebulosity. Trifid Nebula: This diffuse [G/nebula] is a stellar birthplace. Hot, glowing clouds of hydrogen gas light up this compact nebula. Calculating the distance to the Trifid has been difficult, resulting in values ranging from 2,200-5,200 [G/light year]s. Through a small telescope, the nebula can be seen as a faint elongated patch of light with a slight amount of darkening through the center of its brighter side. Larger telescopes (at least 8-inches or 203mm) can begin to [G/resolve] the dark dust lanes that divide the brighter part of the cloud into different segments. Lagoon Nebula: This diffuse [G/nebula] lies just a little north and west of the "Teapot" in [Y/Sagittarius]. Large clouds of hydrogen gas within the nebula are heated by newly formed [G/star]s. These heated gases emit a visible glow which appears red in long-exposure photographs. When viewing the nebula with a telescope, the eye is not as sensitive as photographic film. As a result, it appears as a pale white, irregular cloud. The galactic [G/cluster], [N/NGC 6530] can be found embedded within the nebula. Also, dark bands of dust can be seen. The Lagoon Nebula is approximately 5,150 [G/light year]s away with a total diameter of roughly 115 light years. Because of its large size, it is best to use a low-power, wide angle eyepiece to view the nebula in its entirety. Higher magnification may be used, allowing for only a small portion of the cloud to be seen at a time, but in greater detail. This galactic [G/cluster] lies close to the [F/Trifid Nebula]. It is 2,200 [G/light year]s away and 17 light years in diameter. This galactic [G/cluster] is embedded within the [F/Lagoon Nebula]. Studies have shown the stars in this cluster to be extremely young. If the stars in this cluster actually formed from the Lagoon Nebula, this cluster would then be approximately 5,150 [G/light year]s away. This globular [G/cluster] is a huge sphere of between 50,000 to 100,000 stars. Through a small telescope, look for a small, round fuzzy patch. Larger telescopes can [G/resolve] individual [G/star]s around its border. This [G/Messier] object is unusual in that it is not one specific object. Instead, M24 seems to represents one of the huge clouds of stars near the center of our [G/Milky Way] galaxy. This star cloud, easily visible to the [G/naked eye], contains millions of stars and is best viewed using low-power, wide angle eyepieces or binoculars. Several dark, dust clouds border M24 on one side. Eagle Nebula: This nebula was made famous by photos taken by the [G/Hubble Telescope]. Through the space telescope, a small portion of this nebula was shown in amazing detail, revealing three giant columns surrounded by swirling clouds of gas. This hydrogen gas is heated by young, newly formed [G/star]s buried within the cloud. The hot gases then emit a glow which we can observe. Through a small telescope on Earth, a faint wispy cloud can be seen surrounding a small cluster of stars. The larger the telescope, the more detail can be [G/resolve]d within the nebula. The Eagle Nebula is approximately 8,000 light years away. This galactic [G/cluster] is 4,900 [G/light year]s away. It consists of a few, loosely scattered [G/star]s. The cluster may be difficult to distinguish from the background stars of the [G/Milky Way]. Galactic clusters are best viewed using low-power, wide angle eyepieces. When viewing the cluster, look for a slightly higher concentration of stars amid the fainter background stars. Swan Nebula: This faint diffuse [G/nebula] appears in the shape of a swan floating on a lake. A bright cloud forms the swan's body, then its neck curves up from one side of the body to its small head. There are no bright [G/star]s visible within the cloud, although there are many fainter stars filling the background. It is possible that light from hot, young stars within this nebula is blocked by dense clouds of gas and dust. The Swan Nebula is about 5,700 [G/light year]s away. The brighter cloud that forms the swan's body is about 12 light years across. Through a small telescope, look for a faint slash of light representing the body of the swan. Low-power eyepieces are recommended. Through larger telescopes, it may by possible to use medium power eyepieces. This globular [G/cluster] is more dense and compact than its neighbor [M/M22]. It is also fainter. This cluster is 15,000 [G/light year]s away and about 65 light years in diameter. M28 appears as a round, hazy patch through a small telescope. Larger telescopes are needed to [G/resolve] individual [G/star]s around the edge of the cluster. This cluster is best seen using medium- to high-power eyepieces. This irregular-shaped galactic [G/cluster] contains approximately 30 [G/star]s. This globular [G/cluster] is approximately 36,000 [G/light year]s away and 70 light years in diameter. Through a small telescope, look for a fuzzy "star-like" object. This galactic [G/cluster] is about 2,000 [G/light year]s away and 20 light years in diameter. It contains a scattering of just a few bright [G/star]s against a backdrop of the [G/Milky Way]. M25 is best seen using low-power, wide angle eyepieces. This globular [G/cluster] is 9,600 [G/light year]s away and 50 light years in diameter. Through a small telescope, this huge ball of over 100,000 [G/star]s appears as a hazy, slightly elongated, patch of light. Larger telescopes, 4-inches (100mm) and larger, begin to [G/resolve] individual stars around the edge of the cluster. The larger the telescope, the more stars can be resolved. M22 is best seen using medium- to high-power eyepieces. This scattered galactic [G/cluster] contains approximately 50 [G/star]s and lies extremely close to the bright star Alpha Scuti [S/142408]. The 80 [G/star]s in this galactic [G/cluster] are very loosely scattered. This globular [G/cluster] is approximately 65,000 [G/light year]s away and 80 light years in diameter. Through a small telescope, look for a fuzzy "star-like" object. At least a 10-inch (250mm) telescope is needed to [G/resolve] any [G/star]s within this cluster. This galactic [G/cluster] is 4,900 [G/light year]s away and about 14 light years in diameter. When viewed through a small telescope, it might be difficult to locate the cluster against the backdrop of the [G/Milky Way]. The cluster appears almost round and fairly compact. It is best seen using low-power, wide angle eyepieces. Wild Duck Cluster: One of the richest galactic [G/cluster]s in the sky, the compact group of over 500 [G/star]s is 6,000 [G/light year]s away and 21 light years in diameter. Through a small telescope, it might first look like a globular cluster, but with increasing magnification, it is possible to [G/resolve] the cluster into individual stars. This galactic [G/cluster] contains approximately 40 [G/star]s. The 50,000 to 100,000 [G/star]s found within this globular [G/cluster] are rather loosely packed. Look for a tiny, hazy sphere through a small telescope. Ring Nebula: The Ring Nebula is probably the most famous of all the [G/planetary nebulae] in the sky. It is 1,400 light years away and 0.5 light years in diameter. Through a small telescope, the nebula appears as a tiny sphere. At least a 6-inch (152mm) telescope is needed to [G/resolve] the ring structure of the nebula. This globular [G/cluster] is 50,000 [G/light year]s away and 70 light years in diameter. It can be found just west of the bottom [G/star] in the handle of the "Teapot" of [Y/Sagittarius]. Through a telescope, this cluster appears as a small, bright round patch of light. Because this cluster is compact, it is difficult to [G/resolve] any stars within it, even around the edges. M54 is best seen using medium- to high-power eyepieces. This peculiar [G/nebula] resembles Hubble's Variable Nebula, [C/C46]. The strange, wispy cloud varies its brightness and appearance and astronomers don't completely understand why. Inside the nebula is a variable star which effects the cloud of gas and dust, but does not completely explain its actions. This galactic [G/cluster] contains approximately 75 [G/star]s. This barred spiral [G/galaxy] is situated face-on relative to our view from the [G/Milky Way]. As a result, [G/CCD] images and long exposure astrophotographs show its spiral arms and bar-shaped [G/nucleus] in all their glory. Through a small telescope, however, look for a small, round, hazy patch that brightens towards the center. It is best to observe this galaxy on a dark night, using [G/averted vision]. This globular [G/cluster] is 20,000 [G/light year]s away. While its core is compact, the [G/star]s from the middle of the cluster out towards its perimeter are rather loosely spaced. Through a small telescope, look for a faint, round hazy patch of light. At least a 6-inch (152mm) telescope is needed to [G/resolve] stars around the edge of the cluster. GRS1915-105: This potential [G/black hole]/star system in Aquila cannot be seen visually, but astronomers detect an extremely strong x-ray source at this location. The x-rays are thought to come from material trapped in the black hole's [G/accretion disk]. Material is sucked off the companion star over the course of half an hour, filling the disk and heating it up. Then, the accretion disk empties itself into the black hole. The x-ray's temperature drops by 15 million degrees and the process begins again. This system is 40,000 light years away. This globular [G/cluster] is 46,000 [G/light year]s away and 60 light years in diameter. Through a small telescope, it appears as a faint, round, hazy patch of light. A large telescope is needed to [G/resolve] individual stars around the edge of the cluster. M56 is best seen using medium to high power eyepieces. This globular [G/cluster] is 20,000 [G/light year]s away and 80 light years in diameter. Through a small telescope, it appears as a hazy patch of light. Larger telescopes are required to [G/resolve] individual [G/star]s around the edges. It is best seen using medium- to high-power eyepieces. Foxhead Cluster: This galactic [G/cluster] contains 150 [G/star]s. This [G/planetary nebula] appears as a faint "star-like" object through a small telescope. Barnard's Galaxy: This irregular [G/galaxy] is 1.7 million [G/light year]s away and approximately 10,000 by 5,000 light years across. This galaxy belongs to our [G/Local Group] of galaxies and is best viewed using low-power, wide angle eyepieces. This irregular-shaped galactic [G/cluster] contains approximately 20 [G/star]s. This [G/cluster] of stars was first believed to be an extremely rich galactic cluster, then a loosely packed globular cluster. Today, it is generally considered to be a globular cluster which lies at a distance of 18,000 [G/light year]s. Through a small telescope, look for a fuzzy "star-like" object. At least a 10-inch (250mm) telescope is needed to [G/resolve] any [G/star]s within this cluster. Cygnus X-1:Cygnus X-1 is the best possible [G/black hole] candidate in the sky. While there is no visible star at this particular point, scientists have detected an extremely strong x-ray source. Also, not far away is a faint "companion" star, which appears to be orbiting the x-ray source at the very fast rate of once every 5.6 days. Scientists believe the x-rays are being emitted from super-heated material caught up in the gravitational pull of a black hole. From the orbital period of the companion star, it has been determined that the black hole is 20 to 35 times the mass of our [G/Sun] and lies at a distance of somewhere between 6,500 and 8,000 [G/light year]s. Dumbbell Nebula: This [G/planetary nebula] is approximately 1,000 [G/light year]s distant and 2 light years across. Through a small telescope, look for a hazy cloud with a slightly rectangular shape. Larger telescopes can begin to [G/resolve] the slight narrowing near the middle of the rectangle, thus giving it an hourglass or dumbbell appearance. This globular [G/cluster] is approximately 100,000 [G/light year]s away and 125 light years in diameter. The [G/star]s within this cluster are tightly bound together by gravity to form one of the most compact globulars in the sky. It is also believed to be the most distant. Through a small telescope, look for a fuzzy "star-like" object. This large, bright galactic [G/cluster] contains about 30 stars. Because it lies along the [G/Milky Way], it may be difficult to distinguish the stars of this cluster from the background stars of our galaxy. Crescent Nebula: This faint diffuse [G/nebula] is a crescent-shaped, wispy cloud which lies against the backdrop of the [G/Milky Way]. A seventh [G/magnitude] [G/star] can be found within this cloud of gas and dust. This galactic [G/cluster] is approximately 7,200 [G/light year]s away and 15 light years in diameter. It is a compact cluster containing few [G/star]s. Because it lies along the [G/Milky Way], the stars in this cluster may be difficult to distinguish from the background stars of our [G/galaxy]. V404 Cygni: This binary system consists of a [G/black hole] and a companion [G/star]. Astronomers detect an extremely strong x-ray source at this location which they believe is coming from an [G/accretion disk] surrounding a black hole. Gravity from the black hole pulls material from the companion star. The pull of gravity is so strong, it heats up the matter to the point where it emits x-rays, just before it is sucked into the black hole. This system is 10,000 light years away in the [G/constellation] of [Y/Cygnus]. The approximately 90 [G/star]s within this galactic [G/cluster] are loosely scattered, not packed tightly together. This globular [G/cluster] is closer, brighter, and larger than its nearby neighbor, [C/C42]. Through a small telescope, look for a fuzzy, "star-like" object. Larger telescopes can [G/resolve] individual [G/star]s around the cluster's border. This tightly bound galactic [G/cluster] contains approximately 100 [G/star]s. This spiral [G/galaxy] lies at a distance of 10-20 million [G/light year]s. When observing this galaxy through a small telescope, use a low-powered eyepiece for the brightest image possible. [G/Averted vision] aids in the detection of the tiny, irregular patch of light. Larger telescopes can [G/resolve] a faint mottling within the galaxy. Veil Nebula: This entry represents the western portion of the Veil Nebula, a huge [G/supernova] remnant approximately 1,500 [G/light year]s distant. This faint arc of material appears to be drifting behind the [G/star] 52 Cygni. Look for a faint, narrow arc with a star near its center. The eastern portion of the veil is classified as [C/C33]. Pelican Nebula: This diffuse [G/nebula] is large and very faint. This globular [G/cluster] is approximately 60,000 [G/light year]s away. Through a small telescope, look for a faint, fuzzy "star-like" object. At least a 14-inch (355mm) telescope is needed to [G/resolve] any [G/star]s within this cluster. This entry represents the eastern portion of the Veil Nebula, a huge [G/supernova] remnant approximately 1,500 [G/light year]s distant. Low-power, wide angle eyepieces are essential for observing this tiny, faint arc of light. Large telescopes begin to resolve its filament structure, which is best seen on [G/CCD] images or long exposure astrophotographs. N. American Neb.: This diffuse [G/nebula] gets its name from its unusual shape. Through a low-power, wide angle eyepiece this cloud looks like the North American continent. The nebula is approximately 1,600 [G/light year]s distant and 45 light years in diameter. Charles [G/Messier] described this group as "three or four small stars which resemble a nebula at first sight." In actuality, there is no [G/nebula] or [G/cluster] within this region, just a few faint [G/star]s. This diffuse [G/nebula] appears as a faint, irregular patch of light surrounding a seventh [G/magnitude] [G/star]. Use a low-power eyepiece to locate the object, then switch to a medium-power eyepiece for more contrast. The larger the telescope, the brighter the image and the more detail you can [G/resolve] within the cloud. This globular [G/cluster] is approximately 185,000 [G/light year]s away and could be considered to lie outside of our galaxy. Through a small telescope, look for a faint, fuzzy, "star-like" object. Saturn Nebula: This [G/planetary nebula] lies 4,000 [G/light year]s away and is 0.5 light years across. Look closely to observe a slight haziness around a star-like object. Through larger telescopes, its oval, Saturn-like appearance may be detected. The Saturn Nebula is best seen with high magnification. PG2112+059: This [G/quasar] is over 1 billion [G/light year]s away. Because of its tremendous distance, this quasar is only visible through the largest telescopes. This globular [G/cluster] lies just off the nose of the flying horse, near the bright star [W/Enif]. M15 is approximately 39,000 [G/light year]s away and 130 light years in diameter. X-rays have been detected coming from this cluster, which may indicate the presence of one or more [G/black hole]s hidden within its core. Through a small telescope, look for a faint hazy patch. Larger telescopes can [G/resolve] individual stars around the fringes of the cluster. M15 is best seen using medium to high power eyepieces. This galactic [G/cluster] is approximately 800 [G/light year]s away and 7 light years in diameter. The [G/star]s within this cluster are scattered over a large area of sky, thus making it difficult to view the cluster in its entirety through a small telescope. Instead, one sees only a few bright stars at a time. Try observing the cluster with a low-power, wide angle eyepiece. Then, observe the cluster with binoculars. All the stars of the cluster should be visible within the [G/field of view] of the binoculars. This globular [G/cluster] is a tight ball of over 100,000 [G/star]s. M2 is 50,000 [G/light year]s away and 150 light years in diameter. Through a small telescope, look for a "hazy" star-like object. Larger telescopes are able to resolve individual stars around the edge of the cluster. M2 is best seen with medium or high magnification. This globular [G/cluster] is approximately 40,000 [G/light year]s away and 100 light years in diameter. This dense, compact sphere of stars appears as a faint round ball through a small telescope. Even larger telescopes may have difficulty resolving stars around the edge. This cluster is best observed using low to medium-power eyepieces. This diffuse [G/nebula] is a faint, mottled cloud that lies at the east end of a dark dust lane. It may be difficult to distinguish from the background [G/Milky Way]. This galactic [G/cluster] contains approximately 40 [G/star]s. PG2209+184: This [G/quasar] is over 1 billion [G/light year]s away. Because of its tremendous distance, this quasar is only visible through the largest telescopes. This galactic [G/cluster] is a very loose grouping of approximately 40 [G/star]s. Helix Nebula: Roughly 450 [G/light year]s away and 1.75 light years across, the Helix Nebula is the largest and closest [G/planetary nebula] in our skies. Through a small telescope, look for a small, round, hazy patch. The nebula is best seen with low-power, wide angle eyepieces. This spiral [G/galaxy] is approximately 50 million [G/light year]s away and 32,000 light years in diameter. Through a small telescope, look for an elongated, oval-shaped patch of light. A faint diffuse [G/nebula]. This barred spiral [G/galaxy] is extremely faint and difficult to see, even under the best observing conditions. Large telescopes can begin to [G/resolve] the "barred" portion of the galaxy as a narrow streak of light. Bubble Nebula: Sometimes classified as a diffuse [G/nebula], this cloud of hydrogen gas appears as a dim, irregular haze surrounding a faint star. Its bubble appearance can only be seen on [G/CCD] images or long exposure astrophotographs. This galactic [G/cluster] is 3,000 [G/light year]s away and about 12 light years in diameter. [G/Star]s within this cluster are more tightly packed than in most other galactic clusters. It is best seen using medium-power eyepieces. This [G/planetary nebula] is between 2,000 and 5,600 [G/light year]s away. It appears as a faint, fuzzy "star-like" object through a small telescope. At least a 6-inch (152 mm) telescope is needed to detect its "sphere-like" qualities. This galactic [G/cluster] is 6,000 [G/light year]s away and 50 light years in diameter. It consists of a rich scattering of faint [G/star]s. The larger the telescope, the more stars are visible within the cluster. This cluster is best seen through low-power, wide angle eyepieces. MercuryMercury is named after the messenger god in Roman mythology. Like its namesake, Mercury moves extremely fast across the sky. Faster than any other planet, in fact. Mercury is the only [G/planet] in the solar system without an atmosphere to protect its surface. As a result, Mercury gets very hot during the day, 660^F (350^C) and very cold at night, -274^F (-170^C). The only spacecraft to visit the planet ([G/Mariner 10], 1974) took photos showing [G/crater]s covering the entire planet. What you can see: From Earth, Mercury is too small to see any surface features. Safe viewing of the planet is difficult because of its proximity to the Sun. It is only visible within an hour of sunset or sunrise. With larger telescopes, it is possible to see the phases of Mercury. VenusVenus gets its name from the Roman goddess of beauty. Because it is closer to the Sun than Earth, Venus is only visible in the early evening just after sunset, or in the early morning, just before sunrise. As a result, Venus is sometimes known as the Evening Star or Morning Star. It is extremely bright in the sky because Venus is the closest [G/planet] to Earth and it is covered with a thick layer of clouds that reflects the Sun's light like a mirror. These thick clouds hide the surface of Venus from view and trap the Sun's heat, causing the hottest surface temperatures found on any planet, 900^F (480^C). Since 1962, 22 US and USSR robotic missions have flown to Venus. Most recent [G/lander]: [G/Venera 14] (USSR), 1982. Most recent [G/orbiter]: [G/Magellan] (US), 1990. What you can see: The phases of Venus can be seen as it orbits around the Sun. No surface features are visible because of the thick clouds. EarthThe origin of Earth's name is unknown. Our planet is the only planet in the solar system capable of supporting liquid water. In fact, 70% of Earth's surface is covered by water. Earth is one of the most geologically active planets; volcanoes, earthquakes, hurricanes, floods, fires and severe storms are constantly resurfacing the planet, changing its appearance. Earth is also the only planet in the solar system known to support life. MarsThe planet Mars was named after the god of war in Roman mythology, appropriate because of its reddish, blood-colored appearance in the sky. This small [G/planet], half the size of Earth, has the largest canyon ([G/Mariner Valley]) and largest volcano, ([G/Olympus Mons]) in the solar system. Ancient river beds and flood plains indicate Mars was once warm enough to support liquid water. Today, a combination of frigid temperatures and an extremely thin atmosphere of carbon dioxide make it impossible for liquid water to exist. Since 1964, 14 US and USSR robotic missions have flown to Mars. The most recent [G/lander]: [G/Pathfinder] (US), 1997. The most recent [G/orbiter]: [G/Mars Global Surveyor] (US), 1997. What you can see: Mars appears as a tiny disk with a hint of reddish/orange color. With larger telescopes, polar ice caps and possible dark markings on the martian surface are visible. JupiterJupiter, the largest planet in the solar system, gets its name from the king of the gods in Roman mythology. Over 1100 Earths could fit inside this gas giant planet. Jupiter does not have a solid surface. Instead, it is composed of hydrogen and helium gases. A spacecraft trying to land on Jupiter would pass through thicker and thicker clouds until it is crushed by the increasing [G/jovian] pressure. At its center, there might be an Earth-size solid core. Orbiting Jupiter is the largest [G/moon] in the solar system, [G/Ganymede]. [G/Galileo] discovered Ganymede and three other moons of Jupiter, (Io, Europa, and Callisto) in 1610. These moons were the first objects ever discovered with a telescope. There is one faint ring surrounding the planet which can not be seen from Earth. The ring was discovered by one of five spacecraft that have visited the planet: [G/Pioneer 10], 1973; [G/Pioneer 11], 1974; [G/Voyager 1], 1979; [G/Voyager 2], 1979; [G/Galileo spacecraft], 1995. What you can see: Several dark cloud bands stretching across a pale disk. As many as 4 of Jupiter's 39 moons can be seen, appearing like stars lined up next to the planet. The moons change places around Jupiter from night to night. Through larger telescopes: more details within the cloud bands can be resolved; moon shadows on the disk of the planet are visible. SaturnSaturn gets its name from the king of the mythical Titans. This gas giant planet is the most distant planet that can be seen without a telescope. The most prominent feature of Saturn is its beautiful [G/ring system], the largest in the solar system. The rings stretch across 169,000 miles (273,000 km), yet are only 0.5 miles (0.8 km) thick. [G/Galileo] observed the rings in 1610, but didn't understand what he was seeing. In 1675, G.D. [G/Cassini] discovered a dark gap in the rings. This gap, later named the [G/Cassini Division], is easily seen with 90mm and larger telescopes. Saturn also has more [G/moon]s than any other planet except Jupiter, 31. Several of these moons were discovered by the three visiting spacecraft: [G/Pioneer 11], 1979; [G/Voyager 1], 1980; [G/Voyager 2], 1981. What you can see: A small disk with the white ring system extending from both sides. The moon, [G/Titan], may be visible as a bright starlike object near the planet. The position of Titan changes as it orbits the planet. With larger telescopes: pale cloud bands on the planet can be resolved; ring and moon shadows on the planet, more divisions within the ring system. UranusUranus gets its name from an early mythological god who was a son of Mother Earth. This gas giant planet, discovered by William Herschel in 1781, was the first [G/planet] discovered with a telescope. Uranus is tilted on its side as it orbits the Sun. As a result, its seasons are unusual. For example, during summer at the North Pole, the Sun stays above the horizon for 42 [G/earth years]. At the same time, it is winter at the South Pole, with 42 years of frigid darkness. After 42 years, the seasons are reversed. Uranus has 17 known moons and has a [G/ring system] composed of several dark, thin rings. These rings are not directly visible from Earth, but were photographed by the [G/Voyager 2] spacecraft as it flew by the planet in 1986. What you can see: Extremely tiny disk with possible bluish/green color. With larger telescopes: a more distinct disk, more color. NeptuneNeptune gets its name from the mythical Roman god of the sea. Astronomers began searching for Neptune to explain irregularities in the orbit of [P/Uranus]. Uranus didn't follow its predicted path across the sky, so astronomers thought the gravity from another planet must be effecting the orbit. Using mathematics, they predicted where that other planet should be. In 1846, on the first night of searching, Neptune was discovered. [G/Voyager 2], flying by the planet in 1989, discovered the strongest winds in the solar system on this blue planet, winds of 1500 miles per hour (2400 km per hour). The [G/ring system] around Neptune is composed of a few dark "[G/clumpy]" rings. Of Neptunes 11 moons, [G/Triton], the largest [G/moon], is the only moon in the solar system that travels in a [G/retrograde] direction around its planet, a direction opposite the way the planet rotates. What you can see - extremely tiny disk, with possible bluish/green color. With larger telescopes: a more distinct disk, more color. PlutoPluto was named after the ruler of the underworld in Roman mythology. Discovered in 1930, Pluto is the smallest planet in the solar system. No spacecraft has explored this distant world, but [G/Hubble telescope] images show a [G/planet] of high contrast, bright areas next to dark areas. It is so cold on Pluto that its atmosphere lies frozen on the ground. Pluto has the most elliptical [G/orbit] of all the planets. For twenty years, from 1979 to 1999, Pluto's odd orbit brings it closer to the Sun than [P/Neptune]. What you can see: Because of Pluto's tiny size and extreme distance, it is extremely difficult to see, even with larger telescopes. It appears as an extremely faint, starlike object. MoonPlace Holder AbbeAbbotNamed for Charles Greeley Abbot; American astrophysicist 1872-1973). AbelNamed for Niels H. Abel; Norwegian mathematician 1802-1829). AbenezraNamed for Abraham Bar Rabbi Ben Ezra Abenezra; Spanish Jewish mathematician, astronomer 1092-1167). AbettiNamed for Antonio Abetti; Italian astronomer (1846-1928); Georgio; Italian astronomer (1882-1982). Abul W'afaAbulfedaNamed for Ismail Abulfida 1273-1331) Abul Abulfeda; Syrian geographer. AcostaNamed for Cristobal Acosta; Portuguese doctor, natural historian 1515-1580). AdamsNamed for John Couch Adams; British astronomer (1819-1892); Charles H.Adams; American astronomer (1868-1951); and Walter S. Adams; American astronomer (1876-1956). AgatharchidesNamed for Greek geographer (unkn-c.150 B.C.). AgrippaNamed for Greek astronomer unkn-fl. A.D. 92). AiryNamed for George Biddell Airy; British astronomer (1801-1892). AitkenAkisnamed for Akis, a Greek female name. Al-BakriNamed for A. A. Al-Bakri; Spanish-Arab geographer (1010-1094). Al-BiruniName for Al-Biruni Persian astronomer, mathematician, geographer 973-1048). Al-KhwarizmiAl-MarrakushiNamed for Al-Marrakushi, Moroccan astronomer, mathematician (fl. c.1262). AlanIrish male name. AlbategniusNamed for Al-Batani, Muhammed Ben Geber C. Albategnius; Iraqi astronomer, mathematician 850-929). AldenAlderAldrinNamed for Edwin E. Aldrin Jr.; American astronaut (1930-Live). AlekhinAlexanderNamed for Alexander the Great of Macedon; Greek geographer 356-323 B.C.). AlfraganusNamed for Al Fargani, Muhammed Ebn Ketir Alfraganus; Persian astronomer unkn-c. 840). AlhazenNamed for Abu Ali Al-Hasan Ibn Al Haitham Alhazen; Iraqi mathematician 987-1038). AliacensisNamed for D'Ailly, Pierre Aliacensis; French geographer (1350-1420). AlmanonNamed for Abdalla Al Mamun; Persian astronomer (786-833). AlohaHawaiian greeting. AlpetragiusNamed for Nur Ed-Din Al Betrugi Alpetragius; Moroccan astronomer unkn-c. 1100). AlphonsusNamed for Alfonso X; Spanish astronomer (1223-1284). Alphonsus crater is the middle of three large craters aligned from north to south. Alphonsus is 108 km in size. It has a small peak that is slightly off center. Curving along the eastern side of the crater floor is a series of fissures called Rimae Alphonsus. [K/Ptolemaeus] crater lies directly north, while [K/Arzachel] crater lies to the south of Alphonsus. AlterAmeghinoNamed for Fiorino (or Florentino) Ameghino; Italian natural historian c. 1854-1911). AmiciAmmoniusNamed for Ammonius, Greek philosopher unkn-c. 517). AmontonsNamed for Guillaume Amontons; French physicist (1663-1705). AmundsenNamed for Roald E. Amundsen; Norwegian explorer (1872-1928). AnaxagorasNamed for Anaxagoras. Greek astronomer (500-428 B.C.). AnaximanderNamed for Anaximander, Greek astronomer (c. 611-547 B.C.). AnaximenesNamed for Anaximenes, Greek astronomer (585-528 B.C.). AndersAndersonAnderssonAndronovAndvelNamed for Karel Andvel; Czechoslovakian astronomer (1884-1947). AngoAfrican male name. AngstromNamed for Anders Jonas Angstrom; Swedish physicist (1814-1874). AnnHebrew female name. AnnegritGerman female name. AnsgariusNamed for St. Ansgar Ansgarius; German theologian (801-864). AntoniadiAnuchinAnvilleNamed for Jean-Baptiste Bourguignon Anville; French cartographer 1697-1782). ApianusNamed for Bienewitz, Peter Apianus; German mathematician, astronomer 1495-1552). ApolloApollo 11 SiteApollo 11 Landing Site in [K/Mare Tranquillitatis]. One of the main reasons the Sea of Tranquility was chosen for the first Apollo Moon Landing was because of its relatively smooth terrain, or at least it looked smooth from Earth and high lunar orbit. However, when astronauts Neil Armstrong and Buzz Aldrin approached the intended landing site in the Lunar Module ""Eagle"", they quickly realized they were scheduled to touch down in a heavily cratered boulder field. Only after a couple of minutes of intense maneuvering by Armstrong did they find a relatively smooth place to land. Apollo 11 touched down on the lunar surface on July 20, 1969, with only 20 seconds of maneuvering fuel left in its engines. Once safely on the ground, the astronauts were on the surface for 21:36 hours. They went outside the lunar module once, for 2.4 hours, during which time they traveled 0.25 km and collected 21 kg of samples. The Apollo 11 landing site lies just to the west of the break in the mare's mountainous southern border, close to the mare's edge. To the west of the landing site are twin craters, [K/Ritter] and [K/Sabine]. The two craters lie side by side angling to the northwest. Just to the north of these twin craters are two smaller craters, lined up north to south. This area of the Moon was a popular tourist spot. Just to the north of the Apollo 11 site is where the unmanned Surveyor 5 spacecraft softlanded on Sept. 10, 1967. Two and a half years earlier, on Feb. 20, 1965, Ranger 8 crashlanded on the Moon, just to the northeast. Keep in mind that no telescope on Earth can resolve any of the items left behind by the astronauts. Earth's atmosphere restricts our view and doesn't let us resolve any features smaller than about a kilometer (half mile). The lunar lander was only 4.2 meters in diameter. And, no, you can't see the flag they left behind, either. It is much too small. Same goes for the footprints! Apollo 12 SiteApollo 12 Landing Site in the small [K/Mare Insularum], south of the large crater [K/Copernicus]. One of the goals of Apollo 12 was to see just how accurate a lunar landing could be. So, astronauts Pete Conrad and Al Bean were given the task of bringing their lunar module ""Intrepid"" down as close as possible to the Surveyor 3 spacecraft that had landed on the moon two and a half years earlier. On Nov. 19, 1969, Conrad brought Intrepid down within 200 meters of Surveyor 3, much to the delight of everyone. Apollo 12 was on the surface for 31:31 hours. The astronauts went outside the lunar module twice for a total of 7:45 hours, during which time they traveled 2 km and collected 34 kg of samples. During their second outing, Conrad and Bean hiked over to Surveyor 3 and retrieved several parts from the spacecraft to be brought back to Earth for study. To pinpoint the landing site, locate the large ray crater [K/Copernicus]. From Copernicus there is a string of three medium sized craters swinging down to the southwest. The first of the three craters is a smaller, flooded crater, but the other two (Reinhold and Lansberg)are nice distinct craters with sharp walls and central peaks. Reinhold, Lanberg and the Apollo 12 landing site form a nice equilateral triangle, with Apollo 12 forming the southern point. Keep in mind that no telescope on Earth can resolve any of the items left behind by the astronauts. They are much too small. Apollo 14 SiteApollo 14 Landing Site in the Fra Mauro highlands. Building on the experiences of the missions before it, Apollo 14 was the first lunar mission that had the ""luxury"" of emphasizing scientific study, rather than sheer survival. Originally scheduled to touchdown in the Littrow region, the target of Apollo 14 shifted to Fra Mauro when Apollo 13's moon landing was aborted. On Jan. 31, 1971, astronauts Alan Shepard and Edgar Mitchell brought their lunar module ""Antares"" to a gentle landing on the lunar surface, approx. 170 km east southeast of [K/Apollo 12]'s landing site. Shepard and Mitchell were given the task of finding and return samples of the moon's interior. Scientists hoped that rocks scattered from the impact that formed the large crater [K/Copernicus] (to the north) were lying on the surface of the Fra Mauro region, thus providing astronauts a way to collect samples from deep within the Moon's core without having to drill. The two astronauts collected 43 kg of samples during their two moonwalks. They were on the lunar surface for 33:30 hours, and outside of the lunar module for 9:17 hours, during which time they traveled 3.3 km. Shepard, an avid golfer, surprised everyone (including his NASA supervisors) by fashioning a golf club out of spare parts and taking a swing at the two golf balls he had hidden onboard Antares, thus becoming the first golfer on the Moon. The Fra Maura highlands lie to the south of the large crater [K/Copernicus] and just north of three overlapping, old, flooded craters; [K/Fra Mauro], Bonpland and Parry. Fra Mauro crater is the largest of the three, Parry and Bonpland lie side by side, just to the south. Apollo 14 landed just north of the northern rim of crater Fra Mauro. Keep in mind that no telescope on Earth can resolve any of the items left behind by the astronauts. They are much too small. Apollo 15 SiteApollo 15 Landing Site in the Hadley-Apennine region. This region was chosen as a landing site because of its diverse terrain. Scientists hoped that the astronauts would be able to collect samples from a wide range of lunar ages and geological features, including a mountain range, a rille, and a flooded plain. To help them explore more territory, Apollo 15 marked the debut of the Lunar Rover. Astronauts David Scott and Jim Irwin, in their lunar module ""Falcon,"" landed on the Moon on July 30, 1971. During their 66:54 hour stay on the lunar surface, Scott and Irwin made three excursions lasting a total of 19:08 hours. With the help of the rover, they traveled 27.9 km and collected 77 kg of samples. To find the site, locate the break between [K/Mare Serenitatis] and [K/Mare Imbrium], where lava appears to have flowed between the two. The Apollo 15 site lies just to the south of the break, on the Mare Imbrium side (west side) of the mountains. To the northwest of the site lies [K/Autolycus] crater. [K/Archimedes] crater lies to the west northwest. Keep in mind that no telescope on Earth can resolve any of the items left behind by the astronauts. They are much too small. Apollo 16 SiteApollo 16 Landing Site in the Descarte region of the lunar highlands. Apollo 16 was the first and only mission to land in the heavily cratered lunar highlands where scientists believed portions of the Moon's original crust still existed on the surface. Because of the high concentration of craters, this mission presented a trickier landing site than previous missions, but astronauts John Young and Charlie Duke brought their lunar module ""Orion"" to a safe touchdown on April 20, 1972. The astronauts were on the surface for 71:14 hours. They went outside the module three times. During their excursions, they traveled 27 km in their lunar rover and collected 94 kg of samples. To locate Apollo 16's landing site, follow the dark mare from the Sea of Tranquility south into [K/Sinus Asperitatis]. Just before you get to the two large craters on the southern edge of Sinus Asperitatis, look to the west, near the center of the lighter, rough lunar highlands. Keep in mind that no telescope on Earth can resolve any of the items left behind by the astronauts. They are much too small. Apollo 17 SiteApollo 17 Landing Site in the Taurus Littrow valley. The Taurus Littrow region was chosen as a landing site because of what appeared to be ""fresh"" volcanic vents in the area. If the astronauts found recent vents, or cinder cones, this would help determine if the Moon was still geologically active. Apollo 17's lunar module ""Challenger,"" landed on the Moon on December 11, 1972. As the last manned mission to the lunar surface (to date) Apollo 17's crew broke all of the records set by the other Apollo missions. Astronauts Gene Cernan and Harrison Schmitt were on the surface longer than any other astronauts (74:59 hours), they covered the most territory (35 km) and collected the most samples (110 kg). Schmitt also had the distinction of being the only geologist/scientist to walk on the Moon. Among their many feats, the two explorers found orange soil and performed makeshift auto body repairs on the lunar rover by replacing a damaged fender over one of the tires with a page out of their flight manual. To locate Apollo 17's landing site, look in the rugged northern border of [K/Mare Tranquillitatus], near the eastern edge of [K/Mare Serenitatis]. Keep in mind that no telescope on Earth can resolve any of the items left behind by the astronauts. They are much too small. ApolloniusNamed for Apollonius of Perga 3rd century B.C.; Greek mathematician. AppletonAragoNamed for Dominique Francois Jean Arago; French astronomer 1786-1853). AratusNamed for Greek astronomer (315-245 B.C. ?). ArchimedesNamed for Archimedes, Greek physicist, mathematician (c. 287-212 B.C.). The crater Archimedes is 82 km in diameter and 2.2 km deep, the largest of three craters in the eastern part of [K/Mare Imbrium]. The crater floor appears smooth, while the crater rim appears "wrinkled" or terraced, as if there are several layers of walls within the rim. The small crater [K/Autolycus] lies just to the east, while the crater [K/Aristillus] lies to the northeast. Off to the southwest of Archimedes is a tiny crater, [K/Bancroft]. ArchytasNamed for Archytas, Greek mathematician 428-347 B.C. ?). ArgelanderNamed for Friedrich Wilhelm August Argelander; German astronomer 1799-1875). AriadaeusNamed for Arrhidaeus, Philipus; King of Babylon chronologer (unkn.-317 B.C.). AristarchusNamed for Aristarchus, Greek astronomer (310-230 B.C. ?). The crater Aristarchus is a distinct crater with sharp crater walls and a small central peak. It is 40 km in diameter and 3 km deep. Aristarchus lies on the southern tip of a wrinkled ""island"" in [K/Oceanus Procellarum]. The small flooded crater [K/Herodotus] is just to the west. AristillusNamed for Aristillus, Greek astronomer (fl. c. 280 B.C.). The crater Aristillus is the middle-sized of three distinct craters in the eastern part of [K/Mare Imbrium]. Aristillus is 55 km in diameter and 3.7 km deep. Its central peak looks more like a jumbled pile of rocks. This is a ""ray"" crater, but the rays of debris from the impact that caused the crater may be difficult to see, depending on the Sun's location. The smaller crater [K/Autolycus] is directly south of this crater, while the large crater [K/Archimedes] is to the southwest. AristotelesNamed for Aristotel, Greek astronomer, philosopher (383-322 B.C.). The crater Aristoteles is 87 km in diameter. It has two small peaks that lie within the crater, slightly off center. The crater walls are wide and terraced. The small crater Mitchell lies on the eastern rim. For comparison, Mitchell is 30 km in diameter. ArminskiArmstrongNamed for Neil A. Armstrong; American astronaut (1930-Live). ArnoldNamed for Christoph Arnold; German astronomer (1650-1695). ArrheniusNamed for Svante A. Arrhenius; Swedish chemist; Nobel laureate 1859-1927). ArtamonovArtem'evArtemisNamed for Artemis, Greek Moon goddess. ArtsimovichNamed for Lev Andreevich Artsimovich; Soviet physicist (1909-1973). AryabhataNamed for Aryabhata, Indian astronomer, mathematician 476-c.550). ArzachelNamed for Al Zarkala; Spanish-Arabic astronomer c. 1028-1087). Arzachel crater is a very distinct crater 96 km in diameter and 3.6 km deep. On the crater floor, there is a small crater just to the east of the central peak. A fissure called Rimae Arzachel curves along the floor, just east of the small crater. The fissure is 50 km long. AsadaNamed for Goryu Asada; Japanese astronomer (1734-1799). AsclepiNamed for Giuseppe Asclepi; Italian astronomer (1706-1776). AshbrookAstonNamed for Francis W. Aston; British chemist, physicist; Nobel laureate (1877-1945). AtlasNamed for Atlas, mthological Greek Titan. The crater Atlas is a large eroded crater 87 km in size. The crater floor is fractured by a series of fissures running through it. The fissure system is called Rimae Atlas. AtwoodNamed for G. Atwood; British mathematician, physicist 1745-1807). AutolycusNamed for Autolycus, Greek astronomer (unkn-c. 330 B.C.). The crater Autolycus is the smallest of three distinct craters in the eastern part of [K/Mare Imbrium]. The crater, with its uneven, irregular floor, is 39 km in diameter and 3.4 km deep. The crater [K/Archimedes] lies almost directly west while the crater [K/Aristillus] lies to the north. AuwersNamed for Georg Friedrich Julius Arthur Auwers; German astronomer 1838-1915). AuzoutNamed for Adrien Auzout; French astronomer, physicist 1622-1691). AveryNamed for Oswald Theodore Avery; Canadian doctor (1877-1955). AvicennaAvogadroAzophiNamed for Al-Sufi, Abderrahman Azophi; Persian astronomer 903-986). BaadeNamed for Walter Baade; American astronomer (1893-1960). BabakinBabbageNamed for Charles Babbage; British mathematician 1792-1871). BabcockNamed for Harold D. Babcock; American astronomer, physicist 1882-1968). BackNamed for Ernst E. A. Back; German physicist (1881-1959). BacklundBacoNamed for Roger Baco; British natural philosopher, optician 1214-1294). BaillaudNamed for Benjamin Baillaud; French astronomer (1848-1934). BaillyNamed for Jean Sylvain Bailly; French astronomer (1736-1793). BailyNamed for Francis Baily; British astronomer (1774-1844). BalandinBalboaNamed for Vasco N. de Balboa; Spanish explorer (1475-1517). BaldetBallNamed for William Ball; British astonomer (unkn-1690). BalmerNamed for Johann J. Balmer; Swiss mathematician, physician 1825-1898). BanachiewiczNamed for Tadeusz Banachiewicz; Polish astronomer, mathematician 1882-1954). BancroftNamed for W. D. Bancroft; American chemist 1867-1953). Bancroft crater is only 13 km wide and 2.5 km deep. The large crater [K/Archimedes] can be found just to the northeast. Bancroft crater lies just at the northern edge of a small wrinkled region called [K/Mts. Archimedes], a mountain range that covers about 160 km. BantingNamed for Sir Frederick Grant Banting; Canadian doctor; Nobel laureate (1891-1941). BarbierBarklaNamed for C. G. Barkla; British physicist; Nobel laureate 1877-1944). BarnardNamed for Edward E. Barnard; American astronomer (1857-1923). BarociusNamed for Francesco Barocius; Italian mathematician (unkn-fl. 1570). BarringerBarrowNamed for Isaac Barrow; British mathematician 1630-1677). BartelsNamed for Julius Bartels; German geophysicist 1899-1964). BawaBayerNamed for Johann Bayer; German astronomer 1572-1625). BealsNamed for Carlyle F. Beals; Canadian astronomer (1899-1979). BeaumontNamed for Leonce Elie de Beaumont; French geologist (1798-1874). BecquerelBeerNamed for Wilhelm Beer; German astronomer (1797-1850). BehaimNamed for Martin Behaim; German navigator, cartographer 1436-1506). BeijerinckBeketovNamed for N. N. Beketov; Russian chemist 1827-1911). BelaSlavic female name. BelkovichNamed for Igor V. Belkovich; Soviet astronomer (1904-1949). BellBellinsgauzenBellotNamed for Joseph Rene Bellot; French explorer (1826-1853). BelopolskiyBelyaevBenedictBergmanBergstrandBerknerBerlageBernoulliNamed for Jacques Bernoulli; Swiss mathematician 1654-1705); Jean Bernoulli; Swiss mathematician 1667-1748). (Spelling changed from Bernouilli.) BerosusNamed for Berosus the Chaldean; Babylonian astronomer unkn-c. 250 B.C.). BerzeliusNamed for Jons Jakob Berzelius; Swedish chemist (1779-1848). BessarionNamed for Johannes Bessarion; Greek scholar c. 1369-1472). BesselNamed for Friedrich Wilhelm Bessel; German astronomer (1784-1846). This small, prominent crater lies within [K/Mare Serenitatis], just south of the center of the mare. The crater is 15 km in diameter and 1.7 km deep. Its floor is smooth, with no central peak. When fully illuminated, a light colored ray of material can be seen passing through Bessel. The ray seems to emanate from the crater [K/Menelaus]. BettinusNamed for Mario Bettinus; Italian mathematician, astronomer 1582-1657). BevcvavrBhabhaBianchiniNamed for Francesco Bianchini; Italian astronomer (1662-1729). BielaNamed for Wilhelm von Biela; Austrian astronomer (1782-1856). BilharzNamed for T. Bilharz; German doctor (1825-1862). BillyNamed for Jacques de Billy; French mathematician (1602-1679). BinghamBiotNamed for Jean-Baptiste Biot; French astronomer (1774-1862). BirkelandBirkhoffBirminghamNamed for John Birmingham; Irish astronomer (1829-1884). BirtNamed for William R. Birt; British selenographer (1804-1881). BjerknesBlackNamed for Joseph Black; French chemist (1728-1799). BlackettBlaggNamed for Mary Adela Blagg; British astronomer (1858-1944). BlancanusNamed for Biancani, Giuseppe Blancanus; Italian mathematician, astronomer (1566-1624). BlanchardNamed for J.P. Blanchard; French aeronaut (1753-1809). BlanchinusNamed for Bianchini, Giovanni Blanchinus; Italian astronomer (unkn-fl. 1458). BlazhkoBlissNamed for Nathaniel Bliss; English Astronomer Royal (1700-1764). BobillierNamed for E. Bobillier; French geometer (1798-1840). BoboneBodeNamed for Johann Elert Bode; German astronomer (1747-1826). BoethiusNamed for Boethius, Greek physicist (c. 480-524). BoguslawskyNamed for Palon Heinrich Ludwig von Boethius Boguslawsky; German astronomer (1789-1851). BohnenbergerNamed for Johann Gottlieb Friedrich Von Bohnenberger; German astronomer (1765-1831). BohrNamed for Niels H. D. Bohr; Danish physicist; Nobel laureate (1885-1962). BokBoltzmannNamed for Ludwig E. Boltzmann; Austrian physicist (1844-1906). BolyaiBombelliNamed for R. Bombelli; Italian mathematician (1526-1572). BondarenkoBonplandNamed for Aime Bonpland; French botanist (1773-1858). BooleNamed for George Boole; British mathematician (1815-1864). BordaNamed for Jean Charles Borda; French astronomer (1733-1799). BorelNamed for Felix Edouard Emile Borel; French mathematician (1871-1956). BorisRussian male name. BormanBornNamed for Max Born; German physicist (1882-1970). BoscovichNamed for Ruggiero Giuseppe Boscovich; Italian physicist (1711-1787). BoseBossNamed for Lewis Boss; American astronomer (1846-1912). BouguerNamed for Pierre Bouguer; French hydrographer (1698-1758). BoussingaultNamed for Jean Baptiste Dieudonne Boussingault; French chemist (1802-1887). BowditchBowenNamed for Ira Sprague Bowen; American astronomer (1898-1973). BoyleBrackettNamed for Frederick Sumner Brackett; American physicist (1896-1972). BraggBrashearBrayleyNamed for Edward William Brayley; British geographer (1801-1870). BredikhinBreislakNamed for Scipione Breislak; Italian chemist, geologist, mathematician (1748-1826). BrennerNamed for Leo Brenner; Austrian astronomer (1855-1928). BrewsterNamed for David Brewster; Scottish optician (1781-1868). BrianchonNamed for Charles J. Brianchon; French mathematician (1783-1864). BridgmanBriggsNamed for Henry Briggs; British mathematician (1556-1630). BrisbaneNamed for Sir Thomas Brisbane; Scottish astronomer (1770-1860). BronkBrouwerBrownNamed for Ernest William Brown; British astronomer, mathematician (1866-1938). BruceNamed for Catherine Wolfe Bruce; American philanthropist, astronomer (1816-1900). BrunnerNamed for William O. Brunner; Swiss astronomer (1878-1958). BuchNamed for Christian Leopold von Buch; German geologist (1774-1853). BuffonBuissonBullialdusNamed for Boulliaud, Ismael Bullialdus; French astronomer (1605-1694). The crater Bullialdus is 60 km in diameter and 3.5 km deep. It has terraced walls and a uneven central peak. There are two smaller craters lying just to the south of Bullialdus, and a third small crater lying to the southwest. BunsenNamed for Robert W. Bunsen; German chemist (1811-1899). BurckhardtNamed for Johann Karl Burckhardt; German astronomer (1773-1825). BurgNamed for Johann Tobias Burg; Austrian astronomer (1766-1834). Burg crater is centered within [K/Lacus Mortis]. It is 39 km in size and has a bright central peak, when viewed close to the terminator. Just to the south of Burg are two craters about the same size but almost completed flooded out. Plana crater lies directly south of Burg, just a hint of its former self. Its crater walls are flooded over in some places, but its central peak is visible. Plana crater overlaps Mason crater to the east. Both Plana and Mason are about 44 km in size. BurnhamNamed for Sherburne Wesley Burnham; American astronomer (1838-1921). BuschingNamed for Anton Friedrich Busching; German geographer (1724-1793). ButlerovBuys-BallotByrdNamed for Richard E. Byrd; American explorer, aviator, navigator (1888-1957). ByrgiusNamed for Burgi, Joost Byrgius; Swiss horologist (1552-1632). C. HerschelNamed for Caroline Herschel; British astronomer (1750-1848). C. MayerNamed for Christian Mayer; German astronomer, mathematician, physicist (1719-1783). CabannesCabeusNamed for Cabeo, Niccolo Cabeus; Italian astronomer (1586-1650). CailleuxCajalNamed for Santiago Ramon Y Cajal; Spanish doctor; Nobel laureate (1852-1934). CajoriCalippusNamed for Calippus of Cyzicus; Greek astronomer (c. 330 B.C.). CameronNamed for Robert Curry Cameron; American astronomer (1925-1972). CampanusNamed for Giovanni Campano; Italian astronomer (c. 1200-unkn). CampbellCannizzaroCannonNamed for Annie J. Cannon; American astronomer (1863-1941). CantorCapellaNamed for Martianus Capella; Roman astronomer (c. A.D. 400-unkn). CapuanusNamed for Francesco Capuano Di Manfredonia; Italian astronomer (c. 1400-unkn). CardanusNamed for Girolamo Cardano; Italian mathematician (1501-1576). CarliniNamed for Francesco Carlini; Italian astronomer (1783-1862). CarlosSpanish male name. CarmichaelNamed for Leonard Carmichael; American psychologist (1898-1973). CarnotCarolCarpenterNamed for James Carpenter; British astronomer (1840-1899); Edwin F. Carpenter; American Astronomer (1898-1963). CarrelNamed for Alexis Carrel; French doctor, physiologist; Nobel laureate (1873-1944). CarrilloNamed for Flores Nabor Carrillo; Mexican soil engineer (1911-1967). CarringtonNamed for Richard Christopher Carrington; British astronomer (1826-1875). CartanNamed for E. J. Cartan; French mathematician (1869-1951). CarverCasatusNamed for Casati, Paolo Casatus; Italian mathematician (1617-1707). CassegrainCassiniNamed for Giovanni Domenico Cassini; Italian-French astronomer (1625-1712) and Jacques J. Cassini; French astronomer (1677-1756). The Cassini crater lies just to the south of [K/Vallis Alpes]. All but the outer rim of this shallow 1.2 km deep, 56 km wide crater was flooded by lava. There are two distinct craters within the rim of Cassini. The larger of the two inner craters, Cassini A, is 17 km in size and 2.8 km deep, and lies almost in the center of the older, flooded crater. Cassini B lies off towards the western side of the crater, not far from the crater rim. CatalanNamed for Miguel A. Catalan; Spanish spectroscopist (1894-1957). CatharinaNamed for St. Catherine of Alexandria; Greek theologian, philosopher (unkn-c. 307). Crater Catharina is a very old, very eroded crater about 104 km in diameter and 3,130 meters deep. The northern rim of Catharina has all but disappeared, to be replaced by a ""channel"" coming from the crater [K/Cyrillus]. Even though Catharine is a fairly large crater, it has no central peak. CauchyNamed for Augustin Louis Cauchy; French mathematician (1789-1857). CavaleriusNamed for Buonaventura Cavalieri; Italian mathematician (1598-1647). CavendishNamed for Henry Cavendish; British chemist, physicist (1731-1810). CaventouNamed for Joseph Bienaime Caventou; French chemist, pharmacologist (1795-1877). CayleyNamed for Arthur Cayley; British astronomer, mathematician (1821-1895). CelsiusNamed for Anders Celsius; Swedish astronomer (1701-1744). CensorinusNamed for Roman astronomer (fl. 238-unkn). CepheusMythological astronomer, father of Andromeda. ChacornacJean Censorinus; French astronomer (1823-1873). ChadwickChaffeeChallisNamed for James Challis; British astronomer, mathematician, physicist (1803-1862). ChalongeChamberlinChampollionChandlerChang HengChang-NgoChinese female name. ChantChaplyginChapmanChappeNamed for Jean-Baptiste d'Auteroche Chappe; French astronomer (1728-1769). ChappellCharlesFrench male name. CharlierChaucerChauvenetChebyshevChernyshevChevallierNamed for Temple Chevallier; British astronomer (1794-1873). Ching-TeChinese male name. ChladniNamed for Ernst Florens Friedrich Chladni; German physicist (1756-1827). ChretienChristelGerman female name. CichusNamed for Francesco Degli Stabili (Cecco D'Ascoli) Cichus; Italian astronomer (1257-1327). ClairautNamed for Alexis Claude Clairaut; French mathematician (1713-1765). ClarkClausiusNamed for Rudolf Julius Emmanuel Clausius; German physicist (1822-1888). ClaviusNamed for Christopher Klau Clavius; German mathematician (1537-1612). Clavius is a large ancient crater located in the southern highlands. The crater is around 240 km in diameter, but because it lies near the southern limb of the Moon, the angle that we see the crater causes it to appear more oval shaped. The rim of this crater has been pounded by impacts over the years, leaving new craters where the old rim used to be. Within the crater floor are several smaller craters, the largest of which is Rutherfurd, which butts up against the southern rim. And, for fans of the science fiction movie/book "2001-A Space Odyssey", this is where the monolith was found. CleomedesNamed for Cleomedes, Greek astronomer (unkn-c. 50 B.C.). Clavius is a large ancient crater located in the southern highlands. The crater is around 240 km in diameter, but because it lies near the southern limb of the Moon, the angle that we see the crater causes it to appear more oval shaped. The rim of this crater has been pounded by impacts over the years, leaving new craters where the old rim used to be. Within the crater floor are several smaller craters, the largest of which is Rutherfurd, which butts up against the southern rim. And, for fans of the science fiction movie/book ""2001-A Space Odyssey"", this is where the monolith was found. CleostratusNamed for Cleostratus, Greek astronomer (unkn-c. 500 B.C.). ClerkeNamed for Agnes Mary Clerke; British astronomer (1842-1907). CoblentzCockcroftCollinsNamed for Michael Collins; American astronaut (1930-Live). ColomboNamed for Christopher Columbus; Spanish explorer (c. 1446-1506). ComptonComrieComstockCondonNamed for Edward U. Condon; American physicist (1902-1974). CondorcetNamed for Jean de Condorcet; French mathematician (1743-1794). CongreveCononNamed for Conon of Samos; Greek astronomer (c. 260 B.C.). CookNamed for James Cook; British explorer (1728-1779). CooperCopernicusNamed for Nicholas Copernicus; Polish astronomer (1473-1543). Copernicus is a large crater, 93 km in diameter, 3.8 km deep, with crater walls that rise almost a kilometer above the surrounding terrain. Within the crater, there are a series of 2 to 3 central peaks. The crater walls are layered and material from the impact is spread across the surrounding area in streaks, radiating from the crater itself. Crater details are best seen when Copernicus is near the terminator. The crater rays are best seen when fully illuminated, like during a full Moon, for example. Just north of the crater are [K/Mts. Carpatus]. CoriCoriolisCouderNamed for Andre Couder; French astronomer (1897-1978). CoulombCourtneyEnglish male name. CremonaNamed for Luigi Cremona; Italian mathematician (1830-1903). CrileNamed for G. Crile; American doctor (1864-1943). CroccoCrommelinCrookesCrozierNamed for Francis Rawdon Moira Crozier; British explorer (1796-1848). CrugerNamed for Peter Cruger; German mathematician (1580-1639). CtesibiusCurieNamed for Pierre Curie; French physicist, chemist; Nobel laureate (1859-1906). CurtisNamed for Heber Doust Curtis; American astronomer (1872-1942). CurtiusNamed for Albert Curtz ; German astronomer (1600-1671). CusanusNamed for Nikolaus Krebs Cusanus; German mathematician, philosopher (1401-1464). CuvierNamed for Georges Cuvier; French natural scientist, paleontologist (1769-1832). CyranoCyrillusNamed for Saint Cyril; Egyptian theologian, chronologist (unkn-A.D. 444). The crater Cyrillus is 98 km in diameter, with an off-center double peak. The crater's northeastern rim is covered by the crater [K/Theophilus], while its northern rim is almost completely eroded away. To the south, it looks as if a channel is connecting Cyrillus with the old crater [K/Catharina]. CysatusNamed for Jean-Baptiste Cysat; Swiss mathematician, astronomer (1588-1657). D'AlembertD'ArrestNamed for Heinrich Ludwig D'Arrest; German astronomer (1822-1875). D'Arsonvalda VinciNamed for Leonardo da; Italian artist, inventor, mathematician (1452-1519). DaedalusDagScandinavian male name. DaguerreNamed for Louis Daguerre; French artist, chemist, photographer (1789-1851). DaleNamed for Sir Henry Hallett Dale; British physiologist; Nobel laureate (1875-1968). DaltonNamed for John Dalton; British chemist, physicist (1766-1844). DalyNamed for Reginald Aldworth Daly; Canadian geologist (1871-1957). DamoiseauNamed for Marie Charles Theodor De Damoiseau; French astronomer (1768-1846). DaniellNamed for John Frederick Daniell; British physicist, chemist, meteorologist (1790-1845). DanjonDanteDarneyNamed for Maurice Darney; French astronomer (1882-1958). DarwinNamed for Charles Darwin; British natural scientist (1809-1882). DasDaubr'eeNamed for Gabriel-Auguste Daubr'ee; French geologist (1814-1896). DavissonDavyNamed for Humphry Davy; British physicist (1778-1829). DawesNamed for William Rutter Dawes; British astronomer (1799-1868). Dawes crater is a small round crater 18 km in diameter and 2,330 meters deep. This crater lies right on the border where [K/Mare Serenitatis] opens up and runs into [K/Mare Tranquillitatis]. Just to the west of Dawes crater is [K/Rimae Plinius]. DawsonDe Forestde GasparisNamed for Annibale de Gasparis; Italian astronomer (1819-1892). de GerlacheNamed for Adrien de Gerlache; Belgian Antarctic explorer (1866-1934). De La RueNamed for Warren De La Rue; British astronomer (1815-1889). De MoraesDe MorganNamed for Augustus De Morgan; British mathematician (1806-1871). De RoyDe SitterNamed for Willem De Sitter; Dutch astronomer (1872-1934). De Viconamed for Francesco De Vico; Italian astronomer (1805-1848). De VriesDebesNamed for Ernest Debes; German cartographer (1840-1923). DebusDebyeDechenNamed for Ernst Heinrich Karl von Dechen; German geologist, mineralogist (1800-1889). DelambreNamed for Jean-Baptiste Joseph Delambre; French astronomer (1749-1822). DelaunayNamed for Charles Eugene Delaunay; French astronomer (1816-1872). DeliaGreek female name. DelisleNamed for Joseph Nicolas Delisle; French astronomer (1688-1768). DellingerDelmotteNamed for Gabriel Delmotte; French astronomer (1876-1950). DelporteDelucNamed for Jean Andre Deluc; Swiss geologist, physicist (1727-1817). DembowskiNamed for Baron Ercole Dembowski; Italian astronomer (1815-1881). DemocritusNamed for Democritus Greek astronomer, philosopher (c. 460-360 B.C.). DemonaxNamed for Demonax, Greek philosopher (unkn-c. 100 B.C.). DenningDesarguesNamed for Gerard Desargues; French mathematician, engineer (1593-1662). DescartesNamed for Rene Descartes; French mathematician, philosopher (1596-1650). DeseillignyNamed for Jules Alfred Pierrot Deseilligny; French selenographer (1868-1918). DeslandresNamed for Henri Alexandre Deslandres; French astrophysicist (1853-1948). DeutschDewarDianaLatin female name. DiderotDionysiusNamed for St. Dionysius the Areopagite; Greek astronomer (A.D. 9-120). DiophantusNamed for Diophantus, Greek mathematician (unkn-c. A.D. 300). DirichletDobrovolskiyDoerfelDollondNamed for John Dollond; British optician (1706-1761). DonatiNamed for Giovanni Battista Donati; Italian astronomer (1826-1873). DonnaItalian female name. DonnerDoppelmayerNamed for Johann Gabriel Doppelmayer; German mathematician, astronomer (1671-1750). DopplerDouglassDoveNamed for Heinrich Wilhelm Dove; German physicist (1803-1879). DraperNamed for Henry Draper; American astronomer (1837-1882). DrebbelNamed for Cornelius Drebbel; Dutch inventor (1572-1634). DreyerDrudeNamed for Paul K. L. Drude; German physicist (1863-1906). DrydenDrygalskiNamed for Erich D. von Drygalski; German geographer, geophysicist (1865-1949). DubyagoNamed for Dmitrij I. Dubyago; Russian astronomer (1850-1918); Alexander D. Dubyago; Soviet astronomer (1903-1959). DufayDuganDun'erDunthorneNamed for Richard Dunthorne; British astronomer (1711-1775). DysonDziewulskiEckertNamed for Wallace J. Eckert; American astronomer (1902-1971). EddingtonNamed for Sir Arthur S. Eddington; British astrophysicist, mathematician (1882-1944). EdisonEdithEgedeNamed for Hans Egede; Danish natural historian (1686-1758). EhrlichEichstadtNamed for Lorentz Eichstadt; German mathematician, astronomer (1596-1660). EijkmanEimmartNamed for Georg Christoph Eimmart; German astronomer (1638-1705). EinsteinNamed for Albert Einstein; German-American physicist; Nobel laureate (1879-1955). EinthovenElgerNamed for Thomas Gwyn Elger; British astronomer (1838-1897). EllermanEllisonElmerNamed for Charles W. Elmer; American astronomer (1872-1954). ElveyEmdenEnckeNamed for Johann Franz Encke; German mathematician, astronomer (1791-1865). EndymionNamed for Endymion, Greek mythological character. EngelhardtEotvosEpigenesNamed for Epigenes, Greek astronomer (unkn-c. 200 B.C.). EpimenidesNamed for Epimenides, Greek philosopher, writer (unkn-fl. 596 B.C.). EppingerNamed for H. Eppinger; Czechoslovakian doctor (1879-1946). EratosthenesNamed for Eratosthenes, Greek astronomer, geographer (c. 276-196 B.C.). ErroEsclangonNamed for Ernest Benjamin Esclangon; French astronomer (1876-1954). Esnault-PelterieEspinEuclidesNamed for Euclid; Greek mathematician (unkn-c. 300 B.C.). EuctemonNamed for Euctemon; Greek astronomer (unkn-fl. 432 B.C.). EudoxusNamed for Eudoxus; Greek astronomer (c. 408-355 B.C.). Eudoxus crater is 67 km in diameter with terraced walls. When Eudoxus is on the terminator, look just to the south of the crater. You will see a jagged semi-circle of light, well into the dark part of the Moon. The jagged semi-circle is high peaks within [K/Mts. Caucasus] - the Caucasus Mountains. EulerNamed for Leonhard Euler; Swiss mathematician (1707-1783). EvansEvdokimovEvershedEwenFabbroniNamed for Giovanni Valentino Mattia Fabbroni; Italian chemist (1752-1822). FabriciusNamed for David Goldschmidt Fabricius; Dutch astronomer (1564-1617). FabryFahrenheitNamed for Gabriel Daniel Fahrenheit; Dutch physicist (1686-1736). FairouzFaradayNamed for Michael Faraday; British chemist, physicist (1791-1867). FaustiniNamed for Arnaldo Faustini; Italian polar geographer (1874-1944). FauthNamed for Philipp Johann Heinrich Fauth; German selenographer (1867-1941). FayeNamed for Herve Faye; French astronomer (1814-1902). FechnerFedorovNamed for A.P. Fedorov; Russian rocket scientist (1872-1920). FelixLatin male name. FenyiFeoktistovFermatNamed for Pierre De Fermat; French mathematician (1601-1665). FermiFerneliusNamed for Jean Fernelius; French doctor, astronomer (1497-1558). FersmanFesenkovFeuilleeNamed for Louis Feuillee; French natural scientist (1660-1732). FinschNamed for O. F. H. Finsch; German zoologist (1839-1917). FinsenFirmicusNamed for Maternus Firmicus; Italian astronomer (unkn-c. 330). FirsovFischerFitzgeraldFizeauFlammarionNamed for Camille Flammarion; French astronomer (1842-1925). FlamsteedNamed for John Flamsteed; British astronomer (1646-1720). FlemingFlorenskyFocasNamed for Ionnas Focas; French astronomer (1908-1969). FontanaNamed for Francesco Fontana; Italian astronomer (c. 1585-1656). FontenelleNamed for Bernard Le Bovier De Fontenelle; French astronomer (1657-1757). FosterFoucaultNamed for Leon Foucault; French physicist (1819-1868). FourierNamed for Jean-Baptiste Joseph Fourier; French mathematician (1768-1830). FowlerFoxFra MauroNamed for Fra Mauro, Italian geographer (unkn-1459). Fra Mauro is a very old, eroded crater. Its northern border appears to have been flooded with lava and bombarded by impacts as several small craters lie along its rim. The crater is cut in two by a large crack that runs north/south through its floor. Two craters bump up against Fra Mauro to the south. Bonpland crater is the larger one to the west (60 km). Parry, to the east, is 48 km. [K/Apollo 14] landed just to the north of Fra Mauro. FracastoriusNamed for Girolamo Fracastoro; Italian doctor, astronomer (1483-1553). Fracastorius crater lies at the southern end of [K/Mare Nectaris]. This is an old, highly eroded crater. Its northern border has been completely flooded by the lava that filled the mare. The southern rim has been bombarded by small impacts which has left many small craters along what used to be the crater wall. Fracastorius is 112 km in diameter and has a crack running through it, from east to west. FranckNamed for James Franck; German physicist; Nobel laureate (1882-1964). FranklinNamed for Benjamin Franklin; American inventor (1706-1790). FranzNamed for Julius Heinrich Franz; German astronomer (1847-1913). FraunhoferNamed for Joseph von Fraunhofer; German astronomer, optician (1787-1826). FredholmNamed for Erik Ivar Fredholm; Swedish mathematician (1866-1927). FreudNamed for Sigmund Freud; Austrian psychoanalyst (1856-1939). FreundlichFridmanFroelichFrostFryxellFurneriusNamed for Georges Furner; French mathematician (unkn-fl. 1643). Furnerius is the southernmost of a chain of four old, large craters. It is 135 km in diameter and has several small craters within its walls. There is no central peak. The other craters in the chain are [K/Langrenus], [K/Vendelinus], and [K/Petavius]. South of Furnerius are the heavily cratered lunar highlands. When viewing along the terminator, the dividing line between light and dark will be very jagged, because of the variety of crater wall heights within this heavily cratered terrain." G. BondNamed for George Philip Bond; American astronomer (1826-1865). GadomskiGagarinGalenNamed for Claudius Galen; Greek doctor (c. 129-200). GalilaeiNamed for Galileo; Italian astronomer, physicist (1564-1642). GalleNamed for Johann Gottfried Galle; German astronomer (1812-1910). GaloisGalvaniNamed for Luigi Galvani; Italian physicist (1737-1798). GambartNamed for Jean Felix Gambart; French astronomer (1800-1836). GamowGanskiyGanswindtGaravitoGardnerNamed for Irvine Clifton Gardner; American physicist (1889-1972). GartnerNamed for Christian Gartner; German mineralogist, geologist (c. 1750-1813). GassendiNamed for Pierre Gassendi; French astronomer, mathematician (1592-1655). This flat, shallow looking crater has a distinct central peak and a small crater on its northern rim, giving it a "diamond ring" appearance. Gassendi is 101 km in diameter and 1.9 km deep. The crater floor is rough with rilles, fissures, and hills. The crater wall is rather narrow. The crater on its rim is Gassendi A. GastonFrench male name. GaudibertNamed for Casimir Marie Gaudibert; French astronomer (1823-1901). GauricusNamed for Luca Gaurico; Italian astronomer (1476-1558). GaussNamed for Karl Friedrich Gauss; German mathematician (1777-1855). GavrilovGay-LussacNamed for Joseph Louis Gay-Lussac; French physicist (1778-1850). GeberNamed for Gabir Ben Aflah Geber; Spanish-Arab astronomer (unkn-c. 1145). GeigerGeisslerNamed for Heinrich Geissler; German physicist (1814-1879). GeminusNamed for Geminus; Greek astronomer (unkn-c. 70 B.C.). Gemma FrisiusNamed for Reinier Jemma; Dutch doctor (1508-1555). GerardNamed for Alexander Gerard; Scottish explorer (1792-1839). GerasimovichGernsbackGibbsNamed for Josiah Willard Gibbs; American mathematical physicist (1839-1903). GilbertNamed for Grove K. Gilbert; American geologist (1843-1918), William Gilbert; English geophysician (1544-1603). GillNamed for Sir David Gill; British astronomer (1843-1914). GinzelGiojaNamed for Flavio Gioja; Italian inventor (unkn-fl. 1302). Giordano BrunoGlaisherNamed for James Glaisher; British meteorologist (1809-1903). GlauberGlazenapGlushkoNamed for V.P. Glushko; Russian space scientist (1908-1989). GocleniusNamed for Rudolf Gockel; German physicist, doctor, mathematician (1572-1621). GoddardNamed for Robert H. Goddard; American rocketry scientist (1882-1945). GodinNamed for Louis Godin; French astronomer, mathematician (1704-1760). GoldschmidtNamed for Hermann Goldschmidt; German astronomer (1802-1866). GolgiNamed for Camillo Golgi; Italian doctor; Nobel laureate (c. 1843-1926). GolitsynGolovinGoodacreNamed for Walter Goodacre; British selenographer (1856-1938). GouldNamed for Benjamin Apthorp Gould; American astronomer (1824-1896). GraceEnglish female name. GrachevGraffNamed for Kasimir R. Graff; Polish-German astronomer (1878-1950). GraveGreavesNamed for William Michael Herbert Greaves; British astronomer (1897-1955). GreenGregoryGriggGrimaldiNamed for Francesco Maria Grimaldi; Italian astronomer, physicist (1618-1663). GrissomGrotrianGroveNamed for Sir William Robert Grove; British physicist (1811-1896). GruembergerNamed for Christoph Gruemberger; Austrian astronomer (1561-1636). GruithuisenNamed for Franz von Gruithuisen; German astronomer (1774-1852). GuerickeNamed for Otto von Guericke; German physicist, engineer, naturalist (1602-1686). GuillaumeGullstrandGumNamed for Colin Gum; Australian astronomer (1924-1960). GutenbergNamed for Johann Gutenberg; German inventor (c. 1398-1468). GuthnickNamed for Paul Guthnick; German astronomer (1879-1947). GuyotGyldenNamed for Hugo Gylden; Swedish astronomer (1841-1896). H. G. WellsHageciusNamed for Thaddaeus Hayek; Czechoslovakian astronomer, mathematician (1525-1600). HagenHahnNamed for Friedrich von Hahn; German astronomer (1741-1805); Otto Hahn; German chemist (1879-1968). HaidingerNamed for Wilhelm Karl von Haidinger; Austrian geologist, physicist (1795-1871). HainzelNamed for Paul Hainzel; German astronomer (unkn-fl. 1570). HaldaneNamed for John Burdon Sanderson Haldane; British doctor (1892-1964). HaleNamed for George Ellery Hale; American astronomer (1868-1938); William Hale; British rocket scientist (1797-1870). HallNamed for Asaph Hall; American astronomer (1829-1907). HalleyNamed for Edmond Halley; British astronomer (1656-1742). HamiltonNamed for Sir William R. Hamilton; Irish mathematician (1805-1865). HannoNamed for Roman explorer (unkn-c. 500 B.C.). HansenNamed for Peter Andreas Hansen; Danish astronomer (1795-1874). HansteenNamed for Christopher Hansteen; Norwegian astronomer (1784-1873). HardenHardingNamed for Karl Ludwig Harding; German astronomer (1765-1834). HaretHargreavesNamed for Frederick James Hargreaves; British astronomer, optician (1891-1970). HarkhebiHarlanNamed for Harlan J. Smith Harlan; American astronomer (1924-1991). HaroldScandinavian male name. HarpalusNamed for Harpalus Greek astronomer (unkn-c. 460 B.C.). HarriotHartmannHartwigNamed for Carl E. Hartwig; German astronomer (1851-1923). HarveyHaseNamed for Johann Matthias Hase; German mathematician (1684-1742). HatanakaHausenNamed for Christian August Hausen; German astronomer, mathematician, physicist (1693-1743). HayfordHaynNamed for Friedrich Hayn; German astronomer (1863-1928). HealyHeavisideHecataeusNamed for Hecataeus; Greek geographer (unkn-c. 476 B.C.). HedervariNamed for Peter Hedervari; Hungarian geoscientist (1931-1984). HedinNamed for Sven A. Hedin; Swedish explorer (1865-1952). HeinrichNamed for Wladimir W. Heinrich; Czechoslovakian astronomer (1884-1965). HeinsiusNamed for Gottfried Heinsius; German astronomer (1709-1769). HeisNamed for Eduard Heis; German astronomer (1806-1877). HelbergHeliconNamed for Greek astronomer, mathematician (unkn-c. 400 B.C.). HellMaximilian Helicon; Hungarian astronomer (1720-1792). HelmertNamed for Friedrich Robert Helmert; German astronomer, geodesist (1843-1917). HelmholtzNamed for Hermann Von Helmholtz; German doctor (1821-1894). HendersonHendrixHenryNamed for Joseph Henry; American physicist (1792-1878). Henry FreresNamed for Prosper Henry Freres; French astronomer (1849-1903); Paul Henry Freres; French astronomer (1848-1905). HenyeyHeraclitusNamed for Heraclitus; Greek philosopher (c. 540-480 B.C.). HerculesNamed for Hercules; Greek mythological hero. The crater Hercules lies on the easternmost edge of [K/Lacus Mortis] and just to the west of the old crater [K/Atlas]. Hercules is 69 km in diameter, with a small round crater lying within it. The small crater is near the center, just offset to the south. HerigoniusNamed for Pierre Herigone; French mathematician, astronomer (fl. 1644). HermannNamed for Jacob Hermann; Swiss mathematician (1678-1733). HermiteNamed for Charles Hermite; French mathematician (1822-1901). HerodotusNamed for Herodotus Of Halikarnassus; Greek historian (c. 484-408 B.C.). Herodotus crater is a small, flooded crater with thin walls that lies on the southern part of a wrinkled ""island"" in [K/Oceanus Procellarum]. Herodotus is 34 km in diameter and has a smooth floor with no central peak. The crater [K/Aristarchus] is just to the east. HeronHerschelNamed for William Herschel; British astronomer (1738-1822). HertzHertzsprungHesiodusNamed for Hesiod; Greek humanitarian (c. 735 B.C.). HessHeveliusNamed for Johann Howelcke; Polish astronomer (1611-1687). HeymansHeyrovskyHilbertHillNamed for George William Hill; American astronomer, mathematician (1838-1914). HindNamed for John Russell Hind; British astronomer (1823-1895). HippalusNamed for Hippalus; Greek explorer (unkn-c. 120). HipparchusNamed for Hipparchus; Greek astronomer (unkn-fl. 140 B.C.). HippocratesHirayamaNamed for Kiyotsugu Hirayama; Japanese astronomer (1874-1943); Shin Hirayama; Japanese astronomer (1867-1945). HoffmeisterHoggHohmannNamed for Walter Hohmann; German space flight engineer (1880-1945). HoldenNamed for Edward Singleton Holden; American astronomer (1846-1914). HoletschekHommelNamed for Johann Hommel; Greek astronomer, mathematician (1518-1562). HookeNamed for Robert Hooke; British physicist, inventor (1635-1703). HopmannHornsbyNamed for Thomas Hornsby; British astronomer (1733-1810). HorrebowNamed for Peder Horrebow; Danish astronomer (1679-1764). HorrocksNamed for Jeremiah Horrocks; British astronomer (1619-1641). HortensiusNamed for Martin van den Hove; Dutch astronomer (1605-1639). HoutermansNamed for Friedrich Georg Houtermans; German physicist (1903-1966). HouzeauHubbleNamed for Edwin P. Hubble; American astronomer (1889-1953). HugginsNamed for Sir William Huggins; British astronomer (1824-1910). HumasonNamed for Milton L. Humason; American astronomer (1891-1972). HumboldtNamed for Wilhelm von Humboldt; German philologist (1767-1835). HumeNamed for David Hume; Scottish philosopher (1711-1776). HuttonHuxleyNamed for Thomas Henry Huxley; British biologist (1825-1895). HyginusNamed for Caius Julius Hyginus; Spanish astronomer (unkn-c. A.D. 100). HypatiaNamed for Hypatia; Egyptian mathematician (unkn-A.D. 415). IanScottish male name. Ibn BattutaNamed for Abu Abd Allah Mohammed Ibn Abd Allah; Moroccan geographer (1304-1377). Ibn FirnasIbn YunusNamed for C. Abu Muhammad Ibn-Rushd (Averrdes); Egyptian astronomer (950-1009). Ibn-RushdNamed for Ibn-Rushd; Spanish-Arab philosopher, doctor (1126-1198). IcarusIdelerNamed for Christian Ludwig Ideler; German astronomer (1766-1846). IdelsonIlinInaLatin female name. IngallsInghiramiNamed for Giovanni Inghirami; Italian astronomer (1779-1851). InnesIoffeIsabelSpanish female name. IsaevIsidorusNamed for St. Isidore of Seville; Roman astronomer (c. 570-636). IsisNamed for Isis; Egyptian goddess. IvanRussian male name. IzsakJ. HerschelNamed for John Herschel; British astronomer (1792-1871). JacksonJacobiNamed for Karl Gustav Jacob; German mathematician (1804-1851). JansenNamed for Zacharias Janszoon; Dutch optician (1580-c. 1638). JanskyNamed for Karl Jansky; American radio engineer (1905-1950). JanssenNamed for Pierre Jules Janssen; French astronomer (1824-1907). JarvisJeansNamed for Sir James H. Jeans; British mathematical physicist (1877-1946). JehanTurkish female name. JenkinsNamed for Louise F. Jenkins; American astronomer (1888-1970). JennerJerikScandinavian male name. JoliotNamed for Frederic Joliot-Curie; French physicist; Nobel laureate (1900-1958). JomoAfrican male name. JoseSpanish male name. JouleJoyNamed for Alfred H. Joy; American astronomer (1882-1973). Jules VerneJulienneFrench female name. Julius CaesarNamed for Julius Caesar; Roman emperor, introduced the Julian calendar (c. 102-44 B.C.). KaiserNamed for Frederick Kaiser; Dutch astronomer (1808-1872). KamerlinghKaneNamed for Elisha Kent Kane; American explorer (1820-1857). KantNamed for Immanuel Kant; German philosopher (1724-1804). KaoNamed for Ping-Tse Kao; Taiwanese astronomer (1888-1970). KapteynNamed for Jacobus C. Kapteyn; Dutch astronomer (1851-1922). KarimaKarpinskiyKarrerKasperKastnerNamed for Abraham Gotthelf Kastner; German mathematician, physicist (1719-1800). KatchalskyKathleenIrish female name. KearonsKeelerKekuleKeldyshNamed for Mstislav V. Keldysh; Soviet mathematician (1911-1978). KepinskiKeplerNamed for Johannes Kepler; German astronomer (1571-1630). Kepler is a ray crater. While rather small, only 30 km in diameter, the debris from this crater is scattered in straight rays stretching over 300 km from its center. Because so much of the surrounding rays are easily visible, and have not been covered up by later impacts, scientists believe that Keplar is a fairly young crater. The crater is about 2.6 km deep and has an uneven floor with no central peak. Crater details are best seen when Kepler is near the terminator. The crater rays are best seen when fully illuminated, like during a Full Moon. Kepler is west of another, much larger ray crater, [K/Copernicus]. KhvolsonKibalchichKidinnuKiesNamed for Johann Kies; German mathematician, astronomer (1713-1781). KiessNamed for Carl Clarence Kiess; American astrophysicist (1887-1967). KimuraKinauNamed for C. A. Kinau; German botanist, selenographer (unkn-fl. 1850). KingKiraKirchNamed for Gottfried Kirch; German astronomer (1639-1710). KircherNamed for Athanasius Kircher; German humanitarian (1601-1680). KirchhoffNamed for Gustav Robert Kirchhoff; German physicist (1824-1887). KirkwoodKlaprothNamed for Martin Heinrich Klaproth; German chemist, mineralogist (1743-1817). KleinNamed for Hermann Joseph Klein; German astronomer (1844-1914). KleymenovKluteKnox-ShawNamed for Harold Knox-Shaw; British astronomer (1885-1970). KochKohlschutterKolhorsterKomarovKondratyukKonigNamed for Rudolf Konig; Austrian mathematician, astronomer (1865-1927). KonoplevKonstantinovKopffNamed for August Kopff; German astronomer (1882-1960). KorolevKosbergKostinskiyKovalevskayaKovalskiyKozyrevKrafftNamed for Wolfgang Ludwig Krafft; German astronomer, physicist (1743-1814). KramarovKramersKrasnovNamed for Aleksander V. Krasnov; Russian astronomer (1866-1907). KrasovskiyKreikenNamed for E. A. Kreiken; Dutch astronomer (1896-1964). KriegerNamed for Johann Nepomuk Krieger; German selenographer (1865-1902). KrishnaIndian male name. KroghNamed for Schack August Steenberg Krogh; Danish zoologist, physiologist; Nobel laureate (1874-1949). KrusensternNamed for Adam Johann, Baron Von Krusenstern; Russian explorer (1770-1846). KrylovKuglerKuiperNamed for Gerard Peter Kuiper; Dutch-American astronomer (1905-1973). KulikKundtNamed for August Kundt; German physicist (1839-1894). KunowskyNamed for Georg Karl Friedrich Kunowsky; German astronomer (1786-1846). Kuo Shou ChingKurchatovLa CailleNamed for Nicholas Louis De La Caille; French astronomer (1713-1762). La CondamineNamed for Charles Marie De La Condamine; French astronomer, physicist (1701-1774). La PerouseNamed for Jean Francois de Galoup, Comte De La Perouse; French explorer (1741-1788). LacchiniLacroixNamed for Sylvestre Francois De Lacroix; French mathematician (1765-1843). Lacus Aestatis"Lake of Summer". Lacus Autumni"Lake of Autumn". Lacus Bonitatis"Lake of Goodness". Lacus Doloris"Lake of Sorrow". Lacus Excellenti"Lake of Excellence". Lacus Felicitati"Lake of Happiness". Lacus Gaudii"Lake of Joy". Lacus Hiemalis"Wintry Lake". Lacus Lenitatis"Lake of Softness". Lacus LuxuriaeLacus Mortis"Lake of Death". The Lake of Death is dominated by [K/Burg] crater. This small dark area is roughly 150 km in diameter and is fractured by various fissures running across its floor. Lacus OblivionisLacus Odii"Lake of Hatred". Lacus Perseveran"Lake of Perseverance". Lacus SolitudiniLacus Somniorum"Lake of Dreams". Lacus Spei"Lake of Hope". Lacus Temporis"Lake of Time". Lacus Timoris"Lake of Fear". Lacus Veris"Lake of Spring". LadeNamed for Heinrich Eduard von Lade; German astronomer (1817-1904). LagallaNamed for Giulio Cesare Lagalla; Italian philosopher (1571-1624). LagrangeNamed for Joseph Louis Lagrange; Italian mathematician (1736-1813). LalandeNamed for Joseph Jerome Le Francois De Lalande; French astronomer (1732-1807). LallemandNamed for Andre Lallemand; French astronomer (1904-1978). LamarckNamed for Jean B. P. A. De M. Lamarck; French natural historian (1744-1829). LambLambertNamed for Johann Heinrich Lambert; German astronomer, mathematician, physicist (1728-1777). LameNamed for Gabriel Lame; French mathematician (1795-1870). LamechNamed for Felix Chemla Lamech; French selenographer (1894-1962). LamontNamed for John Lamont; Scottish astronomer (1805-1879). LamplandLandauLanderLandsteinerNamed for Karl Landsteiner; Austrian-American pathologist; Nobel laureate (1868-1943). LaneLangemakLangevinLangleyNamed for Samuel P. Langley; American astronomer, physicist (1834-1906). LangmuirLangrenusNamed for Michel Florent van Langren; Belgian selenographer, engineer (c. 1600-1675). Langrenus is a very nice, sharply defined crater, with terraced walls and a double central peak. It is 127 km in diameter and is the first of a series of four old, large craters that form a crater chain. Scientists believe that crater chains were formed when an object, like a comet, broke apart and the resulting pieces slammed into the Moon, one after the other. The other three craters in the chain are [K/Vendelinus], [K/Petavius], and [K/Furnerius]. LansbergNamed for Philippe van Lansberg; Belgian astronomer (1561-1632). LarmorLassellNamed for William Lassell; British astronomer (1799-1880). LaueLauritsenLavoisierNamed for Antoine Laurent Lavoisier; French chemist (1743-1794). LawrenceNamed for Ernest Orlando Lawrence; American physicist; Nobel laureate (1901-1958), and Robert H. Lawrence; American astronaut (1935-1993). Le GentilNamed for Guillaume Hyazinthe Le Gentil; French astronomer (1725-1792). Le MonnierNamed for Pierre Charles Le Monnier; French astronomer, physicist (1715-1799). Le VerrierNamed for Urbain Jean Le Verrier; French astronomer, mathematician (1811-1877). LeakeyNamed for Louis Seymour Bazett Leakey; British archaeologist (1903-1972). LeavittLebedevLebedinskiyLebesgueNamed for Henri Leon Lebesgue; French mathematician (1875-1941). LeeNamed for John Lee; British astronomer, humanitarian (1783-1866). LeeuwenhoekLegendreNamed for Adrien Marie Legendre; French mathematician (1752-1833). LehmannNamed for Jacob Heinrich Wilhelm Lehmann; German astronomer (1800-1863). LeibnitzLemaitreLentsLeonovLepauteNamed for Nicole Reine De La Briere Lepaute; French astronomer (1723-1788). LetronneNamed for Jean Antoine Letronne; French archaeologist (1787-1848). LeucippusLeuschnerLevi-CivitaLewisLexellNamed for Anders Johann Lexell; Swedish mathematician, astronomer (1740-1784). LeyLicetusNamed for Fortunio Liceti; Italian physicist, philosopher, doctor (1577-1657). LichtenbergNamed for Georg Christoph Lichtenberg; German physicist (1742-1799). LickNamed for James Lick; American benefactor (1796-1876). LiebigNamed for Justus, Baron von Liebig Liebig; German chemist (1803-1873). LiliusNamed for Luigi Giglio Lilius; Italian doctor, philosopher, chronologist (unkn-1576). LindaSpanish female name. LindberghNamed for Charles Augustus Lindbergh; American aviator (1902-1974). LindbladLindenauNamed for Bernhard von Lindenau; German astronomer (1780-1854). LindsayNamed for Eric M. Lindsay; Irish astronomer (1907-1974). LinneNamed for Carl von Linne; Swedish botanist (1707-1778). Linne crater is a small, sharp crater in [K/Mare Serenitatis] that you can really test the resolution power of your telescope optics. This crater is only 2 km in diameter. It is surrounded by a ring of light material. The light ring shows up better when fully illuminated. LiouvilleNamed for Joseph Liouville; French mathematician (1809-1882). LippersheyNamed for Hans (Jan Lapprey) Lippershey; Dutch optician (unkn-1619). LippmannLipskiyLitkeLittrowNamed for Johann Josef von Littrow; Czechoslovakian astronomer (1781-1840). LobachevskiyLockyerNamed for Norman Lockyer; British astrophysicist (1836-1920). LodyginLoewyNamed for Moritz Loewy; French astronomer (1833-1907). LohrmannNamed for Wilhelm Gotthelf Lohrmann; German selenographer (1796-1840). LohseNamed for Oswald Lohse; German astronomer (1845-1915). LomonosovLongomontanusNamed for Christian Sorensen Longomontanus; Danish astronomer, mathematician (1562-1647). LorentzLouiseFrench female name. LouvilleNamed for Chevalier De Louville Jacques D'Allonville; French astronomer, mathematician (1671-1732). LoveLovelaceLovellLowellLubbockNamed for Sir John William Lubbock; British astronomer, mathematician (1803-1865). LubiniezkyNamed for Stanislaus Lubiniezky; Polish astronomer (1623-1675). LucianNamed for Lucian Of Samosata; Greek writer (125-190). LucretiusLudwigLundmarkLutherNamed for Robert Luther; German astronomer (1822-1900). LyapunovNamed for Aleksandr M. Lyapunov; Russian mathematician, engineer (1857-1918). LyellNamed for Sir Charles Lyell; Scottish geologist (1797-1875). LymanLyotNamed for Bernard F. Lyot; French astronomer (1897-1952). MachMaclaurinNamed for Colin Maclaurin; Scottish mathematician (1698-1746). (Spelling changed from MacLaurin.) MaclearNamed for Thomas Maclear; Irish astronomer (1794-1879). MacMillanNamed for William Duncan MacMillan; American mathematician, astronomer (1871-1948). MacrobiusNamed for Ambrosius Aurelius Theodosius Macrobius; Roman writer (unkn-fl. c. 410). This small crater lies just to the west of [K/Mare Crisium]. When fully illuminated, one can see a bright white donut shape within the crater. Bright rays radiating away from the crater can also be seen. Macrobius is 64 km in diameter with a prominent central peak. MadlerNamed for Johann Heinrich Madler; German astronomer (1794-1874). MaestlinNamed for Michael Maestlin; German mathematician (1550-1631). MagelhaensNamed for Fernao De (Ferdinand Magellan) Magelhaens; Portuguese explorer (1480-1521). MaginusNamed for Giovanni Antonio Magini; Italian astronomer, mathematician (1555-1617). MainNamed for Robert Main; British astronomer (1808-1878). MairanNamed for Jean Jacques D'Ortous De Mairan; French geophysicist (1678-1771). MaksutovMalapertNamed for Charles Malapert; Belgian astronomer, mathematician, philosopher (1581-1630). MalletNamed for Robert Mallet; Irish seismologist, engineer (1810-1881). MalyyMandelshtamManiliusNamed for Marcus Manilius; Roman writer (unkn-c. 50 B.C.). MannersNamed for Russell Henry Manners; British astronomer (1800-1870). ManuelSpanish male name. ManzinusNamed for Carlo Antonio Manzini; Italian astronomer (1599-1677). MaraldiNamed for Giovanni Domenico Maraldi; Italian astronomer, geodesist (1709-1788); Jacques Philippe; French astronomer (1665-1729). MarciMarco PoloNamed for Italian explorer (1254-1324). MarconiMare Anguis"Serpent Sea". The small Serpent Sea lies on the northeastern rim of the much larger [K/Mare Crisium]. It covers an area roughly the size of Jamaica. Mare Australe"Southern Sea". The Southern Sea stretches onto the far side, so all of it is not visible from Earth. This mare has an irregular shape that covers an area of 151,000 sq km. There are craters scattered about its surface. Mare Cognitum"Sea that has become known". The Sea that is Known"" was named in 1964 when Ranger 7 sent back the first images of it for viewers on Earth to see. The spacecraft showed that the smooth plain visible from Earth was actually covered with small craters and rocks. This small mare lies just to the east of [K/Oceanus Procellarum], divided only by the small mountain range [K/Mts. Riphaeus]. Mare Crisium"Sea of Crises". The Sea of Crises is a large flooded crater. It appears as an almost perfect dark circle not far from the Moon's eastern limb. Though more of an oval than a circle, our view of this mare is distorted by the angle we are viewing it. From Earth, the Sea of Crises appears to be 435 km by 290 km in size. However, when viewing the mare from directly overhead in lunar orbit, it is actually 435 km by 564 km in diameter. Within the mare, near its western border, there are three small young craters lined up north to south; [K/Swift] (11 km in size), [K/Peirce], just to the south is 18 km in diameter, and [K/Picard], farther south is 23 km in diameter. This mare is roughly the same area as Cambodia. Mare FecunditatiMare Fecunditatis - "Sea of Fecundity". The Sea of Fertility is an irregular-shaped dark area not far from the Moon's eastern limb. This mare is more long and narrow than circular. It stretches almost 600 km north and south and is about 200 km at its widest point. In total, it covers an area of 326,000 sq km, about the same area as Norway. The mare has a very textured surface, as if the lava filling this area just barely covered all of the craters, leaving hints of what lies below. Mare Frigoris"Sea of Cold". The Sea of Cold is unusual because, unlike most maria which are roughly circular, Mare Frigoris is long and narrow, stretching over 1,596 km across the northern limb of the Moon. In total, the mare covers an area of 436,000 sq km, almost as much area as the country of Sweden. Mare HumboldtianMare Humboldtianum - Named for Alexander von Humboldt; German natural historian (1769-1859). Humbolbt's Sea was named after the German explorer, Alexander von Humboldt. This dark flooded crater lies along the eastern limb of the Moon, so only a small portion of it is visible from Earth. Covering 22,000 sq. km., this mare is slightly larger than the country of El Salvador. Mare Humorum"Sea of Moisture". The Sea of Moisture is a flooded crater that lies to the south of Oceanus Procellarum. The mare is 389 km in diameter and covers an area 113,000 sq km, an area slightly larger than Cuba. Its surface is mostly smooth, with a few small craters and some wrinkled terrain to the east. Mare Imbrium"Sea of Showers". The Sea of Rains forms the largest impact basin on the lunar surface and the second largest flooded plain. It is 1,123 km in diameter and covers 830,000 sq km of the Moon's northwestern surface, almost matching the area of Venezuela. The floor of the mare is covered by a series of dorsum or ridges stretching north to south and there are rays (lighter markings) radiating from the crater [K/Copernicus] to the south. These rays are best seen when the Sun is shining straight down on them, during a full Moon. The southwestern border of the mare has been flooded over by lava, which connects the Sea of Rains to [K/Oceanus Procellarum], the Ocean of Storms. Three distinct craters lie clustered together near the northeastern border: [K/Archimedes], the largest of the three at 82 km in diameter, [K/Autolycus], the smallest, and [K/Aristillus]. Mare IngeniiMare Insularum"Sea of Islands". The Sea of Islands is 900 km in diameter and covers an area of 635,850 sq km, an area slightly smaller than the country of Afghanistan. This mare is dominated by the crater [K/Copernicus]. Much of its surface is covered by light-colored rays coming from the impact event that formed Copernicus. Mare Marginis"Sea of the Edge". The Border Sea lies just along the Moon's north eastern limb, as seen from Earth. Although not entirely visible from Earth, the flooded crater that makes up Mare Marginis is between 360-420 km wide and covers an area roughly the size of the Republic of Georgia. Mare MoscovienseMare Nectaris"Sea of Nectar". The Sea of Nectar is a large flooded crater that has a diameter of roughly 340 km and covers an area roughly the size of Portugal. It surface appears fairly smooth with the large crater [K/Fracastorius] lying on its the southwestern border. Mare Nubium"Sea of Clouds". The Sea of Clouds lies at the southeastern end of [K/Oceanus Procellarum]. It is roughly 715 km in diameter, and covers an area 254,000 sq km, an area roughly the size of New Zealand. The surface of the mare is wrinkled and pockmarked with small craters, scarps and fissures. The crater [K/Bullialdus] lies within the mare, towards the western border. Mare Orientale"Eastern sea" The Eastern Sea - only a very tiny bit of this large ringed basin is visible from Earth. What little can be seen lies just along the southwestern limb of the Moon. Spacecraft passing around the far side of the Moon have taken images of this impressive basin with its flooded central crater and surrounding mountain rings, but from Earth's view, the most we can see is a narrow dark strip. Mare SerenitatisMare Serenitatis - "Sea of Serenity". The Sea of Serenity is a very large flooded crater over 700 km in diameter and covering an area over 370,000 sq km (about the same area as Japan). A large impact early in the moon's history probably cracked the lunar crust and allowed lava from the moon's then molten core to seep up and fill in the impact crater. On the floor of the mare, near its eastern border is a series of dorsum, or ridges. An area about 170 km long on the southeastern border of the mare has been overrun by lava. On the northern edge of the border break lies [K/Mons Argaeus]. [K/Dawes] crater lies in the middle of the overflow region, while [K/Rimae Plinius], a series of straight fissures begin at western edge of the break and continue eastward for about 100 km. Mare SmythiiNamed for William Henry Smyth; Smith's Sea was named after William Henry Smith, a British astronomer. Only the tiny edge of this flooded crater can be seen from Earth. Mare Smythii can be seen just along the Moon's eastern limb, passing through the lunar equator. The mare covers an area roughly the size of Guatemala. Mare Spumans"Foaming Sea". The Foaming Sea is a small, roughly circular flooded plain that lies to the south of [K/Mare Crisium] and might look like an eastern extension of [K/Mare Fecunditatis]. This small mare covers about 16,000 sq km, about the same area as the Earthly island of Fiji. Mare TranquitatiMare Tranquitatis - "Sea of Tranquility". This large, roughly circular dark area of the moon was made famous on July 20, 1969 when [K/Apollo 11] landed within its borders. Apollo 11 touched down in the southwestern part of the Sea of Tranquility, near where the smooth plane [K/Sinus Asperitatis] drops down from the south of the mare. The Sea of Tranquility has several small craters scattered across its floor, as well as several fissures along its western border. There is also a wrinkled feature called Lamont towards the western side of the mare. Just northeast of Lamont, you may notice an unusual transition from dark to light terrain. This mare covers 421,000 sq. km, just slightly more area than the state of California. Mare Undarum"Sea of Waves". The Sea of Waves is a small irregularly shaped plain that lies to the southeast of [K/Mare Crisium]. This mare covers about 21,000 sq km, or about the same area as El Salvador. Mare Vaporum"Sea of Vapors". The Sea of Vapors is a small, roughly circular flooded plain that lies to the southwest of [K/Mare Serenitatis] and southeast of the rugged [K/Mts. Apenninus]. This mare is about 240 km in diameter and covers an area 55,000 sq km, about the same area as Costa Rica. It looks like the southeastern border of this mare has been flooded out by lava. The flooding lava spilled out and continued on to the southwest, forming a small bay called [K/Sinus Medii]. MarinusNamed for Marinus Of Tyre; Greek geographer (unkn-c. 100). MariotteMariusNamed for Simon Mayer; German astronomer (1570-1624). MarkovNamed for Aleksandr V. Markov; Soviet astrophysicist (1897-1968); Andrei A.; Russian mathematician (1856-1922). MarthNamed for Albert Marth; German astronomer (1828-1897). MaryEnglish form of Hebrew female name. MaskelyneNamed for Nevil Maskelyne; British astronomer (1732-1811). MasonNamed for Charles Mason; British astronomer (1730-1787). MaunderNamed for Annie S. D. R. Maunder; British astronomer (1868-1947); Edward Walter Maunder; British astronomer (1851-1928). MaupertuisNamed for Pierre Louis De Maupertuis; French mathematician (1698-1759). MaurolycusNamed for Francesco Maurolico; Italian mathematician (1494-1575). MauryNamed for Matthew Fontaine Maury; American oceanographer (1806-1873); Antonia C. Maury; American astronomer (1866-1952). MavisScottish female name. MaxwellMcAdieNamed for Alexander George McAdie; American meteorologist (1863-1943). McAuliffeMcClureNamed for Robert Le Mesurier McClure; British explorer (1807-1873). McDonaldNamed for William Johnson McDonald; American benefactor (1844-1926); Thomas Logie McDonald; Scottish selenographer (unkn.-1973). McKellarMcLaughlinNamed for Dean B. McLaughlin; American astronomer (1901-1965). McMathMcNairMcNallyMechnikovMeeNamed for Arthur Butler Phillips Mee; Scottish astronomer (1860-1926). MeesMeggersMeitnerMelissaMendelMendeleevMenelausNamed for Menelaus Of Alexandria; Greek geometer, astronomer (c. A.D. 98). Menelaus is a distinct crater with thin, sharp walls and a series of central peaks. It is 26 km in diameter and 3 km deep. This crater can be found along the mountainous southern border of [K/Mare Serenitatis]. An unusual ray of lighter material emanating from this crater stretches to the north and intercepts the crater [K/Bessel]. The ray can best be seen when fully illuminated. Crater details are best seen when near the terminator. MenzelNamed for Donald Howard Menzel; American astrophysicist, Smithsonian researcher (1901-1976). MercatorNamed for Gerard De Kremer (Gerhardus Mercator) Mercator; Belgian cartographer, geographer, mathematician (1512-1594). MercuriusNamed for Mercury; Roman mythical messenger. MerrillMerseniusNamed for Marin Mersenne; French mathematician, physicist (1588-1648). MeshcherskiyMessalaNamed for (Ma-Sa-Allah) Messala; Jewish astronomer (unkn- c. 815). MessierNamed for Charles Messier; French astronomer (1730-1817). Messier is actually a double crater; two small craters lying side by side in [K/Mare Fecunditatis]. The crater to the east is slightly oval in shape, while the crater to the west has two bright rays extending away from it to the west. Both craters are approx. 11 km in diameter. The bright rays are best seen when fully illuminated, like during a full Moon. MetiusNamed for Adriaan Adriaanszoon Metius; Dutch astronomer (1571-1635). MetonNamed for Meton; Greek astronomer (unkn-fl. 432 B.C.). MezentsevMichaelEnglish male name. MichelsonMilankovivcMilichiusNamed for Jacob Milich; German doctor, mathematician, astronomer (1501-1559). MillerNamed for William Allen Miller; British chemist (1817-1870). MillikanMillsMilneMineurMinkowskiMinnaertMitchellNamed for Maria Mitchell; American astronomer (1818-1889). MitraMobiusMohorovivcicMoignoNamed for Francois Napoleon Marie Moigno; French mathematician, physicist (1804-1884). MoiseevMoissanMoltkeNamed for Graf von Moltke Helmuth Karl; German benefactor (1800-1891). MongeNamed for Gaspard Monge; French mathematician (1746-1818). MoniraArabic female name. Mons AgnesGreek female name. Mons AmpereNamed for Andre Marie Mons; French physicist (1775-1836). Mons AndreMons ArdeshirMons ArgaeusNamed from peak in Asia Minor (now Erciyas Dagi). Argaeus Mountain is located on the southeastern border of [K/Mare Serenitatis]. Just to the southwest of this mountain, the border of the Sea of Serenity is flooded over by lava and runs into [K/Mare Tranquillitatis]. The base of Argaeus Mountain covers 50 km. The [K/Apollo 17] landing site is just to the northeast of this large mountain. Mons BradleyNamed for James Bradley; British astronomer (1692-1762). Mons DelisleNamed from nearby crater. Mons DieterMons DilipMons EsamArabic male name. Mons GanauMons GruithuisenNamed from nearby crater. Mons GruithuisenMons Gruithuisen Gamma - Named from nearby crater. Mons HadleyNamed for John Hadley; British instrument maker (1682-1743). Mons Hadley DeltMons Hadley Delta - Named from nearby mountain. Mons HansteenNamed from nearby crater. Mons HerodotusNamed from nearby crater. Mons HuygensNamed for Christian Huygens; Dutch astronomer, mathematician, physicist (1629-1695). Mons La HirePhilippe De La Hire; French mathematician, astronomer (1640-1718). Mons MaraldiNamed from nearby crater. Mons MoroNamed for Antonio Lazzaro Moro; Italian Earth scientist (1687-1764). Mons PenckNamed for Albrecht Penck; German geographer (1858-1945). Mons PicoSpanish for "peak". Pico Mountain is a lone mountain peak found in the northern part of [K/Mare Imbrium], just below the crater [K/Plato]. This mountain is 2.4 km high. Mons PitonNamed from Mt. Piton on Tenerife Islands. Mt. Piton is a lone mountain peak that juts out of [K/Mare Imbrium], just to the west of [K/Cassini] crater. The mountain is 2.3 km high and has a base of 25 km. Mons RumkerNamed for Karl Ludwig Christian Rumker; German astronomer (1788-1862). Mons UsovNamed for Mikhail A. Usov; Soviet geologist (1883-1933). Mons VinogradovNamed for Aleksandr Pavlovich Vinogradov; Soviet geochemist and cosmochemist (1895-1975); formerly called Mons Euler. Mons VitruviusNamed from nearby crater. Mons WolffChristian, Baron von; German philosopher (1679-1754). Mont BlancNamed for terrestrial mountain in Alps. MontanariNamed for Geminiano Montanari; Italian astronomer, mathematician (1633-1687). Mts. AgricolaNamed for Georgius Agricola; German Earth scientist (1494-1555). Mts. AlpesNamed from terrestrial Alps. These lunar ""Alps"" stretch from the crater [K/Plato] to the crater [K/Cassini], covering a distance of almost 280 km. This ragged, jumbled line of rocks also gives a rough northern border to [K/Mare Imbrium]. Mts. ApenninusNamed from terrestrial Apennines. The Apennine Mountains form the southern border of [K/Mare Imbrium]. The Apennines are the largest mountain range on the Moon, with heights of some of the mountains reaching over 5 km above the lunar surface. [K/Apollo 15] touched down on the north side of the mountains, towards the eastern edge of the range. Mts. ArchimedesNamed from nearby crater. The Archimedes Mountains appear as a small wrinkled region just south of the crater [K/Archimedes]. [K/Bancroft] crater is on the northwest border of the mountains. The mountain range covers almost 160 km. Mts. CarpatusNamed from terrestrial Carpathians. The Carpathian Mountains mark the southern border of [K/Mare Imbrium]. These mountains are the few remaining high ridges of Mare Imbrium's crater wall, ridges that weren't flooded by lava. The mountains stretch over 400 km in length. Mts. CaucasusNamed from terrestrial Caucasus Mountains. The Caucasus Mountains provide the northern boundary between [K/Mare Serenitatis] and [K/Mare Imbrium]. The mountains were probably a former crater rim that was flooded by lava long ago. Only the highest peaks remain visible. The mountains stretch almost 500 km across the lunar surface. Mts. CordilleraSpanish for "mountain chain". Mts. HaemusNamed for range in the Balkans. Mts. HarbingerHarbingers of dawn on crater Aristarchus. Mts. JuraNamed from terrestrial Jura Mountains. Mts. PyrenaneusNamed from terrestrial Pyrenees. Mts. RectiLatin for "straight range". Mts. RiphaeusNamed from range in Asia (now Ural Mountains). The Riphaeus Mountains are a small mountain range that stretches 189 km across the lunar surface and marks a portion of the eastern boundary of [K/Oceanus Procellarum] and the western boundary of [K/Mare Cognitum]. Mts. RookNamed for Lawrence Rook; British astronomer (1622-1666). Mts. SecchiNamed from nearby crater. Mts. SpitzbergenMts. Spitzbergen - German for "sharp peaks", and named for resemblance to the terrestrial island group. The Spitzbergen Mountains are a very small mountain range that poke up out of [K/Mare Imbrium], just north of the crater [K/Archimedes]. The mountains stretch for 60 km and are 1.5 km high. Mts. TaurusNamed from terrestrial Taurus Mts. Mts. TeneriffeNamed from terrestrial island. MontgolfierMooreMoretusNamed for Theodore Moret; Belgian mathematician (1602-1667). MorleyEdward Williams; American chemist (1838-1923). MorozovMorseMoseleyNamed for Henry G. J. Moseley; British physicist (1887-1915). MostingNamed for Johan Sigismund Von Mosting; Danish benefactor (1759-1843). MouchezNamed for Ernest Amedee Barthelemy Mouchez; French astronomer (1821-1892). MoultonMullerNamed for Karl Muller; Czechoslovakian astronomer (1866-1942). MurakamiMurchisonNamed for Sir Roderick Impey Murchison; Scottish geologist (1792-1871). MutusNamed for Vincente Mut, or Muth; Spanish astronomer (unkn-1673). NagaokaNansenNaonobuNamed for Ajima Naonobu; Japanese mathemetician c.1732-1798 NasireddinNamed for Nasir-Al-Din (Mohammed Ibn Hassan); Persian astronomer (1201-1274). NasmythNamed for James Nasmyth; Scottish engineer, astronomer (1808-1890). NassauNatashaRussian female name. NaumannNamed for Karl Friedrich Naumann; German geologist (1797-1873). NeanderNamed for Neumann, Michael Neander; German mathematician (1529-1581). NearchNamed for Nearch; Greek explorer (unkn-fl. 325 B.C.). NechoNeisonNamed for Edmund (Neville) Neison; British astronomer, selenographer (1849-1940). NeperNamed for John Neper; Scottish mathematician (1550-1617). NernstNamed for Walther H. Nernst; German physical chemist; Nobel laureate (1864-1941). NeujminNeumayerNamed for Georg Balthasar von Neumayer; German meteorologist, hydrographer (1826-1909). NewcombNamed for Simon Newcomb; Canadian-American astronomer (1835-1909). NewtonNamed for Isaac Newton; British mathematician, physicist, astronomer (1643-1727). NicholsonNamed for Seth B. Nicholson; American astronomer (1891-1963). NicolaiNamed for Friedrich Bernhard Gottfried Nicolai; German astronomer (1793-1846). NicolletNamed for Jean Nicholas Nicollet; French astronomer (1788-1843). NielsenNamed for Axel V. Nielsen; Danish astronomer (1902-1970) and Harald Herborg Nielsen; American physicist (1903-1973). NiepceNijlandNikolaevNishinaNobelNobileNamed for Umberto Nobile; Italian artic explorer (1885-1978). NobiliNamed for Leopoldo Nobili; Italian physicist (1784-1835). NoggerathNamed for Johann Jakob Noggerath; German geologist, mineralogist, seismologist (1788-1877). NoniusNamed for Pedro Nunez; Portuguese mathematician (1492(?)-1578). NormanNamed for Robert Norman; British natural scientist (unkn-fl. c. 1590). NotherNumerovNunnNamed for Joseph Nunn; American engineer (1905-1968). NuvslO'DayOberthObruchevOceanus Procella"Ocean of Storms". The Ocean of Storms is the largest mare (flooded plain) on the lunar surface, covering an area almost as large as Saudi Arabia. While it has a circular boundary for its western border, there really isn't much of a border to the east. This mare is approx. 2,568 km in diameter and covers an area of 2,102,000 sq km. The mare runs almost all the way to the northwestern limb. Within the dark terrain, just in from the northwestern edge, there is a rugged ""island,"" about 150 km wide and 250 km long. This ""island"" is bounded by Montes Agricola on the northwest, Rupes Toscanelli on the east and the craters [K/Herodotus] and [K/Aristarchus] on the south. This island also contains Vallis Schroteri, the largest sinuous valley on the Moon. Other than this ""island,"" there are a few wrinkles throughout the mare, but data from Apollo 15 revealed that this mare is very flat. During a full Moon, bright rays can be seen radiating across the mare from the crater [K/Kepler], located on the mare's eastern edge. OenopidesNamed for Oenopides Of Chios; Greek astronomer, geometrician (500(?)-430 B.C.). OerstedNamed for Hans Christian Oersted; Danish physicist, chemist (1777-1851). OhmOkenNamed for Lorenz (Okenfuss) Oken; German biologist, physiologist (1779-1851). OlbersNamed for Heinrich Wilhelm Malthaus Olbers; German astronomer, doctor (1758-1840). OlcottOlivierOmar KhayyamOnizukaOpeltNamed for Friedrich Wilhelm Opelt; German astronomer (1794-1863). OppenheimerOppolzerNamed for Theodor Egon von Oppolzer; Czechoslovakian astronomer (1841-1886). OresmeOrlovOrontiusNamed for Finnaeus (Oronce Fine) Orontius; French mathemetician, cartographer 1494-1555 OsamaJapanese male name OsirisNamed for Osiris Egyptian god of the dead OsmanTurkish male name. OstwaldPalisaNamed for Johann Palisa; Czechoslovakian-Austrian astronomer (1848-1925). PalitzschNamed for Johann Georg Palitzsch; German astronomer (1723-1788). PallasNamed for Peter Simon Pallas; German geologist, natural historian (1741-1811). Pallus is an medium-sized crater that is 46 km in diameter and 1.3 km deep. It has a rugged central peak. The eastern rim of Pallus overlaps the older, slightly larger crater Murchison. The southeastern rim of Murchison has been flooded out. PalmieriNamed for Luigi Palmieri; Italian physicist, mathematician (1807-1896). PanethNamed for Friedrich Adolf Paneth; German chemist (1887-1958). PannekoekPapaleksiParacelsusParaskevopoulosParenagoParkhurstParrotNamed for Johann Jacob F. W. Parrot; Russian doctor, physicist (1792-1840). ParryNamed for William Edward Parry; British explorer (1790-1855). ParsonsPascalNamed for Blaise Pascal; French mathematician (1623-1662). PaschenPasteurPatriciaEnglish female name. PatsaevPauliPavlovPawseyPearyNamed for Robert E. Peary; American explorer (1856-1920). PeasePeekNamed for Bertrand Meigh Peek; British astronomer (1891-1965). PeirceNamed for Benjamin Peirce; American mathematician, astronomer (1809-1880). PeiresciusNamed for Peiresc, Nicolas Claude Fabri De Peirescius; French astronomer, archaeologist (1580-1637). PentlandNamed for Joseph Barclay Pentland; Irish geographer (1797-1873). PerelmanPerepelkinPerkinPerrinePetaviusNamed for Denis Petau; French chronologist, astronomer (1583-1652). Petavius is the third in a chain of four old, large craters that form a north/south line along the southeastern limb of the Moon. This crater is 188 km in diameter and has a rugged central peak. Just outside the crater's northwest wall is the smaller, sharply defined crater [K/Wrottesley]. The other large craters in the chain are [K/Langrenus], [K/Vendelinus], and [K/Furnerius]. PetermannNamed for August Heinrich Petermann; German geographer (1822-1878). PetersNamed for Christian August Friedrich Peters; German astronomer (1806-1880). PetitNamed for Alexis Therese Petit; French physicist (1771-1820). PetriePetropavlovskiyPetrovNamed for Evgenij S. Petrov; Soviet rocketry scientist (1900-1942). PettitNamed for Edison Pettit; American astronomer (1889-1962). PetzvalPhillipsNamed for John Phillips; British geologist, astronomer (1800-1874). PhilolausNamed for Philolaus Of Croton; Greek mathematician, astronomer, philosopher (unkn-fl. 400 B.C.). PhocylidesNamed for Johannes Phocylides Holwarda (Jan Fokker); Dutch astronomer (1618-1651). PiazziNamed for Giuseppe Piazzi; Italian astronomer (1746-1826). Piazzi SmythNamed for Charles Piazzi Smyth; Scottish astronomer (1819-1900). PicardNamed for Jean Picard; French astronomer (1620-1682). PiccolominiNamed for Alessandro Piccolomini; Italian astronomer (1508-1578). PickeringNamed for Edward Charles Pickering; American astronomer (1846-1919) and Willaim H.Pickering; American astronomer (1858-1938). PictetMarc-Auguste Pictet-Turretin; Swiss physicist (1752-1825). PikelnerPilatreNamed for Rozier, F. De Pilatre; French aeronaut (1753-1785). PingreNamed for Alexandre Guy Pingre; French astronomer (1711-1796). PirquetPitatusNamed for Pietro Pitati; Italian astronomer, mathematician (unkn.-fl. c. 1500). PitiscusNamed for Bartholemaeus Pitiscus; German mathematician (1561-1613). PizzettiPlanaNamed for Baron Giovanni Antonio Amedeo Plana; Italian astronomer, geometrician (1781-1864). PlanckPlantePlaskettPlatoNamed for Plato Greek philosopher c.428-c.347 B.C. Plato is a crater 109 km in diameter. When viewing Plato along the terminator, the crater looks like a black bowl with a jagged lip - dots and dashes of sun and shadow. When viewed in full sunlight, Plato has a smooth dark floor with five very small craters lying within. Plato lies completely within a narrow band of mountains called [K/Mts. Alpes]. These mountains form the northern border of [K/Mare Imbrium]. Just south of Plato, within Mare Imbrium is a solitary mountain, [K/Mons Pico]. PlayfairNamed for John Playfair; Scottish mathematician, geologist (1748-1819). PliniusNamed for Gaius Plinius Secundus (The Elder); Roman natural scientist (23-79?). Plinius crater lies just to the south of the southeastern border of [K/Mare Serenitatis]. Plinius is 43 km in diameter and 2.3 km deep. It has a rugged central peak. Just north of the crater is a series of straight fissures called [K/Rimae Plinius]. PlummerPlutarchNamed for Plutarch Greek biographer c.A.D.46-c.120 PoczobuttPogsonPoincarePoinsotPoissonNamed for Simeon Denis Poisson; French mathematician (1781-1840). PolybiusNamed for Polybius Greek historian (204(?)-122(?) B.C.). PolzunovPomortsevNamed for Mikhail Mikhailovich Pomortsev; Russian rocketry scientist (1851-1916). PonceletNamed for Jean V. Poncelet; French mathematician, engineer (1788-1867). PonsNamed for Jean Louis Pons; French astronomer (1761-1831). PontanusNamed for Giovanni Gioviani Pontano; Italian astronomer (1427-1503). PontecoulantNamed for Comte De Pontecoulant Philippe Gustave Doulcet; French mathematician (1795-1874). PopovPorterNamed for Russell W. Porter; American telescope designer (1871-1949). PosidoniusNamed for Posidonius Of Apamea; Greek geographer (135(?)-51(?) B.C.). PoyntingPragerPrandtlPriestleyPrinzNamed for Wilhelm Prinz; German-Belgian astronomer (1857-1910). PriscillaLatin female name. ProclusNamed for Diadochos (The Successor) Proclus; Greek mathematician, astronomer, philosopher (410-485). ProctorNamed for Mary Proctor; American astronomer (1862-1957). ProtagorasNamed for Protagoras Greek philosopher (481(?)-411(?) B.C.). PtolemaeusNamed for Claudius Ptolemy; Greek astrononer, mathematician, geographer (c. A.D. 87-150). Ptolemaeus is a large crater, between 154-164 km in diameter and 2.4 km deep. The crater floor has no central peak, but does have gentle depressions scattered about, with one small crater Ammonius (9 km in size) just northeast of center. Ptolemaeus is the northern most and largest of three craters aligned from north to south. The crater [K/Alphonsus] lies just to the south, its northern rim butting up against Ptolemaeus. [K/Arzachel] crater lies just south of Alphonsus. PuiseuxNamed for Pierre Puiseux; French astronomer (1855-1928). PupinNamed for Michael Idvorsky Pupin; Yugoslavian-American physicist (1858-1935). PurbachNamed for Georg von Purbach; Austrian mathematician, astronomer (1423-1461). PurkynveNamed for Jan Evangelista Purkynve; Czechoslovakian doctor, physiologist (1787-1869). PythagorasNamed for Pythagoras Of Samos; Greek philosopher, mathematician (unkn-fl. c. 532 B.C.). PytheasNamed for Pytheas Of Marseilles; Greek navigator, geographer (b. c. 308 B.C.). QueteletRabbi LeviNamed for Levi Ben Gershon; Spanish-Jewish philosopher, mathematician, astronomer (1288-1344). RacahRaimondRamanNamed for Chandrasekhara V. Raman; Indian physicist; Nobel laureate (1888-1970). RamsayRamsdenNamed for Jesse Ramsden; British instrument maker (1735-1800). RankineNamed for William John M. Rankine; Scottish physicist, engineer (1820-1872). RaspletinRaviRayetRayleighNamed for John W. Strutt, Lord Rayleigh; British physicist; Nobel laureate (1842-1919). RazumovReaumurNamed for Rene Antoine Ferchault De Reaumur; French physicist (1683-1757). RechtRegiomontanusNamed for Johann Muller; German astronomer, mathematician (1436-1476). RegnaultNamed for Henri Victor Regnault; French chemist; physicist (1810-1878). ReichenbachNamed for Georg von Reichenbach; German optician (1772-1826). ReimarusNamed for Nicolai Reymers Baer; German mathemetician c. 1550-c.1600 ReinerNamed for Vincentio Reinieri; Italian astronomer, mathematician (unkn-1648). ReinholdNamed for Erasmus Reinhold; German astronomer, mathematician (1511-1553). RepsoldNamed for Johann Georg Repsold; German inventor (1770-1830). ResnikRespighiNamed for Lorenzo Respighi; Italian astronomer (1824-1890). RhaeticusNamed for Georg Joachim von Lauchen of Rhaetia; Hungarian astronomer, mathematician (1514-1576). RheitaNamed for Anton Maria Schyrle of Rhaetia; Czechoslovakian astronomer, optician (c. 1597-1660). RiccioliNamed for Giovanni Battista Riccioli; Italian astronomer (1598-1671). RicciusNamed for Matteo Ricci; Italian mathematician, geographer (1552-1610). RiccoRichardsRichardsonRiedelRiemannNamed for Georg F. B. Riemann; German mathematician (1826-1866). Rima AgatharchidNamed from nearby crater. Rima AgricolaNamed from nearby Montes. Rima ArchytasNamed from nearby crater. Rima AriadaeusNamed from nearby crater. Rima ArtsimovichNamed from nearby crater. Rima BillyNamed from nearby crater. Rima BirtNamed from nearby crater. Rima BradleyNamed from nearby Mons. Rima BrayleyNamed from nearby crater. Rima CalippusNamed from nearby crater. Rima CardanusNamed from nearby crater. Rima CarmenSpanish female name. Rima CauchyNamed from nearby crater. Rima CleomedesWithin crater. Rima CleopatraGreek female name. Rima CononNamed from nearby crater. Rima DawesNamed from nearby crater. Rima DelisleNamed from nearby crater. Rima DiophantusNamed from nearby crater. Rima DraperNamed from nearby crater. Rima EulerNamed from nearby crater. Rima FlammarionNamed from nearby crater. Rima FurneriusWithin crater. Rima G. BondNamed from nearby crater. Rima GalilaeiNamed from nearby crater. Rima GartnerWithin crater. Rima Gay-LussacNamed from nearby crater. Rima HadleyNamed from nearby Mons. Rima HansteenNamed from nearby crater. Rima HesiodusNamed from nearby crater. Rima HyginusNamed from nearby crater. Rima JansenNamed from nearby crater. Rima KriegerNamed from nearby crater. Rima MairanNamed from nearby crater. Rima MarcelloItalian male name. Rima MariusNamed from nearby crater. Rima MessierNamed from nearby crater. Rima MilichiusNamed from nearby crater. Rima OppolzerNamed from nearby crater. Rima ReaumurNamed from nearby crater. Rima ReikoJapanese male name. Rima RudolfGerman male name. Rima SchroterNamed from nearby crater. Rima SharpNamed from nearby crater. Rima SheepshanksNamed from nearby crater. Rima SiegfriedRima SuessNamed from nearby crater. Rima Sung-MeiNamed for Chinese female name Sung-Mei; part of [Lorca]. Rima T. MayerNamed from nearby crater. Rima VladimirSlavic male name. Rima Wan-YuChinese female name. Rima YangelNamed from nearby crater. Rima ZahiaArabic female name. Rimae AlphonsusWithin crater of same name. Rimae ApolloniusNamed from nearby crater. Rimae ArchimedesNamed from nearby crater. Rimae AristarchuNamed from nearby crater. Rimae ArzachelWithin crater. Rimae AtlasWithin crater. Rimae BodeNamed from nearby crater. Rimae BoscovichWithin crater. Rimae BurgNamed from nearby crater. Rimae ChacornacNamed from nearby crater. Rimae DaniellNamed from nearby crater. Rimae DarwinNamed from nearby crater. Rimae de GaspariRimae de Gasparis - Named from nearby crater. Rimae DoppelmayeRimae Doppelmayer - Named from nearby crater. Rimae FocasRimae FresnelNamed from nearby promontorium. Rimae GassendiWithin crater. Rimae GerardNamed from nearby crater. Rimae GocleniusNamed from nearby crater. Rimae GrimaldiNamed from nearby crater. Rimae GutenbergNamed from nearby crater. Rimae HerigoniusRimae Herigonius - Named from nearby crater. Rimae HeveliusNamed from nearby crater. Rimae HippalusNamed from nearby crater. Rimae HypatiaNamed from nearby crater. Rimae JanssenWithin crater. Rimae KopffNamed from nearby crater. Rimae LiebigNamed from nearby crater. Rimae LittrowNamed from nearby crater. Rimae MaclearNamed from nearby crater. Rimae MaestlinNamed from nearby crater. Rimae MaupertuisRimae Maupertuis - Named from nearby crater. Rimae MenelausNamed from nearby crater. Rimae MerseniusNamed for nearby crater. Rimae OpeltNamed from nearby crater. Rimae PalmieriNamed from nearby crater. Rimae ParryNamed from nearby crater. Rimae PetaviusWithin crater. Rimae PettitNamed from nearby crater. Rimae PitatusWithin crater. Rimae PlatoNamed from nearby crater. Rimae PliniusNamed from nearby crater. Rimae Plinius is a fissure that forms a straight, broken line 124 km long. The western edge of Rimae Plinius runs into the mountains that form the southern boundary of [K/Mare Serenitatis]. Rimae PosidoniusWithin crater. Rimae PrinzNamed from nearby crater. Rimae RamsdenNamed from nearby crater. Rimae RepsoldNamed from nearby crater. Rimae RiccioliNamed from nearby crater. Rimae RitterNamed from nearby crater. Ritter is a small crater, only 30 km in diameter, with an uneven floor. [K/Sabine] crater, almost exactly the same size, lies just to the southeast. The [K/Apollo 11] landing site lies off to the east. Rimae RomerNamed from nearby crater. Rimae SecchiNamed from nearby crater. Rimae SirsalisNamed from nearby crater. Rimae SosigenesNamed from nearby crater. Rimae Sulpicius Named from nearby crater. Rimae TaruntiusWithin crater. Rimae TheaetetusRimae Theaetetus - Named from nearby crater. Rimae TriesneckeRimae Triesnecker - Named from nearby crater. Rimae Vasco da GRimae Vasco da Gama - Named from nearby crater. Rimae ZupusNamed from nearby RitcheyNamed for George Willis Ritchey; American astronomer, optician (1864-1945). RittenhouseRitterNamed for Karl Ritter; German geographer (1779-1859); August Ritter; German astrophysicist (fl. 1890). RitzNamed for Walter Ritz; Swiss physicist (1878-1909). RobertEnglish male name. RobertsRobertsonRobinsonNamed for John Thomas Romney Robinson; Irish astronomer, physicist, meteorologist (1792-1882). RoccaNamed for Giovanni Antonio Rocca; Italian mathematician (1607-1656). RoccoItalian male name. RocheRomeoRomerNamed for Ole Romer; Danish astronomer (1644-1710). RontgenNamed for Wilhelm C. Rontgen; German physicist; Nobel laureate (1845-1923). RosaSpanish female name. RosenbergerNamed for Otto August Rosenberger; German astronomer, mathematician (1800-1890). RossNamed for James Clark Ross; British explorer (1800-1862); Frank E. Ross; American astronomer, optician (1874-1966). RosseNamed for William Parsons, Earl of Rosse; Irish astronomer (1800-1867). Rosse is a small crater, 11 km in diameter with a smooth floor and no central peak. There is a bright ray of light material that radiates from this crater to the northeast. Some believe this crater was formed by a chuck of debris flung up after the impact that created [K/Tycho] crater. RosselandRostNamed for Leonhard Rost; German astronomer (1688-1727). RothmannNamed for Christopher Rothmann; German astronomer (unkn-1600). RowlandRozhdestvenskiyRumfordRungeNamed for Carl David Tolme Runge; German mathematician (1856-1927). Rupes AltaiNamed from terrestrial Altai Mountains. Rupes BorisNamed from nearby crater. Rupes CauchyNamed from nearby crater. Rupes Cauchy is a large scarp, or ditch, that runs across the northeastern section of [K/Mare Tranquillitatis], from northwest to southeast. The southeastern edge of Rupes Cauchy runs into the mountainous eastern boundary of the mare. During sunrise along the terminator (waxing crescent phase), the scarp can be seen as a straight dark shadow. During sunset (waning gibbous phase), the scarp can be seen as a bright line. Rupes KelvinNamed from nearby promontorium. Rupes LiebigNamed from nearby crater. Rupes MercatorNamed from nearby crater. Rupes RectaLatin for "straighcliff" (The straight wall). Rupes Recta is also known as the "Straight Wall". This scarp is approx. 130 km long. It lies within [K/Mare Nubium], just west of the "diamond ring" crater [K/Thebit]. When viewed near the terminator, around a first quarter Moon, the scarp's sharp steep wall casts a shadow that can be seen as a dark straight line. When viewing Rupes Recta along the terminator during a third quarter Moon, the Sun is now shining directly on the steep wall, causing it to appear as a bright white line. Rupes ToscanelliRupes Toscanelli - Named from nearby crater. RussellNamed for Henry Norris Russell; American astronomer (1877-1957); John Russell; British artist, selenographer (1745-1806). RuthHebrew female name. RutherfordRutherfurdNamed for Lewis Morris Rutherfurd; American astronomer (1816-1892). RydbergRyninSabatierNamed for Paul Sabatier; French chemist; Nobel laureate (1854-1941). SabineNamed for Sir Edward Sabine; Irish physicist, astronomer (1788-1883). Sabine is a small crater, only 30 km in diameter. It lies right next to [K/Ritter] crater. Sabine is southeast of Ritter. The [K/Apollo 11] landing site lies off to the east. SacroboscoNamed for John of Holywood, Johannes Sacrobuschus; British astronomer, mathematician (c. 1200-1256). SaengerSafarikSahaSamirArabic male name. SampsonNamed for Ralph Allen Sampson; British astronomer, mathematician (1866-1939). SanfordSantbechNamed for Daniel Santbech Noviomagus; Dutch mathematician, astronomer (unkn-fl. 1561). Santos-DumontNamed for Alberto Santos-Dumont; Brazilian aeronautical engineer (1873-1932). SarabhaiNamed for Vikram Ambalal Sarabhai; Indian astrophysicist (1919-1971). SartonSasseridesNamed for Gellio Sasceride; Danish astronomer, doctor (1562-1612). SaunderNamed for Samuel Arthur Saunder; British mathematician, selenographer (1852-1912). SaussureNamed for Horace Benedict De Saussure; Swiss geologist (1740-1799). ScaligerSchaeberleScheeleNamed for Carl Wilhelm Scheele; Swedish chemist (1742-1786). ScheinerNamed for Christopher Scheiner; German astronomer (1575-1650). SchiaparelliNamed for Giovanni Virginio Schiaparelli; Italian astronomer (1835-1910). SchickardNamed for Wilhelm Schickard; German astronomer, mathematician (1592-1635). SchillerNamed for Julius Schiller; German astronomer (unkn-fl. 1627). SchjellerupSchlesingerSchliemannSchluterNamed for Heinrich Schluter; German astronomer (1815-1844). SchmidtNamed for Johann Friedrich Julius Schmidt; German astronomer (1825-1884); Bernhard Schmidt; German optician (1879-1935); Otto Y. Schmidt; Soviet astronomer (1891-1956). SchnellerSchombergerNamed for Georg Schomberger; Austrian astronomer, mathematician (1597-1645). SchonfeldSchorrNamed for Richard Schorr; German astronomer (1867-1951). SchrodingerSchroterNamed for Johann Hieronymus Schroter; German astronomer (1745-1816). SchubertNamed for Theodor Friedrich Von Schubert; Russian cartographer (1789-1865). SchumacherNamed for Heinrich Christian Schumacher; German astronomer (1780-1850). SchusterSchwabeNamed for Heinrich Schwabe; German astronomer (1789-1875). SchwarzschildScobeeScoresbyNamed for William Scoresby; British explorer (1789-1857). ScottNamed for Robert F. Scott; British explorer (1868-1912). SearesSecchiNamed for Pietro Angelo Secchi; Italian astronomer, astrophysicist (1818-1878). SechenovSeeligerNamed for Hugo von Seeliger; German astronomer (1849-1924). SegersSegnerNamed for Johann Andreas von Segner; German physicist, mathematician (1704-1777). SeidelSeleucusNamed for Seleucus; Babylonian astronomer (unkn-fl. c. 150 B.C.). SenecaNamed for Lucius Annaeus Seneca; Roman philosopher, natural scientist (4 B.C.- A.D. 65). SeyfertShackletonNamed for Sir Ernest Henry Shackleton; English antarctic explorer (1874-1922). ShahinazShalerNamed for Nathaniel S. Shaler; American geologist, paleontologist (1841-1906). ShapleyNamed for Harlow Shapley; American astronomer (1885-1972). SharonovSharpNamed for Abraham Sharp; British astronomer, mathematician (1651-1742). ShatalovShaynSheepshanksNamed for Anne Sheepshanks; British benefactor (1789-1876). SherringtonShi ShenShirakatsiShoemakerNamed for Eugene Merle Shoemaker; American astrogeologist (1928-1997). ShortNamed for James Short; Scottish mathematician, optician (1710-1768). ShternbergShuckburghNamed for Sir George Shuckburgh; British geographer, benefactor (1751-1804). ShuleykinNamed for M.V. Shuleykin; Soviet radio engineer (1884-1939). (Spelling changed from Shulejkin.) SiedentopfSierpinskiSikorskySilberschlagNamed for Johann Essaias Silberschlag; German astronomer (1721-1791). SimpeliusNamed for Hugh Sempill; Scottish mathematician (1596-1654). SinasNamed for Simon Sinas; Greek benefactor (1810-1876). Sinus Aestuum"Seething Bay". Sinus Amoris"Bay of Love". Sinus AsperitatiSinus Asperitatis - "Bay of Roughness". The Bay of Asperity looks as if it was an afterthought. When the lava filled up [K/Mare Tranquillitatis], it looks as if it spilled over its border and filled in some of the rough terrain to the south, forming this bay. The floor of this bay is rough with wrinkles and ridges. Two large craters, [K/Theophilus] and [K/Cyrillus], form the southern border of Sinus Asperitatis. [K/Apollo 16] lies to the west of the bay, in the middle of the heavily cratered highlands. Sinus ConcordiaeSinus Concordiae - "Bay of Harmony". Sinus Fidei"Bay of Trust". Sinus Honoris"Bay of Honor". Sinus Iridum"Bay of Rainbows". Sinus Lunicus"Lunik Bay"-landing area of Luna (Lunik) 2. Sinus Medii"Bay of the center". The Central Bay lies in the center of the near side of the Moon. It is a roughly circular shaped dark area that is about 350 km in diameter. The large, old crater [K/Ptolemaeus]lies to the south of Sinus Medii. Sinus Roris"Bay of Dew". Sinus Successus"Bay of Success". SirsalisNamed for Gerolamo Sersale; Italian astronomer (1584-1654). SisakyanSitaSklodowskaSlipherSlocumNamed for Frederick Slocum; American astronomer (1873-1944). SmithSmithsonNamed for James Smithson; British chemist, mineralogist (1765-1829). SmoluchowskiSnelliusNamed for Willebrod van Roijen Snell; Dutch mathematician, astronomer, optician (1591-1626). Snellius crater lies to the southwest of Wrottesley crater. It is very old with eroded walls and wrinkles and ridges along the floor. It is 82 km in diameter. SniadeckiSoddySomervilleNamed for Mary Fairfax Somerville; Scottish physicist, mathematician (1780-1872). SommerfeldSommeringNamed for Samuel Thomas Sommering; German doctor (1755-1830). SorayaPersian female name. SosigenesNamed for Sosigenes Greek astronomer, chronologist (unkn-fl. 46 B.C.). SouthNamed for James South; British astronomer (1785-1867). SpallanzaniNamed for Lazzaro Spallanzani; Italian natural scientist, biologist (1729-1799). Spencer JonesSporerNamed for Friederich Wilhelm Gustav Sporer; German astronomer (1822-1895). SpurrNamed for Josiah Edward Spurr; American geologist (1870-1950). St. JohnStadiusNamed for Jan Stade; Belgian astronomer, mathematician (1527-1579). StarkStearnsStebbinsStefanSteinSteinheilNamed for Karl August von Steinheil; German astronomer, physicist (1801-1870). SteklovStellaLatin female name. StenoSternfeldStetsonStevinusNamed for Simon Stevin; Belgian mathematician, physicist (1548-1620). Stevinus crater lies to the southwest of [K/Snellius] crater. It is 74 km in diameter and has a single central peak. StewartNamed for John Quincy Stewart; American astrophysicist (1894-1972). StiboriusNamed for Andreas Stoberl; German astronomer, mathematician (1465-1515). StoflerNamed for Johann Stofler; German astronomer, mathematician (1452-1531). StokesNamed for Sir George G. Stokes; British mathematician, physicist (1819-1903). StoletovStoneyStormerStraboNamed for Greek geographer (54 B.C.- A.D. 24). StrattonStreetNamed for Thomas Street; British astronomer (1621-1689). StromgrenStruveNamed for Otto von Struve; Russian astronomer (1819-1905); Otto Struve; American astronomer (1897-1963); Friedrich G. W. von Struve; German astronomer (1793-1864). SubbotinSuessNamed for Eduard Suess; Austrian geologist (1831-1914). SulpiciusNamed for Gaius Sulpicius; Roman astronomer (unkn-fl. c. B.C. 166). SumnerSundmanNamed for K. F. Sundman; Finnish astronomer (1873-1949). Sung-MeiChinese female name. SusanEnglish female name. SverdrupSwannSwaseyNamed for Ambrose Swasey; American inventor (1846-1937). SwiftNamed for Lewis Swift; American astronomer (1820-1913). SylvesterNamed for James J. Sylvester; British mathematician (1814-1897). SzilardT. MayerNamed for Tobias T. Mayer; German astronomer (1723-1762). TacchiniNamed for Pietro Tacchini; Italian astronomer (1838-1905). TacitusNamed for Cornelius Tacitus; Roman historian (c. 55-120). TacquetNamed for Andre Tacquet; Belgian mathematician (1612-1660). TaizoJapanese male name. TalbotNamed for William Henry Fox Talbot; British photographer, physicist, archaeologist (1800-1877). TammTannerusNamed for Adam Tanner; Austrian mathematician (1572-1632). TaruntiusNamed for Firmanus Taruntius, Lucius; Roman philosopher (unkn-fl. 86 B.C.). TaylorNamed for Brook Taylor; British mathematician (1685-1731). TebbuttNamed for John Tebbutt; Australian astronomer (1834-1916). TeisserencTempelNamed for Ernst Wilhelm Leberecht Tempel; German astronomer (1821-1889). Ten BruggencateTereshkovaTeslaThalesNamed for Thales Of Miletos; Greek mathematician, astronomer, philosopher (c. 636-546 B.C.). TheaetetusNamed for Theaetetus; Greek geometrician (unkn-c. 380 B.C.). Theaetetus crater is a small crater that lies just to the southeast of [K/Cassini] crater. It is 25 km in diameter and 2.8 km deep. Compare its size to the largest crater within [K/Cassini], which is 17 km in diameter. ThebitNamed for Ben Korra Thebit; Iraqi astronomer (826-901). The crater Thebit is the largest of three overlapping craters that form a "snowman" on the lunar surface. Thebit is 56 km in diameter with no central peak. Along the western rim of the crater lies a second, smaller crater. That crater has a third crater overlapping its western rim, representing the snowman's head! TheilerNamed for Max Theiler; South African bacteriologist; Nobel laureate (1899-1972). Theon JuniorNamed for Theon Junior Of Alexandria; Greek astronomer (unkn-c. 380). Theon SeniorNamed for Theon Senior Of Smyrna; Greek mathematician (unkn-c. 100). TheophilusNamed for Theophilus; Greek astronomer d. A.D. 412. Theophilus is a large crater, 110 km in diameter and 4,400 meters deep, which has a large central peak. The peak is 1.4 km high and covers a large portion of the crater floor. The crater walls are terraced. A small crater lies within the crater rim to the northwest. Theophilus lies on top of the rim of another crater, [K/Cyrillus]. TheophrastusNamed for Theophrastus; Greek botanist, natural historian (c. 372-287 B.C.). ThielThiessenThomsonTikhomirovTikhovTilingTimaeusNamed for Timaeus; Greek astronomer (unkn-c. 400 B.C.). TimiryazevTimocharisNamed for Timocharis; Greek astronomer (unkn-fl. c. 280 B.C.). TiseliusTisserandNamed for Francois Felix Tisserand; French astronomer (1845-1896). TitiusTitovTolanskyNamed for Samuel Tolansky; British physicist (1907-1973). TorricelliNamed for Evangelista Torricelli; Italian physicist (1608-1647). ToscanelliNamed for Paolo Dal Pozza Toscanelli; Italian doctor, cartographer (1397-1482). TownleyNamed for Sidney Dean Townley; American astronomer (1867-1946). TrallesNamed for Johann Georg Tralles; German physicist (1763-1822). TriesneckerNamed for Francis A. Paula Triesnecker; Austrian astronomer (1745-1817). TrouvelotNamed for Etienne Leopold Trouvelot; French astronomer (1827-1895). TrumplerTsanderTseraskiyTsingerTsiolkovskiyTsu Chung-ChiTuckerNamed for Richard Hawley Tucker; American astronomer (1859-1952). TurnerNamed for Herbert Hall Turner; British astronomer (1861-1930). TychoNamed for Tycho Brahe; Danish astronomer (1546-1601). Tycho crater is located in the heavily cratered highlands to the south. It is a large crater (100 km in diameter) with terraced walls and a large central peak. And, at 4.9 km deep, it is one of the deepest craters on the Moon. When viewing Tycho along the terminator, details of the crater walls and central peak can be seen. When the crater is fully illuminated, a vast ray system can be seen radiating away from Tycho. TyndallUkertNamed for Friedrich August Ukert; German historian, humanitarian (1780-1851). Ulugh BeighNamed for Ulugh-Beg; Mongolian astronomer, mathematician (1394--1449). UreyNamed for H. Urey; American chemist; Nobel laureate (1893-1981). VaisalaNamed for Yrjo Vaisala; Finnish astronomer (1891-1971). ValierVallis AlpesThis ""Alpine Valley"" makes a small, jagged slash across the lunar landscape. It is approx. 180 km long and lies just to the east of the crater [K/Plato]. Vallis BaadeNamed from nearby crater. Vallis BohrNamed from nearby crater. Vallis BouvardNamed for Alexis Bouvard; French astronomer, mathematician (1767-1843). Vallis CapellaNamed from nearby crater. Vallis InghiramiNamed from nearby crater. Vallis PalitzschNamed from nearby crater. Vallis PlanckVallis RheitaNamed from nearby crater. Vallis SchrodingVallis SchroteriSchroter's Valley. Vallis SnelliusNamed from nearby crater. van AlbadaNamed for Gale Bruno van Albada; Dutch astronomer (1912-1972). Van BiesbroeckNamed for George A. Van Biesbroeck; Belgian-American astronomer (1880-1974). Van de GraaffVan den Berghvan den BosVan der WaalsVan GentVan Maanenvan RhijnVan VleckNamed for John Monroe Van Vleck; American astronomer, mathematician (1833-1912). Van Wijkvant HoffVasco da GamaNamed for Vasco da Gama; Portuguese navigator, explorer (1469-1524). VashakidzeNamed for Mikhail A. Vashakidze; Soviet astronomer (1909-1956). VavilovVegaNamed for Georg Freiherr von Vega; German mathematician (1756-1802). VendelinusNamed for Godefroid Wendelin; Belgian astronomer (1580-1667). Vendelinus crater is the second of four old, large craters that form a crater chain. There are several small craters along the eastern side of Vendelinus, including a rather large crater that overlaps its northeast rim. Vendelinus is 131 km in diameter and has no central peak. Other craters in the chain are [K/Langrenus], [K/Petavius] and [K/Furnerius]. Vening MeineszVentrisVeraLatin female name. VernadskiyVerneLatin male name. VertregtVeryNamed for Frank Washington Very; American astronomer (1852-1927). VesaliusVestineNamed for Ernest H. Vestine; American physicist (1906-1968). VetchinkinVietaNamed for Francois Vieta; French mathematician (1540-1603). VilevVirchowNamed for Rudolph Ludwig Karl Virchow; German doctor, pathologist (1821-1902). VirtanenVitelloNamed for Erazmus Ciokek Witelo; Polish physicist, mathematician (1210-1285). VitruviusNamed for Marcus Vitruvius Pollio; Roman engineer, architect (unkn-fl. c. 25 B.C.). VivianiVlacqNamed for Adriaan Vlacq; Dutch mathematician (c. 1600-1667). VogelNamed for Hermann Karl Vogel; German astronomer (1841-1907). VolkovVoltaNamed for Count Allessandro G. A. A. Volta; Italian physicist (1745-1827). Volterravon BehringNamed for Emil Adolf von Behring; German bacteriologist; Nobel laureate (1854-1917). von Bekesyvon BraunNamed for Wernher von Braun, German-American rocket pioneer (1912-1977). Von der PahlenVon KarmanVon NeumannVon ZeipelVoskresenskiyNamed for Leonid A. Voskresenskiy; Soviet rocketry scientist (1913-1965). W. BondNamed for William Cranch Bond; American astronomer (1789-1859). WalkerWallaceNamed for Alfred Russel Wallace; British natural historian (1823-1913). This small flooded crater, 26 km in diameter, is unusual because it is not completely round. Its unusual shape is a result of lava flooding the crater to the point were only its uneven upper rim is visible. WallachNamed for Otto Wallach; German chemist; Nobel laureate (1847-1931). WalterGerman male name. WaltherNamed for Bernard Walther; German astronomer (1430-1504). (Spelling changed from Walter.) Wan-HooWargentinNamed for Pehr Vilhelm Wargentin; Swedish astronomer (1717-1783). WarnerNamed for Worcester Reed Warner; American inventor (1846-1929). WatermanWatsonWattNamed for James Watt; Scottish inventor (1736-1819). WattsNamed for Chester Burleigh Watts; American astronomer (1889-1971). WebbNamed for Thomas William Webb; British astronomer (1806-1885). WeberWegenerWeierstrassNamed for Karl Weierstrass; German mathematician (1815-1897). WeigelNamed for Erhard Weigel; German mathematician (1625-1699). WeinekNamed for Ladislaus Weinek; Czechoslovakian astronomer (1848-1913). WeissNamed for Edmund Weiss; German astronomer, mathematician, physicist (1837-1917). WernerNamed for Johann Werner; German mathematician (1468-1528). WexlerNamed for Harry Wexler; American meteorologist (1911-1962). WeylWhewellNamed for William Whewell; British philosopher (1794-1866). WhiteWichmannNamed for Moritz Ludwig Georg Wichmann; German astronomer (1821-1859). WidmannstattenNamed for Aloys B. Widmannstatten; German physicist (1753-1849). (Spelling changed from Widmanstatten.) WiechertWienerWildtNamed for Rupert Wildt; German-American astronomer (1905-1976). WilhelmNamed for Wilhelm IV, Landgrave of Hesse; German astronomer (1532-1592). WilkinsNamed for Hugh Percy Wilkins; British selenographer (1896-1960). WilliamsNamed for Arthur Stanley Williams; British astronomer (1861-1938). WilsingWilsonNamed for Alexander Wilson; Scottish astronomer (1714-1786), Charles T.R. Wilson; Scottish physicist (1869-1959) and Ralph E. Wilson; American astronomer ((1886-1960). WinklerWinlockWinthropNamed for John Winthrop; American astronomer (1714-1779). WohlerNamed for Friedrich Wohler; German chemist (1800-1882). WolfNamed for Maxmilian Franz Joseph Cornelius Wolf; German astronomer (1863-1932). WollastonNamed for William Hyde Wollaston; British chemist, physicist (1766-1828). WoltjerWoodWrightNamed for Frederick E. Wright; American astronomer (1878-1953); Thomas Wright; British philosopher (1711-1786); Willian H. Wright; American astronomer (1871-1959). WroblewskiWrottesleyNamed for Baron John Wrottesley; British astronomer (1798-1867). Wrottesley crater lies just to the northwest of the large, old crater [K/Petavius]. This crater is 57 km in diameter and has sharply defined crater walls. WurzelbauerNamed for Johann Philipp von Wurzelbauer; German astronomer (1651-1725). WyldXenophanesNamed for Of Colophon; Greek philosopher (570(?)-478(?) B.C.). XenophonYablochkovYakovkinNamed for A. A. Yakovkin; Soviet astronomer (1887-1974). YamamotoYangelNamed for Mikhail Kuzmich Yangel; Soviet rocketry scientist (1911-1971). YerkesNamed for Charles T. Yerkes; American benefactor (1837-1905). YoshiJapanese male name. YoungNamed for Thomas Young; British doctor, physicist (1773-1829). ZachNamed for Freiherr von Zach; Hungarian astronomer (1754-1832). ZagutNamed for Abraham Ben Samuel Zagut; Spanish-Jewish astronomer (unkn-c. 1450). ZahringerNamed for Josef Zahringer; German physicist (1929-1970). ZanstraZasyadkoNamed for Alexander Dmitrievich Zasyadko; Russian rocketry scientist, inventor (1779-1837). ZeemanZelinskiyZenoNamed for Zeno Of Citium; Greek philosopher (c. 335-263 B.C.). ZernikeZhiritskiyZhukovskiyZinnerNamed for Ernst Zinner; German astronomer (1886-1970). ZollnerNamed for Johann Karl Friedrich Zollner; German astrophysicist, astronomer (1834-1882). ZsigmondyZucchiusNamed for Zucchi, Niccolo Zucchius; Italian mathematician, astronomer (1586-1670). ZupusNamed for Giovanni Battista Zupi; Italian astronomer (c. 1590-1650). ZwickyQuadrantidsLyridsEta AquaridsDelta AquaridsPerseidsOrionidsTauridsLeonidsGeminidsUrsids5K Ult Wide 5K Spr Wide 5K Plossl 4K QX Wide 4K Ult Wide 4K Spr Wide 4K S Plossl 3K Plossl MA AndromedaAntliaApusAquariusAquilaAraAriesAurigaBootesCaelumCamelopardalisCancerCanes VenaticiCanis MajorCanis MinorCapricornusCarinaCassiopeiaCentaurusCepheusCetusChamaeleonCircinusColumbaComa BerenicesCorona AustralisCorona BorealisCorvusCraterCruxCygnusDelphinusDoradoDracoEquuleusEridanusFornaxGeminiGrusHerculesHorologiumHydraHydrusIndusLacertaLeoLeo MinorLepusLibraLupusLynxLyraMensaMicroscopiumMonocerosMuscaNormaOctansOphiuchusOrionPavoPegasusPerseusPhoenixPictorPiscesPiscus AustrinusPuppisPyxisReticulumSagittaSagittariusScorpiusSculptorScutumSerpensSextansTaurusTelescopiumTriangulumTriangulum AustraleTucanaUrsa MajorUrsa MinorVelaVirgoVolansVulpeculaJanFebMarAprMayJunJulAugSepOctNovDecSee your dealer.Language:Version Summer SolsticeWinter SolsticeVernal EquinoxAutumnal EquinoxNext Algol Min.Use UP/DOWNTonight's BestUploading...Max_At_GuideSaros_#_Set AlarmTotal EclipseAnnular EclipsePartial EclipsePenmmbral EclipsLunar EclipseSolar EclipseLunar FeaturesLunar N. PoleUmb. Mag:Pen. Mag:Umb. Dur:Pen. Dur:Gamma: Ctr LatCtr LonSun Alt:_Duration:No set todayNo rise todayWidth Set Slew SpeedkmPen. Tot. Par. Ann. Test CompletePress ENTERMODEGOTOGoto PresetSync. On PresetDefine PresetNSEW1234567890UPDOWN?SynchronizeGotoDefineBad KeyMotor StalledPress MODE or ?MS_ResetMS_ContrastMS_BacklashMS_PollashMS_PanelDifferent SitePolar AlignAltAz AlignGerman NorthGerman SouthIndex CatalogScope HomeDateTimeAt StartupAutorstar TutorHome PositionGetting StartedTelescope HelpTraining ErrorDeep Sky ObjectsIn Select MemberDelete Edit NameAsteroidComet Satellite Epoch YearEpoch DayRA Asc. NodeArg. of PerigeeMean MotionAOS Alt:_AOS Az:__LOS Alt:_LOS Az:__AOS in_Tracking Sat.Paused.ENTER to TrackExt. ObjRight Asc.DeclinationEpoch of El.EccentricityEcc. Semi Maj. AxisPerihelion Dist.InclinationIncl. Lon. Asc. NodeArg. of Per.Mean AnomalyAbsolute Mag.Mag. SlopePK Galactic Lon.:WARNINGEnter Rate Adj.Object Position:ExtraSol. PlanetBright StarsMeteor ShowersPeak onPeak Rate /hrDur. StatisticsBest view withMagnificationField of ViewField_=_Mag._=_KB FreeTo Load SoftwareTesting MotorsDownloading Do not turn off.Ctr. POLARISAge: Phase: miRises_Transit_Sets_Sun Rises AtSun TransitsSun Sets AtMoon Rises AtMoon TransitsMoon Sets AtNext Full MoonNext New MoonNext 1st QuarterNext 3rd QuarterCandidate Type: SunMercuryVenusMarsJupiterSaturnUranusNeptunePlutoMoonAlt Enc=_Az Enc =_FocusSetting DefaultCollimation...At LimitPositionPos. =PresetsPosition: 00SetReticle Control:IntensityRateDuty CycleLevel:5 Blink:0RA__=_Dec_=_Time_LST__Timer_Alarm Battery Level:Under ContructionPoint Scope NThen press EnterSet Alt. to 0Set Dec to 90Set RA to HomeCalculating...Sensor Cal.Use SensorsFinding NorthFinding SouthFinding LevelFinding HomeTaking GPS FixAuto AlignmentFind True NFind Mount TiltFind Mount TipConstellations:Named Object:Galaxy:NEBULA:PLANETARY NEBULA:CLUSTER:Messier Object:Invalid Number.Caldwell Object:Searching...Enter NGC #:Object Not FoundEnter IC #:Named Star:Multiple Star:Variable Star:Host Constell.Period: Min. Mag: Max. Mag: Var. Type: Nearby Star:Enter SAO #Enter HD #:Enter HR #:Enter HIP #:SAO:_Glossary:G/GlossaryA]G/Enter Date:Enter Time:Focal Len(mm):Enter Az RatioEnter Alt RatioAltAzScope mountingPolarAdjust MountRA PECDec. PEC Seg:Training RA PECTraining Dec PECUpdating RA PECUpdating Dec PECWaiting..Smart MountErasing...1=On, 2=OffReverse L/ROn OffNorth OnlySouth OnlyNorth & SouthYesNoReverse UP/DOWNAdj. with arrowsDisplay ContrastParking ScopeScope parkedTurn scope off.Land setup:Sky setup:Center referenceobject.Press  untilit is centered.Press ~ untilPress  untilPress  untilPress < untilPress > untilPress ^ untilPress v untilSelect Star:TargetRA_=_TargetDec_=_Center StarBelow HorizonPress ENTERCurrent Targets:TerrestrialAstronomicalErr: Can't del.Err: Not TrainedSmart Mnt. ErrorSmart Mount Err.the active siteDelete Site:IrvineEnter Lat:Enter Lon:Time Zone:Site Name:Error:Site List FullCountry/StateCities index Stateloc:G/State/ProvinceNearest CityG/Nearest CitiesYour First NameYour Last NameAdr. Line 1Adr. Line 2Your CityYour StatePostal/Zip CodeDate of BirthEnter PIN#Use Pin #?Select PIN#None FoundNot Found.Select LandmarkLandmarks FullLandmark NameCenter LandmarkDel. LandmarkH/Right AscensionH/AltitudeH/Local Mean TimeH/AccessoryH/BatteryH/Timer:Timer StatusAlarm TimeAlarm StatusAlign SuccessfulAlignment FailedCheck StarsClosest Object8 Inch F108 Inch F6.310 Inch F1010 Inch F6.312 Inch F1014 Inch F1016 Inch F107 Inch F154 Inch F9 APO5 Inch F9 APO6 Inch F9 APO7 Inch F9 APOLXG w/Custom OTA8 Inch F810 Inch F812 Inch F814 Inch F816 Inch F820 Inch F8LX MaxMountToo near the SunMS_TOURSLargest (mins)Smallest(mins)Brightest (mag)Brightest Faintest (mag)Object TypesNextPreviousMin. El.(deg.)Serial OverrunSerial #Enter Serial#000000P0000000CompleteSIG OCTMount not Az ElLoad DoneChecksum = 16Non 16In TestTesting RATesting DecTEST PASSEDDonePress mintuesAny key to end min. leftGoing HomeTest DoneEnter for nextRA PECDec PECRA & Dec PECHome SensorRA HomeDec HomeRA & Dec HomeGPSCheckSetting Circlesto 0Set Heater Pwr.Focuser SpeedFocuser Pos.Focus PresetsCollimateCalibrate FocusRestoring...Tracking..No Passes soonPass Located...Elements ExpiredMoon, NewMoon, Waxing CreMoon, FirstMoon, Waxing GibMoon, FullMoon, Waning GibMoon, ThirdMoon, Waning CreMessier Caldwell Abell Hicskon Radius Area sq.Avg. Mag. Enter Arp Hickson WDS Gliese UGC MCG NGC IC Black HoleDiffuse NebulaDark NebulaAsterismElliptical Gal.Globular ClusterIrregular Gal.Open ClusterPlanetary NebulaQuasarSpiral GalaxyGalaxyUnnamedCoordinates OnlyMagnitude: B-V Mag. V-R Mag. V Mag. Mag(Size:Count: Angle: Sep. Para.: masGL NN GJ WOSAO HIP #Class: Multi Sep. Dist:LY=TOO MANY LINKS=Link not found:Under ConstructionMag: Mass:xEarthxJup.Diam:Dist:auDay:Dayshrs Orb:yrsGrav:Day Temp:Nite Temp:Moons:Telescope Statuswith this modelIncompatibleHandboxLevel North Err.No Sensor BoardNo GPS DataNo Saved ModelsCan't Find HomePEC Not WorkingNo Dec PEC trainin Polar mountEllipticalS0SaSbScSBaSBbSBcIrregularDwarfDistrubedPecularCompactCraterMountain(s)MareOceanLakeSinusLanding SiteValleyRimaRupeAt Breakpoint: Stack Reg = In Debugger> ddress reakmask [esettack = atch eprom =- Invalid commandAlt=_Az_=_Not AlignedSlewing...Below HorizonCHECK_MOUNTBeyond LimitsFlash Memory ErrInitializing....ERROR:File Space Full.Reorganizing...ENTER to Sync.Synchronized.Sync not allowedon this object Smart DriveNorthSouthEastWestEnter PercentRate_=_Speed FastMediumSlowFineS. Fine/secUnit DoneSending DataProtect Bit SetFail Self TestTest DoneStarfinderComprob motoresERROR en baseERROR en brazoPrepare lapruebaPrueba de MotorBuscando RABuscando Dec Welcome toA U T O S T A RPress 0 to Alignor MODE for MenuRelevelingCenter BrightestStar, Push ENTERPress 0 for TourAUTOMATIC ALIGNSelecting StarLess than 5'from the polePole isSelect ItemObjectSolar SystemMercuryVenusMarsJupiterSaturnUranusNeptunePlutoMoonOverviewLunar 100Landing SitesCratersMountainsMare,Lakes...Valleys,Rills..AsteroidsSelectAddDeleteEditCometsSelectAddDeleteEditConstellationDeep SkyNamed ObjectsGalaxiesNebulasPlanetary Neb.Star ClustersQuasarsBlack HolesHickson ClustersPK CatalogIC ObjectsNGC ObjectsAbell ClustersArp GalaxiesUGCHerschel MCGCaldwell ObjectsMessier ObjectsCustom CatalogsStarNamedSAO CatalogHipparcos Cat.HD CatalogHR CatalogLandolt Stds.Gliese CatalogWash. Dbl. StarsMultipleGCVS(variables)NearbyWith PlanetsSatelliteSelectAddDeleteEditLandmarksSelectAddDeleteEditUser ObjectSelectAddDeleteEditIdentifyBrowseStart SearchEdit ParametersEventSunriseSun's TransitSunsetMoonriseMoon's TransitMoonsetMoon PhasesNext Full MoonNext New MoonNext 1st Qtr Next 3rd Qtr Meteor ShowersSolar EclipsesLunar EclipsesMin. of AlgolAutumn EquinoxVernal EquinoxWinter SolsticeSummer SolsticeGuided TourGlossaryUtilitiesAmbient Temp.Dew HeaterOTA FanBalance ScopeBalance R.A.Balance Dec.TimerSetStart/StopAlarmSetOn/OffEyepiece Calc.Field of ViewMagnificationSuggestBrightness Adj.Contrast Adj.Panel LightAux Port PowerBattery AlarmLandmark SurveySleep ScopeAlign on HomeCalibrate HomePark ScopePark PositionUse CurrentUse DefaultSetupAlignAutomaticEasyOne StarTwo StarDateTimeDaylight SavingsGPS-UTC OffsetTelescopeTelescope ModelCollimationSet DefaultCollimate ScopeRestore Default.Focal LengthAz RatioAlt RatioMountMax Slew RateMnt.Upper LimitMnt.Lower LimitCal. SensorsTracking RateGuiding RateDec. GuidingSiderealLunarCustomReverse L/RReverse UP/DOWNHome SensorsGPS AlignmentCalibrate MotorTrain DriveAz. TrainAlt. TrainRA/Az TrainDec/Alt TrainTargetsHigh PrecisionField DerotatorAnti-BacklashRA/Az PercentDec/Alt PercentSmart MountConfigurationRA PECDec PECRestore FactoryOn/OffUpdateTrainSave AsLoadSiteSelectAddDeleteEditNameLatitudeLongitudeTime ZoneObstructionsAddDeleteEditOwner Info.NameAddressStreetCityStateZip CodeCountryCloneCatalogsToursSoftwareAllDownloadStatisticsSun WarningBeepOTA TemperatureGetting StartedDisplay OptionsCord WrapBrightest StarResetAdjust MountWithout using the hand controller, adjust the mount's latitude setting and azimuth settings until the pole star is centered in the eyepiece. Once the pole star is centered, you should lock the mount in place and press ENTER. If you wish to abort polar alignment, press MODE. AlarmThe Alarm function beeps at a selected time, if active. In the Alarm menu, the Set function enters the alarm time. The On/Off function activates the alarm. The Alarm time is seen in the [H/Telescope Status] Display. After pressing MODE to leave this message, press ENTER to see the alarm menu and use the SCROLL keys to see the alarm choices. AlignFor the telescope to accurately locate objects in the night sky, it must be aligned. The telescope can align the telescope in one of three ways; Easy, One Star and Two Star. Easy align helps by selecting two alignment stars and explaining each step of the process. One Star and Two Star Align expect the user to pick the alignment stars. After pressing MODE to leave this message, press ENTER to see the alignment menu and use the SCROLL keys to see the three alignment choices. Align On HomeThis command is only for use on permenantly mounted telescopes. It assumes that sometime previously the Calibrate Home command was issued. The command causes the telescope to seek the home position. Once this position is located the telescope is aligned and ready for use. Alt RatioAlters the altitude encoder ratio. Do not use this function unless directed to do so by Meade Instructions. Press MODE to leave this message. AltAz AlignPut the telescope in the Alt. Az. home position. The Telescope tube should be level (declination scale to 0^). The Tube should be pointed true north and the telescope should be mounted on the tripod with the control panel on the south side of the tripod. Press ENTER when done. Altitude AxisThe axis responsible for moving the telescope up or down. Autumn EquinoxThe Autumn Equinox gives the local time and date for the beginning of Fall (in the Northern Hemisphere, Spring in the Southern Hemisphere). After pressing MODE to leave this message, press ENTER to see the date and time of Fall. AZ RatioAlters the azimuth encoder ratio. Do not use this function unless directed to do so by Meade Instructions. Press MODE to leave this message. Azimuth axisThe axis responsible for moving the telescope side to side. Press MODE to Return. Battery AlarmThe Battery Alarm function beeps when the batteries are low. In the Battery Alarm menu, use the SCROLL keys (followed by ENTER) to disable (or enable) the low battery alarm. The battery level is seen in the [H/Telescope Status] Display. After pressing MODE to leave this message, press ENTER to start the battery alarm menu. Brightness Adj.Adjusts the brightness of the message display and the keypad. After pressing MODE to leave this message, press ENTER to adjust the brightness. Calibrate FocusYou are about to recalibrate the front focusing system. NOTE:THIS WILL CHANGE YOUR COLLIMATION. After this operation is complete, you must collimate the focuser. Press MODE to abort this operation, or press ENTER to process with focuser calibration. Calibrate HomePerform this function ONLY on permanetly mounted and aligned telescopes. This function causes the telescope the seek the Home position. Once there, it remembers the position so that the scope can be aligned without star references using the "Align on Home" command. Calibrate MotorThis function calibrates the telescope motor encoders and saves the values in the telescope memory. During calibration both motors will move briefly. This function was done automatically when power was first applied to the telescope and does not need to be repeated unless the the telescope handbox is moved to a different telescope. After pressing MODE to leave this message, press ENTER to calibrate the motor encoders. Can't Find HomeThe telescope cannot not detect its Home position. There is probably a sensor problem. Should the problem persist, you will need to send you telescope in for service. You can continue by pressing MODE and perform on or two star alignment without the aid of sensors. CHECK MOUNTSlewing to this object may cause the telescope to hit the mount. Press the GO TO key to proceed. Press MODE to abort. Pressing any key during slewing will stop the telescope's movement. Press MODE to leave this message. CloneThe Clone function transfers data from one telescope to another by the serial interface using a special Meade cable. Data can include objects, software or both and is selected in the Clone menu. The unit sending is put in the Clone mode and the unit receiving is placed in the download mode. Once transfer of data has started, do not interrupt the process or telescope memory will be corrupted. After pressing MODE to leave this message, press ENTER to see the Clone menu and use the SCROLL keys to see the menu choices. ConstellationThe Constellation menu lists all 88 Constellations. Use the SCROLL keys to see the entries and press ENTER to select a Constellation. Information about the Constellation can be seen using the SCROLL keys. Pressing the GO TO key causes the telescope to point at the Constellation or list the stars of the constellation. If stars are listed use the SCROLL keys to see the entire list and press GO TO a second time to point at the stars. For objects to be found, the telescope must be aligned (see the Setup Menu). After pressing MODE to leave this message, press ENTER to see the Constellation menu and use the SCROLL keys to see the menu choices. Contrast Adj.Adjusts the contrast of the message display. In cold weather, this is used to make moving messages more readable. After pressing MODE to leave this message, press ENTER to adjust the contrast. Country/StateFind the nearest Country or State of the current telescope location by pressing the SCROLL keys at the bottom of the keypad. Press ENTER to select a displayed location. Press MODE briefly to abort the selection. Press MODE to leave this message. Ctr.The telescope has selected the brightest alignment star in the sky. Accuracy in performing prior steps determines how close the telescope is pointing at the correct star. Locate the brightest star near the current position of the telescope. Center the star in the telescope viewfinder by pressing the four ARROW keys as needed. Next, center the star in the main eyepiece and press ENTER. If the star selected is behind an obstacle, press a SCROLL key and the telescope will select another star. Press MODE to leave this message. DateAfter reading this instruction, enter today's date using the ARROW keys. When the month is highlighted, press the up or down ARROW keys to change the month. To change the year, use the right or left ARROW keys to select the year, then press the up or down ARROW keys to change year's digits. To make corrections to any entry, use the left or right ARROW keys to move the cursor to desired digit and up or down ARROW keys to change the digit. When the displayed date is correct, press ENTER. The utility Light on top of the handbox has been turned on to illuminate a watch. Press MODE to leave this message. Daylight SavingsIf Daylight Savings time is in effect (clocks are set ahead 1 hour, Spring to Fall), change the display to read "YES" by using the SCROLL keys. If the current time is Standard Time, change the display to read "NO". When the display is correct, press ENTER. Press the MODE key to leave this message. Deep SkyThe Deep Sky menu lists distant astronomical objects. Use the SCROLL keys to see catalogs, which include; Named Objects, Galaxies, Nebulas, Planetary Nebula, Star Clusters, Quasars, Black holes and other catalogs. After pressing MODE to leave this message, press ENTER to see the Deep Sky menu and use the SCROLL keys to see the menu choices. Different SiteAccording to the GPS, the telescope has been moved to a new site. After you press the ENTER key you will shown the site and time zone closest to your new location. Please edit or accept the proposed name proceeding. DownloadDownload causes the telescope to accept data from the serial interface. Data can include object data, software or both. Data can come from another telescope in the Clone mode or from a Personal Computer. A special Meade cable must connect the serial port to the other unit for transfer of data. Once transfer of data has started, do not interrupt the process or the telescope memory will be corrupted. After pressing MODE to leave this message, press ENTER to start the Download menu and use the SCROLL keys to see the menu choices. EasyEasy align is designed to help the novice quickly align the telescope. The telescope selects the best two alignment stars and moves the telescope nearby. After centering the stars, alignment is complete. After pressing MODE to leave this message, press ENTER to begin Easy align. Enter Date:Enter the current date by pressing the ARROW keys. To change between months, press the up or down ARROW keys. Use the left or right ARROW keys to move the cursor to any digit, then press the up or down ARROW keys to change the digit. Press ENTER when the displayed date is correct. The Light on top of the handbox has been turned on to illuminate a watch. Press MODE to leave this message. Enter Time:Enter the current local time by pressing the ARROW keys. Press the right or left ARROW keys to select the desired field or digit to be change, then press the up or down ARROW keys to change the field or the digit. Press ENTER when the displayed time is correct. The Light on top of the handbox has been turned on to illuminate a watch. Press MODE to leave this message. EventThe Event menu lists important astronomical events. After pressing MODE to leave this message, press ENTER to see the Event menu and use the SCROLL keys to see the menu choices. Eyepiece Calc.The eyepiece calculation menu gives eyepiece information, such as; [G/Field of View], Magnification and the best eyepiece for the object currently in view. After pressing MODE to leave this message, press ENTER to see the Eyepiece Calc. menu and use the SCROLL keys to see the menu choices. Focal LengthFocal Length changes the telescope focal length value in the telescope memory. After pressing MODE to leave this message, press ENTER to change the focal length value. German NorthPut the telescope in the polar Home position as described in the Instruction Manual. Use the keypad to set the declination to 90^. Adjust the RA axis so the telescope is directly over the top of the mount. Look through the eyepiece as you move the RA axis back and forth. The stars in the eyepiece will spin around the center of the eyepiece if you have the declination set to exactly 90 degrees. If the stars do not spin around the center of the eyepices, adjust the declination and try the RA axis again until you have the stars swirling around the center of the eyepiece. Now recenter the telescope over the top of the mount USING ONLY the RA control. Next adjust the telescope tripod (DO NOT USE THE KEYPAD) so that the tube is pointing north. Now set the scope's elevation so your latitude is shown by the pointer. If you do not know your latitude, get it from the Setup-Site menu. German SouthPut the telescope in the polar Home position as described in the Instruction Manual. Use the keypad to set the declination to 90^. Adjust the RA axis so the telescope is directly over the top of the mount. Look through the eyepiece as you move the RA axis back and forth. The stars in the eyepiece will spin around the center of the eyepiece if you have the declination set to exactly 90 degrees. If the stars do not spin around the center of the eyepices, adjust the declination and try the RA axis again until you have the stars swirling around the center of the eyepiece. Now recenter the telescope over the top of the mount USING ONLY the RA control. Next adjust the telescope tripod (DO NOT USE THE KEYPAD) so that the tube is pointing south. Now set the scope's elevation so your latitude is shown by the pointer. If you do not know your latitude, get it from the Setup-Site menu. Getting StartedFor a detailed description of the telescope system, press and hold the "?" key at the bottom of the keypad for two seconds then release it GlossaryThe Glossary has definitions of astronomy, telescope and space related terms in alphabetical order. Use the SCROLL keys to pick the beginning letter of a term, and press ENTER. Use the SCROLL keys again to select a term and press ENTER to see the definition. After pressing MODE to leave this message, press ENTER to see the Glossary menu and use the SCROLL keys to select a letter. GPS AlignmentWhen enabled, the telescope will read its location and the correct time using the integrated GPS receiver. When disable, reading of the GPS will be bypassed and the user prompted for the intial time and date. The scope will use the currently selected site a the initial telescope location. Guided TourGuided Tour lists the best astronomical objects for viewing tonight. Objects can be selected using the ENTER key. Pressing GO TO will also move the telescope to any selected object. After pressing MODE to leave this message, press ENTER to see the Guided Tour Menu and use the SCROLL keys to see the list of objects. High PrecisionPlaces the telescope in the High Precision mode to improve accuracy in locating dim objects. In High Precision mode, the telescope will go to a bright object near the target object. After centering the bright object and pressing ENTER, the telescope will then move to the target object. Use the SCROLL keys to select ON or OFF and press ENTER. After pressing MODE to leave this message, press ENTER to start the High Precision Menu and use the SCROLL keys (followed by ENTER) to enable or disable high precision operation. Home PositionPut the telescope in the home position and press the [H/ENTER key]. The home position for this telescope is described in the User's guide or in the Telescope Manual. This home position is required by the telescope to avoid positions that would interfere with telescope operation. This message will repeat until the [H/MODE Key] is pressed. IdentifyIdentify names the object seen in the telescope eyepiece by searching the catalogs. Use the SCROLL keys to see information about the object. For an object to be identified, the telescope must be aligned (see the Setup Menu). After pressing MODE to leave this message, press ENTER to identify the object in the eyepiece. LandmarksLandmarks defines and locates land objects. For landmarks to be added or located, the telescope must be aligned to an existing landmark. To align, use the Select option to chose an existing landmark, point the telescope at the landmark and hold ENTER for two seconds. Press ENTER again to "sync" and the telescope is landmark aligned. After alignment, another existing landmarks can be found using the Select option and pressing GO TO. Use the Add option to expand the list of landmarks. After pressing MODE to leave this message, press ENTER to see the Landmarks Menu and use the SCROLL keys to see the menu of options. Landmark SurveyLandmark Survey moves the telescope to all landmarks in turn, pausing at each one. Landmark Survey is stopped by pressing MODE. For landmarks to be found, the telescope must be landmark aligned. After pressing MODE to leave this message, press ENTER to start the Landmark Survey. Level North Err.Your telescope has experienced a fault in its level and north sensors. Pressing MODE will terminate this operation. You still and use standard one and two star alignments with the scope, but it should be sent in for factory service if the error condition persists. Lunar EclipsesLists eclipses of the Moon. Use the SCROLL keys to see the list by date, press ENTER to select a choice. Use the SCROLL keys to see information about the Eclipse. After pressing MODE to leave this message, press ENTER to see the list of eclipses and use the SCROLL keys to see a particular event. Menu HelpUse the SCROLL keys to see the other menu choices and press ENTER to make a selection. To return to the previous menu, press MODE briefly. If MODE is held for two seconds, the [H/Telescope Status] Display will appear. For a more detailed description of the telescope press ENTER now for [H/Telescope Help]. This message will repeat until MODE is pressed. Meteor ShowersLists Meteor Showers during the year. Use the SCROLL keys to see the events, press ENTER to chose one. Use the SCROLL keys to see information about the meteor shower. After pressing MODE to leave this message, press ENTER to see the list of meteor showers and use the SCROLL keys (followed by ENTER) to see a particular event. Min. of AlgolAlgol is a variable star that changes brightness every 2.8 days. The telescope gives the time of the next minimum brightness. After pressing MODE to leave this message, press ENTER to see the date and time of the next minimum brightness of Algol. Moon PhasesLists the date and time of the next four phases of the Moon. Use the SCROLL keys to select one of the four phases and press ENTER to see the next event. After pressing MODE to leave this message, press ENTER to see the moon phase options and use the SCROLL keys (followed by ENTER) to see a particular event. MoonriseGives the local time of the next Moonrise. After pressing MODE to leave this message, press ENTER to see the moonrise time. MoonsetGives the local time of the next Moonset. After pressing MODE to leave this message, press ENTER to see the Moonset time. Motor StalledThe telescope has detected a motor failure. Moving the handbox between scopes, low battery levels, obstructed or overloaded scopes can cause this failure. If the telescope was stalled, remove the obstruction or overload. After leaving this message, the telescope will recalibrate the motors. The telescope will NEED TO BE REALIGNED before you can resume viewing. Should you continue to get this message with fresh batteries, contact Meade customer support. Press MODE to leave this message. MountSelects the AltAz or Polar telescope configuration. Most telescope are AltAz, the only Polar configuration is with the telescope mounted on a equatorial wedge. After pressing MODE to leave this message, press ENTER to see the Mount menu and use the SCROLL keys to see the options. MS BacklashFor this operation use a terrestrial object. After each step, when the object is centered, press ENTER. Press ENTER now to proceed. MS ContrastUse the scroll up and down keys to adjust the display contrast. Press ENTER when finished. MS PanelThe telescope control panel needs to oriented so that it is on the south side of the tripod. This is the side opposite where the scope is currently pointed. Please reorient the scope as directed and press ENTER to restart the alignment procedure. MS PollashFor this operation use a star near the celestial equator. After each step, when the object is centered, press ENTER. Press ENTER now to proceed. MS ResetThis command will clear all the information entered into the telescope and reset to factory defaults. Press ENTER to proceed, or MODE to abort. Nearest CityFind the nearest City to the current telescope location by pressing the SCROLL keys at the bottom of the keypad. Press ENTER to select a displayed city. Press MODE to leave this message. No GPS DataThe telescope is not receiving any data from the internal GPS. If the problem persists, the scope will need to be returned to the factory for service. You may proceed by manually entering the date and time. Press MODE to continue. No Sensor BoardThe telescope cannot communicate with its auxiarlly sensor board. If the problem persists, it needs to be sent back for factory service. You can still use your scope by performing One star or Two star alginment. Press MODE to abort this operation. ObjectThe Object menu contains catalogs of astronomical, terrestrial and user defined objects. After pressing MODE to leave this message, press ENTER to see the Object menu and use the SCROLL keys to see the list of catalogs. One StarOne Star align is designed for fast alignment of the telescope. The user must select a known star and move the telescope to it manually. This alignment is not as accurate as Easy or Two star alignment. After pressing MODE to leave this message, press ENTER to begin One Star align. Owner Info.Owner Information stores the owners name and address. Use the SCROLL and ENTER keys to select the name or address option. Use the ARROW keys to move the cursor (right or left). Numbers and letters are entered using the up or down ARROW keys. Press ENTER when an entry is complete and correct. After pressing MODE to leave this message, press ENTER to see the Owner Info. menu and use the SCROLL keys to see the options. Park ScopePark Scope moves the telescope to the home position and beeps. At the Home position, turn off the power. The next time power is turned on, if the telescope is not moved and time is entered accurately, no alignment will be necessary. After pressing MODE to leave this message, press ENTER to park the telescope. PEC Not WorkingThe scope's PEC sensors are not responding. You can continue to operated the scope with PEC disabled, but if the problem persists, it will need to be sent in for service. Press MODE to continue. PH Tour ObjectsThe Tour object list is seen using the SCROLL keys. Press ENTER to select an object. Information about a selected object is seen using the SCROLL keys. Pressing the GO TO key will cause the telescope to point at the object. For objects to be found, the telescope must be aligned (see the Setup Menu). Press MODE to leave this message. Point Scope NPoint the front of the telescope in the direction of true North and press the [H/ENTER key]. It is not required that the telescope to be pointed precisely North, pointing it generally North is sufficient. Later in the alignment process, the telescope will select stars to be used for precision alignment. The closer the telescope is pointed at true North the easier it will be to identify the alignment stars. For suggestions on ways to find true North, refer to your User's Guide. This message will repeat until the [H/MODE Key] is pressed. Polar AlignPut the telescope in the polar Home position as described in the Instruction Manual. Use the keypad to set the declination to 90^. True 90 is found when the scope is slewed rapidly in RA and the stars appear to rotate around the center of the field of view. If the stars do not spin around the center, slew with the dec. buttons until the center is found. Adjust the telescope RA axis to HA. 0 (see manual). Next adjust the telescope tripod (do not use the keypad) so that the tube is pointing at the celestial pole. Press ENTER when done. ResetReset returns the telescope to factory defaults and erases all user memory. After pressing MODE to leave this message, press ENTER to reset the telescope. Reverse L/RReverses the action of the left and right ARROW keys. Use the SCROLL keys to select ON (reversed) or OFF (normal) option and press ENTER. After pressing MODE to leave this message, press ENTER to see the Reverse L/R menu and use the SCROLL keys to see the options. Reverse UP/DOWNReverses the action of the UP and DOWN ARROW keys. Use the SCROLL keys to select ON (reversed) or OFF (normal) option and press ENTER. After pressing MODE to leave this message, press ENTER to see the Reverse UP/DOWN menu and use the SCROLL keys to see the options. SatelliteThe Satellite menu is used to locate man-made objects orbiting Earth. Four options (Select, Add, Delete and Edit) are chosen using the SCROLL keys and pressing ENTER. To locate and track a satellite, use the Select function. The other functions modify the existing Satellite table. Satellite orbits vary greatly and need to be frequently corrected. For objects to be found, the telescope must be aligned (see the Setup Menu). After pressing MODE to leave this message, press ENTER to see the Satellite menu and use the SCROLL keys to see the options. Scope HomePut your telescope in the home position and press the [H/ENTER key]. The home position for your telescope is described in the User's guide or in your Telescope Manual. This home position is required by the telescope to avoid positions that would interfere with telescope operation. This [H/Help Menu] will repeat until you press the [H/MODE Key]. Set Alt. To 0Set the [H/Altitude axis] of the telescope to 0 and press the [H/ENTER key]. Put simply, move the telescope tube up or down until it is level. When level, press the [H/ENTER key]. This message will repeat until the [H/MODE Key] is pressed. SetupThe Setup menu is used for the telescope settings required for the operation and alignment of the telescope. After pressing MODE to leave this message, press ENTER to see the Setup menu and use the SCROLL keys to see the options. SiteSite defines the observing location of the telescope. Up to six sites can be saved in the telescope memory. Site options include; Select, Add, Delete and Edit. The Select option determines the current observing site. Add, Delete and Edit options are used to change the Site tables. After pressing MODE to leave this message, press ENTER to see the Site menu and use the SCROLL keys to see the options. Sleep ScopeSleep powers down the telescope to conserve batteries and maintains alignment. Press any handbox key to resume operation. After pressing MODE to leave this message, press ENTER to put the telescope in the low power mode. Smart Mnt. ErrorSmart Mount requires equatorially mounted telescopes to be One Star aligned to operate correctly. Please select and perform a One Star alignment before enabling smart mount. Press ENTER to continue Smart Mount Err.Star position is out of limits. Please check you are attempting to Sync on the correct star. Smart training/updating has been discontinued due to the excessive pointing error. Please check alignment and star before resuming training. Press ENTER to continue. Solar EclipsesLists eclipses of the Sun. Use the SCROLL keys to see the list by date, press ENTER to select a choice. Use the SCROLL keys to see information about the Eclipse. After pressing MODE to leave this message, press ENTER to see the list of eclipses and use the SCROLL keys to see a particular event. Solar SystemThe Solar System menu contains objects in our Solar System, including; eight Planets, the Moon, Asteroids and Comets. For objects to be found, the telescope must be aligned (see the Setup Menu). After pressing MODE to leave this message, press ENTER to see the Solar System menu and use the SCROLL keys to see the object choices. StarThe Star menu contains stars sorted by category. The categories include; named stars, SAO Catalog, Double stars, Variable stars, Nearby stars and stars with Planets. For objects to be found, the telescope must be aligned (see the Setup Menu). After pressing MODE to leave this message, press ENTER to see the Star menu and use the SCROLL keys to see the object categories. StatisticsThe Statistics menu shows the amount of available user memory and the telescope software revision number. After pressing MODE to leave this message, press ENTER to see the Statistic menu and use the SCROLL keys to see the information. Summer SolsticeThe Summer Solstice gives the local time and date for the beginning of Summer (in the Northern Hemisphere, Winter in the Southern Hemisphere). After pressing MODE to leave this message, press ENTER to see the date and time of Summer. SunriseGives the local time of the next sunrise. After pressing MODE to leave this message, press ENTER to see the sunrise time. SunsetGives the local time of the next sunset. After pressing MODE to leave this message, press ENTER to see the sunset time. TargetsThe Targets menu puts the telescope into the terrestrial or astronomical mode of operation. In astronomical mode the telescope tracks the moving sky. Use the SCROLL keys to see the options and press ENTER to make a selection. After pressing MODE to leave this message, press ENTER to see the Target menu and use the SCROLL keys to see the options. Telescope HelpThis description can be discontinued at any time by pressing the MODE key. If the message is moving too fast or slow, press one of the SCROLL keys (triangle keys at the bottom of the keypad). The telescope is a menu oriented system with lists of functions. Functions are activated using the 10 keys of the handbox keypad. Pressing any key firmly and releasing causes a single entry of that key. Holding a key down causes a repeated entry until it is released. The top line of this display shows the currently active function (in this case, Telescope Help). The bottom line shows information or a new menu list. When the bottom line is a list, pressing the SCROLL keys makes items in the list visible (one at a time). To activate a function shown on the bottom line, press the ENTER key. The active function will then be displayed on the top line and new information will appear on the bottom line. The ENTER key is also used to complete data entries. To return to a previous menu, press the MODE key. The MODE key, if held down 2 seconds, will cause the Telescope Status display to appear. The Telescope Status display has information about telescope position, motor speeds, timer, alarm and other telescope status. The GO TO key moves the telescope to objects from the OBJECT menu. The four ARROW keys (near the top of the keypad) move the telescope in four directions at selected speeds. When entering data, the right and left ARROW keys are used to move the cursor to a particular field and up and down ARROW keys scroll through selections, like months in a date. The "Speed-?" key sets telescope motor speeds. To set a motor speed, press the "Speed-?" key to step up through the fixed speed values. The utility light (on top of the handbox) is used to illuminate objects (like a watch). The "0" key turns the light on or off. The SCROLL keys (at the bottom) move through menus and adjust moving message speeds. Pressing and holding the "Speed-?" key for two seconds and then releasing it is used for HELP, and give a brief explanation of the current function. In some messages, there may be bracketed words, called "hypertext". Pressing the ENTER key while a hypertext term is visible, will display information about that term. Pressing the MODE key will return to the original message. The brightness and contrast of this display can be changed using the Brightness or Contrast functions in the Utilities menu. The telescope system description is now complete and information must be entered to operate the telescope. To make these entries without further explanation, press the MODE key. Remember, the "Speed-?" key can be pressed and held for two seconds and then released to explain a particular operation at anytime. For additional assistance entering release it. This message will repeat until the MODE key or the "Speed-?" Key is pressed. Telescope ModelSelect the Telescope model by pressing the SCROLL keys. The telescope model can be found in the Telescope Instruction Manual or on the foil label attached to the telescope tube. Press ENTER when the display is correct. Press MODE to leave this message. Telescope StatusThe Telescope Status Display shows the values useful in operating the telescope and accessories. To enter this display, hold the MODE key for more than 2 seconds and release. Use the SCROLL keys to see values such as; telescope position, time, alarm, timer, battery level and accessory status. The motor slew speed is shown in the upper right corner of the display as a bar graph. While the telescope position is displayed, pressing GO TO, will cause the telescope to request new position values and slew to that location when ENTER is pressed. To return to the previous menu press MODE briefly. TimeThe Time function is used to change local time in the telescope. After pressing MODE to leave this message, press ENTER to change the telescope time. TimerThe Timer beeps after a time period is complete. Use the "Set" option to select a Timer value up to 24 hours. Use the Start/Stop option to begin timer operation. The timer value is in the [H/Telescope Status] Display. After pressing MODE to leave this message, press ENTER to see the Timer menu and use the SCROLL keys to see the options. Tracking RateTracking Rate adjusts rate the telescope uses to follow objects in the sky. There are three rate choices; Sidereal, Lunar or Custom. After pressing MODE to leave this message, press ENTER to see the Tracking Rate menu and use the SCROLL keys to see the options. Train DriveTrain Drive calibrates the telescope motors to improve pointing accuracy. Carefully train each axis. After pressing MODE to leave this message, press ENTER to see the Train Drive menu and use the SCROLL keys (followed by ENTER) to select an axis to train. Training ErrorA retrograde motion of the drive occured during training. Please pick a star in a different part of the sky for training. For azimuth training, pick a star on the opposite side of the sky from the pole. For altitude training, pick a star halfway above the horizon in the east or west. Press ENTER to continue. Two StarTwo Star alignment requires an advanced user (familiar with the sky) to select two stars and manually move the telescope to both during the alignment operation. After pressing MODE to leave this message, press ENTER to begin Two Star align. User ObjectUser Object defines and locates new astronomical objects. Four options (Select, Add, Delete, Edit) are chosen using the SCROLL keys and pressing ENTER. To create and modify the object table, use Add, Delete or Edit. To locate an object use the Select option. For objects to be found, the telescope must be aligned (see the Setup Menu). After pressing MODE to leave this message, press ENTER to see the User Object menu and use the SCROLL keys to see the options. UtilitiesThe Utilities menu has nine options to help operate the telescope. After pressing MODE to leave this message, press ENTER to see the Utilities menu and use the SCROLL keys to see the options. Vernal EquinoxThe Vernal Equinox gives the local time and date for the beginning of Spring (in the Northern Hemisphere, Fall in the Southern Hemisphere). After pressing MODE to leave this message, press ENTER to see the date and time of Spring. WARNINGLOOKING AT OR NEAR THE SUN WILL CAUSE IRREVERSIBLE DAMAGE TO YOUR EYE. DO NOT POINT THIS TELESCOPE AT OR NEAR THE SUN. DO NOT LOOK THROUGH THE TELESCOPE AS IT IS MOVING. TO INDICATE YOU HAVE READ AND UNDERSTOOD THIS MESSAGE, PRESS THE "5" KEY. Winter SolsticeThe Winter Solstice gives the local time and date for the beginning of Winter (in the Northern Hemisphere, Summer in the Southern Hemisphere). After pressing MODE to leave this message, press ENTER to see the date and time of Winter. 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unRRAB H  u2nRRAB H Ww2RRC H w6M H zDCʴZRRAB H ?DSRB H @EVFM: H AFĦ;SRA H BISRB H CORRAB H DNSRA H EP pdRRAB H FP yRRAB H GP/KNM H HQ ߹ZSRB H IU(Ի0M H JW!8M: H KY[PI H L[vnLB H M^SRA H N^ BSRA H Oa,M H PkgZRRAB H Ql1M H Rm< FI H Sr dRRAB H Tu?M H Uv 2RRC H V{9 TM H WA|zPSRA H XLSRA H Y_M H ZnSRA H [ # SRA H \RRAB H ]:~FSR H lr PxI H monRRAB H nS@nSRA H o`$N: H p,ZAND H qÈgM H ret,M H s-e~M H tоRRAB H nRRAB H ;RRAB H  |RRAB H  qSRA H !PM H " dM H $;0xRRAB H %aCEP H 'uM H '`ɦSRA H )@dM: H *N6xRRAB H *qTM H *ZRRAB H +/:M H -.xRRAB H -d\RRAB H .n~M H .ȎM H .,SRA H /:ZEA H 0H&RRAB H 0gxRRAB H 0*M H 1(ZRRAB H 1tW2xRRAB H 1)L1M H 2JDPRRAB H 2JDxRRAB H 3H<ZRRAB H 3xRRAB H 4qRRAB H 6#SRA H 8^5xANA H 81SRA H 9lGRRAB H 9uPEA/SDH 9`SRA H :RRAB H :>jSRA H ;yJxRRAB H ; RRAB H ;7fRRAB H <FxRRAB H IRRAB H ?JZM: H @VM H A(fRRAB H AؒDM H CqxRV H E?xRRAB H EQdM H F<߿FRRC H !I/1RRAB H "IURRAB H #J=TDI H $JjB^E/SD H %KSRA H ?RRAB H @RRAB H AixE H B RRAB H C*9TM H D*8JM H EuSRA H Fu,ZRRC H GuRRAB H H RRAB H IxRRAB H J3,M H KRRAB H L8RRAB H MHRRAB H NG,M H ORRAB H PZSRB H QGF ZRRAB H Rt;lPSRB H S4PnRRAB H T#4%M H U6RRAB H V SRA H WISR H X )UV: H Y(^M H Z 8SR H [7-4xRRAB H \U+"$@M H ]7=trM H ^!SRB H _sAHSRA H `5RRAB H a (RRAB H bCRRAB H cnM H txRRAB H u&|RRAB H v@SR H wZRRAB H x:RRAB H @RRAB H )~PSR H $ZSRB H 3"M H $6"M H ~"dSRB H SRB H PZSRB H Q3Y@CEP: H Q3RRAB H `+|RRAB H #SR H ,NTM H *RRAB H NxCEP H M+nRRAB H z-pM H z52L H %SRB H -fxRR H ,DdRRAB H .6M H  xRR H .nRRAB H KxSR H xRRAB H L(4M H .E,M H /TM H !dRRAB H (RR H %Z-6M H  M H .$nRR H xRRAB H )M H h@02RRAB H h=M H w74RRAB H hMZSR H  nSR H VPSR H bRRAB H 8`RSRA H InM H >M H IRRAB H ! xRRAB H "/RRAB H #@vM H $ ZRRAB H % E: H &8BRRAB H 'FRRAB H (GHnSR H )GRRAB H *FnSRB: H +)'RRAB H ,IPSRA H -)@XRRAB H .)>xRRAB H /84PM H 0eCEP H 1G?xRRAB H 2e34@M H 3 SR H 4SRA H 5GJ0RRAB H 6eZhM H >UnRRAB H ?d*RR H @FDRRAB H A0E/SD:H B&RRAB H C2PSRB H D:@nSR H ERR H FCM H GDTFSR H H$.RRAB H ITPRRAB H Jr &RRAB H K F>dL: H L@X8hM H M VSRA H N dSRB: H OT=VRRAB H P$VnRRAB H Qr=dRRAB H R-E H S 2dRRAB H T1DRR H U%E H VH(SRA H W7RRAB H X0>SRA H YsZAND H Z6SRA H [&F\hM H \)|M H ]M H ^RRAB H _bLRRAB H `"NhM H  O56I: H  RRAB H  )ZRRAB H  %M H  R2DSCT H  xSRA H  .FSRB H  "0RRAB H  4SRA H  NPRRC H  BnRRAB H xM H  9HM H  /ZPRRAB H  ]0RRAB H  ?-TM H  0MSRA H  {*2RRC H  "nRRAB H  SRB: H  ]DZRRAB H  ]ERRAB H  tE H  RRAB H  ~xRRAB H  lKRRAB H  {ERRAB H  <RRAB H  ,SRB: H  *L: H  AnRRAB H  B.ZSR H  42L H  .~nRRAB H  *RRAB H  RRAB H  ;dRRAB H  MhM H =RRAB H dRRAB H u5SR H RRAB H "RRAB H  $SRA H  $RR H ezRRAB H )FZRRAB H ndSRB: H  d2RRAB H VL.SR H 3%SRA H RRAB H  SRA H 9nL H !RRAB H "$hM H #<4>M H $(2M H %ApnRRAB H &GRRAB H 'F!,M H (RPRRAB H )UZRRAB H *UNL H +G$FRRAB H ,s9dFRR: H -.&M H .s?SR H / (L H 0?SRA H 1RRAB H 2 hM H 33SRA H 4'nRRAB H 54FL H 6-PSRB H 7ZUV: H 8T@xSR: H 9rSR H :pnRRAB H ?wE/SD H @1"M H AtdL H BDRRAB H CIRRAB H D xRRAB H E&dRRAB H FDXSRA H Gb*nnRRAB H H.dSRB H ISKdRR H J'ZRRAB H KqCdFE H LdSRA H MRRAB H N8RRAB H O<RRAB H P dnRRAB H QR9RRAB H RR@:M H S?dRR: H T RR H U-*RR H V( JM H W6:xRRAB H X$(E H YESRA H Z9 RRAB H [3SR H \<RRAB H ]>RRAB H ^o)$RR H _2xE: H `ZRRAB H aF\RRAB H b(4RRAB H c#R@E/SD H dPrnRR H e#HRRAB H fA?ZRRAB H g_- rM H h3@M H i8$rM H jCnRRAB H k4"M H l@!RRAB H mNZSR H nOVRRAB H o^dRRAB H p^9RR H q#ZRRC H rnRRAB H sm@RRAB H t|=BdRRAB H u12SRB: H v)VM H w00RRAB H xN':RRAB H y0@vdRRAB H z bSRA H {LRRAB H | JSRB: H }]GRRAB H ~r M H 6NZE: H HRR H HE H M FL H k|M H >-\2SRB H SR H RRAB H )SRA H  nL H RRAB H D|RRAB H )FRRC H ExRRAB H ":RRAB H ?rSR H HZISRA H >xRRAB H FSR H 02SR H L.SR H .EZSRB H L:^2RRC H LD@M H  ZL H jJD2L H @M H ZRRAB H pM H LRRAB H %dRRC H  RRAB H DJ(L: H C<xRRAB H  SR H  *xRRAB H RRAB H " dL: H "3,M H "F TM H # 2L H "D,M H "'dRRAB H "8TM H # #SR H &p-dSR H &JM H &L2RR H 'ZSRB: H &ARRAB H '$ (2SRB H '4nRRAB H 'o SRB H 'vE H 'BDRRAB H '~2RE H 'oDM H '~@0RRAB H ' SRA H 'I6RRAB H '4x2E: H 'H|M H (AdSRB H (nfRR H (n6M H (%SRB H ) (RRAB H )@*PSRB H );FSR H ) SRA H ):@RRAB H )$RRAB H *! \@SRA H *?NdSR H !)HZdL H "*:xSR H #*0)RRAB H $*0,RRAB H %*KM H &*JM H '*&FSRB H (**SRA H )+ PSR H *+>8RRAB H ++MxRRAB H ,+'xRRAB H -+MH(/hM H .+":,F(L: H ?-< $nSRB H 5LPCEP: H 5aEXL H 58CEP H 5/MEA/SDH 5I@RRAB H 6Q 2L H 6o4RRAB H 6`8M H 6`xRRAB H 6o>RRAB H 6`FCEP H 69PZRRAB H 7|CEP H 7#ZRRAB H 7_pZL H 7}RRAB H 7#ARRAB H 72@RRAB H 7^M H 7!(RR H 7nRRAB H 73JM H 8OxE H 8@',M H 8EPUV: H 8OI^RR H 8C(2RRAB H <"#SRA H SRA H =;EXRRAB H =w).nRRAB H ='(E H =EFL H =1nRRAB H =@nRRAB H >I (L H >:RLM H >g,M H >+BRRAB H >ICdRRAB H >v;0xRR H >'M H > 2RRC H >6RRAB H ? nRRAB H ?*2E H ?f0RRAB H ?9&PRR H ?vRRAB H ?AHSR H ?":SRA H ?4PRRAB H @)"RRAB H @ DnSR H @GLPSRB: H @8~dSR H @xSRA H @tRRAB H A .BSR H @;lE H A(%ndL H DCPSR H CFFRRAB H CMSR H CElPL H D=BJM: HDa4PL HDRRAB HD&M HD#4nRRAB HEoRRAB HEQdSRB HEVRRAB HEo2RR: HEotM HE~PL HE 6UG HE FRRAB HE z2SR HFRRAB HE$SRB HE;xRRAB HF#'ZRR HFnZL H FP/2SRB H!FdRRAB H"FRRAB H#F8RRAB H,GO3ZL H-GnPRRC H.GvRRAB H/G9RRAB H0G*<FL H1H]CEP: H2G4FSRA H3H0(SRA H4H x(M H5HPRR H6HN@dRRAB H7H<RRAB H8H3UV: H9I0"RRAB H:INPSR H;IPRRAB H<IzBjRRAB H=H{hNB H>I*nRRAB H?IIRRAB H@J"M HTFRRAB HUnPRRAB HTEdSR HU#G~FSRB HURRAB HUE HU+"ZSR HV"RRAB HU'FRRC HVO|RRAB HV|rRRAB HV1;E HV|#4fSRA HVZRRAB HV SRB: HW<SRB: HWIRRAB HWl SRB: HWRRAB HW]6RR HW{:rnSR HW2SRB HW"SRA HWFRR HX+M HW<RRAB HX nRRAB HX/(RRAB HWIrRRAB HX #RRAB HXM E HX\56dRR HXMRRAB HYLnRRAB HYL&ځSRB HLB: HҗINS HD w-EB/DMHM: HTˤFEA HRCB HnxLB: HIdSRB: H4RV: HF葾SR HY`RR HFRR H.nLB: H:hdLB: HD"ZAND HxSR: HbE HA|ZLB: HATxRV: HrPEW: HMFEW: HXZAND HjBxSR: H<LB: HFnLB: H"eSR H")$,M: H%&dRR: H&ZLB: H&ʹRRAB H&CEP: H'$$ZEA H'o`PLB: H(PtxE: H(FRR: H)@LB: H)SR: H)PLB: H,LzLB H-RV: H/IPLB: H B6hL: H EpPRR: H E~0RR: H EoRRAB HF_(dLB: HI/xSRC: HKJPRR: HMXdLB: HNuI: HQTyPRR: HPHLB: HRbEA HRFRR: HWݬPEW/KWHYFLB: HZRR: H^GE: HaRM Hc3SRA HcdRR: He|xE HgxI: H yIx\cLB H!'9ȱSRA H"0fp(sTM H#6`u pM H$?9`DM H%I/ y{.SRB H&`sYM H'ab yt5SRB H(HM H) B,M H* IM: H?b}-INA: H@hM: HA,SR: HB`ZRRAB HCtxSR: HDorM HE|xnUG: HFz FCEP: HGwdSR: HHvSR: HI]vJSR: HJOUG: HKlLL HLvPRR: HM\NM HNvm"M: HO%0M HPa nSR: HQp¼M: HR _T2L HS ZJM HTM: HUj^M: HVi@M HWn¸M: HXG$(SRB HYZAND:HZM: H[hM H\ вM H]AM: H^ SR: H_SR: H` M: Ha `TM Hb!WB",M: Hc!X M: Hd#(hM: He%aUG: Hf${M Hg(vM Hh(`*M: Hi+nM: Hj,L|M Hk,j8M Hl,`,M Hm.JTM: Hn/gSR: HoX\SRA Hpk JM: Hq[8M: Hr*%LB: HsExSRD HtFWFL Hu"\ZL Hv dSR Hw?>2LB HxB.2LB HyR%llACV HzbldRR: H{܀dL H|i NA H}[e7SR: H~æif} M Hõfh7M: Hip,} M Hhh7M: Hie^s*M Hg"7M: H;f z/M Hj~7SR HjBrM: HIh7SR: Hg7M: H hX;2M HǓe$7M: Hg^J M: HjV@~M H8hl7M: HȰdJxM HȰd\L7M: H*(1GCAS HhDv#SR: Hi)M Hɂi^tM Hɠh:7M: Hʁjt7M: Hi*4/M Hj~SR: HfnE{0M H5e7M: HCd>tM: HRehzM Hec'M Hg|7M: HѶV~1SR HZ>p[M HjfnwWM HXqPM HԕZz"$SR: H\ M: HWWaSR: HVY1}M HY~8M Hy7M: H?vh} M: H/v@7M: H-vTu M Hvh7M: Hz7M: Hu(ZSRA Hu(7SR: Hv7SR: HGYٹM H a<,SR: H#dmvL: H#NL: H7 HPlNA HQ3SRA He@rdSRA HlGCAS H/>SR: HCzSR: HykNB H8UtSR: Hr`SDOR HB ACYG:H1GLxGCAS H=9 nRRAB HRq*PEA HG^M HH?qSRA HIM HVV "M HVW ˏEA HVX :xSRC HVY ܘpDCEP HVZ ]RCB HW R_ bUDCEP HWW }бM HWX Ȓ <,EA/SDHWY ͫ.ZEA/SDHWZ E^xvDCEP HX xDaFDCEP HXX !RWCEP HXY  7EA/SDHXZ EA/SDHY tlcDCEP HYY gMGEA/DMHYZ xF}JDCEP HZ `‹M HZZ wh͠EA/SDNAA VINT NAB  SRA NAC 05EA/SDNAD `gI NAE _p{dCEP NAF ZQSRA NAG  [(γM NAH 4_,CEW/KWNAI l.ȾRR NAK J&$M NAL mdEA NALP?LB: NAM z5EA/SDNAN 3`4`UEB/DMNAO XlM NAP UydEA NAQ ~"ZEA/SDNAR )xSR NAS FEA/SDNAT hZLB NAU |Z䕯SRA NAV |ndDCEP NAW }|M NAX ±SdSRA NAY )e0LB NAZ _ LB NBB ˷k PLB NBC ·TPPLB NBD OdnLB NBE @]SR NBF ax,ZSRA NBG ۸hSR NBH tFSR NBI rdSR NBK #h<PLB NBL )0SR: NBM .$ISB: NBN w+`XEA/SDNBO {q8ԵxRRAB NBP "INT(YNBQ <,P NBR 1(گRRAB NBS thINS NBT ͈xINS NBU <QNgIGCAS NBV AFEB/KENBW IGAL NBX NnI NBY ԯD>ZI NBZ R_FSR NCC A(E NCD Q{9EA/D NCE aSRC NCF SO:/EA/D NCG mr@M NCH  hSRB NCI D?INST(NCK *{dRR NCL 2pSR: NCM }5B7SN+PSNCN tEA/SDNIW v\4dINS NIX QelXM NIY 2RRAB NIZ [M NKK X6UV NKL Y6UV NKM Z"lUV NKN O<UV NKO =dTTUV NKP 1\UV NKQ nhUV NKR #`@UV NKS ZlUV NKT /VXUV NKU Gb"UV NKV _rrUV NKW CUV NKX 7UV NKY aJUV NKZ IUV NLAMD^vY6EA/DMNLL FidUV NLM PUV NLN R:UV NLO bOFUV NLP 5YPUV NLQ OUV NLR 4G"UV NLS ZUV NLT RPhUV NLU Y [UV NLV BXUV NLW CxUV NLX <UV NLY c"UV NLZ RtUV NMM GJUV NMN D.UV NMO W\6UV NMP KUV NMQ d,UV NMR [&cUV NMS UTUV NMT IjPUV NMU  !^Z,UV NMV  BlUV NMW  J UV NMX  kP^`UV NMY  [:UV NMZ  zlUV NNN  a 6UV NNO  UUV NNP  QnUV NNQ  =V@UV NNR  -b~,UV NNS  =@2UV NNT  LHzjUV NNU  R4UV NNV  jX|UV NNW  OdUV NNX  KNtUV NNY  xT,UV NNZ  RDUV NOO  HbUV NOP g.UV NOQ `UV NOR  ^dUV NOS  [bUV NOT XK4UV NOU vSUV+BYNOV dUG NOW uMfkUV NOX XJUV NOY JUV NOZ QUV NPHObhDSCTCNPP Q&JUV NPQ O<UV NPR 6G&UV NPS EUV NPT WUV NPU HUV NPV 5S`UV NPW b^@UV NPX rLl"UV NPY qUUV NPZ &\UV NQQ JUV NQR C7h@UV NQS R UV NQT oTTUV NQU 38DUV NQV KHUV NQW >JUV NQX NHUV+BYNQY 2ZUV NQZ XV UV NR ^A4M NRR rINSA NRS ʸ4}CST NRT "KCST NRU ͈!0M NRV n@^RVB NRW NiEA/SDNRX ȬsL:M NRY prINT NRZ IXל?EW/KWNS \wM NSS I4ܮnRRAB NST nSDCEP NSU  RCB NSV ((nEA/SDNSW 8|cSCWB NSX (eD,M NSY HdLB NSZ ttv*DCEPSNT INT NTHEtXDSCTCNTT SRB NTU W rJSRB NTV _wx"SRA NTW LxdLB: NTX ]t0WSRA NTY >2EA NTZ Ku rM NU ACST NUPS?BbDSCTCNUU `o׹M NUV 5MM NUW  g`LB NUX B6INT NUY .4OM NUZ jlJINT(YNV |bM NO_9UV NP};UV NQ9UV NRYUV NSH>NUV NT|A^UV NU UV Nby^YUV NcKUV NdTFUV NeKI$JUV NfxWzUV NgW*UV NhTnUV NiVUV NjbC2UV NkNUV NlY&UV Nm5`UV Nn c2UV No ^,UV Np9MpXUV NqNtUV NrWUV NsTZ|UV NtOn6UV NuGN^UV Nv7UV Nw!EKhUV Nx!^FZUV Ny"EPUV Nz!Y.UV N{"DTUV N|"lL"UV N}#PUV N~#%M`UV N#W^UV N#CUV N$$42UV N$3@<NUV N$XUV N$NDUV N$I`^UV N%ncXUV N7 N&OW\,UV N%FFUV N&^5xUV N'?:`UV N(ZUV N*^2UV N+U^UV N, F^UV N,F@UV N-YUV N. g,UV N1>UV N2CNVUV N=tK6xUV NYgVL"M Ngwp 4,EA/SDNwmnRRAB NbINS NpnINSB N~XvZZA NjXSR N;E(dINA: Ne^LB N,RRAB Nk &UG: Ns|UV N<,UV N\U66UV NCp|UV NY8UV NW^lUV N @:UV N5F|UV Nk|UV N>^UV N#[hUV N}?UV N X[UV N YVlUV N ;BUV N WpUV N YF|UV NXUV NiUV Ne`UV NZUV NIj2UV N6O"UV NSxUV N_jEA/DSND`lFUV NbJUV NqDUV NS6UV N80UV N3oUV NU^UV NJZUV NpH:UV NNUV Nz]UV N_TdUV NX:UV N!TeTUV N\@UV N"QUV NPhUV NSUV NRUV N^26UV N͕EA/D/N84UV NvACV N$`RUV N$P,UV N&"VUV N(>aUV N)fpUV N.FDSCTCNjDSCTCN4dUV Nq@qLB: N ôoDSCTCN}UV NYCpUV NgD8z ACV NLUV N@H>UV 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