STAR ATLAS CONTAINING Maps of all the Stars from 1 to 6.5 Magnitude between the North Pole and 34 South Declination, and of all Nebula; and Star Clusters in the same region which are visible in telescopes of moderate powers. CCUt!) erplanatorp m 11 V DK. HERMANN J. KLEIN. IKANSI ATKI> AM) AKU'TI.I) TOR ENGLISH READERS BY EDMUND MCCLURE, M.A, M.R.I.A. WITH EIGHTEEN MAPS. BY Z. A.. yTTlTJCHJ, PUBLISHI I) I XI. I- R THE DIK1 i THE COMMITTEE OF GENERAL LITfcRATfKE AM) l.DHAII'.N \l : y THE sorll. IV I OR PROMOTING LIIK1STIAS KNOWLEDGE. jC4i London : SOCIETY K,K PROMOTING, CHRISTIAN KN()\VLMI)(iK. N'iRTIirMHKKUANI) AVKNTIC. CHARING CROSS. W.C. I. i.'l-CICN VICTORIA STREET. EC. BKHillTON : 135. NORTH STREET. NE\Y YORK : E. & ]. B. YOUNG & CO. [888. k ; , TABLE OF CONTENTS. IntroJuction . . 1 1'al'li. lor turning Si Table tor turning Degrees fnr* i- Double Star . ;Vi '" 70 A' \ariable. . . .71 107 Double Star. . ! 71 T Variable Triple Star 4 1 Double Star . 17 17 17 1 Q into Si.li real Time . 3 al Time at Jl.au Aquila, The Eagle. 52 Triple'star . IN 18 II . . , t ^ filiations ... 5 Star Magnitti'. . . 6 Numb, r of the I'ixi-.l (Sheet VI., XL, XII.) 1 D,.iiM,. Star . . .59 4440 Star Cluster (Sheet \ V \ ff. Auriga, The Waggoner. (Sheet I., 11., III.) 4 Doable Star . . .22 "* - .7 Variable Stars . . . 7 Di-tunce of the Fixed Stars . 8 Me Stars ... 8 Star Clusters . . . <> ila- .... 9 Explanation of the Maps . 10 Description of the more interesting Fixed Stars, < 'lusters and Nebulie 1 -^ ) . . .60 11 Double Star . . .61 * ,, ... 61 R Variable. . . .61 4470 Star Cluster . 61 "82 61 23 Double Star . . .61 4487 Nebula . . .61 X Double Star . . .61 * Altair M i Variable . 996 Star Cluster Z 645 Double Star R Variable Capella . 1 4 Triple Star . * 1067 Star Cluster Z 681 Double Star 1101 Star Cluster . 22 22 23 2.1 S3 24 21 24 M n Variable . . fi2 >. 24 Andromeda. (Sheet II.. V.. VI. R Variable . 1 1 & Multiple Star . . .63 57 Double Star . . . 63 Z 2628 Double Star . . 63 V IK 1 1 1137 Nebula 1166 Star Cluster 26 Double Star . Jt 25 II 27 116 Nebula . . ! W J5 1295 Star Clutter (Sheet 117 .. ... 13 XVIII.) . 29 ft Double Star . 13 111.1.01.. Star Cluster Ar * navl8 ' The Shl P *#>. 9 Triple Star . 41 Double Star . 29 29 y Triple Star ... 16 -t VIII., IX. S 872 ... 30 VJ7 N.t.iila . . . 16 I 1097 Quintuple Star . 34 66 11 ... 31 r >7.l . . . 17 Z 1121 Double Star . . 34 14.11 Star Cluster 32 49:14 ... 71 1351 Star Cluster . . 34 S030 Double Star . . 71 1564 . . 35 Bootes. Aquarius, The Water Bearer. (Sheet XII.) 1 Triple Star ... 65 1567 Nebula ... 35 1.171 Star Cluster . . 35 5 Double Star . . . 35 1630 Star Cluster . . 36 1632 Star Nebula . . 36 (Sheet III., IV., V., X.) 1 Double Star . n;:t7 Nebula . r Double Star . T Variable 47 47 47 47 T Variable . . . .65 4 Double Star . . .6.5 Aries, The Ram. Double Star . Arcturus 47 47 462ft Nebula . . . 6 (Sheet II., VII.) t Double Star . 47 I- 1 Double Star ... 66 y Double Star 15 8 Variable .... 47 4678 Nebula . . 67 * ... 15 Z 1S50 Double Star . 47 41 Double Star . . . 69 Z 196 . . .15 R Variable 47 . fi'-i II ... 16 w Double Star 47 ... 70 11 Variable ... 16 Triple Star 48 r ... 70 30 Double Star ... 17 t Double Star . 48 N Variable . . . . 70 33 ,, . . .17 { it ... 48 IV :59 Double Star 44 1919 1926 * /* Triple Star Pago 48 48 48 48 48 49 Camelopardalis, The Giraffe. (Sheet I., II., III., IV., VI.) 52 Double Star . 38,5 . 390 . 396 . 801 Nebula' . 485 Double Star 1 2 7 940 Star Cluster 634 Double Star 780 Triple Star 1051 ,, 1541 Nebula . 1127 Triple Star 1691 Nebula . 18 18 18 19 20 20 21 22 22 22 23 29 33 34 34 36 Cancer, The Crab. (Sheet III., IV., IX.) Triple Star ... 36 It Variable. . . .36 V . . . .36 ' i 2H07 Double Star . .-.1 : \ \ /.' Vaiiable 111:. Nebula , p Di.ul.le St;.r . _ rt 4f\n 58 68 . . y I* U Variable. .11 52 (9 i Double Star . Crater, The Cup. i -03 ... I.M7 Star Cluster , Double Star . 59 C,2 62 '/ . m Double Star . 12 52 52 (Sheet XIF.) Equuleus. The Foal. 4230 Star* Cluster (Sheet 52 Cygnus, The Swan. Sheet I ., II , V , VI.) i'iblc ' l ... ni.) 273.1 Double Star . 1 Triple Star 2 Double Star . ^> 1 v i>7 i j 66 66 66 . XVII., XVIII.) . l-'il Nebula Z 2101 Double Star . 1211 Nebula 1 2104 Double Star . 53 53 1511 Star Cluster Hi Double Star . i j / 1 1 ''- y Triple Star 62 Oil (17 /* v Variakle. a . . . . 53 54 * I'.ll Nebula 62 69 ... jS Multiple Star . VI J Double Star . 4294 Star Cluster (Sheet 54 1 7 I >ouble Star . 62 XV.) .11 X Variable .... 62 Eridanus, The River 68, u Variable . 55 ij/ Double Star . 63 Eridanus. ; Double Star .',.-, I'.ll Star Cluster 32 a" Double Star 63 63 (Sheet VII., VIII.) Z2190 ... 83 ... 55 55 /' Variable. 64 1 2 Double Star . 18 Z2215 56 4575 Star Cluster 64 692 Nebula 18 P Triple Star 56 I 1 ' Mouble Star . 65 709 . 18 4343 Nebula 56 4600 Nebula 65 Z 422 Double Star 19 95 Double Star . 56 52 Double Star . 65 32 19 Z 2277 57 T Variable .... 65 A . . 20 100 67 A Triple Star 65 826 Nebula 20 T Variable .... 67 59 Double Star . 66 o 1 Double Star . 21 Z 2289 Double Star . 57 . 66 55 2'2 110 59 61 Double Star . 66 * 22 Nebula .... 66 4645 .Star Cluster 67 Gemini, The Twins. Hydra. r Double Star . 67 r T (Sheet II., III., VIII.) (Sheet IX., X.) " it ... 4681 Star Cluster 67 68 1325 Star Cliuter 29 Z 1245 Double Star . 36 O "7 Nova 1870 .... p. Quadruple Star 68 68 1360 . . . >i '\ ariable .... ft Double Star . 29 30 HO i 15 Triple Star . -S Variable .... 3< 37 37 Delphinus, The Dolphin. 15 . . . y Triple Star . 30 31 T . . . . 37 37 $ Double Star . (Sheet V., XII.) i Double Star 31 T' ... 33 4586 Nebula C4 38 . . . 32 2102 Nebula 39 & Triple Star * Multiple Star . /' Variable .... 65 65 65 1467 Star Cluster Variable .... A* ,, . . . 32 32 33 Double Star 3128 Nebula R Variable . 41 II 46 y I louble Star . 65 1490 Star Cluster 33 Nebula 66 1508 x Double Star . 33 33 Lacerta, The Lizard. Draco, The Dragon. (Sheets T., III.. IV., V. VI .) 1534 Star Cluster o Double Star . 33 34 34 [Sheet II., V.) 4755 Star Cluster (Sheet XVII.) . 69 2HJI Nebula 39 164'. Star Cluster 34 4773 , , X4 ' 2!l 1- S Variable. 34 8 Uuadruple Star 69 VI Page I'agc Page Lepus, The Hare. (Sheet VI I I.I R Variable t Double Star X ,, ... 22 23 23 Lynx. (Sheet I., II., III., IV.) 4 Double Star . 5 Triple Star 12 ... 30 30 31 19 Double Star . 4256 Star Cluster Nova of 1848 4264 Star Cluster 4268 53 53 53 64 54 64 9 Triple Star 24 X 958 Double Star H- 31 QO 1270 '. 54 1112 Star Cluster 24 . 32 36 Double Star 54 (3 Multiple Star . 25 2 1009 32 R Variable 54 a. Double Star 25 19 . . 33 u 54 4o Multiple Star. 28 2 1333 C8 39 Double Star '. 54 y Double Star 29 38 . .3 1811 Nebula 39 Double Star . 5 38 4287 Star Cluster 4296 Nebula 54 55 Leo, The Lion. 4302 . . . 2 2166 Double Star . 55 55 (Sheet III., IV., IX.) Lyra, The Lyre. Nora of 1604 65 w Double Star 38 (Sheet IV., V., VI.) 22173 Double Star . 55 1861 Nebula 38 \T 53 / 55 1863 38 ega . . . . 59 54 ,, . . 55 6 Double Star . 7 38 38 and 5 Double Stars .' f Double Star . 59 59 4315 Star Cluster 61 Double Star . 55 53 J ) R Variable a Regulus .... 38 39 |3 Variable .... 4447 Ring Nebula (Sheet "vvr "> 60 fin 4346 Star Cluster 67 Double Star . 56 56 y Double Star 49 39 39 -A. V 1 . i . . . Multiple Star . DU 60 T 70 56 57 2184 Nebula 2194 ... 39 40 R Variable 17 Double Star . 60 61 jj . 73 4390 Nebula 57 57 2203 ,, ... 40 fi ,, ... 61 4110 Star Cluster 58 2207 40 4485 Star Cluster 61 54 Double Star . 40 9 Double Star . 61 2279 Nebula 40 unon. 2301 ... 40 Monoceros, The Unicorn. (Sheet II., III., VIII.) 2352 ... 2373 ... 40 41 (Sheet VIII., IX.) 905 Star Cluster. R Variable .... 22 22 2377 ... 41 4 Triple Star . 30 627 Double Star . 22 . Double Star . 41 5 Eed Star 30 96 li Eed Star . 22 r ,, ... 41 8 Double Star . 30 1005 Nebula 23 88 ... 41 T Variable .... 30 i Double Star 23 90 ... 41 1408 Star Cluster 30 652 ,, ... 23 93 ... 41 1415 30 23 |3 Multiple Star . 41 1 1 Quadruple Star . 30 ,, ... 23 Leo minor, The Little Lion. (Sheet III., IV.) 1713 Nebula ... 37 R Variable . . .38 2104 Nebula . . .39 2 92 1 Double Star 1424 Star Cluster 1425 Nebula 14 Double Star . . 1435 Star Cluster 2 950 Multiple Star . 1440 Star Cluster 31 31 31 31 31 31 31 T Multiple Star . m Double Star . . . i, Triple Star y Variable .... \? Double Star . 31 A 32 ... 24 24 24 24 24 25 25 2178- ... 39 1453 ,, 32 33 25 2274 ... 40 1465 32 o j t ... 25 2287 ... 40 1474 32 A Triple Star 26 Libra, The Balance. (Sheet X., XI.) a. Double Star . Multiple Star . 48 48 1483 ,, tf"Variable 1611 Star Cluster 2 1183 Double Star . 29 Triple Star . 1637 Star Cluster 33 34 35 36 36 36 2 747 Double Star . 1 1 79 Great Nebula (Sheet XVI.) 1184 Star Cluster i Triple Star 1185 Nebula 26 26 27 27 27 J Variable .... 48 1193 Nebula around E. 27 i Triple Star 48 Ophiuchus. a- Multiple Star . 28 S Variable .... 49 1225 Nebula 28 2 1962 Double Star . 49 (Sheet XI.) Triple Star 28 ? Double Star . 52 1226 Nebula . " . 28 Lupus, The Wolf. * ,, ... 4211 Star Cluster 52 52 1227 (Sheet XVIII.) 1267 28 29 (Sheet X., XL) 4238 . . 53 52 Double Star . 29 VII I'M. i PUB ; D Star . H H-J'.t StarUluster . . 59 l.'.l" v, ... 14 4l,J . . 69 a Variable .... ula 1 1 A 1 Variable . . .59 A' Vaiial.le 1 1 l|.:7 Star Clu-ter XV.; ' ila 1 j 1111 Nebula . * Double Star . ia Piscis austrinus. The Serpens, The Serpent. Pegasus. Southern Fish. ' IV . V . X . XI.) il . \ 1 . Ml S 1 1.) r Cluster . . 49 y 1 ) i ' u 1 f 1 c St;ir 1 1 "' Double Star . . .49 Star Clu-ter Sagitta, The Arrow. - ''II 49 1 iK.uMe Star . Sheet V., VI., XII.) . D m'-i. 81 IT . *' Variable . . r.i 61 * Double Star . . . p.i 1 ' 1 S Triple St ir 62 * " ' ,, . . K ... . 1 'Jo Star Clu-tir .r . $ Triple St ir II ... .)() /.' Variable I'.' D..uMe Star . . 51 ! iipl- Star . '.ula ,.;,' .. . .55 ': 1',.'! '.;. >; ir . >'>* ,, . . .58 i ,. '.la ihle Star . 7o 70 70 Sagittarius, The Archer. Sextans, The Sextant. Variab! . -ter 70 70 71 A \aiiablc Double Star . 1750 Nebula . . 37 . 37 Ursa minor, The Little Bear. 3614 ^t-bula 361,5 . 46 . 46 s Double Star . . 37 (Sheet I., II., IV., V., XIII.) 84 ~ Double Star . . . 47 1765 Nebula . 37 a. Polaris . . 11 T ,, . . . 47 1781 . 37 TT' Double Star . . 50

8.6 10 9 58 21 10 9 58.4 20 19 f><; l:i 24 -j:i ; 4 If on any day the first point of Aries, of which the R.A. is 0, passes the meridian of an observer at noon, an hour after noon, a point of the heaven of R.A. 15 will he on the meridian, after two. hours a ; point of R.A. 30, after three hours a point of 45 etc. The Right Ascension of a star, or,its.d!stauce.from the first point of Aries, instead of being expressed in degrees, can thus be indicated .Uy the/ number of hours, minutes, and seconds, which have elapsed from the time of culmin- ation 1 of the "first point of Aries until the time this star passes the meridian, or culminates. Thus instead of expressing the Right Ascension of the bright star Vega by 277 30' we may say that it amounts to 18 30 m - For, as 360 pass the meridian in 24 hours, in one hour 15 will pass, and in 1 time minute 15 minutes of arc, and in 1 time second, 15 arc seconds. Thus 277 30' turned into time are equal to 18 h 30 m - In many star maps Right Ascension is expressed in degrees of an arc only. The practice of astronomers, however, without exception, is to reckon the R.A. in time only. Therefore in the present atlas the parallels for Right Ascension are given in hours and parts of an hour. In case it is required to turn time into arc measurement, the following table will readily serve the purpose. Table for Turning Sidereal Time into Degrees. Hours. Degrees. Minutes. Degrees. Minutes. Degrees. I 1 ' 15 i"> 15' 31'" 7 45' 2 30 2 30 32 8 3 45 3 45 33 8 ]5 4 60 4 1 34 8 30 5 75 5 1 15 35 8 45 6 90 6 1 30 36 9 7 105 7 1 45 37 9 15 8 120 8 2 38 9 30 9 135 9 2 15 39 9 45 10 150 10 2 30 40 10 11 165 11 2 45 41 10 15 12 180 12 3 42 10 30 13 195 13 3 15 43 10 45 14 210 14 3 30 44 11 15 225 15 3 45 45 11 15 16 240 16 4 46 11 30 17 255 17 4 15 47 11 45 18 270 18 4 30 48 12 19 285 19 4 45 49 12 15 20 300 20 5 50 ]2 30 21 315 21 5 15 51 12 45 22 330 22 5 30 52 13 23 345 23 5 45 53 13 15 24 360 24 6 54 13 30 25 6 15 55 13 45 26 6 30 56 14 27 6 45 57 14 15 28 7 58 14 30 29 7 15 59 14 45 30 7 30 60 15 2. The sidereal day begins, as already mentioned, at the instant in which the first point of Aries passes the meridian of the observer. The Sidereal time at any moment is therefore equal to the distance, expressed in time, of the first point of Aries westwards from the meridian ; in Table for Turning Degrees into Sidereal Time. 1 1 l 2 ; i 5 . : N !i h in h m b m h m h m h m h m h m h m b m 1) 1 - 1.' 16 20 24 28 32 36 10 in II 48 52 56 1 1 4 1 8 I 12 1 1(1 90 1 ','11 1 2t 1 28 1 32 1 31 i 1 40 1 II 1 48 1 62 1 56 2 2 ; 2 8 2 12 16 2 20 2 24 2 28 2 32 2 36 10 2 40 2 II 2 IN 2 52 2 56 3 3 4 3 8 3 1-2 3 16 i 20 3 24 3 28 3 32 3 3 40 3 II 3 48 3 52 3 56 (in I n 1 1 4 8 4 1.' 4 16 4 20 1 -.'1 4 28 4 32 4 70 1 to 1 H 1 is 4 52 I 56 5 5 1 5 8 5 12 5 16 80 5 20 5 24 5 28 5 32 5 36 5 40 5 11 B IN 5 52 5 56 no 6 i; 4 6 8 6 12 6 i<; 6 20 fi 24 G 28 6 32 6 3<; 100 6 40 6 11 6 48 fl 52 c, .-,i; 7 7 1 7 8 7 12 7 it; no 7 20 7 24 7 28 7 32 7 :it; 7 lo 7 11 7 48 7 52 7 :,r, 120 8 8 4 8 8 8 12 8 16 8 20 8 24 8 28 8 32 8 3i i 130 8 to 8 44 8 48 8 52 8 56 ! 9 4 9 H 9 12 ID 110 9 20 !> 24 9 28 9 32 ! 36 9 40 9 11 9 48 9 52 9 .-ii; L50 10 10 4 ID 8 10 12 10 16 10 20 10 24 in 28 10 32 10 3(i 160 10 40 10 H 10 48 10 02 10 -Mi 11 11 4 11 8 11 1-2 H i<; 170 11 20 11 24 11 28 11 32 11 36 11 40 11 II 11 48 11 11 .-(, 180 1-2 !-' 4 12 8 12 12 1'2 16 12 20 12 24 12 28 12 12 31 i 12 40 12 44 12 48 12 52 12 56 13 13 4 13 8 13 12 13 in 200 13 20 13 -21 13 28 13 32 13 36 13 40 13 11 13 48 13 52 13 56 210 14 14 4 14 8 14 12 14 16 14 20 14 24 H 28 14 32 14 31; 190 H 40 14 11 14 48 11 52 14 15 1-1 4 15 8 15 12 l'i 16 230 15 20 J"> M 15 28 15 32 15 36 15 40 15 44 15 48 n .V2 1. 56 240 16 16 4 16 8 16 12 16 16 16 20 16 24 16 28 16 32 Hi 36 960 16 40 16 11 16 48 16 52 10 56 17 17 4 17 8 17 12 17 16 960 17 20 17 24 17 28 17 32 17 36 17 40 17 44 17 48 17 52 17 56 270 18 18 4 is 8 18 12 18 16 18 20 18 24 18 28 is 32 18 3i > 280 1- 40 18 11 18 48 18 52 18 56 19 19 4 19 8 19 12 19 1C 290 1!) 20 19 -21 19 28 19 32 19 36 19 40 19 44 19 48 19 52 19 56 MO 20 20 4 20 8 20 12 20 16 20 20 20 24 20 28 20 32 20 31; 310 20 40 20 44 20 is 20 52 20 56 21 21 4 21 8 21 12 21 n; 320 21 20 21 24 21 28 21 32 21 36 21 40 21 44 21 48 21 52 21 :,; 880 22 22 4 22 8 22 12 22 16 22 20 22 24 22 28 2-2 32 22 3(i 22 40 22 44 22 48 22 52 22 -.; 23 23 4 23 8 23 12 23 16 350 23 20 23 24 23 -Js 33 ;v2 23 :;i; 23 40 J3 44 23 48 23 23 56 Minutes. 0' 1 2" ; 4' i |. r ' 9' 0' 10 20 m 40 1 20 m 4 44 1 24 m 8 48 1 28 m o 1-2 52 1 m o it. o .-><; i m 20 1 l m m o '.'I 1 4 1 44 m 28 1 8 1 IN m 32 1 12 1 52 m > o 3t; l in 1 56 30 40 50 2 2 40 3 20 2 4 2 44 3 -2 1 2 8 i- 3 28 2 12 2 .VJ 3 3-2 2 Hi 2 56 3 3(i 2 20 3 3 40 2 .'1 3 4 3 44 2 28 3 8 3 48 2 32 3 12 3 52 2 36 3 If, 3 4 other words it is equal to the R.A. of the point of the celestial sphere then passing the meridian. Conversely the Right Ascension of a fixed star expressed in hours and parts of an hour is equal to the sidereal lime of its passage through the meridian. In most cases the observer requires to find out the mean or civil time of the place in which he is at the moment when a certain star, whose llight Ascension is given, is on the Meridian. This can easily Le ascertained with the help of the following table, which gives the approximate sidereal time of mean noon for every day in the year. If the exact sidereal time be required, the Nautical Almanack for the year must be consulted. Sidereal Time at the moment of Mean Noon. 2 . 5 "S g P | February .d I a 8 p. 40 7 38 9 40 11 42 13 41 15 43 17 41 16 17 18 19 48 19 52 21 51 21 54 23 41 23 45 1 43 1 47 3 41 3 45 5 44 5 48 7 42 7 46 9 44 9 48 11 46 11 50 13 45 13 49 15 47 15 51 17 45 17 49 17 18 19 19 56 21 58 23 49 1 51 3 49 5 52 7 50 9 52 11 54 13 52 15 55 17 53 19 20 20 22 2 23 53 1 55 3 53 5 55 7 54 9 56 11 58 13 56 15 59 17 57 20 21 20 4 22 G 23 57 1 59 3 57 5 59 7 58 10 12 2 14 16 3 18 1 21 22 20 8 22 10 1 2 3 4 1 6 3 8 2 10 4 12 6 14 4 16 7 18 5 22 23 20 12 22 14 5 2 7 4 5 6 7 8 6 10 8 12 10 14 8 16 10 18 9 23 24 20 16 22 18 8 2 11 4 9 6 11 8 9 10 12 12 14 14 12 16 14 18 13 24 25 20 20 22 22 12 2 15 4 13 6 15 8 13 10 16 12 18 14 16 16 18 18 17 25 26 20 24 22 26 16 2 19 4 17 6 19 8 17 10 20 12 22 14 20 16 22 18 21 26 27 20 28 22 30 20 2 23 4 21 6 23 8 21 10 24 12 26 14 24 16 26 18 25 27 28 20 32 22 34 24 2 26 4 25 6 27 8 25 10 27 12 30 14 2S 16 30 18 28 28 29 20 36 28 2 30 4 29 6 31 8 29 10 31 12 34 14 32 16 34 18 32 29 30 20 40 32 2 34 4 33 6 35 8 33 10 35 12 38 14 36 16 48 18 36 30 31 20 43 36 4 37 8 37 10 39 14 40 18 40 31 .;ITT - 5 - I i m-tun . i, it' it be required to find out at what Lour of the day ou the 15th April, the .Star fa-tor, ^ht Ascension is 7 U 27 m , is ou the Meridian : ii-real time of Meridian passage = Hight .Wuision = 7 h 27 m Sidereal time at mean noon uu loth April . . . . = l h 3A m Ditferonoe: 5 k 52 m It mu-t l.e Urnr in mind that tin- diH'eu-nee is expressed in sidereal hours, 21 of which an '') 56.9 xhorter than 'Jl 1 of mean time. It follows, therefore, that 5 h 52 m sidereal time an \>~, , or -(M-akin- muchly, l m shorter than the corrosponding mean time, and tlu> must be Mibtractcd frotu the result given above. Castor will therefore be on the Meridian at 5 U SI Constellations and the Names of Stars. Already in the earliest ages the chief fixed stars had received names, and many i <>n figurations fancifully representing natural or mythical objects, were grouped into n-tellatioiis. In the 10th century, when more exact information had been obtained with regard to the southern heavens, constellations were duly marked out there also; nay, e\.n in the last century several new constellations were added to the number, and introduced into astronomical maps. That there was no great resemblance between the constellations and the objects whose names they bore, it is needless to say. The practice which obtained in the old star atlases, of surrounding the stars composing a constellation with an outline of the ]>crson or object which the constellation was supposed to represent, was, therefore, purely fanciful. Until quite recently the greatest uncertainty prevailed, not only with regard to the boundaries, but even as to the number of the constellations. It was finally, however, decided that only those constellations should be recognised which are to be found in Argelaiuler's Neue Uranontett i< . The present atlas will therefore be found to contain only those constellations which arc given by Argclandcr, the fantastic figures suggested by their names being omitted. The following is a list of the constellations visible from our earth, which are to be found in Argelander's Uranomctrie. Andromeda, Andromeda. Aquariitx, The Water-carrier. Af n-inarki-il, however, that the estimation of the magnitude of faint stars is vt-ry unvrt:iin. Thus Stnive deviates tho faintest companions of double stars which he could see through the U-inch refracting telescope of Dorpat as of the 12th magnitude, which according to Arjji-laii'lrr's scale would he of the 14th magnitude, and judged by John Ilerschcl would be -tied with stars of the J!is : 7 .:, = 6054 8.6 9.0 = 52> :>.! to !i- r > Magnitude = 21973. onil tin- '.'.") ina.u'iiitude the stars increase in number so much that it is no longer I ilc to observe them individually or to number them. The desire and the need to place upon our star maps the faintest stars, has in tho meantime led to the employment of photography for tin 1 purpose, and as a result we are now able to map out tho celestial spaces and to give therein \vhich approach the limit of visibility in our greatest telecopcs. The first experiments in this line attended by successful results were carried out at the Paris Observatory by the brothers Henri. With the aid of an object glass of 6-in. aperture, expressly constructed for this purpose, they were able to photograph several star clusters, in which stars even of the 12th and 13th magnitude became visible upon the plate. These results led to the construction of a larger instrument of 340 millimetres aperture and 3 to 4 metres focus. This was applied to a large ordinary telescope which served during the time of exposure to keep one and the same point of the heavens continually in the field. The result surpassed all expectation, for stars up to the 16th magnitude were successfully photographed stars which were so faint that it was impossible to sec them by the eye through the same telescope. Here, one might say, in the proper sense of tho word, was an astronomy of the invisible, and it must have been with a peculiar joy that the observers saw upon the photographic plate pictures of stars which since tho beginning of things had never been revealed to human eye. In order to photo- graph such faint stars long exposure was necessary, namely one hour and twenty minutes, while stars of the first magnitude gave forth their image in the 200th part of a second. Variable Stars. Certain fixed stars exhibit a periodical change in their brightness which in some cases occurs with great regularity, but in the majority of instances more or less irregularly. The first discovery of this variability was made by David Fabricius in the year 1 596 in tho case of the star o in the Whale. This star appeared on the 13th August of that year to be of the 3rd magnitude, whilst in the October following it was no longer visible. That this was a ease of variability was first recognised by Holwarda in the year 1636, and the star received, therefore, the name Miro, the wonderful. Since this time numerous variable stars have been discovered, the latest list, drawn up by C. Pickering, embracing somewhere about 200. According to the kind and manner of variability these stars have been divided into five classes. 1. The so-called new stars (Now) which burst out suddenly and vanish away slowly. 2. Stars of great variability within the space of several months. These stars vary by several magnitudes, being often visible in maximum to the naked eye, whilst in minimum they arc frequently not within the scope of powerful telescopes. 3. Stars of slight and irregular variability which have no recognisable fixed period. 4. Stars of fairly regular variability whose periods are of a few weeks only. 5. Stars whose variability is confined to a few hours, and which shine during long periods with a constant light. These are called variables of the Algol type, Algol having been the first discovered of the class. In the lists and upon the star maps the variables arc distinguished by the letter R, provided they had not already been indicated by Greek letters before they were found to be variable. In reference to the causes which bring about this variability there is great obscurity.* In the case of any star of the Algol type one is led to think of the periodical passage of a dark planet between the star and us, in other words to regard it as a partial eclipse of the star. Where the periods of variability are long and irregular the causes arc very obscure. As to the new stars (Novcp), the sudden outbursts and slow fading away of any one of these seems to indicate some kind of great catastrophe, probably a collision with another cosmical mass. Distances of the Fixed Stars. The distances of the fixed stars from our earth are without exception so considerable that up to the present it has been possible only in a few instances to obtain a substantial value for their parallax. From this it appears that even the nearest fixed star is still four billions of miles away, and one must conclude, on the ground of analogy, that the faintest stars which can be seen by the improved telescopes of to-day are many hundreds, or even thousands of billions of miles distant.f Double Stars. If one survey the heaven with a telescope one meets frequently twin stars which lie so near to each other that they can be separated only by a glass of a certain power. These arc called * In the Bakcrian Lecture delivered at the Royal Society, April 12th last, by J. Norman Lockyer, F.R.S., and afterwards published in Nature, a new theory is advanced to account for variability. Mr. Lockyer considers that " new stars " are produced by the collision of meteor swarms, and that the more or less regular variables arc owing to the periastron passage of one swarm through another (see Nature, May 2J, 1W8, p. 7!(). In this Lecture Mr. Lockyer endeavours to show that the heavenly bodies are all formed from meteoric dust, and that the differences between them are simply owing to the different degrees of condensation of the dust, and the conse- quently greater or fewer number of collisions of the particles ; the slight condensation and comparatively few collisions giving rise to the weak light of the fainter nebula;, while the closely condensed swarms show, through all their stages, bright nebulae, nebular stars, and real suns. Entron. I In the Thirteenth Annual Report of the Savilian Professor of Astronomy, read June 6th, 1888, Dr. Pritchard gives a very interesting account of his later operations for stellar parallax, by photographing small portions of the heavens. He is satisfied, not only witli the convenience of this method, but also with its unimpeachable accuracy. The following are the results obtained so far : 61i Cygni . . . 0-4289 0-0180 61 ! Cygni . . . 0-4353 0-0152 ^ Cassiopeia; . . 0-0356 0-0250 Polaris .... 0-052 0-0314 a. Cassiopeiee . . o' ; 072 d'-042* Cassiopeia; . . 0-187 0-039* y Cassiopeia; . . < 0-05 0-047* [EDIT.; " I). .ul, I,- Stan. Tlic bright! >t of tin' pair is called tin- primary,'' the otliiT iU "companion uently, !I..A. v, r, both star- illy bright. The place of the companion in relation to the primary 1 by distance ami angular poMti n. 1>> H meant merely the appai :ho companion from its primaiy. Tin- appearance of i, :i owing 1 > the two -.tars being in almost the same line in rcg.ir-l to the , \\liile their rc.il distance from each other may bo immensely great. :.- are, however, numcrc.il> instances in which tin il propinquity. In these cases the ani: 'ion v.iri' .11 manner a* to in -\\< ite a motion of revolution round a common I' ially tho>e male since the time of W. Herschel and F. W. Struve, have pi..\ei that many double or multiple stars possess a physical connection with each otht r. The angle of position is the angle which a line drawn from the companion to its primary forms \\ith the hitter's circle of Declination. The angle of position is calculated from north through east to south and west. i:ntiil>er i.f Double St usidorable, about 7,000 being known at the present time. There are a!> > triple, quadruple and quintuple stars, but their number is not large. The primary and companion are not infrequently of different colours ; white and blue, yellow and blue, and green and blue stars being found together. Except in a few cases, however, the.-e colours are only faintly visible, and it requires a certain amount of practice and a powerful ope to he able to distinguish them. Star Clusters. Groups of stars collected more or less closely together in a small space are called star- clusti rs. Some few star-clusters can be distinguished, though imperfectly, with the naked eye, as for instance, the Pleiades in Taurus and a cluster in Cancer, but generally they can be clearly through the telescope only. Indeed many of them appear misty and nebulous even in < of ordinary size, a powerful instrument being required to resolve them. Most star clusters seem to be globular in shape, with a strong condensation towards the centre. Frequently the btars in the centre of a cluster arc crowded so closely together that they seem a nebulous mass, around which the external stars are collected. The relative positions of the various stars in these star clusters have been decided by exact measurement in a few cases only ; but the recent strides that have been made in the application it photography to astronomical observations lead us to hope that we shall ere long be able to obtain records of their most minute detail.''. We shall thus by the comparison of photographs taken at intervals of sufficient time, arrive at valuable information with regard to the relative motions of the component stars of these clusters. Nebulae. Nebula- are among the most remarkable objects to be found in space, but the majority of them cannot be studied in detail except by the aid of the most powerful telescopes. At the present day upwards of 6,000 Nebula- are known to astronomers. John Herschel prepared a general catalogue containing 5079 Nebula- and Star clusters. For the sake of brevity the Nebula? arc usually distinguished by the numbers assigned to them in llerschel's catalogue, and this course has been followed in the present work, where the numbers are accompanied by tin General Catalogue). * Sec Editoriil Note p. ; 1. 10 Whilst most Nebulae cannot be clearly observed except with a powerful telescope, there are several hundreds, however, which may be studied on a clear night with an ordinary glass, if the weakest power be employed. Viewed in detail, it will be seen that their shapes are various ; some round or elliptical, some spindle-shaped, some like planetary disks (Planetary Nebula;}, others ring shaped (Annular Nebula;), others spiral (Spiral Nebula-), while many are quite irregular in outline. The Spectroscope shows that the Ncbulao are masses of incandescent gas* in which hydrogen and nitrogen play an important part. Possibly in these glowing masses we have before us the germs of future worlds, or it may be in some cases the disintegrated remains of former solar systems. Explanation of the Maps. The general maps in this atlas include that portion of the heavens which is visible in central Europe, and they cover as far as 33 South Declination. The stars are divided by a system of conventional signs into six classes of magnitude according- to their apparent brilliancy. The system of numbering adopted is, as a general rule, that of Bayer, by means of the small letters of the Greek and Latin alphabets. Such variable stars as are not given by Bayer, are marked, as is usual, by the capital letters of the Latin alphabet, beginning with R, the word var being added. A number of especially interesting variable stars, which at their maximum do not attain to the sixth magnitude, are also given. These' stars are distinguished by a small circle. Stars catalogued by Struve as Double Stars, if they have not been noted by Bayer, bear the number they possess in Struve's catalogue with the letter - prefixed ; all other numbers attached to stars are those of Flamstced's catalogue. Star clusters and Nebula} are distinguished by small circular groups of dots, and the accompanying number is that assigned to each in Herschcl's General Catalogue. Lastly, the boundary lines of the various constellations are taken from Argelander. Description Of the more interesting Fixed Stars, Star Clusters, and Nebulae contained in the Maps of this Atlas. The following list, in which the various stars, etc., are arranged in order of Right Ascension, gives a fairly complete account of what is scientifically known at the present time of each object upon the Maps. To find in this list any star .or nebula contained in the Maps, it is only necessary to take the approximate Right Ascension of the object from the Map and also its number or letter. These will indicate, without trouble, the object in the descriptive Catalogue. The Right Ascension and Declination here given arc those for the year 1880, North Declination is shown by the sign +, South Declination by the sign - The Nautical Almanack furnishes the annual variation in Right Ascension of the principal stars, and from this the Right Ascension for any year can be readily calculated. * But see Note p. 8. [Ecrr.] Qk Qm 0" 17" O h IS-" 0" IS" 1 0" 19- + Os _"., -f- 14 31' + 8 9' + 55 8' + :57 55' 10 0' + 63 24' 0" 23- + 59 10' 0" 25 60 0" + 6 18' Cassiopeia. This star, > mag., has at 5' distance a faint com- panion of 11 mag. Burnham, who dliM-rved this star with the 18-inch refractor at Chicago, states that he aw more than a dozen very faint stars ncaier to the primary than this companion. (See nole j>. 8.) 7 Pegasi. 2.5 mag., with two faint companions, 11 an 0" 43- 49-n p 63- O h 58- 0" 59" + -1" IT + til 3 8' - 26 1 1 ' + 27 4' + 18 32' + 60 4' + 37 51' + 81 14' + 44' + 20 50' i .1^ tin- en. I nf Au,'ii-t, INS:,, was probably not owing to t ruption of inc m le^vnt gas, lint r.itlu r to other circumstances. Of the various posMble theories, that which attributes the phenomenon to version of cosmic motion into heat and light seems the most ,l>lt>. 117. Companion of the great Nebula in Andromeda. Viewed through a t.-lesri.pp of low power this has the appearance of a nebulous star. In reality it is a star-cluster, but a very powerful instrument is re-quired to distinguish the separate star<. 120, Star Cluster in Cassiopeia, discovered by Caroline Herschel. The stars are scattered somewhat coarsely over a space of from 15' to 20' in diameter, and range from '> to 10 mag. 138, Nebula in Cetus was discovered by Caroline Herschel, Sept. 23, 1783; it is long, narrow and bright, and is preceded by a star of 9 magnitude. n Cassiopeiae, a yellowish star, 4 mag., with a purple coloured companion of 7.5 mag., discovered by Herschel, 17 Aug., 1779. The distance of the companion in 1882 was 5.2"; the angle of position 165.7; the time of revolution round its primary as calculated by Duner is 176 years : the parallax, according to Clausen, is 0.371", indicating a distance from the earth of eleven billion miles. 65, Piscium, a double star, discovered by Herschel in 1783. 15oth stars arc of 6 mag., and their relative position does not seem to vary. Distance 4.3". 66, Piscium. Recognised as a double star at Fulkowa, the primary being 6 mag., the companion 7 mag. Miidler, in 1X43, found the distance to be 0.6". Dembowski, in 1885, could only perceive a single star of elongated form. Burnham, in 1880, calculated the companion's distance to be 0.4". The velocity of revolution of the companion is very high. -/ Cassiopeiae. This star, 3 mag., has a companion of 9.5 mag., at distance 432", angle of position 327. There are nearly a dozen very minute stars nearer to the primary, but they can only be seen with a telescope of the highest power. (See note p. 8.) /A Andromedae, a double star of 4 mag. and 11 mag., first recognised as such by John Herschel. The distance of the companion is 49" ; its angle of position 110.5"; only visible with a very powerful telescope. V Cephei. a variable star of the Algol type, discovered by Ceraski in 1880. The star is generally 7 mag., but diminishes to 9.5 mag. in periods of 2.5 days. With a powerful telescope, two faint companions, of 11.5 and 13 mag. respectively, may be seen. 26, Ceti, a double star. Primary 6 mag., companion 9 mag. ; distance 16" ; angle of position 253. The position of the companion does not seem to vary. V Piscium, a double star, consisting of two white coloured stars of 5 mag. ; distance 30". They can be easily " divided " with the help of a pocket telescope. No change has been observed in their relative positions during the last 130 years. 14 Itight Ascension 1880. Declination 1880. ^ Itight Ascension 1880. Declination 1880, l h O' n + 4 16' l h 5 m + 30 47' l h 7 m + 23 57' I 1 ' gm + 6 56' l h u- + 71 59' I'- 12 m + 58 9' ll 14 m 1 8' l h 15 m + 88 40' 1" 17* + 67 30' 15"' "4*' 1" 19" + 8 55' 1" 24 m + 2 16' 1" 25 m + 60 2' l h 25" 7 29' l h 27 m + 30 4' 77, Piscium, a beautiful double star ; primary 6 mag., companion 6.8 mag. ; distance 32.8". No change has been observed in their position. y Piscium, recognised as a double star at Pulkowa. Primary 5 mag., companion 10 mag. ; distance 2.5". <$ Piscium, 6 mag., with a remarkably faint companion at 7.6" distance ; angle of position 22. Piazzi calls it a double star, but it is quite evident that his telescope would not have enabled him to see it had it been as faint then as it is at the present day. Piscium, a beautiful double star, easy to observe, the primary and companion being 5 mag. and 6 mag. respectively. The distance and angle of position have not undergone any essential alteration since Struve measured them in 1821, the former being 24", the latter 64. S Cassiopeiae, a variable star of long period, discovered by Argelander in 1861. At maximum it is 6.7 mag., though it is often less than 8 mag. ; at minimum it is under 13 mag., or it becomes quite invisible. The period is 615 days. 256, Star Cluster in Cassiopeiae, a large cluster, rich in stars and nearly round in shape. The stars range from 7 to 10 mag. Discovered by Herschel, 18 Sept., 1787. There is a double star in the cluster of 8 and 9 mag. 42, Ceti, a double star, 6 and 7 mag. Distance only 1.3". a. Ursae Minoris, the Pole Star. 2 mag. ; gives a yellowish light. It has a companion of 9 mag., distance 18.5", which was discovered by Herschel, 17 Aug., 1779. According to Peters' calculation, its parallax is 0.08", indicating a distance from the earth of 40 billions of miles, but this result is very untrustworthy. (Sec note p. 8.) ^ Cassiopeiae, a triple star. Herschel saw only the primary 4.4 mag. and a companion 8.5 mag., at distance 30". Struve, in 1831, was the first to divide this latter into two separate stars of 8.9 and 9.5 mag. respectively, distance 3". 307, Nebula in Pisces, a bright and fairly large nebula, with an increase of brilliancy towards the centre ; 4 stars near to it. R Piscium, a variable star of yellowish colour with a long period, discovered by Hind in 1851. At maximum it is from 7|- to 83 mag., at minimum it is as low as 12 J mag. ; it gains more quickly in brilliancy than it loses, and the period is 345 days. 341, Star Cluster in Cassiopeia. This is not a very large cluster, but it contains several stars of 6 to 9 mag., among others a red-coloured star of 8 mag., and a double star, primary 6 mag., companion 10 mag., distance 13.6". 3 i2, Nebula in Cetus, faint and rather small, much brighter towards the centre. Discovered by Herschel, 10 Sept., 1785. 352, Nebula in Triangulum. Discovered first by Messier; very- large and faint, but easy to observe in consequence of its extent. With a seven-foot telescope Herschel saw it dimly, and best with a low power. With a ten-foot reflector, the most brilliant part was resolved into separate stars, and when a still stronger instrument was employed, almost the whole nebula was resolved into stars, which seemed to Herschel nothing more than 15 lliKlit A -- !> '!' 1" 38- 4G- l h l k 47' l k 50- l h 51- l k 53- 1" 56- 80 + I- r 10' 59' + 60 +60 - n - 38' 551 17' 84' + 18 42' + 37 23 r 2= 11' ..illest imnu'inable points. Tliis nebula is nearly '(<' in extent. Lord Kosse observed in it nodes i.f li^lit, and the well-known njiirul arr..ni:< iu< nt shown by his in several similar objects. 1, Nebula in Cetus. ! i i<\ II, .-,! 1 :i Dae., 17:ts. This i i- fail ly brilliant, with a brighter nucleus, and is (I* long by 1 Abroad. .', Nebula in Pisces, discovered by Mi'chain in Sept., 17SO, and de>eribed by him as a starl< -> n, -bulu of fairly large dimensions, but very dull and difficult to observe. Messier confirmed this view. Sir John liel, on the other hand, describes it as a globular star cluster, capable of bcinjj clearly resolved into separate stars, whose brilliancy iiu gradually at tirst, and then suddenly at the centre. Lord Rosse, with the help of his great tclevope, dettrti d a spiral arrangement of the stars. \ ^'el saw it in October, 18G7, with the 8-inch refractor at Li-ij>-ic, a- a f.iint, globular star cluster, 3' in diameter, the star* being a little more densely collected to wards the centre. , Nebula in Perseus, the preceding of two nebula- which stand at a di-taoce of 2' from one another. Me'chain saw it first, 5 Sept., 1780, and described it as a small, faint, starless nebula. Messier believed it to consist of small stars intermingled with nebula ; this, however, was a mistake. The nebula is fairly brilliant. 392, Star Cluster in Cassiopeia, a beautiful object, 15' in diameter, rieh in stars, ranging from brilliant to faint minute points ; a double star, primary 9 mag., companion 10 mag., distance 8", is to be seen in the cluster ; also a red coloured star 8 mag. in the southern portion. X Ceti, 5 mag., at distance 3' stands a star of 7 mag. .', Nebula in Perseus. In this Hcrschel, 4 Sept., 1784, discovered four separate starry nebulae, three standing in a line, the fourth at right angles to them ; that at the angle is much the largest. D'Arvest observed these nebula; a second time. According to Lord Rosse, there are three others near them, but Dreyer thinks these to be identical with those observed by Herschel. y Arietis, a beautiful double star, primary 4.2 mag , companion 4.4 mag., observed by Hooke in 1044, and described by him as remarkable in the highest degree. It can be divided with the help of a small telescope : Distance 8", angle of position 179. There is besides, at distance 4', angle of position 84, a faint star, first seen by J. Herschel and South in 1 v.': 1 .. liurnham discovered that this star is also double, but its division is extremely difficult. Between it and y he saw another very faint star. 1 >!, Star Cluster in Andromeda, MO' in diameter, containing numerous, brilliant, coarsely scattered stars, visible to a keen eye without the aid of a telescopes a nebulous star. Herschel first observed it 21 Sept., 1786'. >. Arietis, a double star, primary o mag., companion 8 mag., distance 38", can be divided by a good pocket-telescope. 1 !!);, Arietis, a quadruple star, primary mag., companions 9, 10 and 12 mag. respectively. The brightest companion is at distance 8* I", an-le of position i a. Piscium, a beautiful double star, primary (which is green in colour) 2.8 mag., companion (which is blue in colour) 3.9 mag., distance 3". The movement of the companion is very slow. 16 Kight Ascension 1880. Declination 1880. l h 56" l h 5T m 2 h 3 m 2" 11" 13= + 32 42' 41 + 25 22' + 29 44' + 24 30' + 56 36' 3 31' + 41 47' Trianguli. This star 5.5 mag. has panion, distance 4", angle of position 116.8. instrument to distinguish this companion. an exceedingly faint corn- It requires a very powerful 7 Andromedae, a gold-coloured star, 3 mag., with a blue companion, 6 mag. Distance 10". The colour of both stars is very intense, and they are easily recognised as a double star. In 1842, however, Struve discovered that the companion is itself a double star, consisting of two separate stars of 6.7 mag. and 8.5 mag. respectively, distance only 0.5". At present this distance is still less (0.3"), and a refractor of great power is required to divide the companion. 14, Arietis, a triple star ; the primary 5.6 mag., has at distance 93", angle of position 36.4, a companion 8.9 mag., and a second at distance 106", angle of position, 278.5. Herschel had measured the distance of the nearer companion in 1783. 6, Trianguli, a double star, primary (which is yellow) 5 mag., com- panion (whicli is blue) 6 mag., distance 3.8". Discovered by Herschel in 1781. H Arietis, a variable orange-coloured star, discovered at Bonn in 1857, and since then frequently observed. The period is 186.2 days. At maximum the star is 7.6 to 8.5 mag. ; at minimum 12 mag. and under. When approaching its maximum the increase in brilliancy is often fur weeks together very slow. 512, 521, Two large Star Clusters in Perseus, being one of the most magnificent objects of its kind in the heavens. The larger of the two ^ is 30' in diameter, and consists of a large number of stars ranging in magnitude from 6.5 to 13 and 14. Vogcl and Lament have measured this cluster with the micrometer. The southern cluster h is smaller, being 15' in diameter and less rich. The stars appear condensed towards the centre. Photo graphs have been taken of both clusters by the brothers Henry, at Paris, and Dr. Lohse at Potsdam. o Ceti (Mira), a variable star with long period, and the first whose variability was detected. D. Fabricius observed it early on the morning of 12 August, 1596, as somewhat brighter than a. Arietis. In October it had disappeared. He saw it again in February and March, 1609 ; then Holwarda observed it in 1638, and recognised its periodical variability. According to Argelander's calculations the period is 331 J days, but it is very irregular, and the difference of period is sometimes as much as 25 days. Its magnitude at maximum also varies greatly, being sometimes as much as 2 and often not more than 5. At minimum it is 9 mag., being the same magnitude as that of a companion at distance 2', angle of position 85. The star is of a deep red colour, and gives an interesting spectrum. 527, Nebula in Andromeda, fairly brilliant, 15' long by 3' broad, with a dark cleft in the middle. Discovered by Miss Herschel in August, 1783. According to John Ilerschel it is a vast, flat, nebular ring, which is seen obliquely by us. 17 U|M \ t>" 19" _' -jo-' -.I1..D 1MO. 2" 34- 2 h 35" 2" 37- 2" 37- 2" 40- 2" 42- 2" 42- 2 b 43- 2 k 43- + ;> 52' 43' 1 41 + 38 33' + 26 33' + 42 17' 31' + 2 44' 8 4' + 55 24' + 17 2' + 1G 58' + 26 45' . Cassiopeiae il v?tij). A triple star, discovered by W. Herschel. The primary 1.2 mair. ha- nm- companion 7.1 inn^., di.-tamv 1.5", and a second companion 8.1 rang., distance 8.9". The nearer companion is not easily distinguished. /.' Ceti, u variable stur, first recognised as such by Argclunder, 18C6. At maximum it reaches sometimes 7 mag., at minimum, 13 mag. Period, 1C,7 days. ".II, Planetary Nebula in Cetus, rather faint, with a diameter of from 3' to 4' ; there arc several stars round it. Discovered by W. Hcrschcl. G Jan., 1785. v Ceti (2 281). A double star, 1.5 mag., with a faint companion of 9.5 mag. Distance, 7.7" ; angle of position, s:j . 30, Arietis. A beautiful double star, not difficult to observe. Its primary is G mag. ; companion, 6.5 mag. ; di-t unv, :JH.G". Both stars are white in colour. , No change in position has been noticed since the time of Bradley. 1T& , Nebula in Andromeda. Faint, 10' in length, spindle-shaped, and surrounded by several faint star?. 33, Arietis (2 289). A double star, first seen by Herschel 27 Sept., 1779. Primary, 5.8 mag. ; companion, 8.7 mag. ; distance, 28.5" ; angle of position, '559.4. No change in position has been observed. 584, Star Cluster in Perseus, having a diameter of 15'; discovered by Messier. The stars range from 9 to 1 1 mag., and are coarsely distrib- uted ; with a small telescope upwards of 100 stars can be distinguished. 600, Nebula in Cetus, first discovered by Mechain in 1780. It is small, fairly brilliant, and is preceded by one star, and followed by two others. According to Lord Rosse the nebula shows spiral arrangement. 7 Ceti (2 '2W)- A star of yellow colour, 3.5 mag., with a companion li.'i mag.; distance, 2.4"; angle of position, 2~~ G04, Nebula in Cetus. Faint, oval in shape, with a slight increase in brilliancy towards the centre ; apparently a star cluster situated at an immeasurable distance. f, Persei (2 307). 4 mag., with a companion (of bluei.-h colour), 8 mag. ; distance, 28". There arc also several very faint stars near it. T Arietis. A variable star, discovered by Auwers 1870. At maximum, 8 mag. ; at minimum, 9.5 to 10 mag. Period, 324 days. Of a reddUh colour. * Arietis (.2 311). Triple; magnitudes, 5.5, 8, and 10; recognised as triple by Hcrschol in 1779. The nearest companion is at distance 3.3" : angle of position, 121 '. The faint outer companion at distance 25"; angle of position, 110. 41, Arietis. The primary is 4 mag. Herschel saw a f.iint companion in 1779 at distance 126" (angle of position, as calculated by Burnham in 1879, v.':;n >, then in 1782 a second at distance 34", angle of portion . Finally, Struvc, at J'ulkowa, discovered yet another very faint companion (11 mag.) at distance 16". The distance of this latter, as calcu- feted bv Burnham in 1879, was 21", angle of position 266. 18 High* Ascension 1880. Declination 1880. 52 2 h 58 m 3 h O 3 h 7 m 3 h 7 m 3 h 7 m 3 h 9 m 3 h 16" 3 h 19"' 3 h 21 3 h 21 m ;f 22 m + 20 f ./ + 38 + 24 52' 23' 47' + 40 30' 1 + 46 29 + 65 + 40 39' 47' 28' 13' 2' -15 49' + 59 + 55 -21 31' 2' 46' + 35 15' E Arietis (S 333), a double star, primary 4.5 mag., companion 6 mag., distance 1.5". As conjectured by Struve, the primary probably varies from 4.5 mag. to 0.5 mag., and the companion also seemed to him variable. Engelmann supports this theory. Persei. This orange-coloured star was first recognised as variable in 1854, by J. Schmidt. The period is seemingly quite irregular, and the brightness at maximum varies considerably. 52, Arietis (S 346), triple, but cannot be clearly divided except by a very powerful telescope. The primary, 5.5 mag., has one companion at distance 0.7"; the outer companion, which is very faint (11 mag.), is at distance 5". /3 Persei (Algol), one of the most interesting variable stars. The variation was discovered as far back as 1767 or 1769, by Montanari, but Goodricke, in 1782, was the first to recognise its true nature. According to his account, the star remains invariable for 24 days, and then decreases in 4^ hours to 3.7 mag., and during the next 4 \ hours it increases to 2.2 mag. The period is 2 days 20h. 48m. 53.4s. This is not constant, there being a difference of a few seconds in the course of the year. 94, Ceti, 5.5 mag., has a very faint companion at distance 5.7", which it needs an extremely powerful telescope to distinguish. 658, Star Cluster in Perseus. A beautiful cluster 8' in diameter, very rich in stars of 10 mag. and under. Discovered by W. Ilerschel, 27 Dec., 1786. 12, Eridani, a star of 3.5 mag., with a companion 7.5 mag., distance 2.4", angle of position 316. 52, Camelopardalis. A star of 6.5 mag., with a companion 7 mag., at a distance of only 0.5". A very difficult object. 2 369, Double Star in Perseus. The primary, 7 mag., is of a yellowish-white colour ; the companion, 8 mag., is blucish- white. The distance, 3.5", seems to be increasing, but very gradually. 692, Nebula in Eridanus, rather faint, large, irregularly round in shape, gradually increasing in brilliancy towards the centre. A star, 7 mag., precedes the nebula. 2 385, Camelopardalis. The primary, 5 mag., is yellow in colour ; the companion, 9 mag., distance 2.4", angle of position 161, is white. 390, Camelopardalis. Primary 5 mag., greenish- white in colour, with a faint companion 9.5 mag., distance 15", angle of position 160. 709, Nebula in Eridanus, discovered by W. Ilerschel ; fairly bright, elongated, but small, with a nucleus, followed southwards by a small and very faint nebula. 11 Persei, a variable star. At maximum it sometimes reaches as much as 8 mag., and at minimum becomes frequently less than 13 mug. Period, 208.5 days. According to Schoeufeld it remains at 1'-' m:ig. anil under for two months' time. ; } h ._>;,, 3 h 27- 3 k 38- B 63' 21' 4.94 4' + o IV + 1' 45' + 33 35' :l j 20 3 h 40- 3 h 40- 3" 42" 3 fc 42- 3 h 47- 3 h 48- 23 44' + 52 18' + 10 46' + 23 41' + 31 32 3 19 717, Star Cluster in Perseus, l.u-.- i IV in diameter), contains about JO stars coarsely scutti'inl. I 1 rand !> HtMM-hfl, 2S Dec., 17!''.'. 3!), Camelopardalis, a star (i 5 mag., with a faint companion, 8 mag., distance 20.3 ". 7,Tauri (1 11J , il mag., with a companion 10 mag., distance 'J :ilicd liy \V. Hi T-i'hfl, South and John Herschcl. !ut Stru\r, with tin- Doqut lUTractor, divided the primary into two stars if almost equal brilliancy, at a distance of only 0.0" from one another. 2 4'J,', Eridani, a double star, primary G.5 mag., companion 8 mag., distance 6.5". The primary is yellow, the companion blueish. -l^n, Tauri. Triple G.5, 9 and 9.5 mag. The first companion is at dista angle of position '>'> . The second at distance 38", angle of position 301. The primary is yellowish. o Panel (- 431) a star 5 mag., with a faint companion 9.5 mag., distance _' 7G8, Nebula in the Pleiades, discovered by Tcmpcl, 19 Oct., 1859. An extremely faint nebula, situated near the star Merope. The brothers 1 1 . i.ry have discovered, by the aid of photography, another very faint nebula which seems to proceed from the star M.iia, but this can only be seen with a most powerful telescope. (Cf. Sheet xiii.) * n in the Pleiades, quadruple and a very beautiful object even as seen with a small telescope. The primary 3.5 mag. has one companion 6.5 mag. at distance 118", angle of position 289, a second 7 mag., distance 116", angle of position ''. 14 3 . Lastly there is a small star, 9 mag., at distance 115" from the companion of G.5 mag., angle of position 303; n is also known by the name Alcyone. (See Sheet xiii.) 77"), Star Cluster in Perseus, small, consisting of about 30 stars, ranging in magnitude from 11 to 13, besides one star of 10 mag. The whole is from 2' to 3' in diameter. 30, Tauri (i 452) primary 5 mag., companion 9 mag., distance 9". 1 453, (Atlas) in the Pleiades, a star 4 mag. In 1827 and 1830 Struvc fancied that he could distinguish a companion to this star of 8 mag., distance O.b". It was, however, never seen afterwards by Struvc or any other observer. Even liurnham always found the star to be single and perfectly round. ^ Persei (2 4G4). Quintuple. The primary 2.7 mag. has, at distance 13" a companion 9.5 mag., at distance 90" another of 10 mag, and a third 10 mag., at distance 122". There is besides a faint star of 12 mag., distance 3-3", angle of position 28(i . 32, Eridani (i 47u), primary 5 mag., yellowish, with a companion 6 mag., distance G.7", of a blueish colour. Discovered by W. Herschcl in 1781. *Thc fuller traces of ni-biilo*itv wliirli. in 1>-8.">. n]il nminl Main and Merop* 1 , are now shown on more wnsitive plates '!>- 10- 7 .,,, ].J,, + " 4" l:- 4' 4" 15- + -'5 4 h 15'" + !'' IV 4 h 17 n, 4" 18- + :\:\ + 22 59' 1' 4 h 21 4 h 22 + 30 + 9 6' 54' 4" 22- + 15 42' 4 k 23- + ,W 39' 4 fc 23- + :K) 44' 4" 23- + 15 23' 4" 25- + 42 Of 4 h 29" -f 16 10' 4 fc 29- + 9 r,.v o* Eridani 618). A < ' ni:i., with a companion 9 mng., which i . ul>lf star. The Ooapurioa i< at distance 8'2", and tho two stars which com JUKI- it are at distance 3.f>" from one another. Dis- covered by W. i i in 1*7:5, with the help of a G-inch reflector. i , Star Cluster in Perseus, the stars arc coarsely scattered, fairly numerous, and many of them are of fair brilliancy. Discovered by W. Bftnebd, 28 Dec., 1790. $ Tauri, a double star, primary (which is reddish) 5.5 mag., com- panion 8.5 mag. Distance (in 1S7 : '. ">!", angle of position 2I> . X Tauri (2 528), a star 6 mag., with companion 8 mag., distance '/' Tauri, ;i variable star of irregular period, discovered by Hind, 1 S <>1. It is preceded l m by a very remarkable variable nebula (Q.C. 839). This latter had been frequently seen since 1854, but in 18(51 d'Arrest could not find any trace of it even with the great refractor at Copenhagen. According to Argelander, the star T was of 9.4 mag. in 1S52 ; but since 18C9 it has always been less than 11 mag.; its brilliancy has seem- ingly decreased at the same rate as that of the nebula, a noteworthy fact, since it seems to indicate some sort of relation between tho two phenomena. 1 ">:!3, Persei, primary 0.5 mag., companion 7 mag., distance ID". * Tauri, two stars of 5 mag. and G mag. respectively, at distance W!" from one another ; between the two there is a minute double star of 11.2 and ll.G mag., distance 5". 2 548, Tauri, a double star of 6 and 8 mag., distance 14". A' Tauri. First recognised as a variable star by Hind in 1819. It is of a deep red. At maximum it fluctuates between 7.4 and 9 mag. ; at minimum it is less than 13 mag. Period of variability nearly 325J days. 6' Tauri, two stars of 4 and 4.3 mag., distance 337". Can be recog- nised as a double star with the naked eye. In spite of their great apparent distance, the stars seem to stand in a physical relation to each other. 1, Camelopardalis (2 550), a star of 6.1 mag., with a companion G.2 mag., at distance 10.4". 2 552, Persei, a double star, G mag. and 6.5 mag., distance 8.9". Both stars are white. 80, Tauri (2 554), 6.5 mag. A very close double star, the companion 7.5 mag., being, in 1879, only at distance 0.6", and this is continually decreasing. MI Persei. Two stars of from G mag to 7 mag., at distance 114'.'. In Herschel's time these stars seem to have been much fainter. Tauri (Aldebaran), a red star 1 mag., with a very interesting spectrum (Vogel, Class I la). It has a companion 10 mag., at distance 113". Burnham discovered a second companion at distance 30.4", angle of position 109; but it is so faint as to be visible only in a most powerful telesr. 88, Tauri, 5 mag., with companion 8 mag., distance 70". Discovered by W. Herschcl, 24 Sept., 1780. 22 Itight Ascension 1880. Declination 1880. 4 h 30 m 4 h 4 h 4 h 4 h 4 h 35 38 4 h 45 4 h 48 m 4 h 50 m 4 h 52 m 4 h 53 m 4 h 54 m 54 m 59 m O m -f 53 15' + 15 41' + 22 44' 9 1' -f 10 43' f 17 20' + 53 33' 5 22' 37 43' 7 57' + 53 41' + 43 39' 14 59' + 3 26' + 1 1' + 37 12' 2, Camelopardalis (2 506). 6 mag., yellowish, with a blueish com- panion, 7.4 mag. ; distance (according to Engclmann, 1883), 1.9" ; angle of position, 291.9. a Tauri. Two stars of 4.6 and 5.5 mag. ; distance, 429" ; can be divided by the naked eye. T Tauri. 4.5 mag., with an easily distinguished companion, 7 mag., at distance 63". Discovered by Chr. Mayer. 55, Eridani (2 590). A star of 6.2 mag., with a companion, 7 mag. ; distance, 9". The primary is yellowish, the companion white in colour. Found to be double by "W. Herschel in 1783. 905, Star Cluster in Orion, consisting of 18 stars of from 8 to 11 mag. Somewhat scattered. Vogel has measured their relative positions with the micrometer. V Tauri. A variable star, first recognised as such by Auwers, 1870. The star is reddish. At maximum it reaches 8.3 mag. ; at minimum it diminishes to 13 mag. Period, 168.6 days. 7, Camelopardalis (2 610). A star of 5 mag., with a very faint companion (11.3 mag.), at distance 25". Dembowski, in 1864, discovered that the primary was itself a double star, having a companion of 8 mag. at distance 1.2". b Eridani, 6 mag., with companion 8 mag., distance 64". 4, Aurigae (2 616). A star 5.5 mag., giving a greenish light, with a companion 7 mag., distance 6". First recognised as a double star by W. Herschel, 30 Oct. 1779. It Orionis. A variable star, of a deep red colour, discovered by Hind in 1848. At maximum it reaches almost 9 mag., at minimum it is less than 13. Period, 379 days. According to Schoenfeld the increase in brilliancy from 10 mag. upwards occupies 70 days ; the decrease from maximum to 10 mag., 105 days. 940, Star Cluster in Camelopardalis, fairly large and conspicuous. The stars are of various magnitudes, and are closer together towards the centre. e Aurigae. Recognised as variable by Schmidt and Heis. The star is 3 mag., but has been seen at times as a star of 4.5 mag. The variations of brilliancy are, however, very irregular, and are often for a long time imperceptible. li Leporis. A variable star of a bright red colour, called a "crimson star " by Hind. Schmidt, in 1855, was the first to recognise it as variable. The period is about 438 days, but seems to be very irregular. At maximum the star is 6 to 7, at minimum 8.5 mag. It has a remarkable spectrum. 2 627, Orionis, 6.5 mag., with a companion of nearly 7 mag., at distance 21". This latter has not undergone any perceptible change since 1831. 96 B., Orionis. A remarkable red-coloured star, estimated by Lalande and Bessel as of 7 mag., but by Birmingham, in 1871, as of 6 mag. The red tint is also probably slightly variable. 996, Star Cluster in Auriga. This is really not a cluster, but rather a rich field of stars. Herschel first saw it 17 Jan., 1787. The most brilliant stars contained in it are of 7.5 mag., the faintest J.1.5 mag. 23 \% 1MO. .-- 6" 1" 5" 1" 5" " o h 3 5" 3- 5" 5" 8- 5" 8- 5* 8- 3 f ^ I -I ) 81' 52' -V + 16 32' + + -' 53' - 12 1' 53 27' 52' + 32 33' 13 5' 20' 100"), Nebula in Orion, fairly brilliant, 3' in diameter, und gradually fading towards tin- i'd<,vs. It forms a triangle with two stars, 10 mag. and I 1 ,' lua.:. iv-;i ( tivoly. Discovered by HiTsehcl, '2 Jan., 17- i Orionis. A star of G mag., with a companion 7 mag., at dist.. 1.1", angle of position & 1 '' l">, Anrigae. A double star, primary G.o mag., companion 8 mag., distance 12", angle of jiosition -' 1 t'l'll. Camelopardalis. A star of !.." mag., with a companion 8 mag. In 1834 the distance was 31..V, but in 1880 it was only 20"; angle of position 60. I" ; !<), Star Cluster in Taurus, 20' to 25' in diameter, rich and fairly crowded with stars ranging from 11 mag. to 11 mag. Discovered by Hfisrhrl, in Feb., 17SI. 2 G"'J, Orionis. A double star, primary (5.5 mag., companion 8 mag., Ji-tance only 1.7", angle of position (Struve, 1830) 184. ? Orionis t- ;.>!). A yellow star, 4.7 mag., with a companion mag., of a blueish white ; distance 7". No change has been observed in the position of the companion since Herschcl's time. i Leporis 1 (>-~>5). A greenish star, "> mag., with a faint companion 1".") mag; distance 12.8". This distance does not seem to vary. The angle of position, 337, also seems to be nearly invariable. R Aurigae. A variable star, first recognised as such at Bonn Observatory in 1862. At maximum it reaches G.o to 7. -3 mag., at minimum it is almost 13. Period 465 days. The changes in brilliancy are sometimes very peculiar. a. Aurigae (Capella). A white star, 1 mag., with companion 9 mag ; distanct 1 '''. angle of position 146.2 (discovered by Herschcl). Burnham found two other very faint companions, magnitude 12 and 13 mag., distance 78" and 126", angle of position 317 and is ; n sj,, rtivilv . Struve (in 1838) conjectured that Capella had become more brilliant than formerly, apd that it was at one time fainter than Vega. J. Herschel supported this theory. 14, Aurigae (2 652), triple. The primary, 5.5 mag., has a companion 7 mag., at distance 14. o". This was first seen by W. Herschel, 24 Sept., 1780. Struve, in 18:50, discovered another very faint companion (11 mag.) at distance 12.G", angle of position 342 . x Leporis (2 661). A double star, primary 5, companion 8 mag., distance 2.5". According to Struve, the primary is yellowish, the companion blueMi. f. Orionis (Rigel) (2 668). A brilliant star, 1 mag., with a companion 8 mag., distance !i.(l". Discovered by W. Herschel, and a very beautiful object in a powerful telescope. The companion, as remarked by Burnham in 1 S 71, is itself a double star, but it is such a difficult object that Burnham hiiiiM-lf, with the 18-inch refractor at Chicago, only at times succeeded in " dividing " it. Other observers have so far been unable to do so. There is yet another very faint star at distance 44", angle of position 1.5. According to Scidcl, ft is in a slight degree variable. 24 Kight Ascension 1880. Declination 1880. 5 h 11 5 h 5" 17 m L/ 5 h 18 m 18 m lym 20'" + 20 0' + 39 59' + 39 13' + 46 51' 58' + 3 26' + 17 l(i' -24 54' + 33 17' 2 31' + 6 14' 24 38' + 35 3 13' + 2 59' + 35 47' 674, Tauri, a star of 6.5 mag., with a companion 9 mag., distance 10.5", angle of position 147.3. X Aurigae. 5 mag., with a companion 9 mag., distance 121". Burn- ham found yet another very faint star at distance 40", angle of position 198. 1067, Star Cluster in Auriga, a beautiful group of stars slightly denser towards the centre. A star of 7 mag. outshines all the others. Discovered by Ilerschel, 18 Oct., 1786. 2 681, Aurigae, a double star, primary 6.5 mag., companion 9 mag., distance 23.2", angle of position 180.8. T Orionis. This star, 4 mag., has three very faint companions. Burn- ham gives the following measurements : A B Distance 36.2" Angle of position 249.1. AC 36.1" 60.0. Bb 4.0" 50.6. It was Burnham who discovered that B is a double star : B is 10.5 mag., C 11 mag. m Orionis (2 696), a greenish-white star 5.5 mag., with a companion (white) 7 mag., distance 31.7", angle of position 28.1. No change of position has, as yet, been observed. Ill, Tauri, a star of 5.5 mag., with a companion 8 mag., distance 75", angle of position 271. Ilerschel had already made the measurements. Triple star in Lepus. The primary is G mag., the nearer companion which is at distance 3.5", is 9 mag., the farther companion, which is at distance 59", is 8.5 mag. 1101, Star Cluster in Auriga fairly large, and rich in stars, slightly denser towards the centre. f> Orionis, 3.5 mag., with a companion 5 mag., at distance 110". Dawes, in 1848, discovered that the primary was itself a double star, having a companion of 5.5 mag. at distance 1". J It requires a very strong instrument to " divide " this star. 7 Orionis, a star of 2 mag., supposed by J. Herschel to be slightly variable. Gould, too, finds slight variations, but only of about ^ mag. 1112, Star Cluster in Lepus, a splendid globular cluster discovered by Mechain, and which Messier described as a starless nebula with a brilliant centre. Ilerschel was the first to resolve the nebula into stars. 1114, Star Cluster in Auriga, a somewhat crowded circular cluster, 4' in diameter, consisting of small stars ranging in magnitude from 9 to 12. Discovered by W. Ilerschel, 17 Jan., 1787. vj/ 3 Orionis, a star of 5.5 mag., with a very faint companion of 11 mag., distance 2.9", angle of position 322. 1119, Star Cluster in Auriga, a beautiful object, about 10' in diameter. Discovered by Messier. A brilliant star may be observed in the centre. The stars are of unequal brilliancy. Its form, according to Messier, is quadratic. The cluster is not at all nebulous if examined with a power- ful telescope. 1MO. DoclinkU^n 1UO. 5" 22" 6" 23- + 25 3' 20' 51' 6" 23- 5 h 24 5" 24- 5 h 25- 6 k 25- 6 h 26- 5" 27- 6 k 28- 1 11' + 5 51' + 34 9' + 3 12' + 16 59' 23' 21 56' 17 55' + 34 4' 118, Tauri (2 7l, Star Cluster in Auriga, discovered by Messier, and a splendid object. Seen with a pocket - telescope, it looks like a nebulous star. Messier says that the stars are very crowded, and slightly mingled with nebula. They are of 10 mag. and under. Over 500 may be seen with a powerful telescope. Diameter of the whole 24'. 810, Orionis. A double star, G.5 and 8.5 mag. Distance 4.2", angle of position, according to Struve (1830), 289. 1310, Star Cluster in Orion, 7' to 8' in diameter. The stars are, however, small and somewhat crowded. a. Orionis (Betelgeux), a brilliant red star, 1 mag., which (as discovered by W. Herschel) has a companion of 10 mag. at distance 161". Burnham saw, besides this, several much fainter stars nearer to a. Betelgeux is variable, as discovered by J. Herschel in 1836, but the period of variability teems to be very irregular. The star has an interesting spectrum which has been carefully studied by Huggins. 9 Aurigae, a triple star. Primary 3 mag., nearer companion 7 mag. The farther, 9 mag. The distance of the former is 2" of the latter 45" According to 0. Struve there is a fourth star 10 mag. at distance 125", angle of position 350. 1325, Star Cluster in Gemini, a cluster of 6' to 7' in diameter, con- taining coarsely-scattered stars of 7 to 11 mag. W. Herschel discovered it 16 November, 1784. 1360, Star Cluster in Gemini, a very splendid object, seen by Messier, 20' in diameter. The most brilliant stars in it are of 9 mag. The field of vision is, however, filled with stars ranging from this magnitude to the faintest points of light. 1361, Star Cluster in Orion, fairly considerable, consisting of about 30 stars of 9 to 10 mag., among others a double star (2 848) of 7 and 8 mag., distance 2.3". This is a little north of the centre of the cluster. 41, Aurigae (2 845), a double star, 6 and 6.5 mag., discovered by Herschel. The distance (8.0") and angle of position (353) do not seem to vary. 2 8.y>, Orionis, 6 mag., with a companion 6.7 mag., distance 29.3". 30 Right Ascension 1880. Declination 1880. 6 h 3 m gh gm 6 h 7 m 6 h 7 m gh 8m 6 h gm gh n gh Jgm gh 16 m gh lg m gh 19 m gh 21" gh 21- 6 h 22 m gh 23 m 11 8' + 5 29' + 12 50' + 36 12' + 22 32' 6 14' + 59 25' + 22 34' + 58 29' + 4 39' + 7 9' + 12 43' + 20 52' 4 41' 6 57' 4, Monocerotis. A triple star ; the nearer companion discovered by Burnham ; the farther by Knott. Primary A is 6.5, B 9.5, C 10 mag. Measurements according to Dembowski, 1876. : A B distance 3.1". Angle of position 178 AC 8.9". 244.5 1376, Star Cluster in Orion, 5' to 6' in diameter, a rather crowded collection of brilliant and faint stars. 1383, Star Cluster in Pegasus, a beautiful cluster from 7' to 8' in diameter. With a low power, the field of vision seems filled with numerous stars of 10 to 12 mag. In two places the stars are densely crowded, and one of these places looks like nebula in a small telescope. 2 872, Aurigae. Primary 6.5, companion 7 mag. The distance (11") and angle of position (217) do not seem to vary. n Geminorum. This yellow star, as discovered by Schmidt, in 1865, varies between 3.2 and 4 mag. Period of variability about 229 days. 5, Monocerotis, a star of 4.5 mag. of a decided orange colour. 4, Lyncis (2 881). This star, 6.5 mag., has a companion 8 mag., but this latter is so near to the primary that it can be divided only by a most powerful telescope. 0. Struve (1847) found p = 95.6, d= 0.87". jix- Geminorum. A yellow star 3 mag., with a very faint companion (11 mag or less) at distance 72", angle of position 77. 5, Lyncis (2 894), triple, primary 6, the nearer companion 10.5, the farther 8 mag. Burnham (1879) calculated : AB. p = 139.1, di= 30.3" ; AC : p = 272.5, d = 95.9". 8, Monocerotis (2 900). A yellowish star 4.5 mag., with ablueish companion 6.7 mag., distance 13.7". Can be divided with a small telescope. T Monocerotis, A variable star, whose light fluctuates between 6.2 and 7.6 mag. within a period of 26.8 days. The changes of brilliancy were detected by Gould in 1871. According to Schoenfeld the maximum and minimum of brilliancy fluctuate somewhat at different periods. 1408, Star Cluster in Monoceros. Consists of 40 or 50 stars of from 10 to 11 mag., rather coarsely scattered upon a nebulous background. This last is difficult to see. 15, Geminorum, yellowish, 6.5 mag., with a blueish-white companion 7.5 mag., distance 31". 1415, Star Cluster in Monoceros, contains a yellowish star 6 mag. (10 Monocerotis). 11, Monocerotis (2 919). Quadruple, A 5.5, B 6, C 6.5, D 12 mag. The three brilliant stars were first seen by Herschel, the faint companion by Burnham. Duner (1871) calculates : A B Distance 7.2" Angle of position 132.2 BO 2.3" 105.0 Burnham: AD 25.8" 56.1 1MO. Declination ISM. 24- +11 -'-'' 6 h 2G m -f 4 57' 6 b 26- + 10 15' 6" 28- + 7 40' 6" 3l m -f 1G> 30' 6" 32- + 10 59' 6" 34- -f- 10 0' 6" 36- -I- 59 34' 6" 37- + 25 15' 6 k 38- -f- 43 42' 6 k Se- + 56 52' eP- 40- 16 33' - 'X'l, Monocerotis, a star of 6.5 mag., with a companion of nearly 8 mag. Di:-t:i!.< 1 ii", angle of position 4. 1 !-.'!, Star Cluster in Monoceros, visible on a clear night, with the naked eye as a nebulous star. With a telescope it is seen to be a somewhat dense cluster of stars, one of which (12 Monocerotis) is of 6 mag. 1425, Nebula in Monoceros. A very interesting object, fairly bright, comet-shaped, or rather fan-shaped, extending from a star of 10 to 11 mag. The whole is probably 1J' long. 14, Monocerotis (2 938), yellowish-white, f>.5 mag., with a very faint companion (12 mag.) Distance 10", angle of position 209.9. . 7 Geminorum, a star of 2.5 mag. with 2 faint companions at a con- siderable distance. Burnham gives the following measurements. A B Distance 141.7" Angle of position 335.5 J AC 294.7" 133.0 1435, Star Cluster in Monoceros, large, containing about 40 stars of !).-" to 12 mag., which are irregularly distributed. S (15) Monocerotis (2 950), the chief star of a coarsely scattered star cluster (G.C. 1440) 6 mag., with two companions, one 9 mag., distance 3", the other 11.5 mag., distance 16". The primary is surrounded by a thin veil of nebula, aud, as discovered by Winnecke, varies about half a mag- nitude. The duration of light variability is only 3 days 10 h 38". The colour of this star is described by Struve as green, it is now yellowish. 12, Lyncis (2 948), triple, 5.2, 6.1 and 7.4 mag. Discovered by W. Uerschel in 1780. The nearer companion is at distance 1.4"; the further at distance 8.7". f Geminorum. This white star of 3.5 mag., has a companion of 8.5 mag., at distance 111", angle of position 94. 56, Aurigae. 6 mag., of a clear white colour, with a blueish-white companion 8 mag., at distance 48", angle of position 21.1. 2 958, Lyncis. 6 mag., consisting of two white stars of almost equal magnitude, at distance 5". a. Canis Majoris (Sirius). The most brilliant fixed star in the heavens ; viewed with a powerful telescope, it is of dazzling splendour, and may be compared to a sun. The ancients described Sirius as red, at present it is perfectly white ; it has probably changed its colour since the days of Ptolemy. Bessel (in 1844) was the first to declare that Sirius must have a companion, as its proper motion showed irregularities which could be only explained by this hypothesis. In January, 1862, the companion demanded by Bessel's theory was discovered by the younger Clark with an 18-inch refractor; it was afterwards actually seen with smaller instruments, and Auwers estimated the time of its revolution at 49 years. The companion is 8.5 mag., and in 1860-70 was at distance 10", but this has gradually decreased, and the companion cannot now be distinguished except by a telescope of great power. 32 Bight Ascension 1880. Declination 1880. 6' 41- + 41 12' 1451, Star Cluster in Auriga, fairly rich, coarsely scattered, with a double star near the middle. Discovered by "W. Herschel, 3 Feb., 1788. 6 h 42 m 3 3' 1453, Star Cluster in Monoceros. Coarsely scattered, not rich, contains stars of 8 to 11 mag. 20 37' 1454, Star Cluster in Canis Major. A magnificent object, described and recognised as a star cluster by Messier. The smallest astronomical telescope will suffice to distinguish separate stars in it. Seen with the lowest power of a refractor, the whole field of vision seems full of stars of various magnitudes. A splendid sight ! 6 h 42 m + 59 34' 14, Lyncis (2 963). A very difficult double star. The primary is 6 mag., and of a golden colour; the companion 7.1 mag., and of a purple red, according to Struve. Distance 0.8", angle of position 64.1 ; the latter is slowly increasing, while the distance seems to diminish. A very powerful instrument is required to divide the companion from the primary. 6 h 46 m + 36' 1465, Star Cluster in Monoceros. 20' in diameter, rich in small stars. Near the centre there is a triple star 8 and 9 mag., for which Burnham (1880) gives the following measurements : A B ; distance 20.9", angle of position 80 ; A C ; distance 8.6", angle of position 281.9. 6 h 48 m + 13 20' 38, Geminorum (2 982). Primary 5.4 mag., and yellowish, companion 7.7 mag., and blueish. Distance 6.3", angle of position 164 (1878). The colours of both stars are relatively intense. 6 h 48 m + 18 8' 1467, Star Cluster in Gemini. A triangular cluster consisting of small stars densely crowded. The whole, in the average telescope, looks like a nebula. Discovered by W. Herschel, 30 Dec., 1783. gh 5]m - 13 53' //, Canis Majoris (2 997), a yellowish star 4.7 mag., with a blueish companion 8 mag., distance 2.5" (1878), slowly decreasing, angle of position 342, apparently unchanged since 1831. 6 h 52 m + 10 25' 1474, Star Cluster in Monoceros, consisting of a large number of coarsely scattered stars of 10 to 11 mag. 6 h 54 m -13 32' 1479, Star Cluster in Canis Major, somewhat scattered, 20' in diameter. The stars are from 8 to 11 mag. Discovered by Herschel, 8 Feb., 1785. 6 h 56 m + 52 56' 2 1009, Lyncis, a double star 6.7 and 6.8 mag., both of a brilliant white colour. Distance 3", angle of position 156; this latter has probably decreased since Struve took the measurement in 1830. 6" 57 m + 20 45' Geminorum, a star of a deep yellow colour, 3.7 mag., recognised as variable by J. Schmidt in 1844. The variation of brightness = 0.8 mag., and lasts 10 days 3 h 4S m . The decrease in brilliancy is somewhat more rapid than the increase. has two companions 7 and 10.5 mag. The first at distance 94", angle of position 352, the latter 87", nngle of position 84. Kicht A- :. !--, DKlitutioo ; r, h 57- .s K/ -15 --'7' 7" 0- + 22 53' 7" cr + 27 23' 7" 2- + 10 14' 7 h 4m -26 12' fh JQB + 13 59' 7 h II" 1 + 16 45' 7" 12" + 73 3 19' ,,, -13 0' 7 H i, -15 25' 7" 13- + 55 3 April, rilied l.y him as a cluster of small stars of different magnitudes, near to a star of 7 mag. The cluster consists of stars ranging from s to 13 mag., one of them being red in colour. Diameter 30'. 't Canis Majoris. According to Montanari, this star was scarcely visible in l(!?i) ; in It.'.i:; Muraldi t'oimd it to be 4 mag. Later on Hodo c.-tinmtcd it at 4.5 mag., and Flamsteed at 3 mag. It is apparently variable. R Geminorum. A variable star, discovered by Hind in 1848. At maximum it is (i.5 mag., at minimum less than 12 mag. The star is of a deep red colour, and the variation in brilliancy is somewhat irregular. According t<> Schoenfeld, the brilliancy of the star at maximum is often the same fur weeks at a time. 1490, Star Cluster in Gemini, discovered by W. Herschel, 11 Mar. 1785. A coarsely scattered cluster wbich contains within itself another cluster of small size. Thi latter, Rosso says, consists of six or seven stars of from 10 to 12 mag. R Canis Minor-is. A variable star, discovered at Bonn Observatory in 1854. At maximum it scarcely reaches 7 mag.; at minimum it is 9.5, sometimes 10 mag. Period, about 335 days. This star has so far received but little attention. S Canis Majoris. A red star, 2 mag., considered by Gould to be variable. 1508, Star Cluster in Gemini, consisting of numerous stars of 10 mag. and under. Irregularly round in shape and rather denser towards the centre. The whole is 4' in diameter. X Geminorum (2 1061). A star of 4 mag., of a greenish-blue light, with a companion 10.3 mag. Eoglemann (1882 87) calculates : distance 9.5", angle of position 32.1. 2 1051, Camelopardalis, triple, found to be so by Struvc. The primary is 7, the nearer companion 9, the farther 7 mag. The former is at distance 1.2", angle of position 268, the latter at distance 31", angle of position 81.5. 1511, Nebula in Canis Major. A large nebula, discovered by W. Herschel, 31 Jan., 1785, and described by him as resembling a parallelogram in shape, with a streak towards the south. The nebula has been imperfectly sketched by J. Herschel and Lassell. The best representation is that of Tempcl. (Vide sheet xviii.) 1512, Star Cluster in Canis Major, discovered by Caroline Uerschel. Large and rather dense. 19, Lyncis (2 1062). A star of 6.5 mag., with a companion 7.5 mag., distance 15". S Geminorum (2 1066). A yellowish star, 3.2 mag., with a reddish companion 8.2 mag Distance 7", angle of position 205.2 (according to Enplcmann, 1883). 1513, Star Cluster in Canis Major, fairly large, contains several brilliant stars. The brightest of these (30 Canis) is G.5 mag., with several companions, one of 9 mag., distance 84", angle of position 78. 34 Eight Ascension 1880. Declination 1880. 7 h 22 m 7 h 22' 7 h 25 m 7 h 25 m 7 h 26 m 7 h 27 m 7 h 3 7 h 31" 7 h 31 m 71, 3 6 m + 14 1 11 19 9 32 + 65 57' + 8 34' + 32 9' 21 C 50' 14 14' 14 12' + 5 32' -f 23 44' + 64 21' 1534, Star Cluster in Gemini, fairly rich, contains about 40 stars of 10 mag., and several fainter ones. Lord Rosse saw in this place 70 stars of 11 mag. and under, within a space 15' in diameter. 2 1097, Navis, a star of 6 mag. with 4 companions. The primary (A. has a companion (B) at distance 20", angle of position 312, and another companion (C) at distance 20", angle of position 311. In 1875, Dem- howski discovered that A is itself double having a companion 8 mag., d:= 0.8", p = 166. Then Burnham found another very faint star, d = 3l"p==41*. U Monocerotis, a variable star, identified as such by Gould in 1872. At maximum it is 6 mag., at minimum somewhat under 7 mag. Period of variability, 46 days. 1541, Nebula in Camelopardalis, very large, rather elongated, moderately bright with an increase of brilliancy at the centre. S Canis Minoris, recognised as variable by Hind in 1856. At maximum it is sometimes 7, but often only 8 mag., at minimum less than 11 mag. Period 332 days. a Geminorum (Castor), one of the most beautiful double stars in the heavens, 2.7 and 3.7 mag. It can be divided with a small telescope (distance 5.5"). Both stars give a greenish light. The period of revolution round their common centre of gravity is about 1,000 years. Near by are two stars 10 and 11 mag. 1549, Star Cluster in Gemini, a beautiful object discovered by "W. Herschel, 19 Nov., 1783. The stars are numerous and densely crowded. Diameter 6'. 2 1121, NaYis, a double star, 7 and 7.5 mag., distance 7.5". Close by is the double star 2 1122, 6.5 and 8.5 mag., distance 19.6". This belongs to the following cluster. 1551, Star Cluster in Navis, a rich group, 15' in diameter, of small stars rather densely collected. Among them are some fairly brilliant stars. Discovered by W. Herschel, 4 Feb., 1875. a Canis Minoris (Procyon), a brilliant star 1 mag. It has several very faint companions. Lament saw one of them (B) at distance 57", angle of position 262. There is another small star at distance 327", angle of position 84, which is (as discovered by Bird) itself double. There is also another companion d = 643" p = 99.7. This too, is double (2 1126) and consists of two stars 6.5 and 7.5 mag., distance 1.5". Burnham has also calculated the positions of two other companions of a. : d = 97", p = 22.7., and d = 47.8", p = 82.3. This latter is very faint (13 mag.) S Geminorum, recognised as variable by Hind in 1848. The star is of a yellowish red colour, and at maximum is scarcely 8 mag., at minimum it falls below 13 mag., or in other words disappears entirely for the average telescope. Period 294 days. The variability is not quite regular. 2 1127, Camelopardalis. Primary 6 mag. with one companion 8 mag., d = 5.2", p = 340, and a second (10 mag.) d = 11.2", p= 175 35 Right \ Dnlination .- 7 h 7 h :37" I 1 7 h 7" 39- 7* 42- 7" 7" 48- 7" 52- 7" 54- 17' 55 28 30' + 24 41' + :W 3 44' -23 35' -11 M' + 24 2' 19' + 2 33' 10 27' AB AC AD A I. Co Distance 41.4" 174.7" 206.3" 229.2" 1.4" !";, Star Cluster in Navis, extends over 30', and is visible with a 'mall : , discovered by Messier. The stars range from 7.5 to 11 mag. In this clustor W. Hrrsuhel found a faint, planetary nebula 2' in diameter, which Rosse declares to be annular. 1 ">i)7, Nebula in Navis. A planetary nebula, somewhat blurred at the edges. It look-* like a nebulous star in ordinary telescope.". ft Geminorum (Pollux). A brilliant star of 1.5 mag., with several companions, all of which are very faint. W. Herschel saw one of them in 1781, South another in 1825, and Struve a third in 1836. Burnham was the first to obtain a complete view of the whole system, and ho discovered th;it the nearest companion is itself double, 10 and 12.5 mag., but the distance is so small that it can be divided only with a very powerful telescope. Burnham gives the following measurements of the whole system, 1879-80 : Angle of position 275.3 71.2" 90.0- 76.3 132.6' The double star C c is a very difficult object, even for the 18-inch refractor at Chicago. Burnham gives the magnitude of B as 13.5 ; D, 9.5 ; E, 9. x Geminorum. A yellow star, 4 mag., with a companion 8.9 mag., distance 6.3", angle of position 2:36. The distance is probably slowly increasing, and the angle of position also. Geminorum (2 1135). A star of 6 mag., with a very faint companion 11 mag., distance 22", angle of position 212. 1571, Star Cluster in Navis, discovered by Messier, 8' in diameter, and fairly rich in stare of 8 mag. and under. 5, Navis (2 1146). 5.6 mag., and yellowish, with a companion 7.8 mag., distance 3.4". T Geminorum. Discovered to be variable by Hind in 1848. The star is red, and at maximum is 8 mag. ; at minimum it disappears. Schoenfeld found that the increase in light becomes much slower when once the star has reached 9.5 mag. On the whole, however, it gains more rapidly than it loses in brilliancy. Period 288 days, with slight fluctuations. I' Geminorum. Recognised as variable by Hind in 1855, and one of the must remarkable stars of its kind. The star is generally very faint, and without essential change, but at uncertain intervals it suddenly increases to 9 mag. Schoenfeld saw it gain as much as three magnitudes in 24 hours. No certain period can be given. 14, Canis Minoris. 5.5 mag., with two companions 7 and 8 mag., distance 76" and 112", angle of position 66" and 153. Hill, Star Cluster in Monoceros. A somewhat crowded cluster of stars, ranging from small to very faint. According to W. Herschel, who discovered the cluster 23 Feb., 1791, the crowded part is 5' to 6' in diameter. 36 Eight Ascension 1880. Declination 1880. Bight Ascension 1880. Declination 1880. ? h 56 m + 9 46' gh p. 8 54' gh 3 m 2 38' 8 h 5 m -12 34' 8 h 5 m + 18 1' gh gm -12 34' gh gm 5 26' gh 1Q m + 12 6' 8 h 15 m + 17 40' 8 h 20 m + 27 20' 8 h 20 m + 24 56' 8 h 25 m + 18 30' 8 h 29 m + 7 2' 8 h 33 m + 20 22' gh gym + 19 28' 8 h 39 ra + 29 12' gh 40 m + 78 40' 1617, Nebula in Canis Minor, fairly faint, small (30"), elongated, with sudden increase of brilliancy at the centre. 2 1183, Monocerotis, a yellowish white star of 5.5 mag. with a com- panion 8 mag., distance 31". 29, Monocerotis (2 1190), a yellowish star 5 mag. with two faint com- panions 9.5 and 9 mag., distance 31.6" and 67", angle of position 105 and 245. 1630, Star Cluster in Navis, 20' in diameter, coarsely scattered, rich in small stars, among them a double star. Discovered by W. Herschel, 31 Jan., 1785. Cancri (2 1196), a triple star, consisting of a double star 5.5 and 6 mag., distance only 1", and a farther companion 5.5 mag., distance 5.4". W. Herschel saw the inner companion in 1781, but later on, neither he nor South could distinguish it. Struve was the first to find it again in 1826. 1632, Navis, a nebulous star, 6.7 mag. 1637, Star Cluster in Monoceros. Fairly large and crowded with stars of 9 mag., also a pretty double star. .R Cancri, discovered to be variable by Schwerd in 1829. The star is yellowish red, at maximum 6.5 at minimum 12 mag. The period is 354 days and seems to be gradually lengthening. V Cancri, found to be variable, by Auwers in 1870. At maximum it is under 7 mag., at minimum less than 12 mag. The period is nearly 270 days.

tar, '',.' mag., with a blucish companion 7.S mag., distance '-\J>'. 1 1 olden, with the great refractor at Washington, saw another very faint companion, d = 20", p = 194. ^Schiaparelli finds the primary to he itself douhle, (187585). EDIT.] 1711, Nebula in Ursa Major, fairly brilliant, large, brighter at first gradually, then .suddenly towards the centre, whore is a star 10 mag. 17 U, Star Cluster in Cancer, discovered by Messier, and described as a star cluster with nebula. Herschel resolved the whole into stars of from 8.5 to 12 or 13 mag. They number over 200. There does not seem to be any common centre to the cluster. A. beautiful object! 1713, Nebula in Leo Minor. A. very faint nebula followed by a star of 8.5 mag. Rather more brilliant towards the centre. 1~>, Hydrae. This star, 6 mag., has (as discovered by Herschel) a companion 7 rnag., at distance 46", angle of position 356. Burnham divided the primary into two points of light at 0.5" distance, and found an additional companion at distance 50", angle of position 52. 5 Hydrae, variable, discovered by Hind in 1848. The star is a yellowish-red. At maximum it is sometimes 7.5, though often only 8 mag. ; at minimum it is under 12 mag. Period 256.4 days. i* Cancri (- 1291). 6 mag., with a companion 6.7 mag., distance 1.4". T Hydrae. Found to be variable by Hind in 1851. At maximum seems to be 7 mag., though often only 8 mag., at minimum it is under 12.5 mag. Period 289.4 days. i Ursa Majoris, 3 mag., with a companion 10 mag., distance 10", angle of position 357. a. Cancri. A star of 4 mag., with a very faint companion, distance 11.4", angle of position 325. 66, Cancri (2 1298). A white star of 6.5 mag., with a companion 8 mag., distance 4.6". 67, Cancri. A star of 6.5 mag., with a remote satellite. It is at distance 103", angle of position 323. 1750, Nebula in Ursa Major, rather faint, but extensive. Rosse's tele- scope shows this object as a formless, nebulous mass of an uneven character. a* Ursae Majoris (2 1306). 5 mag., and somewhat greenish, with a companion 8 mag., distance 2.6", angle of position 245. 1311, Cancri. A star of 7 mag., with a companion of equal brilliancy, distance 7". 1765, Nebula in Ursa Major, faint, fairly large, with a sudden increase of brightness towards the centre, with a kind of nucleus. 1781, Nebula in Ursa Major, fairly brilliant and large, with an increase of brightness towards the centre, where there is a star. Herschel thought it resolvable. 6 Hydrae, 4 mag., with a companion 11 mag., distance 53", angle of position 175. 38 Right Ascension 1880. Declination 1880. 9 h llm + 35 52' 2 1333, Lyncis, 6.5 mag. with a companion 7 mag., distance 1.4". gh llm + 37 19' 38, Lyncis (2 1334), a star of 4 mag. with a companion 6.7 mag., distance 2.8", angle of position 237. 9 h 12 m + 34 15' 1811, Nebula in Lynx, fairly brilliant, of moderate size and consider- ably brighter on its succeeding side. To the south are 3 small stars. gh 14 m + 51 30' 1823, Nebula in Ursa Major, fairly brilliant, 6' in diameter. In Rosse's telescope it shows some resemblance to the nebula in Andromeda. gh 14 m + 50 3' 39, Lyncis (2 1340), 6.5 mag. with a faint companion 8.5 mag., distance 7". f)h 21 m + 46 8' 41, Ursae Majoris, 6.5 mag. with companion 8 mag., distance, 82", angle of position 162. 9 h 22 m + 9 34' u Leonis (2 1356), a difficult double star 6 and 7 mag., both yellowish. The distance is, at times, so small, that even the most powerful telescopes show only an elongated star. Engelmann (1884) calculated : distance 0.66", angle of position 91.4. The motion of the companion seems to indicate 110 years as the period of revolution. 9 h 22 m + 63 35' 23, Ursae Majoris (2 1351), 3.8 mag. with a companion 9 mag., distance 23", angle of position 272. 9 h 23 m 2 15' r 1 Hydrae, 5 mag. with a satellite 8 mag., distance 67", angle of position 3. 9 h 25 m + 22 2' 1861, 1863, Nebula in Leo, large and brilliant, appearing as a double nebula in powerful telescopes ; with a very strong instrument a third nebula is visible. According to Tempel, the whole is a large, spindle-shaped nebula, at least 15' long, with 3 nodes, of which the southernmost is fainter than the northernmost, and the middle one is of a stellar nature and very brilliant. The spindle shape is ill-defined towards the north. 9 h 26 m + 10 15' 6, Leonis, 6 mag., somewhat reddish with a companion 9 mag., distance 38.8", angle of position 74.3. The position of the companion has not altered since Herschel's time. 9 h 29 m + 14 55' 7, Leonis, a star of 6 mag. with a companion 8 mag., distance 42", angle of position 79.5. 9 h 38 m + 35 4' R Leonis Minoris, a variable star, identified as such by Schoenfeld in 1863. At maximum it is 6 mag., sometimes only 7.5 mag. : at minimum it is under 11 mag. Period 375 days. 9 h 39 m + 72 50' 1909, Nebula in Ursa Major, about 1' in extent, elongated, fairly brilliant, with a nucleus in the centre. 9 h 41 m + 11 59' R Leonis, a variable star identified as such by Koch in 1782, of a deep red colour, and gives a peculiar spectrum. At maximum it is 5 at minimum 10 mag. Period 313 days. 9 h 44m + 54 38' Ursae Majoris, an exceedingly close double star 5 and 5.5 mag., distance only 0.2". It can only occasionally be divided even with the most powerful telescope. 9 h 46 m + 69 41' 1949, 1950, Nebula in Ursa Major, two nebula discovered by Bode at 30' distance from one another, the preceding one 15' long, is the more brilliant of the two, and has a nucleus like a star of 8.5 mag. The succeeding one is smaller and fainter. 39 - AonMun MM. I r ' . -f '>' 30' 9, Sextantis. A red

  • h star, 7 mag., with a companion 8 mag., ili-tunrc .Vi", angle of position 292. 7 7 200s, Nebula in Sextans, discovered by Herschel, fairly brilliant, with an increase of light towards the centre which resembles a star of "."i mag. Very faint when viewed with a small telescope. 10" >2 m + 1-2 J 33' a- Leonis (Regulus). A brilliant star with a beautiful spectrum. At distance 3' is a star 8.5 mag., which has the same proper motion as a. There is an extremely faint companion at distance 3.3", angle of position 88.5. 10 h 7 . + 71 (' 2021, Nebula in Draco, fairly brilliant, large, round, with an increase of brilliancy towards the centre, at first gradual then abrupt. 10 ii g" + i j r 2038, Nebula in Sextans, fairly brilliant, small, round, with a sudden increase of brightness towards the centre. It is followed in the field of vision by another fainter nebula not noticed by W. Herschel. . + 20 27' 7 Leonis (2 1424). A golden-yellowish star, 2 mag., with a greenish- red companion of 3.5 mag., distance 3.4". According to Struve, the most beautiful star in the northern heavens. Singularly enough, W. Herschel gives both stars us white. 10 h 19 18 2' 2102, Nebula in Hydra. A planetary nebula nearly 1' in diameter, fairly brilliant. W. Herschel saw no traces of a starry nature in it. To Secchi, on the other hand, it appeared quite differently ; within a circular nebula he distinguised two star clusters, which are bound together by a shining ring composed of two semi-circles of stars. There is also a star in the nebulous space at the centre. Tempel thinks the nebula very won- derful. He considers it to be a small, oval, brilliant disc of light surrounded by sharply defined, densely collected stars. Tn the southern central and northern portions shine out a few stars of greater brilliancy. "These," says Tempel, "like living pulsating points, form a striking contrast to the dark background which is totally free from nebula." 10 h 21" + 29 7' 2104, Nebula in Leo Minor, fairly brilliant, elliptical in shape, with | a kind of brilliant nucleus in the centre. 10 h 29 m + 9 16' 49, Leonis (2 1450). 6 mag., with a companion 9 mag., at distance 2.4", the position of which docs not seem to alter. 10" 31- + 54 8' 2158, Nebula in Ursa Major, planetary, with blurred edges, containing 2 stars of 10 mag. lO'-Sfi- + 69 24' R Ursae Major-is. A variable star, recognised by Pogson in 1853. At maximum it is sometimes 6, though often only 8 mag., at minimum 12 mag. Period, 303 days. 1P37* _l_ *7^o QQ' -j- *o oo 2178, Nebula in Leo Minoris, fairly bright, with an increase of brilliancy towards the centre. There is a star surrounded by the nebula. Rosse sees spiral coils round a luminous centre. L&3~ u + 1-2 20' 2184, Nebula in Leo, discovered by Mi-chain, and described as a very faint starless nebula ; it really is fairly brilliant, large and round, blighter at the centre, with a nucleus resembling a star of 10 mag. 10 h 37 m + 5 23' 35, Sextantis i- 1466). 6.5 mag., with a companion 7 mag., distance 67", angle of position 240. t 6-7 40 Right Ascension 1880. Declination 1880. 10 h 40 m 10 h 42 m O h 45 m 10 h 47 m 10M9 m 10 h 52 m 10 h 53 m 10 h 54 m 10 h 55 m 10 h 57 m 10 h 59 m 12 '12 m + 12 27' + 13 16' 8 10' + 57 37' + 25 24' + 59 33' + 29 37' + 4 16' + 57 2' + 28 37' + 37' + 56 19' + 55 40' + 53 26' + 18 46' + 59 26' + 58 39' + 32 12' companion is 2194, Nebula in Leo, very brilliant, irregularly round in shape, with a nucleus, probably resolvable. 2203, 2207, Nebula in Leo, double, fairly brilliant and large, the second nebula has a nucleus like a star of 9.5 mag. A third very faint nebula follows and forms a triangle with the other two. 41, Sextantis. Triple. The primary is 5, the farther companion 9, the nearer 11 mag. Burnham gives (1879) the following measurements : A B d = 26.9", p = 304 ; A C d = 233", p = 72 This not visible except in a very powerful telescope. 2245, Nebula in Ursa Major. Fairly brilliant, of moderate size, and irregularly circular in shape, gradually brighter towards the centre. Followed to the northward by a star 10 mag., distance 2'. 54, Leonis (2 1487), a star 4. 5 mag. with a blueish companion 7 mag., distance 6.5". 2 1495, Ursae Majoris, 6 mag., yellowish, with a companion 8 mag., distance 34". 2274, Nebula in Leo Minor, large, brilliant, supposed by Herschel to be a globular star cluster at an immeasurable distance. 2279, Nebula in Leo. According to Tempel, this is a large and thick spindle-shaped nebula 5' long by 1.5' broad, with 3 distinct nebular nodes in its major axis. In all of these faint stars are visible. About 6' north of the middle node, Tempel repeatedly observed a small nebula. /3 Ursae Majoris. A greenish- white star, 2.3 mag., with a very faint companion, distance 245", angle of position 354. 2287, Nebula in Leo Minor, fairly brilliant, with what looks like a nucleus in the centre. According to Herschel this nebula is really a resol- vable star cluster. 2301, Nebula in Leo, fairly large, oval, with a star-shaped nucleus. Several stars follow it. 2318, Nebula in Ursa Major, discovered by W. Herschel, 7 April, 1789, elongated, fairly brilliant, with a star in the centre. According to Herschel, however, the latter is merely accidentally projected on the nebula. 2343, Nebula in Ursa Major, large, planetary, discovered by Mechain in 1781. According to J. Herschel it is 2' 40" in diameter and of uniform brilliancy throughout. Rosse sees two dark openings in the nebula with a star in each. Huggins considers it to be a mass of incandescent gas. 2 1520, Ursae Majoris. A star of 6 mag., with a companion 8 mag., distance 13". 2352, Nebula in Leo. A faint nebula, considered by d' Arrest to be variable. Schoenfeld found it to be brilliant in 1861, but in 1863 it was occasionally invisible. At present it is very faint. 2360, Nebula in Ursa Major, fairly brilliant, but small, with a nucleus. 2362, Nebula in Ursa Major, fairly brilliant, of moderate size, much brighter towards the centre, with what seems to be a nucleus. I Ursae Majoris (2 1523). A yellowish star, 4 mag., with a greyish- white companion 5 mag. This latter moves with great rapidity, its period of revolution being only 60 years. Distance in 1882 1.9", but now rapidly increasing. - 41 Iliicht 11" PJ" 1 1" 14- 11" 18- 1 1" 22- U h23 1 1" 26" 1P32- ] 1" 42- :<:, + 11 ir 3' 31' ' 59' -28 36' -r IV 2' + 17 28' + 45 46' + 20 53' + 15 15' 111.47.- 11" 52- sa- il 1 - .->7 m -f 37 39' + 17 '.'' + 54 3' + 51 37' + 45 I-. 1 ' v Ursae Majoris i.l 1 .VJ4), yellowish 3.5 mug., with a very faint eolii|>.i!lioii H>."> ina::., di-tain-i 7 ", alible <>f Jniti(ill 117 . Nebula in Leo. double, fairly brilliant, the succeeding one bciii. it. Tin 1 nebulae arc spiral-shaped with central nuclei which i to be surrounded by elliptical rings. The nebula 2373 is 7' long by 2' broad, thr other '>' long by '2\' broad. / Leonis (- l.VJtii.ayi-lluwi-h star I mag. with a blueish companion 7 mag., di-t < r Leonis, 5 mag., yellowish with a white companion 7 mag., dis- tance '' . I .-ily observed. 57, Ursae Majoris (?. l;")-i:i), 5 mag., with a companion 8 mag., distance .">. 1", angle of jwsitiou 7. In Hydra, two stars, 5.5 and 6.5 mag., distance 8.7". 88, Leonis (2 1547), yellowish 6.5 mag., with a faint companion 9.3 mag., distance 15", angle of position :}_'" . 90, Leonis (i 15.V2), a star of 6 mng., with a companion 7.5 mag., distance 3", angle of position 209.4. At distance 63", angle of position J3-J , is a star of 9.5 mag. 2 1561, Ursae Majoris, 6.5 mag., with a companion 8 mag., distance 10". 93, Leonis, 4 mag., with a companion 8.4 mag., distance 74". ft Leonis, - 2 mag., with a very beautiful spectrum, has a number of faint stars in its vicinity. Knott gives the following magnitudes and positions : B 8 mag. C 10 mag. D 7 mag. E P2 mag. F 11 mag. A B 4' 4'2" distance. 206.2 angle of position. AC 11' 30" 186.9 AD19'30" 201.6 AE 5'-r 116.1 A F 10' 0" 120.0 Bumham found another star at distance 77", angle of position 3 45 \ He also found D to be a very close double star 6 and 11 mag., distance 1.5". 2(X)0, Nebula in Ursa Major, a fairly brilliant nebula 3' to 4' in diameter, with an increase of density towards the centre. 65, Ursae Majoris (2 1 .">79), 6 mag., with a blueish companion 8.5 mag., distance 37". There is also a star of 6.5 mag. at distance 1 14". 2635, Nebula in Ursa Major, a faint nebulous appearance between two stars, 7' long by 4' broad, according to Ilersclicl. Tempel estimates it as at the most only '2V in diameter, and sajs he sees 3 brilliant stars round its speckled centre. 2660, Nebula in Ursa Major, discovered by W. Hcrschel, 12 April, 1789, brilliant, 5' long by 1 J' broad, increasing in brightness towards the centre, with a brilliant nucleus. 2680, Nebula in Ursa Major, brilliant, fairly large, with a sudden increase of brightness towards the centre. Rosso finds it to be of spiral structure. a 42 Right Ascension 1880. Declination 1880. ll h 58 m 12 h l m 12 h 4 m 12 h 5 m 12 h 7 m 12 h 10 m 12 h 10 m 12 h 12 m 12 h 13 m 12 h I3 m 12M3 m 12 h 16 m 12 h 16'" 12 h 17 m 12 h 19 m 12 h 19 m + 22 8' + 43 44' + 19 13' + 40 33' + 15 34' + 41 20' + 13 48' 3 17' + 15 4' + 47 59' -18 35' + 5 8' + 26 31' + 10 29' + 13 34' + 18 52' 2, Comae Berenices (2 1596), 6 mag., with a companion 7.5 mag., distance 3.7". 2723, Nebula in Canes Yenatici, fairly bright, elongated, with a very brilliant nucleus. Discovered by Herschel 14 Jan., 1788. 2752, Star Cluster in Coma Berenices, of moderate size, very bril- liant, globular, the stars are more densely collected towards the centre. 2 1600, Canum Yenaticorum. A star of 6 mag., with a companion 7 mag., distance 1.4". 2786, Nebula in Coma Berenices, a large pale nebula 15' long, with a star-like centre. Discovered by Mechain 5 Mar., 1781. Tcmpel found another small round nebula to the southward. 2, Canum Yenaticorum (2 1622), a reddish star 5.5 mag., with a blueish companion 8 mag., distance 11.4", angle of position 260. The colours are fairly decided. 2806, Nebula in Yirgo. 9' to 10' long, brighter in the centre. Dis- covered by Herschel 8 April, 1784. It is spindle-shaped, and Tempel saw two accompanying nebula. The one preceding it to the south is 5' long, oval in shape, and has 3 brilliant nodes ; it is situated towards the centre of the principal nebula : 35 s 6^'. To the south there follows a small star 10 11 mag. The companion nebula on the north, which follows it, is round, 1' in diameter, and very faint. 2 1627, Yirginis, 6 mag., with a companion 6.5 mag., d = 20", p= 196. 2838, Nebula in Coma Berenices. Discovered by Mechain 15 Mar., 1781, and described as a starless nebula. Vogel observed it with the 8-inch refractor at Leipsic, and found it to be large, brilliant, and apparently resolvable at the centre, where there are two bright starlike points. With magnifying power 192, a spiral arrangement was visible. 2841, Nebula in Ursa Major, brilliant, with a nucleus, fairly large. Discovered by Herschel. No trace of resolvability. A continuous spectrum shows that this nebula is a very distinct star cluster. E Corvi, recognised as variable by Karlinski in 1867. At maximum it generally reaches 7 mag. ; at minimum it is ll - 5 mag. Period 319 days. 2878, Nebula in Yirgo. Discovered by Messier 1779. A very faint nebula in which Herschel recognised two nuclei. 12, Comae Berenices, 5 mag., with a companion 8 mag. Distance 66", angle of position 169. 2890, Nebula in Coma Berenices. Discovered by Mechain 15 Mar., 1781, fairly large, round and faint. 2930, Nebula in Yirgo, a fairly brilliant, circular nebula, which suddenly increases in brightness towards the centre. Discovered by Messier. 2946, Nebula in Coma Berenices. Discovered by Mechain, and described as faint and starless. Herschel calls it brilliant. A star 9 mag,, follows 2' southward. -- joh.jp, 4- 36' ."" 4- ii '"> 40' l-.""Jl'" 12* 25 m 12* 28" 12*30- 12*30- 12" 30" 12*30- -f 8 4-42 18' 15 4-13 4-26 4-15 4- 8 4-19 4-13 4-28 4-12 51 3' 26' 5' 21' 2' 13' 37' 6' 4-26 39' 1, Nebula in Virgo. Com.- into sight at the same moment as the '2 KJO, brilliant, round, with nucleus in the centre. Also discovered 1'V Mrv-irr, 3' to 4' in diameter. 297-J, Nebula in Coma Berenices, fairly brilliant and large, increasing in brightness towards the centre, at which there is a star. 300-J, Nebula in Canes Yenatici, fairly brilliant and large, was resolved into stars by llt-rsi-hrl's great telescope. 17, Comae Berenices. A star of 5.5 mag., with a companion 6 mag., distance 14.V. 3021, Nebula in Virgo. Discovered by Oriani in 1771, and described by Messier as a nebula, which can be seen but with difficulty in a 3}-foot telescope. On right and left is a star of G mag. An insignificant object in small instruments. 3041, 3042, Nebula in Canes Yenatici. A double nebula. The preceding one is faint, fairly small, and irregular in shape, the other which follows 3' to the south is larger and more brilliant. In Herschel's tele- scope it was partly resolvable into stars. S Coral 2.5 mag. with a companion 8 mag., distance 23", angle of position 214. 3035, Nebula in Virgo. Discovered by Messier, of moderate brilliancy, round and large, brightest in the centre. 3043, Nebula in Coma Berenices, faint, round, with nucleus. 3049, Nebula in Virgo. Discovered by Messier in 1781, and described as a starless nebula, situated between two stars of 6 mag., which come into view at the same moment. It is elliptical, and the northern part is brighter than the southern. Lassell and Vogel have made maps of this nebula. 307"), Nebula in Virgo, of moderate brilliancy, with a sudden increase of brightness towards the centre. Preceded by a star of 9 mag. 24, Comae Berenicies (2 1657), 5 mag. and yellow, with a blueish companion mag. Distance (1863) 20", angle of position 271. :{0!)7, Nebula in Virgo. Discovered as a very faint starless nebula by Messier ; it is round and brighter towards the centre. Vogel observed it with the Leipsic Refractor, and describes it as very brilliant 2' in extent, suddenly denser at the centre, with a brilliant nucleus. 3101, Nebula in Coma Berenices. Fairly bright and large, gradually more brilliant towards the centre. Three stars follow it. 3105, Nebula in Virgo, a faint, double nebula, coming into view at the same moment as two others still fainter. Tcmpcl has made a map of the whole with the neighbouring stars. 3106, Nebula in Coma Berenices, a somewhat faint nebula, very large, 3-4' in breadth, brighter towards the centre, with a nucleus like a star of 10 mag. Preceded by four faint stars. Bight Ascension 1830. Declination 1880. Kiprht Ascension 1830. Declination 1880. 12 h 31 m 4- 60 9' 12 h 32 m + 12 29' 12 h 32 m -f 7 39' A2 h 33 m 26 5' 12 h 34 m -10 58' 12 h 35 m -12 20' 12 h 36 m 47' 12 h 36 m + 33 12' 12 h 38 m + 2 39' 12 h 38 m + 12 13' 12 h 39 m + 61 45' 12 h 39 m + 15 2' 12 h 42 m 5 9' 12 h 45" 9 41' 12 h 45 m + 41 47' T Ursae Majoris, recognised as variable at Bonn in 1860. At maxi- mum it is sometimes 7, though often only 8 mag. ; at minimum under 13. Period 256 days. The star is of a reddish-yellow colour. 3121, Nebula in Virgo. Discovered by Messier in 1779, and described as a very faint nebula. John Herschel calls it brilliant, large, irregularly round, bright towards the centre, and probably capable of being resolved into stars. R Yirginis, a reddish-yellow star, whose variability was recognised by Harding in 1809. At maximum it is 6.5 to 7.5 mag. ; at minimum 10 to 11 mag. Period 146 days. 3128, Nebula in Hydra. Discovered by Messier in 1780, and de- scribed by him as a very faint starless nebula not easy to distinguish. Near it is a star of 6 mag. In 1786 the nebula was resolved into separate stars by F. W. Herschel's 20-foot reflector, these being very densely collected towards the centre. The cluster is 4' long by 3' broad. 3132, Nebula in Yirgo. An elongated, elliptical nebula, brighter at the centre. With a low magnifying power several stars come into view at the same time as the nebula. 2 1669, Yirginis. A star of 6 mag., with a companion of nearly equal magnitude. Distance 5.8". 7 Yirginis (2 1670), a yellowish star 3 mag., with a somewhat fainter companion. This latter is at present easy to observe (d = 5.2", p = 336, 1882) : its period of revolution is 170 years. There is also another faint star (11.5 mag.), d= 103", p = 80. 3165, Nebula in Canes Yenatici, a strip of nebula 12' long, but faint, with a small star in the centre. 3176, Nebula in Yirgo, somewhat faint, starless, brightest at the centre. 3182, Nebula in Yirgo. Discovered by Messier, who, however, did not see a faint nebula which precedes it. Somewhat faint. As seen with the Leipsic refractor, it seems capable of being resolved into stars. S Ursae Majoris, of a reddish-yellow, recognised as variable by Pogson in 1853. The changes of brilliancy are somewhat irregular. At maximum it is 8, at minimum 10, sometimes 11 mag. Period 225 days, is apparently, slowly increasing. 2 1678, Comae Berenices, 6 mag., with a companion 7 mag., distance 32". 3227, Nebula in Yirgo, fairly large, but not very brilliant, increasing in brilliancy towards the centre, with a kind of nucleus which Herschel thought resolvable into stars. 2 1682, Virginia, 6.5 mag., yellowish, with a reddish companion 9 mag., d=32", p = 307. 3258, Nebula in Canes Yenatici. Discovered by Mechain, and de- scribed by him as a starless nebula, of fair brilliancy, 2.5' in diameter, with brilliant centre. Several stars come into view at the same moment as this nebula, one of them a double star which follows it. 45 Kiirht A IMO. ], .- 1 .)h 1 ".in 1 .C -i r in. j.jh ,;. -fir 53' :" -f -_>r 64' 13* 4- 13 h 4 m 13" 5- ,h p. 11 56' 58' -f :, t 44' 14 49' -f 11 36' -4- 18 10' . . Mi-h, ami at maximum S mai;., at minimum 13 mag. Period nearly 207 i! S Nebula in Yirgo. Two faint nebula) at 8' to 10' distance from another. Di.-i-nvi -r< -87), r> mag. and yellowish, with a blucish companion 8 mag., distance 1.3", and a second companion 9 mag., distance Nebula in Yirgo, double, faint, with other small, faint nebula; in the vicinity. TVmpel has mndc a map of this group of nebula;. + 39 8' 4 54' + 37 42' 18 48' 1 li'.'i-j, Canum Yenaticorum. Tin- brightest star in the constellation and known by the name of " Cor Caroli." The star is a little over 3 mag., and has a companion (> mag. at distance 20", in whose position no change has yet been observed. 2 1695, Ursae Major-is, t'>.~> mng. with a companion 8 mag., d = 3.2", p=287. :!'; 12, Nebula in Coma Berenices. A brilliant nebula of fair si/e with a core-like density at the centre. There is a small star in this nebula. 4 Yirginis, a star of 4 mng., with a very faint companion (12 mag.), d=241" p = 120. l-J, Comae Berenices (- 1728). Two stars of 5 mag., but whose distance is so small that they may be considered one of the most difficult of double stars. Struve, who discovered their duplex character in 1827, could generally only distinguish an elongated star, actual division being only occasionally possible. Dcmbowski too, in 1863, saw only an elongated star ; Burnham, however, in 1879, measured the distance as 0.07", angle of position 1MJ . Since 1882 the division has been easier than heretofore, but still requires an instrument of the- first class. 15, 17, Canum Yenaticorum, two stars of nearly equal brilliancy, 5.5 mag. The distance is 4' 30", still they cannot bo divided without a telescope. 8 Yirginis, triple, i.o, 9 and 10 mag. The nearer companion is d = 7.1", p = 344 J , the farther and fainter, d= 71", p = 2!>7 . .7, Nebula in Canes Yenatici, a fairly brilliant nebula, 6' long by 1.5' broad, discovered by Herschel 1 May, 1785. Increases abruptly in brilliancy towards the centre, where it has what looks like a nucleus. :;|.Vi, Star Cluster in Coma Berenices. Discovered by Messier in 1777, and described as a starless nebula. In reality it is a star cluster in which, according to Rosso, 4 or 5 condensations are visible. A very beauti- ful object. 46 Kight Ascension 1880. Declination 1880. 13 h 10 !3 h 19 m 13 h 20 m 13 h 23 m 13 h 25 m 13 h 27 m 13 h 32" 13 h 32 m 13 h 32 m 42 40' 55 33' 2 45' -22 40' 47 49' 6 35' -17 16' 36 55' + 9 30' 3474, Nebula in Canes Yenatici. Discovered by Mechain in 1779, and described as a faint and starless nebula. According to Herschel, it is 10' long by 4', with a bright nucleus. Huggins finds that it gives a continuous spectrum which proves it to be a star cluster at an immeasurable distance. Ursae Majoris, 2 mag., and greenish-white, with a companion 4.5 mag., distance 14". One of the most beautiful double stars in the heavens. At 11' 47" distance from is g or Alkor, and, in addition, a star 8 mag., distance 8.5', together with several fainter ones. W Yirginis, recognised as variable by Schoenfeld in 1866. At maximum it is 9 mag., and at minimum 10 to days. The change of brilliancy is very uniform. 10.4 mag. Period 17.3 E Hydrae, a deep red star, recognised as variable by Maraldi in 1704. At maximum it is 4 to 5.5 mag., at minimum 10 mag. Period 437 days, formerly it seems to have been longer. 3572, Nebula in Canes Yenatici. Discovered by Messier in 1773, and described as a faint, starless nebula, but double, each portion being bright in the centre, and 4J' in diameter. W. Herschel describes it as a brilliant, circular nebula, surrounded by a faint, nebular halo and accompanied by a second nebula. J. Herschel's description and drawing were also wrong. Rosse's telescope showed the true structure of the nebula, i.e., a spiral mass which seems to be wound round a brilliant centre (Vide Plate xvi). These spiral coils have also been clearly dis- tinguished and mapped out by Yogel, with the help of the Leipsic 8-inch refractor. It would thus seem that we have here a mass of a really nebulous character coiling in vast convolutions round an enormous centre, yet spectrum analysis contradicts this theory. The nebula has a con- tinuous spectrum similar to that of the stars, and without any bright lines, which are never absent from the spectra of true incandescent nebulae. S Yirginis, recognised as variable by Hind in 1852 ; the change of brilliancy is somewhat irregular. At maximum the star is 6 mag., some- times only 8 mag., at minimum under 12 mag. Period 374 days. 3614, Nebula in Yirgo, faint ; according to Lassell, a spiral with two arms. 25, Canum Yenaticorum (2 1768). A star of 5 mag., with a com- panion 7.5 mag., distance (when discovered by Struve in 1829), 1.05". It has decreased since then, and Engelmann, in 1883, calculated it as 0.8". The companion's angle of position was 151. Apparently the distance is now increasing again. 3615, Nebula in Yirgo, brilliant, 9' to 10' in length, with two nebulous nodes in the centre. There is one star to the south of it, and several fainter ones to the north. Tempel discovered some very faint nebula) in its vicinity. 47 Declination Iff i:r i:V' !_ 13 i:t l l 11" 9 m 14" 10- 14" 1-2- 14" !!>"' 1 I" 22 14 h 23 ra 14 h 23 m 14" 32" 14" 34" 14" 35' 1, Bootis. 1 \17-2 . a star of G mag., with u faint companion 9 mag., nee i x ". -f I c .i' 84, Yirginis 1 1777), il in:i^, with a companion rt mag., distance :i.;Y' -f- -js .Y.I' .!i;.lii, Star Cluster in Canes Yenatici, discovered by Messier an mag., with a very faint companion, d = 8.5", p = :i.V2 . + 49 55' ** Ursae Majoris, :i mag. According to Gcmmil, who is supported by Kspin, this star is variable. Period 4-J days. More exact information is not forthcoming. -f. 2 T T Yirginis, a star of 4 mag., with a faint companion 8.5 mag., d = 7!", p=-2fli . + 19 38' T Bootis, a star of 9.5 mag., seen by Baxcndall 9th April, I860, on 1 1th April it was 10 mag., and on 20th 13 mag., on the 23rd it became iuvi>ible, and has not since been seen. 52 -2-2' * Bootis (2 1821), a star of 4 mag., of a greenish-white colour with a blueish companion at 12.7" distance. 19 49' * Bootis (Arcturus), a brilliant star 1 mag., with a beautiful spectrum (Vogel, class Ila.). Its colour is a bright reddish-yellow. At distance 4:V is a star of 9 mag. [See Note p. 71.] + 51 "i.V /Bootis. This star l.o mag. has a companion "." mag., at distance 38". Struve (1830) saw thp primary as double; Miidler, too, in ls|-J, believed he could do so ; sinte then no similar observation has been made, and its duplex nature i*, therefore, doubtful. _|_ 540 -j i S Bootis. A variable star of a reddish colour, discovered at Bonn in 1800. At maximum it is 8 inag., at minimum it becomes invisible. Period 272 days. 1 41' ? Yirginis (2 1846), 5 mag., with a companion 10 mag., d = 4", p = 103.5. 5 26' .'{900, Nebula in Virgo, of moderate brilliancy, small, condensed at the centre, thought by J. Hcrschel capable of being resolved. 28 49' 2 1850, Bootis, 0.5 mag., with a companion 7 mag., d= 25", p = 263. 27 16' A' Bootis, a variable star, at maximum it is 6 mag., and reddish in colour, at minimum it sinks to 12 mag. Period 223 days. Recognised as variable at Bonn in 1858. + 14' liiiC.J, Nebula in Yirgo, discovered by W. Herschel 11 April, 1787, and classed by him among the brilliant nebula. J. Ilerschel considered it capable of being resolved into stars. -f- in :,(',' * Bootis (2 1804), a star 4 mag., with an easily distinguished companion 6 mag., distance 0.6". 48 Kij;ht Ascension 1880. Declination 1880. 14 h 35 m iM 14 h 44 m h 46 m 14 h 4G m 14 h 50 m 14 h 55 14 h 5G m 15 h 0" 15 15 h 7 m 15 h 10 m 15" + 14 15' + 27 35' 15 33' + 19 36' + 49 12' 20 52' 8 2' + 54 23' + 48 8' 19 20' + 19 44' + 38 43' + 33 46' Bootis (2 1865). The primary, 3 5 mag., has two companions, the nearer 4 mag., is at present so close to the primary that only instruments of the first class can distinguish it. According to Perrotin, the distance in 1883 was 0.6", the angle of position 297. The farther companion is at distance 90", angle of position 27. e Bootis (2 1877), one of the most beautiful of the double stars. The primary is 2.5 mag., and yellow, the companion 6 mag., and blue. Dis- tance 2.9". The colours are very decided, and their contrast has a pretty effect. a Librae, 2.5 mag., with a companion 5 mag., distance 230". Bootis (2 1888), 4.5 mag., and yellowish, with a red companion 6.5 mag. The distance of this latter is rapidly decreasing. In 1882 it was 3.9", while in 1829 it was, according to Struve, 7.2". The angle of position is also rapidly changing. The period of revolution seems to be 130 years. 39, Bootis (2 1890), a double star 6 and 6.5 mag., distance 3.6". The primary is white, the companion reddish. Anonyma in Libra, a remarkable multiple star. The primary is 6 mag., one companion (B), 7.5 mag. The rest are all very faint. Burn- barn (1878), gives the following measurements : ABdz= 15.1" p = 290 AEd= 69.4" p= 52.5. A C d = 120 6" p = 322 ADd=z 52.5" p = 171.0 A F d = 105.5" p = 166.5. The primary and the more brilliant companion compose a system with very decided proper motion. The other stars do not really, but only appear to, belong to it. S Librae, variable and belongs to the Algol type. Schmidt recognised its variability in 1859. Period 2 days 7 h 21. 3 m . The changes of brilliancy only occupy 12 hours. At maximum the star is 5, at minimum 6 mag. 4029, Nebula in Draco, irregular, faint but large. Discovered by W. Herschel, 5 May, 1788. 44, Bootis (2 1909), a yellowish star 5 mag., with a blucish companion 6 mag., distance 5". Both primary and companion seem to be variable to a slight degree. 1 Librae, a star 4.5 mag., with a companion 9 mag., d = 57", p = 110. Burnham found the companion itself to be double, consisting of two stars of 10 mag., distance 1.9". 2 1919, Bootis, 6.5 mag., and somewhat yellowish, with a white com- panion 7 mag., distance 25". 2 1926, Bootis, 6.5 mag., with a faint companion 9 mag., d 1.4", p 259. A difficult double star. S Bootis, 3 mag., and white. At distance 105", is a companion 7.5 mag., whose position has not changed for 50 years. .. .... j.-h ,. 2 , 15 h 14- i.V- it;- i.v< i; 15" 18- 15"29- 15 s 32- + 2 31' + 2 13' + 10 49' + 27 17' + 32 5' -19 57' + 14 45' + 31 48' + 30 43' + :<7 48' + 10 57' 8 24' los.t, Star Cluster in Serpens. Observed by Messier in 1764, and described as a beautiful, circular nebula 3' in diameter. Messier says, " In ..r it can l>e SI-CM very well with tin ordinary telescope of 1' focus." Kirch, in 17D-2, was the first to discover this nebula. Messier could find in it no trace of stars. Nevertheless, an average telescope shows that it is a cluster of stars and no nebula. Herschel, with his 40-foot reflector, could distinguish over 200 stars, though towards the centre they were so densely placed that it was impossible to resolve them. Rosse says the cluster is 7' to 8' iu diameter, the stars ranging from 12 to 15 mag. 5, Serpentis (2 1930). 5 mag., with a faint companion 10 mag., d = 10.6", p = 40.8, the position of which does not seem to alter. Struve, in 1836, believed the primary to be itself double, but this view has not been since corroborated. 2 1931, Serpentis. 6.5 m;ig., with a companion 7.5 mag., d = 13.5", p = 173. No change of position has been noticed in last 50 years. 2 1932, Coronae. The primary is 5.5 mag., and has a companion 6 mag. ; both white. Distance, according to Engelmann, 1883, 1.2", angle of position 308. U Coronae. A variable star of the Algol type, recognised by Winnecke in 1863. At maximum 7.6 mag., at minimum 8.H mag. Period 3 days 10 11 51.2". The decrease in brilliancy occupies 4.5 h , the increase 5.2 h . The brilliancy at maximum varies somewhat. S Librae, variable, slightly reddish in colour, at maximum only 8 mag., at minimum under 12 mag. The changes of brilliancy are very irregular. Discovered by Borrelly in 1872. S Serpentis. A reddish star, noted by Lalande in 1794 as of 8 mag., but which could no longer be found by Harding in 1807. Its variability was not recognised till 1828. At maximum it is 7 8 mag., at minimum under 12 mag. Period 361 days. S Coronae, of a reddish-yellow, recognised as variable by Ilcncke in 1860. Maximum 8, minimum 12 mag. Period 361 days. n Coronae ( 2 1937). A yellow star of 5.2 mag., with a golden coloured companion 5.7 mag ; it is extremely close to the primary, the distance (Engelmann, 1884) being only 0.6". it. Bootis. A yellow-greenish star 4 mag., with a companion (/**) 7 mag., distance 108", angle of position 172"" This latter is itself double, but, at present, can be divided only with a most powerful telescope. S Serpentis (2 1954), yellowish, 3.5 mag., with a companion 4 mag., d = 3.5", p = 190. 2 1962, Librae, two stars 6 mag., distance 12". A\ ' 50 Eight Ascension 1880. Declination 1880. 15 h 34 m + 36 38' 2 1964, Coronae. A otar of 7 mag., with a companion 7.5 mag., distance 15.5". Burnham found that this companion was itself double, distance 1.3". 15 h 35 m + 37 2' Coronae (2 1965), 4 mag., with a companion 5 mag., distance 7". 15 h 36 m + 80 50' a 1 Ursae Minoris (2 1972), 6 mag., yellowish, with a yellowish com- panion 7 mag., d = 30", p = 83. 15 h 37 m + 26 41' 7 Coronae (2 1967). A greenish-white star 4 mag., with a reddish companion 7 mag., distance (when discovered by Struve in 1826), 0.7". - In the following year it could no longer he divided, and it was not seen again until the end of the fiftieth year, and then only with great difficulty. Even Burnham, in 1880, found the primary star only, and apparently quite round. Engelmann, however, in 1883-84, occasionally saw it as clearly elongated. 15 h 38 m + 6 48' Scorpionis, .m r^ily observed double star, 4 and 7 mag., distance 40.5" ; thus observed by both Herschel and South. Mitchell, however, at Cincinnati in 1846, found that the companion is itself double, and consists t' (>."> mag. at distance 1.8". Lastly Burnhum in 1874 divided the primary also into two stars, but the distance is only 0.8". Serpentis (2 2021). Primary 6.5 mag., companion *6.7 mag., distance 3.7". -1-2' Star Cluster in Hercules. A magnificent cluster visible on a clear night, with the naked eye, as a light cloud, as remarked by Hallcy, who d it in 1714. Messier observed this object in 1764, and says, that it can be seen with a 1-foot telescope as a starless nebula, brilliant, circular, brighter at the eeiitn-. Its diameter is estimated by Messier to be G', and the same astronomer remarks that the nebula is situated near two stars of 8 mag., of which ono is above, the other beneath it. A 4-inch refractor will resolve the nebula into stars, and Secchi, with his 9-inch refractor, found the stars to be distributed over a space 8' in diameter. Their number is probably 5,000 to 6,000, and Rosse has noticed a remark- able spiral grouping among them. [The great 36-in. refractor of the Lick Observatory has thoroughly resolved the central glow of nebulosity into separate points. ED.] 42.34, Nebula in Hercules. A blueish, planetary nebula, circular, 8' in diameter, and ill-defined at the edges. Its spectrum shows the nebula to be composed of incandescent ga., It-ing characterised by the three bright lines, of which the first is the most brilliant. Elsewhere the spectrum is dull and continuous. Webb describes the appearance of this nebula by saying that it looks like a star which has not been properly focusscd in the telescope. 1'.':;^, Star Cluster in Ophiuchus. DiMOVWtd l'\ M.-Mrrin 17ii!, and described as a faint, circular, starless nebula, 3' in diameter, near which there is a star of 9 mag. In 1783, Herschcl's reflector resolved the nebula into stars showing a cluster of 7' to 8' in diameter, at the centre of which the stars are very densely collected. 19, Ophiuchi (2 2096), G mag., with a companion 9 mag., d = 22.2", p = 93. 2 2101, Herculis, a star of G mag., with a companion 9 mag., d = 4.2", p = 57. 4244, Nebula in Hercules, n large, round but faint, planetary nebula, discovered by W. llerschel 12 May, 1787. It forms a triangle with two stars of 6 mag. 2 2104, Herculis, a pretty, double star, 6.5 and 8.5 mag., distance 6". S Herculis, of a clear red colour and variable, discovered at Bonn in 1856. At maximum it is 6 mag., sometimes only 7 mag., at minimum it decreases to 11.5 and 12 mag. Period 303 days. 425G, Star Cluster in Ophiuchus. Discovered by Messier, 29 May, 1764, and described as a faint, circular, starless nebula, which cannot bo dis- cerned without difficulty with a 3-foot telescope. W. llerschel was the first to resolve this nebula into a densely crowded star cluster. These stars are partially visible in a 4-inch refractor. Nova Ophiuchi, 1848. On 28 April of this year, Hind saw a star 4.5 mag., of a yellowish-red colour in this place where it had never before been visible. The star maintained this brilliancy till 10 My ; it then began to decrease and is now under 12 mag. - 54 Right Ascension 1880. Declination 1880. 16" 54 m 16 h 56" 29 56' 26 5' 16 h 58 m 16 h 59 m 17" 3 m 17 h 3 m 17 h 8 m 9 m 17 h 10 17 h 10 m 24 36' 22 32' -15 56' + 54 38' -26 25' 26 25' + 14 32' + 24 59' + 1 21' 17 h 24 9' 18 25' + 43 16' 4261, Star Cluster in Scorpio. A beautiful nebula, discovered by Messier, 7 June, 1771, and described by him as like a comet. The nebula was resolved into stars by W. Herschel, with his 20-foot telescope. It is beyond the reach of ordinary refractors. 4264, Star Cluster in Ophiuchus, discovered by Messier, 5 June, 1764, catalogued by him as a starless nebula, situated on the parallel of Antares, 3' in diameter, and of which a good view can be obtained with 3J-foot telescope. W. Herschel, in 1784, proved it to be a globular star cluster. 4268, Star Cluster in Ophiuchus, discovered by "W. Herschel, 2' to 2J' in diameter, brilliant and more condensed towards the centre, easily resolved. According to "W. Herschel, the stars are of a faint red colour. 4269, Star Cluster in Ophiuchus, discovered by W. Herschel, 21 May, 1784. It is globular, fairly brilliant, round, somewhat condensed towards the centre, and easily resolved. R Ophiuchi, reddish, and recognised as variable by Pogson in 1853. At maximum it is not more than 7.5 mag., at minimum it is under 12. Period 302 days. /. Draconis (2 2130), 4.5 mag., with a companion 5 mag., distance 2.7". 4270, Star Cluster in Ophiuchus. A globular cluster, fairly bril- liant, large and round, with a sudden increase in brightness towards the centre, can be resolved into stars. It is followed by a faint nebula. 36, Ophiuchi, 5 mag., and of a golden yellow, with a companion 6 mag., distance 4.7", angle of position 211 (1870). a Herculis (2 2140), a variable star of a yellowish-red colour, 3 mag., recognised as such by Herschel in 1795. The changes in brilliancy are not very great, but very irregular. At minimum it is over 4 mag. It has a companion 6 mag., distance 4.7". S Herculis (2 3127), 3 mag., of a greenish -white, with a blueish com- panion 8 mag., distance 19.5". A beautiful object. U Ophiuchi, a remarkable variable star, discovered by Sawyer in 1881. It is generally of 6.1 mag., and at minimum decreases to 6.8 mag. The period is only 20 h 8 m , and the change of brilliancy occupies the short space of 4 hours. In this respect it is the most interesting of all the variable stars known at present. The star naturally belongs to the Algol type. 39, Ophiuchi, 6 mag., with a companion 7.5 mag., distance 11". 4287, Star Cluster in Ophiuchus, discerned by Messier, and de- scribed as a faint, circular nebula 3' in diameter. In 1784, Herschel resolved it into stars, with a 20-foot reflector. 4294, Star Cluster in Hercules. Described by Messier as a starless nebula, with a brilliant centre, easily discerned with a small telescope. A refractor of moderate power will resolve the nebula into stars which are distributed over an area 8' in diameter. The centre could not be re- solved even in Rosse's telescope. 17" l.T 17" 14" 17 20 17 h i'" 17 h -J:r 17*89- 17*30" 17" 31 + 33 14' 12 43' 17 42' :57 16' + 11 29* -23 39' Jl" 23' 57' + 9 40' + 13 15' + 55 16' 3 10* 17 h 31 17" 35- 17*36- 17" 39- + 21 4' + 75 48' + 24 34' + 2 37' ' Hercules, a v ni.iMi' .-; ir. varying from 4.5 to 5 mag., and rod in colour. Tin- |>rrio, Serpentis, 4 mag. There is a star of 8 mag., d = 48", p = 32. J-Ji'Ci, Nebula in Ophiuchus. A brilliant nebula, discovered by W. Herschfl, 17 June, 17*4. It is of considerable size, brighter towards the centre, and can be resolved into numerous very small stars with a power- ful telescope. $ Herculis (2 2161), a greenish -white star, 4 mag., with a com- panion (also somewhat green), 5.5 mag., distance 36". 2 2166, Ophiuchi, ' mag., with a companion 7.5 mag., distance 2.7". 430*2, Nebula in Ophiuchus, annular, faint and small. Nova in Ophiuchus, 1604. At this point there appeared, in October 1604, a star of 1 mag., with a sparkling light second to Venus only in brilliancy. It remained till the spring of 1606, continually decreasing, and then vanished entirely. 2 2173, Ophiuchi, a star of 5.7 mag., golden-yellow in colour, with a companion which is very close to its primary. The distance as esti- mated by Schiuparelli, in 1882, is only 0.3". 53 /, Ophiuchi, a star of 6 mag., recognised as double by Herschel in 1781. The companion is 7.5 mag., and apparently does not change its position. Distance 41", angle of position 191. :>!, Ophiuchi (2 2184), 6.5 mag., with a very faint companion, d = r21.4", p = 77. v Draconis, two stars of 5 mag., visible to the naked eye as a star of 4 mag. Distance 62". 4315, Star Cluster in Ophiuchus. A globular cluster, 7' in diameter, easily seen as a circular nebula. Messier discovered it in 1764, and described it as a starless nebula, not large, faint, standing near a small star of ! mag., easily seen with an ordinary 3J-foot telescope. W. Herschel resolved the nebula into stars with his 20- foot reflector. With a 4-inch refractor, evidence of its resolvability is apparent. It is surrounded on three sides by several brilliant stars. 2 2190, Herculis, 6 mag., with a companion 8.5 mag., d = 10", p = 24. 4321, Nebula in Ursa Minor, 3' in extent, brighter towards the centre. W. Herschel, who discovered it, took it to be a star cluster at an immeasurable distance. 83, Herculis (2 2194), 6.5 mag., with a companion 8 mag., at dis- tance 16.3". The distance seems to be slowly increasing. 61, Ophiuchi (I 2202), a double star, 6 and 6.5 mag., d = 20", p = 93. No cli;mgc of position has been observed since Herschel's time. 56 Eight Ascension 1880. Declination 1880. 17 h 40 m > 17 h >17 h 42 m 17 h 44 m 17 h 17 h 50 m 17 h 54m 17 h 55 m ^ 7 h ggm 17 h 56 m 17 h 57 m 17 h 57 m ] 7 h 57 m 17 h 58 m 27 47' + 17 46' + 27 48' + 72 12' + 23 6' 19 0' + 51 30' + 2 56' 23 2' 30 2' + 21 35' -24 23' 8 10' 22 31' X Sagittarii, recognised as variable by J. Scbmidt, in 1866. The star varies between 4 and 6 mag., within a period of 7 days. 2 2215, Herculis, 6.5 mag., with a companion 8 mag., distance only 0.7", angle 301. (1878.) P Herculis (2 2220), 3.5 mag. and yellowish, with a companion 9.5 mag., d 31", p = 244. In 1856 Clark discovered that the companion itself is double, consisting of 2 stars of 11 mag., which were then at dis- tance 1.8". This distance has since steadily decreased, and is now only about 0.5". A very difficult object. ^ Draconis (2 2241), a star of 4.5 mag., with a companion 5 mag., distance 31". Recognised as double by Flamsteed. 4343, Nebula in Hercules, small, round, rather brighter towards the centre, with a small nucleus. 4346, Star Cluster in Ophiuchus. A beautiful cluster discovered by Messier, 20 June, 1764. Its diameter is 15', and in this space there are nearly 80 stars of 9 to 12 mag. The stars seem to be scattered over the whole field of vision, the lowest magnifying power must, therefore, be used. y Draconis, 2.5 mag., with a very faint companion 11 mag., d = 125", p = 116. Burnham saw, besides, an exceedingly faint star, 13.5 mag., d = 21", p = 152. 67, Ophiuchi. This star 4 mag. has, at distance 55", a red companion 8 mag. The contrast of colour in these stars is pretty. 4355, Nebula in Sagittarius. A group containing several nebulae. Erroneously described by Messier as a star cluster. In 1784, Herschel saw 3 nebula?, with a double star in their midst. J. Herschel found this star to be triple. Either the star or the nebulas seems to rapidly change its position. /H J.Q 4359, Star Cluster in Sagittarius, globular, fairly brilliant, con- densed towards the centre. The stars are exceedingly small. 95, Herculis (2 2264), 5 mag., somewhat greenish, with a companion 5.5 mag., distance 6". 4361, Star Cluster in Sagittarius, a very beautiful object discovered by Messier in 1764, and described by him as a star cluster. It really consists of several nebula, with a triple star and numerous others near to it. r Ophiuchi (2 2262), 5 mag., with a blueish companion 9 mag., d = 100", p 127. The primary, as discovered by "W. Herschel, is itself a double star. Schiaparelli in 1882 found d = 1.9", p = 252. The period of revolution is nearly 200 years. 4367, Star Cluster in Sagittarius, discovered by Messier in 1764, and a beautiful object. The stars are of 8 mag. and under. Messier says they are mingled with nebula, , i: . ' .- . Declination 1 7 h 59" 17" .V.I" 18" 0- 18 k 3 4" 18" 5- 18" 6 18" 6- 18 k 7" 18" 9" IK" 1I 90 + 2 + 48 29' 23 14' + 26 5' :t j 58' + 31 0' + 16 27' -21 36' + 49' - 21 5' 7'. 3 59' IK 2s' "" Sagittarii. reeoglrind us variable by J. Schmidt in 1866. At maximum it i* ."., at minimum ('<.*> mag. The period seems to be from 7 to S da}-. . (, Nebula in Draco. l> >ered by Herschel, 15 Feb., 1786. it as a planetary nebula of great brilliancy, disk 3">" in diameter, one alible vi-ry ill-defined. A long and careful examination iweaN a lirilliant, well-defined centre, round in shape. The nebula can i v. i\ \\cll with u .'(J-inc'li refractor. It gives a beautiful spectrum of bright lint--, lluggins found the 3rd line the faintest. Vogel, on the other hand, declares it to bo quite as brilliant as the second. 7<>, Ophiuchi >;! 2272), 4 mag., and yellow, with a red companion, 6 mag., distance (Schiaparclli, 1 - '. Since Herschel's time, this companion has completed more than a full revolution round the primary. Period of revolution, !."> years. The parallax is 0.10", the distance from the earth = 1,300,000 radii of the earth's orbit. The mcnn distance of the com- panion from its primary is t,:iio million kilometers, or nearly 30 radii of the earth's orbit, and the whole mass of the system is equal to about three times that of our sun. 1 JJ77, Herculis, mag., with a companion 8 mag., at distance 27". l.(7(), Star Cluster in Sagittarius, large and fairly rich. 100, Herculis (S I'-JSO), two stars 6 mag., distance 14". 73, Ophiuchi (X 2-2H1), a difficult double star 6 and 7.5 mag. The distance seems to have decreased since Struvc observed it. In 1876, it was only 1". T Herculis, a variable star, discovered at Bonn in 1857. Its bril- liancy ranges from 7 to 12 mag. It is of a deep red colour. Period 165 days. 2 22.s!>, Herculis, a star of 6 mag., with a companion 7 mag. Dis- tance, only 1.2''. -i, Star Cluster in Sagittarius, a fairly large, and scattered cluster of stars, ranging from 9.5 to 11 mag. i, Nebula in Ophiuchus, fairly brilliant, plauetary. Its spectrum contains the three early recognised bright lines, of which the first is the most brilliant, the last (falling on F), the faiir /* Sagittarii, a quintuple star, primary :!.."> mag., and yellowish, has a companion 10 mag., d = 25", p= 11!) ; another 10 mag., d = 50" p = 115. The other two companions seen by llurnham, arc merely faint points of light. 40, 11, Draconis ^1 2:U>.>;. Seen with the naked eye, these look like a star of 5 mag. They are really two stars 5.2 and 6 mag., dis- tance 20". l:t!)7, Star Cluster in Sagittarius. A rich star cluster, discovered :\ Messier, 20 June, 17<>4. Nearly 1J J in diameter. Visible to the naked eye as an off-shoot of the Milky Way. i 58 Kight Ascension 1880. Declination 1880. 18 h 12 m - 13 50' 4400, Star Cluster in Scutum Sobieski. A cluster of small stars discovered by Messier on 3 June, 1764. It is 8' in diameter, and in the Finder looks like a faint nebula. 18 h 13 m - 17 12' 4401, Star Cluster in Sagittarius. Discovered by Messier at the same time as the cluster just mentioned, and described as less brilliant than it. Messier says that it looks like a nebula when seen with an ordinary 3 3 foot telescope, while with a powerful instrument stars only are visible. Diameter 5'. Contains a double star 8.5 and 10.5 mag., distance 25". 18 h 14 m -16 15' 4403, Nebula in Sagittarius. Something like a horse-shoe in shape. Discovered by Messier 3 June, 1764. He describes it as a luminous, star- less streak, 5' to 6' in length, spindle-shaped, not unlike the nebula in Andromeda, but very faint. There are two stars near it, parallel with the equator, but visible only in a telescope. In clear weather a very good view of this nebula may be obtained with an ordinary 3|-foot telescope. W. Herschel was the first to get a perfect view of it. According to Holden, one arm of this nebula has changed its position. The spectroscope shows the nebula to be a mass of incandescent gas. 18 h 17 m -24 56' 4406, Star Cluster in Sagittarius. A densely crowded cluster of very minute stars. Seen by Messier, 27 July, 1764, and described as a starless, circular nebula, not easy to distinguish with a 3J-foot telescope. Diameter 2' A powerful instrument is required to divide it. 18 h 18 m -20 36' 21, Sagittarii. A star of 5 mag., which has, at distance 2", a faint companion 8 mag., discovered by Alvan Clark. 18 h 21 m + O 9 7' 59 d, Serpentis (2 2316), 6 mag., yellowish, with a companion 7.5 mag., d = 3.9", p = 314. 18 h 22 m + 6 29' 4410, Star Cluster in Ophiuchus, large, coarsely scattered, discovered by Caroline Herschel in 1783. 18 h 22 m + 58 44' 39 b, Draconis (2 2323), 5 mag., with a companion 8 mag., d 3.1", p = 2.3. Also another 7 mag., d = 90", p = 22. 18 h 23 m + 74 29' 4415, Nebula in Draco. A remarkable nebula, fairly large and brilliant, preceded by two stars. According to Tuttle it is variable in brilliancy. D'Arrest in writing on this subject to J. Herschel, 8 May, 1863, says that on 24 Sept., 1802, Tuttle's nebula was so brilliant and remarkable in the Finder, (2 min. long and 80" broad) that he is convinced it has increased in brilliance since J. Herschel and his father observed it. /18 h 23 m + 71 16'

    0' 8 1'.' + 38 40' 4 9 31' 1 5' + 39 33' + 37 29' 5 50' + 20 26' + 60 56' I !_' I, Star Cluster in Sagittarius, discovered by Abraham Ihlr, mold not dMtagakb any star in it, catalogued it as cir- cular, and easily seen with a common u-liwopo of 3J' focus. It is sur- rounded by ."> irregularly placed stars. Herscbel's 10-foot telescope resolved l.ula into a star cluster. Towards the middle the stars are denser; diaineti-r .^'. 1 l _'.. Star Cluster in Scutum Sobieski, large, fairly rich, and of moderate density. l>i-o.vm-iJ l.y \\~. Hurschel, 16 June, 1784. Lyrae ^Vega). This splendid star, 1 mag., has near it several faint stars, but their connection with it is merely optical. One of them, which was used by Struve and Briinnow as a comparison star for cal- culating the parallax of Vega, is of '..:, mag, d = 48", p = 156, another of '.( mag., d = 1JO", p = 40'. Winnccke and Burnham have also measured a very faint star (13 mag.), d = 52", p = 292. H _".!. Star Cluster in Scutum Sobieski, large and rich, but the stars are little more than minute luminous points. 1 i:i-', Star Cluster in Scutum Sobieski. 2' in diameter. Discovered by Messier, 5, Aquilae (2 -..MT'.l), (> mag., with a blucish companion 7.4 mag., distance 13.2". There is also a second companion 11 mag., d = 27.3", p = It:. . and 5 Lyrae. A very interesting pair of double stars, first observed by Flamsteed, though with keen fight and under specially favourable cir- cumstances, E and 5 Lyrae can IK; seen as clearly separated. The distance, according to Auwers, l8i-J, is -Jds". The fact that each of these stars is itself double was verified by Christian Mayer, and in 1823 John Herschel discovered three other very faint stars between t and 5 Lyrae. The distance of the two components from s is, according to Dembowski, 1863, 3.045". The distance of both stars from 5 Lyrao was in the same year . and seems to be slowly decreasing. Lyrae, a star of 4 mag., with a companion 5.5 mag. ; distance 44". Recognised by Flamsteed. R Scuti Sobieski. Recognised as variable by Pigott in 1795. The change of brilliancy is very irregular ; at maximum the star is sometimes 4.5 mag., though it is often under 5.5 mag., at minimum it is 6, sometimes 8 mag. The period is irregular. 110, Herculis, 1 mag., with a companion 11 mag., d = 61", p = 92. Burnham saw a still fainter companion, d = 45", p = 95. -J !(:{, Draconis, (i mag., with a companion 9 mag. According to Struve, in 1N32, d = 1.9", p = 259. GO Uiftlit Ascension 1880. Declination 1880. 18 h 45 m 6 25' 18 h 46" 18 h 46 m 18 h 47 m 18 h 48 m 18 h 49 m 18 h 50 1 18 h 50 m 18 h + 33 13' + 10 12' - 8 51' 30 37' + 32 53' + 4 3' + 33 49 + 43 47' 4437, Star Cluster in Scutum Sobieski. Discovered by Kirch in 1681, and described later by Messier as a cluster of small stars, only visible with a good instrument. The stars can be clearly seen with a 3 J -inch refractor. Lament and Helmert have taken the measurements of the whole cluster by Trigonometry. /3 Lyrae, a variable star with three companions, a pretty spectacle when seen with the telescope. The primary is yellowish white, at maximum 3.5 mag., at minimum 4.5 mag. The period of the change of brilliancy is 12 days 21 h 51 m , with a double maximum and minimum. The spectrum of this star occasionally contains bright line?. Of the companions, the most brilliant is 7.4 mag., d = 45.6, p 149 ; a second, 8 mag., has d = 66", p = 318 ; a third, 8.5 mag., d = 86" p = 19. Finally, Burnham has seen a fourth very faint star (11 mag.) d = 46", p = 248. 4440, Star Cluster in Aquila, a beautiful object, consisting of stars 9 to 12 mag. Vogel has measured 62 of them with the micrometer. 4441, Nebula in Scutum Sobieski, brilliant, large and nearly circular, more condensed towards the centre. According to Herschel it is resolvable into stars. 4442, Nebula in Sagittarius, discovered by Messier in 1778, and described as a faint nebula with a brilliant centre. According to Herschel it is a globular star cluster consisting of very minute stars. 4447, Nebula in Lyra, the beautiful and easily- observed Ring nebula. Discovered by Darquier, at Toulouse, 1779, between /3 and 7 Lyrac. He describes it as very delicate, with well-defined boundaries, of about the same size as Jupiter, and looking like a planet that is about to become extinct. Messier describes it as a luminous cluster, apparently composed of small stars. It is, indeed, remarkable that this nebula, which appears like a disk, with a bright border, has a brilliancy wherein one fancies one can see twinkling star-points. Rosse and Bond maintain that they have succeeded in resolving it into separate stars, but its spectrum is one of bright lines which indicate that it is really composed of incandescent gas. A minute star of 10 mag. follows the nebula closely. [The 36-in. Refractor of the Lick Observatory shows three stars in the central space, where Lord Rosse's drawing gives a blank field. See Nature, August 9, 1888. ED.] 6 Serpentis, a yellowish white star 4 mag., with a somewhat faint companion at distance 21". Multiple Star in Lyra. The primary, 6 mag., has a companion 6.5 mag., d = 45", p = 351. Struve repeatedly ohserved this double star, but Burnham in 1879 was the first to discover that the primary is itself double, there being tear it a small star of 10 mag., d ~ 1.7", p = 126. -fi Lyrae, a variable star discovered by Baxendell in 1856, of a reddish colour. The change of brilliancy is but slight, the star varying between 4.3 and 4.6 within a period of 46 days. 61 ,-- ttin IK 1 ' :, 1 Lfi _ | n I..H- i- f - 3' HI 19' in 1 + 4 3' ll h 10- - 57' 19" 11- 1 8' J()h J2 m + 2 ( .> 58' 19*1-2- + 87 55' 11)" 1-2" + 52' 19" 13- + <> 2 ' 19" 16- + \* 57' + -21 25' 26- + 27 42'. 19 1 ' + Hi' 12' 19" 34- + I'- 1 56' 19 h 34- 16 34' 19 h 36" + 26 32' 19" 37- + 1P 32' 19" 37- 14 11, Aquilae. '> 111,11:. :m 1 white, with a faint companion '."..' urn:., ili-t mo- 17.1", ;inu r lf "f |>"-itiii -JVJ . Discovered by W. u li 29 .' UK . I7--1. An uptical double star. /* Aquilae, i\\<> >t:ir- '. HKI^., distance 3(5", recognised as a double star by llnidi' /,' Aquilae. :i vanul.lr 4ur of a deep red colour. At maximum it is _'., at minimum 11 mag. Period 345 du\ 17 Lyrae, (- ~t('il), n yellowish star (5 mag., with a companion 10 mag. d= 3.7", p ;.'! . l!7<), Star Cluster in Aquila, fairly large, rich, somewhat dense, diaim-tcr 12' to l.V. Discovered by W. Herschel, 30 July, 1785. r, Lyrae, (- -4S7), a blueish star l.~> mag., with a companion, d - p = 84. 448J, Star Cluster in Aquila, consisting of sturs from 9 to 1*2 mag., > c-red by W. Herschel. 11^"., Star Cluster in Lyra. Di-coveml by Messier '23 January, 177'.i, as a starless nebula in Lyra. In 1784 Herschel resolved it into stars. It appears dull in a 3J-inch refractor; 4' to 5' in diameter. S Lyrae, 4.5 mag., with a companion 8.5 mag., d = 101", p = 70. 23, Aquilae (2) -249^), mag., yellowish, with a faint companion 9.5 mag., d = 3.4", p = 11. 4487, Nebula in Aquila, fairly large, round, of moderate brilliancy. According to Rosse it is of spiral arrangement. i! 2")04, Yulpeculae, C.5 mag., with a companion 8 mag., d = 9". (i Yulpeculae, appearing to the naked eye like a star of 4 mag. In reality '2 stars of 4 and 5 mag., d = 403". ft Cygni, a reddish yellow star 3 mag., with n blue companion 5 mag., distance 34". The primary is variable, but the variations of brightness are not important ; the colour also varies slightly. f Sagittae. 6 mng., with a companion 7.5 mag., d 92", p = 81. /.' Cygni, of a deep red colour, at maximum 6 mag., at minimum very faint (3 mag.) Recognised as variable by Pogson in 1852. The period is, t, 417 days. [Reported Aug. 13, 1888, to have a remarkably bright line (apparently F) in its spectrum, thus indicating a change in its con- stitution since Duner's observations in 1879 80 and 1882. EDIT.] 54, Sagittarii, (i mag., with a companion 7.5 mag., d = 45", p = 42, and another very faint companion, discovered by Bumham, d = 36", p = 245. 4508, Star Cluster in Yulpecula, very large, fairly rich in stars, not very dense. The stars range from 9.5 to 12 mag. X Aquilae, G mag., with a companion 7 mag., distance only 0.6". 4510, Nebula in Sagittarius, a planetary nebula, discovered by Herechel 8 Aug., 17 mag., with a oompailioil ii". Struve calls both stars white, but at present one star seems to be yellowish, the other gives a greenish light. 4- Cygni (2 '2005), a white star of 5.6 mag., with a companion ~i.~> mag., distance :!". |.-):t-2, Nebula in Yulpecula, Ilosse's "Dumb-bell Nebula." First discovered in 1704 and described by Messier as an oval, starless nebula. A 4-inch refractor shows two contiguous nebuloo of moderate brilliancy, surrounded by some stars. The great telescopes of the two Hcrschels showed no more than this. The best drawing seems to be that of Sccchi, who recognised the existence of a multitude of stars between the two nebulae. According to Huggins these latter give a spectrum of bright lines, and are therefore really masses of incandescent gas. 1:<, Sagittae, 6 mag., with a companion 7.5 rang., d = 340", p = 13. 16, Yulpeculae, two stars of mag., at distance of only 0.0" from one another. They can be resolved in none but the largest telescopes. 4543, Nebula in Sagittarius, discovered by Mechain in 1780 as a starless nebula. l$ut even Messier recognised stars in it, and W. Herschcl resolved the whole into a star cluster. I'itt, Star Cluster in Cygnus, large, 15' in diameter, very rich in stars of considerable brilliancy and very dense. Discovered by W. Herschrl 11 Sept., 17s'. i. 2 2628, Aquilae, yellowish, G mag., with a reddish companion 8.5 mag., d = 4.2", p = 346. No motion has been observed in the companion since the time of Struve. 6 Sagittae, (2 2(W7), G mag., with a companion 8 mag., d = ll.-J", p = 327\ and a second companion 7.5 mag., d = 76.5", p = 225. 2 2G44, Aquilae, a double star 6 and 7 mag., d = 3.6" p = 208. The primary is of a blueish, white colour. 4559, Star Cluster in Yulpecula, a not very dense cluster of moderate brilliancy, fairly rich in stars, some of 6 to 13 mag. Schultz at Upsala has obtained accurate measurements of this cluster. 2 _''" I, Aquilae, a star of 6.5 mag., with a companion 8 mag., d = 12", p = -2" I . . o ; , Cygni, a star of -3 mag. with a companion 5 mag., d = :; p = 3'23, and a second companion 7 mag., d = 107", p = 173. Kight Ascension 1880. Declination 1880. Kight Ascension 1880. Declination 1880. 20 h ll m igo 55' 20 h 13 m + 37 40' 20 h 13 m -19 30' 20 h 13 m + 77 21' 20 h 14 m 15 10' 20 h 17 m + 19 43' 20 h 19 m + 40 20' 20 h 20 m 18 36' 20 h 22 m 18 12' 20 h 23 m 18 59' 20 h 27 m + 25 24' 20 h 28 m + 6 59' a 3 , a 1 Capricorni, two stars 3 and 4 mag., both yellowish, distance 376". Each of them is itself double, a 3 has a companion 10.5 mag., d = 7.4", p = 150. This companion again was found to Be also double by Clark in 1862, and consists of two stars of 11 mag., distance only 1.2". They can be divided by the very largest telescopes only. There is a third star (9 mag.), d = 154", p = 156. The star a 1 has near it a star of 8.5 mag., d = 44.3", p = 221. Burnham found also a small star of 14 mag., d = 40", pm!82, but this was only visible in the 26-inch refractor at Washington. P Cygni, a star of 5.6 mag., which suddenly increased in the year 1600 to 3 mag., disappeared in 1621, but was again seen in 1655 by Cassini as a star of 3 mag. ; it then again disappeared. Since 1677 it has been 5.5 mag. without variation. It gives a yellowish light. a Capricorni, a star of 6 mag., with a companion 9 mag., d = 54". Seen by Herschel. x Cephei, (2 2675), greenish white, 4 mag., with a companion, 8 mag., d = 7.3", p = 124. /3 Capricorni, 3 mag., and of a golden yellow, with ablueish companion 6 mag., distance 205". Between the two stars somewhat to the north of a line joining them is a star of 11 mag., which as discovered by J. Herschel, is itself double, and consists of two stars of 11.5 mag., distance 3". In Herschel 's opinion no telescope can distinguish the moons of Uranus if it cannot make these two stars clearly visible. Only large and powerful instruments can do this. 4572, Nebula in Sagitta, planetary, but described by J. Herschel as capable of being resolved into stars. Lament speaks of it as a circular mass of nebula having a distinct nucleus in the centre, but without any trace of resolvability. The nucleus was not visible in Herschel's telescope. The nebula is placed between a number of stars. 4575, Star Cluster in Cygnus, a moderately rich but rather small cluster containing stars of 10 to 12 mag., besides several more brilliant. it Capricorni, a somewhat yellowish star of 5 mag., with a faint companion 10 mag., d = 3", p = 146, discovered by Burnham. Capricorni, 5 mag., with a companion 8 mag., d = 3", p = 173. There is also a distant companion 7.5 mag., d = 236", p = 151. o Capricorni, 5.6 mag., with a companion 7 mag., distance 22". Recognised as a double star by Bradley. 2 2695, Yulpeculae. The primary is 6 mag. and white, the companion 8 mag. The position of the latter, according to Engelmann's calculations, 1884, d = 1.4", p = 81.5. 4586, Nebula in Delphin, faint, somewhat brighter towards the centre. A star of 9 mag. precedes it. "W. Herschel resolved the nebula into stars. 65 0,,h ._>,,, . 20" 33" 2. i' :?iy< 20*40" 20" 41" 20" 41- 20*41- IP 1-2-" 20*43- 20*44- 20" 45- i. 1UO. + GO* 3 16' 27' 54' + 14 11' + 4' + 15 29' 31 52' + 15 58' + 30 18' + 15 42' + 30 17' + 33 56' + 36 3' 5 35' 6 4' i. Star Cluster in Cepheus, a beautiful, rich star cluster from 8' in iliiimi'trr. MiMMvriviI l.y Herschel 9 Sept., 1798. '1, Star Cluster in Yulpecula, discovered by W. Henchel, bril- liant, fairly large and rich, containing many brilliant stars densely massed together. & Delphini ( i -2704), a greenish star of 3.4 mag., with a faint companion 11 mag., d = :r,..Y', p - :w:>.H". There is a second exceedingly faint companion, d = '27.')", p = 115. Finally, Burnham found the primary to be itself double, consisting of two stars at a distance of only 0.26". 1, Aquarii, ii star of 5 mag., with two very fuint companions (11 mag.), whose positions Burnham calculated in 1879 as follows : d = 55.8", p = 217.4 ; d = 72.9", p = 38.9. a Delphini, 4 mag., with a companion 9.5 mag., d = 35", p = 278. There are in addition throa exceedingly faint stars near the primary, d = 20", p = 225 ; d = 45", p = 350 ; d '= 81", p = 114". Auwere in 1858 found from numerous comparisons that * fluctuates in brilliancy to the extent of about half a magnitude, within a period of about 14 days. Since the date named this change of brilliancy does not seem to have been again noticed. 49, Cygni (2 2716), 6 mag. and yellowish, with a blueish companion 8 mag., distance 2.7". In both stars the colours are easily recognisable. T Delphini, variable, discovered by Baxendell in 1860. At maximum it does not exceed 8 and often scarcely 9 mag., at minimum it is 13 mag. Period 331 days. 4600, Nebula in Cygnus, a remarkable, irregular nebula, fairly bright and large. It extends beyond 52 Cygni. Discovered by ITerschel 7 Sept., 1784 ; as seen by him it extended over more than 1, indeed, with the highest magnifying power, almost 2. y Delphini (2 2727), a star of 4 mag., golden yellow in colour, with a greenish-blue companion 5 mag., distance 11". 52, Cygni (2 2726), yellowish, 4 mag., with a companion 9 mag., distance 6.2". T Cygni, recognised as variable by Schmidt in 1864, it is usually about 6 mag., and yellowish- white in colour. The changes of brilliancy are slight but unmistakeable. ' Cygni, 5 mag., with a companion 10.5 mag., distance 85", angle of position 104. Strove discovered that the primary is itself double, consisting of two stars of 5.5 mag., distance 0.6". A very difficult object. T Aquarii, recognised as variable by Qoldschmidt in 1861. At maxi- mum it is often somewhat above 7 mag., but at minimum it diminishes to 13 mag. Period 203 days. 4, Aquarii (2 2729), a very difficult double star. The primary is 6 mag., and somewhat yellowish, the companion 8 mag. According to Burn- ham (1879), the distance is only 0.6", angle of position 167. 66 RiKht Ascension 1880. Declination 1880. RiKht Ascension 1880. Declination 1880. 2Qh 47 m 12 59' 20 h 50 m + 4 4' 20 h 53 m + 3 50' 20 h 56 m + 15 45' 20 h 56 m + 47 3' 20" 56 ra + 6 42' 20 h 56 m + 47 3' 20 h 57 m + 1 4' 20 h 58 m 11 50' 20 h 58 m 6 18' 20 h 59 m + 23 21' 21 h lra + 38 10' 21 h 3 m + 41 45' 4608, Star Cluster in Capricornus, discovered by Mechain as a faint nebula. Messier, too, observed it, and remarked a small telescopic star close to it. Herschel, in 1783, resolved the nebula into stars, and the 40- foot reflector, 4 Oct., 1810, with a magnifying power of 280, showed separate stars even in the centre of the cluster. It is nearly 2' in diameter. Several other stars appeared in the field of vision, but they were, as Herschel remarked, quite distinct from the minute points of light to he found in the cluster itself. 2 2735, Equulei, a star G mag., with a companion 8 mag., d = 1.8", p = 287 1, Equulei, (2 2737) a yellowish star of 5 mag., with a blueish com- panion 7 mag., distance 10.8". The primary, as discovered by Struve, is a narrow double star of 5.7 and 6 mag., distance, according to Engelmann (1884), 1.26". 4625, Nebula in Delphinus, fairly brilliant, not large, round, brighter at the centre. 59, Cygni (2 2743), 5.6 mag., with a companion 9.5 mag., d = 20", p = 352. 2, Equulei (2 2742), two stars of 6 mag., distance 2.6". No per- ceptible change has been observed in their relative positions during the last fifty years. /' Cygni (2 2743), a star of 5.6 mag., greenish-white, with a com- panion 9 mag., d = 20", p = 352; there is also a second companion 10.5 mag., d = 26.7", p = 141. 2 2744, Equulei, a star of 6 mag., with a companion 7 mag., distance 1.5", 4628, Nebula in Aquarius, a beautiful, planetary nebula, discovered by "W. Herschel, 7 Sept., 1782. The disc appears to be somewhat blurred at the edges in a telescope of medium strength. Lassell saw a bright ring within the nebula, and Rosse calls it " Saturn nebula." The spectrum, according to Huggins, shows it to be of a gaseous nature. Vogel also finds the three bright lines in it. 12, Aquarii, 6 mag., with a companion 8 mag., d = 3", p = 190. H Yulpeoulae, a variable star, which at maximum seldom reaches 7.5 mag., and at minimum disappears even in the most powerful telescopes. Period nearly 140 days. Discovered at Bonn in 1858. 61, Cygni (2 2758), 5 mag., with a companion 6 mag., both golden yellow in colour, but of slightly different tints. The distance is 20", and the change of position is rapid ; it has not yet been possible, however, to calculate the period of revolution. According to Struve, the parallax of this star is 0.5", its distance from the earth is, therefore, about eight billion miles. Nebula in Cygnus, recognised by "Webb, 14 Nov., 1879, as a star of 9 mag., surrounded by nebula. Schmidt describes the nebula as elongated in shape, being 8" to 10" in length, condensed towards the centre, which seems of a stellar nature. Vogel finds the spectrum to contain the three bright lines very clearly marked, the rest of the spectrum being faint and continuous, - 67 A - - IUO. ... 1180. 21" 5 m 2l h 7"' 21" 8- 21" 8 2 l h > 31' :(7 32' + 34 23' + 58 7' + 19 17' + 6 18' 11 39' 1 21' + 70 2' 7 Equulei, "* mat:., yellow, witii a companion ( mag., distance 366". Tin- primary i* itself double, having a small star 10 mag. at d = 2.1", p = '27 J.."> . Burnliam also saw a very faint star, d = 41", p = 10. I'. l.">, Star Cluster in Cygnus, an extensive but not very rich cluster of stars of 10 mag. A star of 7 mag. follows it on its edge. T Cephei. riTu^iix-d as variable by Ceraski in 1879. At maximum the star is 5.5, at minimum '.) mag. Period 390 days. - -27.SO, Cephei. The primary ii (>, the companion 7 mag., and both are white. Wilson (1873) calculates, d = 1.0", p = 224.3. No change of position has been observed since the time of Strove. J Equulei (2 2777), 5 mag. and yellowish, with a companion 10 mag. In 185*2 Otto Struve found that the primary is itself double, having a companion 10.5 mag. near to it. Burnham (1880) calculates : ABd = 0.35", p = 29. AC d = 22.7", p = 37.9. The primary can only be divided with a most powerful instrument. r Cygni, 4 mag., a difficult double star, discovered by Clark in 1874. According to Burnham, the companion is at d = 1", p = 150. Hall saw another very faint companion, d = 16", p = 260. v Cygni, a star of 4.5 mag., with two faint companions of 10 mag., d = 15", p = 219, and d = 21.5", p = 178. 2) '27110, Cephei, 6 mag. and red, with a companion 10.5 mag., d = 4.5", p = 46.5. 1 Pegasi, a yellow star 4.5 mag., with a companion 8.9 mag., d = 37", p = 301. /B Equulei, 5 mag., with a companion 10.5 mag., d = 67", p = 309, and, in addition, a second companion 11 mag., d = 86", p = 276. The first companion is itself a double star of 10 and 11 mag., distance 6.5". Burnham also found a very faint star, d = 32", p = 260. This latter is visible in a very powerful telescope only. 4670, Star Cluster in Pegasus, recognised as a nebula by Maraldi as far back as 1745. Herschel resolved it into a globular cluster of stars. With a 5-inch refractor it has this appearance, though the centre cannot be resolved. At the edges are scattered a large number of stars of from 11 to 12 mag. Diameter 3' 4' 4678, Nebula in Aquarius. In the average telescope this appears to be of moderate brilliancy and circular, with a small faint star at the eastern edge. Discovered in 174(3 by Maraldi, was resolved into stars by 1 1 er-chel. /3 Cephei (2 2806), a greenish-white star of 3 mag., with a companion 8 mag., d = 13.6", p = 250. 68 Right Ascension 1880. Declination 1880. 21 h 28 m + 47 54' 4681, Star Cluster in Cygnus, a large and beautiful cluster, discovered by Messier in 1764, visible in a small telescope. 21 h 32 + 6 5' 3, Pegasi, a star of G mag., with a companion 7.5 mag., d = 39", p = 349. No change of position has been noticed since it was first observed by W. Herschel. 21 h 34 m 23 43' 4687, Star Cluster in Capricornus, described by Messier as a strip of starless nebula visible only with difficulty. It can be resolved into stars with a 5-inch refractor. Herschel saw the stars with a 10-foot reflecting telescope. 21 h 35 m + 56 54' 2 2816, Cephei. Triple, with a distant companion. The primarv A is / 6 mag., B 8, C 8, D 9. Wilson and Seabroke's calculations (1873) are as follows: A B p = 122.3, d = 11.7" ; A C p= 339.9, d = 19.8"; A D p = 174.2, d = 50". 21 h 37 m + 78 5' I, Nebula in Andromeda, u .small, brilliant, planetary nebula; 15" in (liamrti r, iliM-m-. iv 1 l>y \V. Herscbcl, 6 Get, 1784. Lasscll rccog- ni-r.l in it n nucleus with two oval rings, Rossc a spiral arrangement. The spirt rum (according to Huggins) contains four bright lines indicating a gaseous nature. R Aquarii, a star of a somewhat deep red colour, recognised as vari- able by Harding in 1811. It varies from 6 to 11 mag. Period apparently somewhat under 390 days. 107, Aquarii, 5.6 mag., with a blueish, white companion 7 mag., d = 5.8", p = 138. 502M, Star Cluster in Pegasus. A cluster of coarsely scattered stars of 10 mag. and upwards. 5031, Star Cluster in Cassiopeia. Discovered by Caroline Herschel in 1783, between j and Cassiopiea. The stars are numerous but not brilliant, and the whole object is a beautiful sight in a powerful telescope. R Cassiopieae, recognised as variable by Pogson in 1853, of a deep red colour. At maximum it is 5.5, at minimum 12 mag. The period is about 4'2(5 days and seems to be decreasing. a Cassiopieae (2 3049). Discovered to be double by W. Ilerschel, 31 Aug., 1780. The primary is 5.4 mag. and greenish, the companion 7.5 and deep blue in colour. The colours in both are very intense. The position of the companion does not seem to alter, d = 3", p = 326. 2 3050, Andromedae, two stars 6 mag., distance 2.9". 85 Pegasi. A star of 6 mag., with a companion 9 mag., d = 15", p = 30, also an exceedingly faint companion 13 mag., d = 62", p = 277. Finally, Burnham (1878) found that the primary is itself double, there being an extraordinarily faint star near it, distance only 0.7", angle of position 287. This companion cannot be discerned save in an instrument of the first class. EDITORIAL NOTE. In " The Extension of the Law of Gravitation to Stellar Systems," by Prof. Asaph Hall (Gould's Astron. Journal. 177), it is shown that there is a theoretical difficulty in applying Newton's Law of Gravitation to double stars, a difficulty which is increased by the so-called " runaway " stars, like Groombridge, 1830, stars moving through space with the speed of a comet at perihelion, and yet with no visible attracting body near them. Prof. Hall's recent /' it determination of the parallax of Arcturus (only -\- 0.018 0.022) if accepted brings this star within that category, for it has a great proper motion (amounting to 373 miles per second at right angles to line of sight, and 55 miles per second in the line of sight). The following Table gives some of the stars of which the parallax, and motion across, have been ascertained ; 72 STAR'S NAME. Magnitude. Parallax = Distance in years of light. Annual Motion across. = Miles per second. a Centauri .... 1 900 3-57 3-674 11'9 61 Cygni . . . . . 5 511 6-31 5-221 30- Lalande 21,185 . . 7 501 6-45 4-734 27-7 Groombridge 34 . . 8 307 10-52 2-801 26-2 Lalande 21,285 . . 8-5 260 12-43 4-403 49-5 o Argelander, 17,415 9-5 247 13-08 1-200 14-2 a Draconis .... 5 222 14-56 1-925 25-3 Sirius 1 193 16-74 1-252 19- 70 Ophiuchi . . . 4 162 20-0 1-108 20- a, Lyrse .... 1 153 21-12 0-347 A. 7 Groombridge 1830 . 7 147 22-0 7-053 *J i 140- i Ursoe Majoris . . 3 133 24-29 0-525 11-6 a. Bootis 1 127 25-44 2-258 52- y Draconis .... 2 092 35-12 0-063 2- a. Aurigse .... 1 046 24-12 0-438 27-8 Pole Star .... 2 046 24-12 0-045 2-9 Printed by PERBY, GAEDNEE & Co., 21 & 22, Cursitor Street, London, Right Ascension^ Klein, Star.A&aa. 17'.' IB? w M* lfl aw K-Ixnlon. oviir.lt. iirliul. in ,l,,lrr ioht Asrouxuni" '' Di-fluuiluin- ">8 Kl.-lH Sl.n-AU.is * HV I o vni Right Ascension = 13^ Declination- +58 Klein, Star Atlas. S P C K-London. NIA. Right Ascension = 18*> Declination^ 58" Klein , S tar Adas . S P C KLondon. .V" *r.t. \ \ Right Ascension^ 2 Z^Dedination -+ 58 Klein. Star Allan . S P CKIxndon. Right Ascension- 2 2*M)edinaiian -- 3 3 31 * r* ,* . a e ' & 10" O ipT rriri <1 f ' ' j^ *. < 1 tf TTW * t W . t. 10" # -f .* -i- t I -fzo 20v :$o i i i- Kleiii, Slar^Ulas. VII. ,. a- I 1 ' .- v- ("' *.- ' . . h . . . . . Hj> . . " '*'**' 1 , . * ! . - m\ >* * n* M ' no * ' ^ i 4 M I M \ "" ' * * i . ' i f < i . . 4 I 4 . * * *"' g . ^ . > ' * f . , r . & * i . . . t . . * '*+ M o/y. K ' + f + ^ A , , . . i 1 f . .. \ ^ * .TO" +* *>" i r~ 1^ O* .- S P r K london. Dedination= + 90 Klein, Star Aflas. .(?". ii ."' ovw.it. nrbiila . Tor Pronuilnifi ChruiUaji KmwlFd^.Londcn. Right Asrensioii= 6 1 . 1 Declination =-3 Klein, Star Atlas. VIII . .v~ 1 * 4 ** t IP* t h P* I , p V . ' & "" * ^ . < ^ * '- ^ . M \ a: ' fc ***** *" ' M * * * t ' ' ' '.. . . 1 - ^ * I ' . f-", . ' A/wr * '. rf ' , .** * ' ** -d t f. **~ . t ... * . ' :.* t N i * -"jr . . r* a * -4- ; . iT f 4 M 1 4 *> H u A -4 . ' .. , i 1 ^ * "4 . ' & , . . * 4 '" . * * . i or rturirr '' Right Ascension = 10^ Declination = -3 i J 2* m~ ] 1> W" 2 am. ^ .-^ 1-1 " A ^ 7 14 C itlillOT . + V m t * / * * * a '(f 5? $ 4 s /. "* f +> i r y ttgS | O .,, 1 ao . ' E- **** -f . & _ ? ', , =J7J " & .'yj Z2O7* am* j^ sS- > MJ% \ . . OH 5u - 2O " *' t f fix * A ' * J * *# ''' Sw JGs* X 4- t .4 *. 4 A V rv^- J.*, * t f* 4* 10 * 4 fc i i #. * ,1t2S *+ 30" 1 * Klein, StarAQas. IX. 40* ft7 \\ h <0M *> 8* * * . i IT .. . . * . . " f ' . . . T *' . .- If . . % > / : ' '*' L - . . . . . * ; *4 ' ' \ ^ 4 . . k ^ . * . ^ * jl ~ !*. sn : .. . * * 4" fc . ^ r~rr . 4* . * A * ^. ., f M> * jj . * ? w o cr E R. . j*t ** .V . o [' * # r ^* * . 1 . . -. j i * t T / * 4 - 1 T * r 1 . ik ^ f % . ^ V . * . 4-* * . , I . > . | * * \ * . . t tr V *< i * t .TV T -f . i ! * - 9* 8* . S V C. Right Asceusiem= 14^Declination.=-3 * 20* * k C: U i . " * ,? * t M* i >^ . >f * Of ' -.4-- -*/' * 10i ja Wl ^f- I* y* * "* * 30 /; \ *i ^ f y Klein, SlarAflas . X. : e- 1 :> I- 1 2" a" . . . < ** . * . . ' A J | . * 4* 1 B E R ? * . o * J 1 1 i * + * ' * K . . " .**.* "~ . ft * A % *> . . * * < UY* S j _ **" * V ^ ' . **- 1 * . * < . + i - A ' i t * 'I iA,/7 no _ .0 " * i ( . t ; 9 T 4* T * . * T ' i . * * . A t *- .J- , * }f> . . X 'T ' . * ^ . . . C A T'E R . *^t . , f * KiC,l % Klein, Still- AQas. XI. . . "V M . >', ' m n i19 * . 22* . V * M * * . . L'. gj .r . . . * ...,* *- ^ ' . . " . ' 1 . 4. B *" ** f . . *' ' * i . . .. (SP i f * * . in # // 9 V* f ' g) ^> 1 . , I"-' .4 . . * . 5= . + + *. , a>" . 1 e * * . f to . *3 * * .<* /'* ' * i +V M . -f # "*" ; TOO . . -^- ' .^^ * r ^ + B . . * * * ** * . . . f . . V*" jjjf;. ,/' ' i jm. C 11 * j a , n 2 3* >" 2" Kloin, Stai-AdaK. XII . ) * 1" * i J _ 3 ()" i . . . f t ^ . . * . '* . t ; A*" _ f . T g * * . ' Jfe . ' " . ' * * ^* ^ ' . . (.,. .* * ' . <> o ^^ * * . ' 1 J '. . . ' . . * t . * * * * -*: M * i raw ' * . . . . * .. . . ' . * . . * .. . / \ . \ m * f . H * . -~ i i * . * * . * ' -**- OB . * < 2 ' a* * . * . v ' . * f . . ' __ ***^ . ^ . - *' * * * ' . *>- m~ 2 1* j p 2 O k S I' C K :, I 1 I .K London SITY Kt. Asc. I9h 55" Decl. + 37 45'. Part ol the constellation of the Swan (Cygnus.) lleliographical reproduction from a photograph by the Brothers Henri of Paris, without modification. In tl Klein, Star- Atlas \M. The Omega Nebula after Molden and Trouvelot. i.. C. 4403. .l.i in the Lyre (Lyra) after Holden. C, 4117. Spiral Nebula lands (Canes Venatici) after Kosse. G. C. 3572. Crab Nebula in the Bull (Taurus) after Rosse. C-. C. 1157. S. P. C. K. London. G. C. 250, in Cassiopeia. (1 (J. Q. C. 4230, in Herkules. G. C. 4755, in Klein, Star- Atlas. Heliosraphical reproduction of Star clusters fron XVII. i,. I HI .1, in v asMni|'-i;i k iotographs taken by Eugen von Gothard in Hereny. NlV Nebula GC.1227 after Tempel Nova 1 572 The New Star in Cassiopeia and its surrour after D'Arrest. Nebula G.C. 1511 after Tempei Nebula G.C. 4-175 and its surroundings. The Nebula G.C. 3105,3108, 3109 after Tempel. Klein. Mar At XVIII. lebula GC 3165 after Tempel Star Cluster G.C1295 after O.Lohse Star Cluster GC4230 after Trouvelot S }'. i K i...n.l..i 14 DAY USE RETURN TO DESK FROM WHICH BORROWED rSTRCSOMY, MATHEMATICS- STATISTICS, LIBRARY c is due on the last date stam This boolos^ue^on'tKe last date stamped below, or on the date to which renewed. Renewed books are subject to immediate recall. LD21-100m-6,'56 (B9311slO)476 General Library University of California Berkeley UNIVERSITY OF CALIFORNIA LIBRARY r '