BOUGHT WITH THE INCOME FROM THE SAGE ENDOWMENT FUND THE GIFT OF Slenrg W. Sage 1891 ■2..3..e..f:f^ /.3///af.,. 6896-1 Cornell University Library arV11676 A new star atlas for the library the sc 3 1924 031 324 001 -nx The original of tliis book is in tine Cornell University Library. There are no known copyright restrictions in the United States on the use of the text. http://www.archive.org/details/cu31924031324001 A NEW STAR ATLAS FOB THE LIBRARY, THE SCHOOL, AND THE OBSERVATORY IN TWELVE CIRCULAR MAPS (WITH TWO INDEX PLATES) INTENBBD AB A COMPAITCON TO 'WEBB'S OBIESTIAI. OBJECTS EOS COMMON TEM)S0OPE3' WITE A LETTERPRESS INTRODUCTION ON TEE STVD7 OF THE STABS ILLUSTRATED BT SEVERAL WOODCUTS BT EICHAED A. PEOCTOE *Why did not somebody teaoh me the OonstellatioiiB, and make me at home in the Btany heavens, which are always overhead, and which I don't half tnow to this day?* Ojlrltlb BS7IBBD AND OOBBEOTBD BT T. E. BSPIN (1896) TWENTY-SECOND IMPRESSION LONGMANS, GEEEN, AND CO. 39 PATERNOSTER BOW, LONDON NEW YORK, BOMBAY, AND CALCUTTA 1908 All rights reset'ived. PEEFAGB TO THE NINETEENTH EDITION. The new edition of Webb's ' Celestial Objects ' baa necessitated a revision of tbe maps of Proctor's ' New- Star Atlas.' On maps of so small a scale it has been impossible to insert tbe whole of the contents of ' Celestial Objects,' Vol. II, I have therefore only- entered the new double stars brighter than magni- tude 6-5. All the variable stars in Webb have been inserted, and many subsequently discovered. In one or two cases the constellation boundaries have been slightly altered, and where they differed on two maps in the last edition, they have now been made uniform. Many of the stars entered from the ' Bedford Cycle ' as double or triple have been omitted, since they cannot be recognised as double or triple in the modem sense. As amateurs set much value on the exact magnitudes of the stars, in this edition will be found a list of the magnitudes of the brighter stars down to 30° S., taken from the Harvard Photometry. T. E. ESPIN. Tow Law, E.S.O., Co. Dubham : 29, 1895. PREFACE. This Atlas is reduced from my large Star Atlas. The plan on wliick it has been constructed — briefly described in the accompanying letterpress — needs no special discussion here ; because I have already fully dealt with it in the introduction to the large Atlas. I may remark, however, that the present work afibrds new and striking evidence of the advan- tages of the plan; for we have here a little book which can be carried in the pocket, while the small Atlas published by the Society for Diffusing Useful Knowledge is printed on sheets about sixteen inches square ; and yet the scale of the accompanying maps is larger than that of the S.D.U.K. Atlas. The re- duction in size is gained chiefly by a reduction in the distortion of the maps, the maximum expansion due to this cause being fifty -eight times greater in the S.D.TJ.E. maps than in the present (see note at pp. 11, 12). Moreover, the twelve maps of this Atlas overlap, a fifth part of the heavens being in- cluded in the overlaps; so that each of the twelve maps exhibits a tenth part of the heavens. vi PREFACE. No pains have been spared to clear the maps of all which could cause confllsion to the beginner; but this has been done in such a way that the more advanced student may find nothing wanting. For example, the meridians and parallels are drawn in to every fifteenth, instead of every fifth degree (as usual) ; but, since all the intersections of these lines to every fifth degree are marked in the maps (with a small cross), the places of stars can be determined, from catalogues or the like, as readily as though the lines themselves were marked in. In like manner all the longitude and latitude lines, except the ecliptic and the solstitial colures, are omitted; but their intersections to every fifteenth degree are marked (with a small dotted cross), and any student who is sufficiently advanced to require these lines will be able to recognise very readily where they lie, or to pencil them in if need be. I consider their omission, and the omission of all but every third of the me- ridians and parallels usually introduced, to be abso- lutely essential for the convenience of the majority of those who will use these maps ; though the maps would, undoubtedly, be imperfect if the position of these lines were not indicated. The method of indicating the effects of precession is also novel. Instead of a precession-triangle in the comer of each map, with instructions for obtaining compass measurements, I have placed precession- arrows over the maps (always on latitude-parallels, 15° 30°, &c.) ; and these show at once by what amount PREFACE. 7ii Stars in the neighbourhood are precessionally dis- placed in one hundred years. In passing, however, let me call the student's attention to the fact (often forgotten) that the stars suffer no real displacement, and that, he will do well to regard the effects of precession as shifting the meridians and parallels bodily in a direction contrary to that indicated by the arrows. The constellation boundaries are somewhat darker than I would have had them if I had not had to con- sider the requirements of beginners. It seems to me very necessary that the extent of each constellation should be recognisable at a glance (at least by most of those who wUl use these maps). Indeed, if no other means would suf&ce for this, the spaces should be coloured as in geographical maps. I think the pre sent arrangement meets all requirements. As to the consteUation-figures, I conceive that few will be disposed to regret their omission from the present Atlas. The old usage — by which a star's place was indicated by a reference to the club of Orion, or the northern claw of the Crab, or the southern wing of the Virgin, and so on — is happily falling into disuse ; and, as the number or letter of a star is always mentioned, even by those who employ the ancient practice, no dif&culty can ever arise in finding any star referred to. It is of more importance to notice that the present Atlas is specially intended to serve as a companion to Mr. Webb's excellent treatise, ' Celestial Objects vlii PREFACE. for Common Telescopes.' With a very few excep- tionsj all tlie objects mentioned in that work are shown in this Atlas. The exceptions relate to ob- jects (some twenty in all, perhaps) which could not be introduced without overcrowding. I have to thank Mr. Webb for the careful revision of the Atlas, so far as the objects to be included in his treatise are concerned. In the course of this revision he has noticed several discrepancies between the constellation outlines in this work (based on the British Association Catalogue) and those used in Smyth's ' Bedford Cycle.' As Mr. Webb's ' Celes- tial Objects ' is closely associated with the ' Cycle,' he has not thought it desirable to remodel the arrangement of the constellations ; and, on the other hand, as this Atlas is a miniature of my ' New Star Atlas,' I should have been unwilling to change the constellation outlines, even if I did not entertain the opinion that Baily's changes result in an immense improvement. The student will therefore be prepared to find that some few objects described in ' Celestial Objects ' as in one constellation are here shown in another. But no diflSculty need arise on this account, because Mr. Webb in every case mentions the right ascension and declination of the several objects. The letterpress introduction has been prepared for the use of beginners, who often find it difiicult to compare the heavens with the maps of a star-atlas. I would recommend, as a convenient supplement to the information contained in these pages, my work PEE FACE. is entitled the ' Half-Hours with the Stars.' ' Its twelve maps show how the stars are placed, night by night and hour by hour, throughout the year in England. Thus they serve a purpose wholly distinct from that of such a star-atlas as the present. Each work is, however, complete in itself; and, as the ' Half-Hours with the Stars ' suflBces to teach the merest beginner the names and places of all the lead- ing star-groups, so the present will enable the learner to identify all the stars of the first five orders of magnitude ; that is, all the stars except the faintest of those seen on very dark and clear nights. EICHAED A. PEOCTOR. Bkighton : December 1871. ' Now published by Longmans, Green & Co., price 3s. 6d. CONTENTS. pAa2 The Stabey Hea.vxns scEHomro cs lies a Houow Glcibe J Tills G^LOEE SEEMINGLY TITENS iiOIIirP AN AxiS ... 2 Oenesal effects of this tubntng Its hate RBStnLTINO HOYBMENTS OF THB STAHS BASIXY BECOONISBD IN A FEW MINUTES ..... . . The Stab-sphbee eotates 36C irxrvs (bouohly) in a yeab Plan on which the pbeseht Atlab HCTiraBg the Heavens Use of the Index Maps How TO COMPAEE THE MaPS WITH THB HeAVENS Tables I. and II., showing whehb the Stars in each Map abe TO BE LOOKED FOE AT DIFFEEENT HOUES AND SEASONS . 3 4 5 6 7 13 14 20 Table III., showing what Constellations ase yisiblb in England, and in wba.t paet of the Sky, at diffeeent HOCBS and seasons 22 Table IV.— List of Constellations (Latin and English names), with the Map in which each Constellation is to be found ........... 24 Table V. — ^LiST of Star-names 26 The Magnitudes of Stars according to the Eabtabd Photometry 28 xu CONTENTS. LIST OF WOODCUTS. sins. 1 AKD 2. DiAOBAMS IIXUSTEATINS CONSTEUCTION OF AtI.AS 3 AND 4. „ .. , „ . 6 AND 6. „ „ „ „ . FAOa 9 10 1) 7. Showing wheee the Beabs, Pointers, &c., aee to be looked foe at different hotjes and seasons 15 8 AND 9. Showinq towabds what pakts of the Sky the Staks IN THE SETEBAIi MAPS OF THIS AtLAS ABE TO BE LOOKED FOB AT DIFFEBENI HOnES AND SEASONS 18, 19 HOW TO LEARN THE STARS. On a clear, but dark night, we see many hundreds of stars ol various orders of brightness. Those who are but beginning the study of the heavens are impressed with the feeling that it must be a very difficult task to become familiar with all the star-groups, and to learn the names of the brighter orbs. The task appears yet harder when they are told that the stars seen on one night or at one hour are not the same as those seen on other nights or at other hours — that the aspect of the starry heavens is in fact continually changing. Yet nearly all wish to know the stars, even though they may not wish to engage in the actual study of astronomy. In reality, it is by no means so difficult as might be supposed to recognise all the chief star-groups — -or constellations, as they are called — and to learn the names of all the leading stars. One may, without much trouble, become so well acquainted with the stars as to be able to recognise even three or four seen through a break in a cloudy sky. I propose now to show how such knowledge is to be gained. In the first place, the student must iearn what is the true arrangement of the stars as distinguished from that which he sees at any instant from some standpoint on the earth. He views the heavens as a dome, or hollow half-globe, on the inside of which the stars are spread in hundreds. But he must remember that beneath the horizon there is another similar half-globe, passing right round under his feet, and similarly bespread with stars. If the earth were perfectly transparent, and the light of the sun were lost, the observer on B J. A NEW STAR ATLAS. tarth would find himself placed seemingly at the centre of a vast hollow glohe covered with stars. And if he could con- tinue to watch this globe hour after hour, Jay after day, and year after year, he would find that all the stars* kept their places on the globe, but that the globe itself seemed to turn bodily round, as if on an axle passing through his own position. There Mould be a ceaseless and perfectly uniform turning round of the sphere of stars, but in other respects there would be no perceptible change in the position of any of the stars. The earth not being transparent, we see at night but one half of this rotating sphere ; and the light of the sun being sufficient to obliterate that of the stars, we cannot in the day- time see the sphere of stars at all. But the learner must remember that one and the same stai-sphere surrounds him on all sides, below as well as above the horizon, and at all hours, by day as well as by night. It is because the stars do not change in their position ore this sphere that they are called ^sed stars. Their fixity enables us to recognise the groups which they seem to form. A well-marked group of stars, once re- cognised, cannot easily be forgotten ; and it becomes thence- forth a sort of skymark whence the learner can proceed to other groups. And as there are certain star-groups which al- ways continue above the horizon, the observer who has learned to recognise some of them, can on any clear night extend his survey from these known groups to others that are unknown. It is easy to see why some groups are never carried below the horizon, notwithstanding the continual rotation of the star- ephere. Two points of the turning sphere are necessarily fixed. These are called the poles of the celestial sphere. In England one of these poles — the north pole of the heavens lieg due north, and rather more than halfway above the horizon, towards the point overhead (called the zenith). The other point is, of course, below the horizon, due south, and rather more than halfway down towards the point directly under the observer (called the nadir). If the observer iaces * The light of the sun being obliterated, neither the moon nor anj of the planets would be visible. HOW TO LMARN THE STARS. 3 due south, the stars near the horizon on his left hand, or towards the east, have lately risen, and are passing higher; those near the horizon on his right hand, or towards the west, are about to pass below the western horizon. Those which rise above the horizon nearly dne east, will pass higher and higher till they are due south, when they will be rather less than half- way from the southern horizon towards the point overhead. Thence they will descend until they are nearly due west, when they will pass below the horizon. If the observer, having d'oly recognised the nature of this motion (which corresponds exactly with the seeming motion of the sun on a spring or autumn day), remembers that it is brought about by the rota- tion of the whole sphere of the stars, he will at once see what must be the nature of the stellar motions in other parts of the heavens. He will see that stars which rise on any part of the horizon from east to south will follow a similar course, but shorter and shorter the nearer their place of rising is to the south point ; their elevation when due south will also be less and less ; and they will follow a descending course precisely resembling their ascending course, setting just as far to the west of the south point as they rose to the east of it. A star which is on the horizon when due south can only be seen for a minute or two, just grazing the southern horizon. Stars which rise in any part of the horizon from east to north, will also continue to pass higher and higher tiU they are due south, following a longer and longer course, the nearer their place of rising is to the north point; their elevation when due south will also be greater and greater ; and they will follow a de- scending course precisely similar to their ascending course, setting just as far to the west of the north point as they rose to the east of it. A star which is on the horizon when due north performs a complete circuit before it again reaches the horizon, when it is due north as before ; its highest point being reached when due south after half a circuit, at which time it is but about thirteen degrees from the point overhead. No stars within the circuit of such a star ever reach the horizon at all. Bach performs a complete circuit, which is smaller and smaller ^ A NEW STAR ATLAS. the nearer the star is to the pole of the heavens. A staT which, when due north, is about 13 degrees above the horizon, is almost exactly overhead when half a circuit has been com- pleted. Stars nearer to the pole than this are due north when at their highest in their circuit as well as when at their lowest. But let the student bo reminded that all these varieties of motion are the effects of but one single turning movement. He must not suffer himself to be confused by these motions as described (1 have, however, described them as clearly as I could) ; but if he finds doubt arising in his mind, when he is actually studying the stars, let him face due north, and, looh- ing towards the north pole of the heavens (a point rather more than halfway above the northern horizon towards the point overhead), let him remember that the stellar sphere moves as though turning bodily round on an axis, — running from that pole through his own station (which is at the centre of the sphere) to a point directly opposite the former, — the rotation being such that stars near the pole move round it in a direc- tion contrary to that in which the hands of a watch move. It will serve equally well if he faces due south, and remembers that the stellar sphere is being earned round fi-om left to right, as though on an axis passing through his station and the invisible pole (which lies below the southern horizon, and rather more than halfway down towards the point directly beneath him). The rate at which the stellar sphere rotates must next be considered. Roughly speaking, the sphere of stars may be said to turn round once in each day ; but in reality it turns rather more qidehly, so as to make one complete rotation in about four niMuies less than a day. Thus a star which rises in the east takes six hours (less about one minute) to reach the highest part of its path, when it is due south ; and it takes the same interval in passing to its setting-place in the west. It is, there- tore, twelve hours above the horizon. Stars whose place of rising lies nearer the south are less than twelve hours above the horizon. Stars which rise to the north of the east point are more tlian twelve hours above the horizon. Stars which touch HOW TO LEARN THE STARS. 5 ti pass above the northern horizon take twenty-four hours (lesa about four minutes) in circling round the pole of the heavens. It is well to remember that the resulting motion of the stars can be easily recognised in a very few minutes. This may be shown in a variety of ways. If a star is seen above or beside some distant object, as a tree or hou.se, then if the student re- main in an unchanged position for a few minutes only, he will see that the star has perceptibly changed its place. If the star is towards the east, it seems to have moved xipwards and towards the right. If it is towai-ds the west, it seems to have moved towards the right, and downwards. If it is towards either the south or the north, it seems to have moved horizon- tally towards the right. (All stars near the horizon move to- wards the right, though onlj^ those towards the north and south move horizontally.) Ten minutes will produce an un- mistakable change of place.* * It is strange how little familiar most persons are with the fact that the stellar motions are thus obvious. The notion seems to prevail that only the astronomer in his protracted night-watching can become cogni- zant of the stellar motions. One of the most beautiful and touching descriptions in all Dickens's works — the death of Stephen Blackpool, in Hard Times — is somewhat impaired by the introduction of an im- possible star, shining for hours down the deep chasm into which the poor fellow had fallen. The mouth of the Old Hell Shaft was so narrow a chasm as to be concealed by tall grass. Stephen fell far down ; and the star was so bright that he could show it to Eaehael among all the other stars visible on an autumn night. Certainly no such star exists in the catalogues of astronomers. It is probable, however, that Dickens may have heard some such story about a bright star — Venus or Jupiter — only the star cannot have been seen just overhead. Novelists and poets sometimes introduce astronomical details rather unhappily. Ons has made the new moon rise at one o'clock in the morning; another makes midnight moonless though the moon had risen at eleven ; in the Portent ' (a tale which appeared in one of the early numbers of the Cm-n- hill) a star is made to shine midway between the horns of the crescent moon ! But, perhaps, all the slips of the sort ever made are outvied by one in the opening lino of Chapter XII. Book IV. of Our Mutual Friend. Tennyson is singularly accurate in all astronomical details. In Maud iuch details are somewhat freely introduced ; but so correctly th.it Mr. Hind himself could take no exception to any of the astronomical stat«- ment*. 6 A NEW STAR ATLAS. So muv.h for the motions of the stars on any given night. But there is also an apparent motion of the star-sphere from day to day. I have mentioned that the star-sphere turns once completely round on its axis in the course of rather less than twenty-foui hours. Thus in twenty- four hours it has gone rather more than once round. Hence, if we look at the heavens night after raght at the same time, we notice precisely the same kind of change as when we look at the heavens hour after hour on the same night. Suppose that we look at the stars at ten o'clock on any night and note their position, and that again we note the position of the stars at eleven o'clock on the same night ; then, if afterwards we examine the stars night after night at ten o'clock, we shall find that at the end of about fifteen days they have at this hour the same position that they had on the first night at eleven o'clock — that is, they have ad- vanced by one hour's motion. In a month or thereabouts, they will be found to have advanced by two hours' motion. In a year they advance by twenty-four hours' motion, that is, by one complete rotation, so that they have resumed their original positions. In fact, in the course of a year the star- sphere turns round once oftener than there are days in the year.* If the learner, recalling the nature of the rotation to which the star-sphere is subject, remembers also that (roughly) the star-sphere turns round once in a day, he will know what changes to expect as any night progresses, and if he further remembers that (roughly) the star-sphere makes one extra turn in the year, he will know what changes to expect as the year progresses. Now, to aid the student in learning the names and features * The amount by which the stars hare advanced each night on the position they held at the same hour on the preceding night is by no means so small as is, perhaps, commonly imagined. This is easily tested. Let there be an upright of any sort a few yards to the north of the observer's station, and let him notice the exact hour when a star (at a fair height above the horizon) appears from behind the edge of this upright. At this hour on the next night he will find that, as seen from the same station, the star is about two moon's breadths past the upright's edge. The observer should look through a fixed tube placed itt the same position on each night. sow TO znARN THE STARS. 7 of the star-groups, maps may be devised on one of two plans. Either we may have maps showing the aspect of the heavens at diiFerent hours and at different seasons ; or, we may have maps constructed with sole reference to the star-sphere itself. Maps of the former kind form perhaps the simplest possible introduction to a knowledge of the heavens. If they are properly constructed, the learner can at once turn to the map representing the heavens at any hour and season of any yeai (such maps serve for all years), and then. he can at his leisure compare the stars he sees with those pictured in the map. In my work, entitled Half-Hours with the Stars, the maps not only serve these purposes, but they show at once towards what point of the horizon and at what height each star is situated. Maps of the second class are, however, absolutely necessary to supplement the information given by the others. All considerations are sacrificed to simplicity in the construc- tion of maps of the former kind ; no meridians or parallels can be shown ; none but the brighter stars can appear; only those parts of the star-sphere can be included which actually rise above the horizon ; and a variety of details, which even the beginner soon begins to require,* must necessarily be omitted. Maps of the latter kind form an atlas of the stellar globe, and can be made to include any details which may be desired. The present work is an atlas of this sort. It pictures in twelve maps the stellar sphere which surrounds our earth ; and it is as suitable for use in one country as in others — at our * It must not be supposed, however, that such maps are useful only for beginners. It is most convenient, even for the advanced student of astronomy, to have a book from which he can at once determine what stars are above the horizon,, and in what positions, at any hour of any night. I believe, also, that such a work as my Constellation- Seasons (now out of print), in which the equator, ecliptic, colures, &c., were depicted, is calculated to serve very useful purposes. If the lithographs of those charts had been better drawn than they actually were (owing to the difficulties met with in transfer work), I should not have suffered the work to be out of print, especially as the sale of the first and only edition was very encouraging. If I should at any time republish tha «ork, I should redraw the maps for photolithographic reproduction. 8 A NEW STAR ATLAS. antipodeB as here in England, in the Western as in the Rastem Hemisphere. But a globe may be pictured in maps in many different ways ; some useftil for one purpose, some for others. Tt is necessary to describe the plan on which the present atlas has been fornied, before considering its use in helping the student of the heavens. Any flat pictures of portions of a globe must necessarily be somewhat distorted. The larger the portion, the greater will be the distortion. Yet we must not divide the celestial globe into too many parts to form a celestial atlas ; because if we do, the student will be puzzled to know how these parts fit in, so to speak, to form the globe. There is a similar objection to the irregular division of the celestial globe. Some regular plan of dividing the globe into a moderate number of portions must be employed. Only two such plans (out of five which are possible) need be here considered. According to one, the globe is divided into six equal portions ; according to the other, into twelve. The first is easily understood. Imagine a case shaped like a die or cube — that is, with six square sides — the sides being made of some elastic material ; and conceive that by blowing air into this case the six elastic sides are made to bulge out in such sort that the case becomes globe-shaped. Then the six sides, which had been square and flat, are changed into curved surfaces, all four-pointed and all alike in shape and size. If we suppose the star-sphere divided into six such portions, and an atlas constructed to show these portions in six separate maps, such an atlas would correspond to the first plan. The fault of this mode of dividing th^ star-sphere is that the six parts are too large to be well shown on a flat surface. The distortion, especially for parts near the corners of the six portions, must be considerable. The plan has been employed in Mr. Keith Johnstone's atlas, and in the atlas published by the Society for Diffusing Useful Knowledge ; but the distortion IS so great in these atlases that a small space on the star- sphere occupies an area more than five times greater if it falls near an angle of the map than if it ^alls near the centre. The HOW TO LEARN TIIJE STARS. ehape of a ttar-group is also so modified as to render the recog- nition of the group very difficult. For example, the stars within a small square space, such as a a, fig. 1, y,e. i. are thrown into a space of the shape and size of Ac", if they chance to fall near the angles of a map.* The other plan (employed in the present atlas) is also readily described. Suppose a piece of card to be cut into the form represented in fig. 2, and half through along the dotted lines. Then, if the five pentagons round abode be bent up till /coincides with /', h with h', and so on, and the like with the Fig. 2. n itt pentagons round q r s t u, and if these sets of six pentagons be bent up (from the line fp) till g coincides with g and g', h with h and h', and so on, a closed figure will be formed. It is re- presented in two positions in figs. 3 and 4, the dotted lines being supposed to be seen througli the figure. Now, imagine the * The shape of the distorted figure -will only be as A o when the square space has a certain position with respect to the corner. In other cases A a may be thrown into a diamond-shaped figure as large as A c ; or into intermediate shapes, — always as large, however, as a c. This Tariety causes the eSects of the distortion tfi be yet more perplexing than they would otherwise be. 10 A NEW STAR ATLAS. twelve faces of this figure to be made of some elastic material, and that as in the former case air is blown in until the fixture becomes globe-shaped. Then the twelve faces, which had been five-cornered and flat, are changed into curved surfaces, all five- pointed and all alike in shape and size. In the present atlaa the star-sphere is supposed to be divided into twelve such por- tions, one of which is represented in each of the twelve maps following the two index-maps. The five angles of these five cornered spaces are shown by the five marks A on the circular i border of each map, but each map includes more than the five- pointed space — in fact each map includes the space within a circle carried (on the sphere) round the five-pointed space Fre. 3. Fig. 4. proper to the map. Thus there results a symmetrical ovei- iapping of the maps, each map overlapping and being over- lapped by five other maps. But for this many star-groups would be inconveniently broken up (as in other star-atlases) where the map-edges fell ; as it ia, groups that would be thus broken are shown in two maps. This mode of dividing the star-sphere having been adopted, the next point to be considered was the choice of a mode of presenting the several divisions. I need not enter here mto a consideration of the various methods available for mapping any given portion of the heavens.* It will be suffi- * They are described, and their principal properties compared, in ray Unndbook of the Stars. The properties of the gnomouic projection at BO IV TO LEAliN THE STARS. II FlH. &. cient to note that the plan employed in the present work reduces the distortion to its least possible amount. If the same method of mapping were employed as in the two celestial atlases above referred to, the present plan for dividing the sphere would still reduce the distortion so greatly that a sphere as A a (fig. 1 ) would be expanded (near the angles of a map) only to the size and shape a b,* instead of a c. But the method of mapping actually employed so reduces the distortion that a space as a a, fig. 5, is ex- panded (near the border of a map) only to the size and shape a a' — a distortion which is not only the least possible in maps including so large a portion of the heavens, but is scarcely discern- ^ ible save by practiced eyes.'f applied to the mode of dividing the sphere employed in this atlas, are discussed in the letter-press introduction to my Gnomonic Star-Atlas, * In my Gnomonic Atlas this method of construction is actually em- ployed, and the twelve maps are included in two sheets by the method of nrrangement indicated in iig 6. It will be noticed that all the maps Fig. 6. E B J. y H. ^ E<7 /' ■ ) r \^^ rff: E e ><'X. ^y \<6 ^ B^ have straight edges (this being a peculiarity which results friim the law of projection). The comparison of fig. 6 with the two index-plates in the present work, will serve to illustrate the arrangement of the twelve portions into which the star-sphere is divided. t The following facts serve to illustrate the advantages possessed by the present atlas in these respects over the atlases referred to in cho la A NEW STAR ATLAS. But it still remains to decide how the twelve divisions of the «tar-sphere shall be portioned ovit. It is easily seen, however, that since every five-pointed face has a face directly opposite to it (see fig. 4), two such opposite faces should be assigned to the northern and southern polar regions, the poles of the star- sphere being placed at the centres of these two maps. The remaining ten maps, five northern and five southern, interlap, as shown in fig. 4, their ten common angles lying alternately north and south, of a medial circle between the two poles (the celestial equator as it is called), represented in fig. 4 by the regular ten-sided figure a b cde f * text. A small area whose surface would be represented by 14 if it fell at the centre of ono of the S. D. U. K. maps, is so distorted if it fall near the angles aa to have an area of 72, an increase of 68 ; such an area in the present atlas is increased only from ] 4 to 15 when it falls near the edge of the map, an increase of only 1, that is one fifty-eighth part of that in the S.D.XI.K. maps. Again, owing to distortion, each map of the S. D. TJ. K. series covers a surface almost exactly twice as great as that of the corresponding part of the sphere. The maps of the present series cover severally a surface exceeding only by about one twenty- eighth part the actual surface of the corresponding portions of the sphere. * There still remains some choice as to the adjustment of northern and southern polar maps, and witli them the remaining ten maps, but practically the choice rests between two positions. There is a certain circle through the poles called the equatorial colure (see the index-plates), from one half of which all measurements around the celestial equator are taken, as from a starting-place. It is necessary for purposes of symmetry that this half of the equinoctial c, 10 - 2 , South (high) 00 „ 2 „ 4 „ 6 ., 8 „ 10 : ■West M „ 10 ,. 2 ., 4 „ 6 ,. 8 a rN.-East ) ? . 6 „ 8 „ 10 „ 2 ,. * ■^ S.-East 1 „ 3 „ 5 „ 7 „ 9 ,. 11 S.-West *« „ 11 >, 3 „ 5 ., 7 „ 9 ^ [N.-West j „ 8 „ 10 ,. 2 ,, * ., 6 I A..M. Sept. 6 Not. 18 Jan. 30 April 13 June 24 2 A.M. Aug. 21 Nov. 3 Jan. 14 March 29 June 9 i A.M. Aug. 6 Oct. 19 Dec. 30 March 13 May 25 4 a.m. July 21 Oct. 3 Dec. 14 Feb. 26 May 10 5 A.M. July 6 Sept. 18 Nov. 29 Feb. 11 AprU26| 6 a.m. June 22 Sept. 3 Nov. 13 Jan. 24 April 10' Table II. 6F.M. Jan. 25 April 11 June 22 Sept. 3 Not. 14 7 P.M. Jan. 10 March 27 June 7 Aug. 18 Oct. 30 8 P.M. Dec. 26 March 11 May 23 Aug. 3 Oct. 15 9 P.M. Deo. 10 Feb. 23 May 7 July 18 Sept. 30 10 P.M. Nov. 27 Feb. 8 April 22 Julys Sept. 15 ' 11 P.M. Nov. 11 Jan. 23 April 7 June 18 Aug. SO Midnight Oct. 27 Jan. 8 March 22 June 3 Aug. 16 North Map 1 Mapl Mapi Mapl Mapl ' .tfj S.-East ,. * „ 6 „ 8 „10 „ 2 W S.-West „ 2 >■ 4 , 6 „ 8 „10 Tforth ~| I " 8 „10 , 2 ,. * .. 6 N.-E.)Ba3t- S.-E. ferly S „ 6 „ 8 ,10 „ 2 „ 4 v S „ 5 „ 7 , 9 ,-11 „ 3 i South ^3 „ 3 „ 5 . 7 „ 9 >.ll :i S.-"W. 1 West- N.-w. I «iy „ 11 „ 3 , 5 ., 7 .. 9 ■ „ 10 „ 2 , 4 „ 6 -' 8 1 A.M. Oct. 11 Dee. 23 March 7 May 19 July 30 2 A.M. Sept. 26 Dec. 8 Feb. 20 May 4 July 16 3 A.M. Sept. 11 Not. 24 Feb. April 19 June 30' 4 A.U. Aug. 26 Nov. 9 Jan. 20 April 4 June 15 5 A.M. Aug. 11 Oct. 25 Jan. 5 March 19 May 31 6 A.M. July 26 Oct. 9 1 Dec. 20 Maicil4 May 18 sow TO leAmn the STAMS. 2, 4iours shown in the hour-column. Part of the celestial epaoe «hown in Map 3 never rises in our latitudes. The student wiU notice that the part corresponding to the top of the Maps 2, 3 — 11, lies towards the pole, and that the celestial space corresponding to a map is only placed vertically, so to speak, when due south or due north. But there is nothing in this that need inconvenience him, if he will notice only that the several maps can always be turned round so as to agree with the actual position of the included star-groups. For instance, supposing the observer is ex- amining the part of the heavens shown in Map 4 at midnight on September 21, when this region is situated as shown in fig. 8 ; then, if he holds the map as printed, he will not find the star-groups on the heavens in the same position as in the map. But fig. 8 shows him that the angle where Map 4 overlaps Maps 1 and 2 is uppermost at the moment ; and he has but to hold the map so that this angle (in the upper right- hand corner) is highest, to have the constellations of this map in their proper position. He then has Orion leaning back- wards, as in the heavens at the time, Taurus over Orion's head, Perseus over Taurus, the Twins almost horizontal on Orion's left ; and so on. But if the hour is midnight on January 8, he finds from Table II. that the space corresponding to Map 4 is in the south-west, high up ; and turning to fig. 9, he finds that this space has the position marked as Map 2. The angle where Map 4 overlaps Map 1 and Map 6 (now placed as Map 4 in fig. 9) is almost exactly overhead. Holding the map with this angle (in the upper lefl>-hand corner) highest, he has the constellations in their proper relative positions- Orion leaning forwards, and the Twins over Orion's head, and Taurus facing Orion on his right. And with equal simplicity the suitable position for any map at any hour may be ascertained. The following table will be found convenient also for some purposes. It has been formed from my ' Constellation Seasons ' * * The dates are, howeTer, altered. In preparing the Constellation Seasons I paid cftrefiil attention to the sun's varying motion in longitude, 22 A NEW STAR ATLAS. s J5 S s '5 i. » '^ g .i o 1 "^ ■ • c: ^' ;= ," *J •=: .X g ■g .; g ^ -3 g .„- ,- = .= 6 <1 § a ~ « S -§ O '5 g i -^ 1-1 S) = S o .S . 2 at j;- - sT g- r If >; ^ 'S «- "C -- - 53 '^ «-" ^" *S ri fl4 P^ S S5 I' .S o c c> a* c: .„ c ^ iP^^.2 0^-5.2oSc3^. j=|^fM;> -1=1 -S"" S ;> -5= 1 « i I -i I .i § -I ^ « S g =f K-^..£f ^ 1 I =e § S £ :. 2' ^ ,-RS[jnv -JfO^fl ■■'°-''*K '-lor^W •('')jo{i;H -sajnoJOH fe fc ' ■ Bsifi BSJfi usaji .■I <= kj 9 .5-5= f- o S f; g. < ^ _(=ii-imtciot>oooa2Wi>c>oOh;ii5^tHt.>,o^e3t,ar®S^<(e as i . W W . . « p4 . f4 &i . . f4 f4 . 63 H . W W i ;!2;p£l!2;a} aWizjai ^ H jzj ai !z;Kl!z;M"|zif=!!z;oa!2;W»ai -^ a o M ^ 3 -a -S .S « SS:^ gS« S2^ go°iS 24 A NEW ST AM ATLAS. (published in 1866) ; but for the idea of this particular appli- cation of that work I am indebted to Mr. Lockyer's ' Ele- mentary Lessons in Astronomy.' The following list of constellation-names* in Latin and English, will be found useful. Only those constellations are admitted into the list which are recognised in the catalogue of the British Association : — Table IV. Andromeda, The Chained Lady (Map 2). Antlia, The Air-Pvmp (Map 7). Apus, The Bird of Paradise (Map 12). Aquarius, The Water -Bearer (Map 11). Aquila, The Eagle (Map 10). Ara, TTie Altar (Map 9). Argo, The Ship Argo (Map S) : subdivided into — (i) Carina, The Keel. (ii) Malus, The Mast. (iii) Puppis, The Poop. (iv) Vela, TTie Sails. Aries, The Bam (Map 4). Auriga, The Waggoner (Map 4). Bootes, TkeHerdsman (Map 8). Cfelum, 77ie Sculptor's Tools (Map 3). Camelus, TTte Camel (for Came- leopardalis) (Map 1). Cancer, The Crab (Map 6). Canes Venatiei, The Hunting Dogs (Map 8). Cams, T%e Bog (for Canis Major) (Map 6). Canis Minor, The Lesser Dog (Map 5). Capricornus, The Sea- Goat (Map 11). Cassiopeia, The Lady in the Chair (Map 1). Centaurus, The Centaur (Map 7). Cepheus, The Monarch (Map 1). Cetus, The Sea-Monster (Map 3). Chamseleon, The Chameleon (Map 12). Circinus, The 12). &c., forgetting, in my anxiety to secure accuracy, tnat, as a matter of fact, the year must simply be portioned out into intervals as nearly equal as possible. Those who possess my Constellation Seasons would do well to pencil the above dates in place of those mentioned at the foot of the several plates. Lockyer's ' Lessons ' should be similarly corrected. * In the present atlas I have not thought it advisable to introduce fcll the new names which I have used in my large atlas ; but some of thr changes I retain, because they cannot in any way perplex the learner and are much more convenient than those in use. Thus the constella- tion \'ulpecula et Anser is here called Vulpea, Corona Eorealis is callea Corona, Cameleopardalis is called Camelus ; and so on. JlOfV TO LEAMJSl TMB STAJi§, 25 Colnmba, Noah's Dove (Map 5). Comn BereniceE, Berenieis Hair (Map 8). Corolla, The Wreath (tot Corona Australis) (Map 9). Corona, The Northern, Crown (for Corona Borealis) (Map 8). Corvus, The Crow (Map 7). Crater, The Cup (Map 7). Crux, The Cross (Map 12). Cygnvis, The Swan (Map 10). Delphinus, The Dolphin (Map 10). Dorado, The Sword-Fish (Map 12). Draco, The Dragon (Map 1). Equuleus, The Little Horse (Map 11). Eridanus, The Biver Eridanus (Map 3). Fornax. 71i« Furnace (Map 3). Gemini, 2%e Tmni (Map 6). Grus, 'l%e Crane (Map H). Hercules, Hercules (Map 10). Horologium, ?!&« Cloci: (Map 3). Hjdra, 77te Bea-8erpent (Map 7). Hydros, I'M Water-Snake (Map 12). ' Indus, The Indian (Map 11). Lacerta, The lizard (Map 2). Leo, The Lion (Map 6). Leo Minor, Ihe Lesser Lion (Map 6). Lepus, The Hare (Map 5). Libra, The Balance (Map 9). Lupus, The Wolf (Map 9). Lynx, The Lynx (Map 6). Lyra, The Lyre (Map 10). Mensa, The Table Mountain (Map 12). Microscopium, 2'he Microscope (Map 11). Monocoros, The Unicorn (Map 5). Musca, The Bee (Map 12). Norma, The Rule (Map 9). Octans, The Octant (Map 12). Ophiuelius, The Serpent- Bearer (Map 9). Orion, The Giant Hunter (Map i)- PaTo, The Peacock (Map 12). Pegasus, The Winged Horse (Map 2). Perseus, The Rricuer (Map 4). Phcenix, The Phoenix (Map 3). Pictor, The Painter's Easel (Map 5). Pisces, The Fishes (Map 2). Piscis, The Southern Fish (for Piscis Australis) (Map 11). Reticulum, The Net (Map 12) Sagitta, The Arrow (Map 10). Sagittarius, The Archer (Map 9). Scorpio, The Scorpion (Map 9). Sculptor, The Sculptor's Work- shop (Map 11). Serpens, The Serpent (Map 9). Sextans, The Sextant (Map 6). Taurus, The Bull (Map 4). Teleseopium, The Telescope (Map 9)- Toucan, The Toucan (Map 12). Triangula, The {Northern) Tri- angles (Map 2). Triangulum, The (Southern) Triangle (Map 12). Ursa, The Bear (for Ursa Major) (Map 1). Ursa Minor, The Lesser Bear (Map 1). Virgo, The Virgin (Map 7). Volans, The Flying-Fish (Map 12). Vulpecma, The Fox (Mpp 10). z6 A NEW STAU ATLAS. To this table of constellation names the following table ol star-names may be added : — Table V.— Star- Names. •• Andromedse, Al/pkeraiz. C Ceti, Baten Kaito». B , Mirach, Mizar. a , Mira. y , Mmach. a. , Menkar. Aquarii Sadalsmid. a Columbae, Pkaet. a , Sadalmelik. a Coronse, Alphecca. 5 , Skat. a Corvi, Alchiba. y Aquilae, Tarazed. S , Algores. a , Altair. a Crateris, Alkes. $ , Alshain. B Cygni, Albireo. a Arg4s, Canopus. a , Arided, Beieb Adiyc y Arietis, Mesartim. tt' , Azelfafage. B , Sheratan. a Delphini, Svalomn. a , Hamal. a Draconis, Thuhan. a Auriga;, Capella. (3 Alwaid. 8 , Menkalinan. ri Bootis, Muphrid. a Eridaui, Achernar. a , Arcmrus. y' — , Zaurae. e • — , Tear, Mizar, Mirach, B , Curta. Pulcherrima* y Geminorum, Athena. B , Nekkar. e , Mebsuta. a Canum Ven., Cor Caroli. 8 , Wasat. $ Canis, Mirzaon. a- , Castor. a , Sirius. B — — , Pollux. , Adara. K Hereulis, Mdrsie. B Canis Minoris, Gomeiea. B , Komeforos. D, , Frocyon. a , Has Algetki. a- Capricorni, Secunda Giedi. a Hydrae, Alphard, Cor Hydra. 5 , Deneb Algiedi. u. Leonis, Regvius, Cor LeonU. B Cassiopeiae, Ohaph. y' Leonis, Algeiba. a , ScJiedar. S , Zosma. a Cephei, Alderamin. B , Smeb Aleet, Denebola B Cephei, Alphirk. Deneb. y , Errai. « Leporis, Ameb. B Ceti, Viphda. a Librae, Znben el Genubi. * A name given by modern astronomers to express the extreme beauty of this double star (orange and green) viewed with a good telescope. HOW TO LEAUN THE STARS. V » Librae, Zuhen el ChavuUi. y , Zuben Hakrahi. a Lyrae, V^a. e , Sheliak. y , 8iUa2ihat. a Ophiudii, Sas Alhaffue. /3 , Cebcdrai. 8 Orionis, Bigel. -, Bellatrix. -, Mintaka. -, Mnilam. , Betelgmx. f Pegasi, ^Enif. f , Soman. B , Sckeat. a. , Markab. y , Algenib. $ Persei, Algol. a , Mirfak. - Piscis, Fomalhaut. a Piscium, Kaitain. e Sagittarii, Kaus Austraiit. a Scorpioais, Aniares, Cor Seor- a Serpentis, TJnukalhai. Tj Tauri, Alcyone (Pleiad). a , Aldeboran. , Nath. 1 tJrs8s, Talitha. a , JDubhe. , Merak. y , Pheoda. i , Alioth. ( , Mizar. 80 , Alcor. II , Alkaid, Benttnasch. a Ursse Minoris, Polaris. /S .. , Kochab. ft Virginls, Zavijatu. * , Vindemiatrix. a , Spica AnAmech, fipica. *,* I did not think it desirable to have the names of any but the brightest stars placed in the maps themselves, which wmild haT« been much cumbered even though only stars down to the second mag- nitude had been named. The above list gives at least as many names as the student need care to cumber his memory with. I could wish, for my own part, that all save those names which appear in the atlas itself eoold be finally dismissed from star-atlases and catalogues. A NEW STAB ATLAS. The Magnitudes of Stars according to the Harvard Photometrt. 3-8 7 4-7 8 4-9 1 4-3 K 4-4 A 3-9 ^ 5-0 3 4-6 e 3-8 II 4-8 K 4-6 3 3-1 « 4-8 o 4-7 c 4-1 12 4-2 f 3-1 A. 3-6 S 3-5 V 4-8 P 4-4 K 3-8 1 5-0 Andromeda. • 2'1 c 4-4 cr 4-9 c 4-4 e 4-3 A" 3'9 p 5-3 1 4-6 TT 4-4 j3 2-2 5 3-4 * 4-3 c 4-6 Aquwnus. J 4-9 « 4-3 T' 4-1 p 5-3 A 8-8 y ■ 4-1 S 3-4 ir 4-6 86 4-8 i 3'8 88 3-5 a 4-8 89 4-9 V 5-2 f> 4-2 V 4-2 X 5-1 3-2 4-3 t' 5-5 ^i 4-5 /* ■4-7 u 5-8 (c 4-9 7 2-8 J 4-3 IT 5-7 ' 5-2 46 51 « 4-4 Cepheus. 9 4-8 Q 3-5 11 4-8 24 4-9 y 4-5 A 5-3 { 4-4 € 4-2 1 3-6 {' 4-4 e 3-8 9 4-9 r 3-6 ^ 4-4 X 4-8 V 4-9 i 3-8 S 41 V 3-8 € Coma. 5-0 7 4-7 24 5-0 23 4-9 31 Corona. a-o f 4-7 X 5-6 7 4-2 f 4-1 ir 5-6 r 5-2 5 4-6 •r 5-2 K i.7 IT 6-3 50 c 4-5 7 3-8 K 4-7 \ 5-4 5 30 /» 5-2 48 4-6 50. 4-1 ( 4-6 T 5-2 P 4-6 «■ 50 t 3-6 T 4-5 O 4-9 7 3-4 7 3-6 TT 4-3 \ 4-6 a 2-7 94 50 K 50 36 5-0 42 4-4 V 5-8 « 4-5 v' 5-1 f' 50 » 4-3 f 31 a 4-1 B 4-4 K 3-9 (8 80 t 40 9 5-4 e 4-6 * 5-0 14 5-3 16 5-5 5 3-0 X' 5-0 22 4-7 V 4-0 ■/' 4-8 7iO^ TO LEARN THE STAKS. 81 2-8 Gortms. 7 2-8 5 3-1 f 5-5 Crater. V 4-4 S 3-9 7 4-2 c 5-0 Cygnm. 4-7 26 5-2 a," 5-6 28 4-8 49 5-8 o' 4-9 a 1-5 0^ 3-8 52 4-3 33 4-4 e 2-7 32 4-1 \ 4-6 34 (P) 4-9 56 5-0 36 5-6 57 4-6 7 2-3 y 4-1 39 4-6 59 4-6 41 4-1 ? 3-7 a;l 6-6 61 6-1 a2 5-0 63 5-1 DelpMnm f 5-3 K 6-1 i 6-1 Draco a 4-0 15 5-0 P^ .4-7 17 5-2 w 4-9 16 5-6 * 4-5 18 6-0 5 3-9 19 4-7 7 2'3 M 5-2 40, 41 5-2 f 3-3 39 4-8 y3 30 1> 4-2 k' 4-9 Eqtms. X 37 7 4-8 a 4-1 » 4-6 9 80 1 56 c 4-9 c 3-5 T 3-9 (T 4-3 V 44 70 51 71 5-3 P 4-2 72 50 75 5-3 ttI 4-9 ^ 4-4 ^4 4-4 t 4-1 i 5-3 K 6-1 3 4-6 < 4'7 .3 6-1 a 4-0 7 42 ;8 3-7 A. 4-1 15 5-0 c^ .4-7 ,45 4'8 4 5-3 17 5-2 a, 4-9 4'6 K 38 16 5-6 i(/ 4-5 u 4-8 6 5-1 18 6-0 I 3-9 S 3-2 10 4-7 19 4-7 7 2'3 59 4-9 a 3-6 Ai 5-2 40,415-2 t, 4-5 » 3-3 f 3-3 39 4-8 ir 4-5 e 4-1 ,3 3-0 ^ 4-2 a 4-7 D 2-8 k' 4-9 X 3'7 « 3-9 6-4 7 4-8 o 4-1 B 4'9 6:6 32 A NEW STAR ATLAS. r' 4-7 t' 4-8 V 3-9 i 6-4 6 6-1 P' 5-4 P' 5-4 t' 41 12 3-8 c 4-8 V 3-5 f 3-2 c 3-9 7 2-0 e 3-2 30 4-6 u 4-7 K 4-8 'P 4-2 T 3-9 7 3-8 w 4-7 6 2-8 4-2 o' 4-1 22 5-4 39 4-9 S 4-8 0^ 4-5 TT 4-4 v' 3-3 T« 4-3 v^ 40 T' 4-8 „« 4-4 32 4-8 Gemini. f 3-4 56 5-0 9 3-7 t 4-0 38 4-8 P 4-1 T 4-6 a 1-6 \ 3-6 V 4-2 s 3-6 4-7 Hercules. 1 3-7 P 4-1 50 5-8 \ 4-3 53 5'4 ( 3-9 € 40 ^ 3-5 60 4'9 4-0 S 3-3 1 3-9 IT 3-7 V 4-6 68 4-9 95 4-5 69 4-9 96 Hydra. 51 26 4-9 \ 3-9 27 4-9 J" 41 B 20 *> 5-2 t' 4-9 V 3-3 ■H 4-6 X' 5-2 I 41 x' 5-5 K 4-9 1 3-8 u* 4-3 /3 4-2 »' 4-7 '*' S'l Zacerta. 4 4-6 a 3-9 5 4-8 8 5-3 6 4-6 9 4-8 »' 3-8 53 3-9 54 4-6 55 6-0 M 4-3 a 4'2 * 4-7 2-9 A 4-4 r 4-1 K 3-6 $ 1-1 T 5-3 <(> 4-9 98 5-4 tf 4-0 102 4-5 104 4-9 106 4-8 109 3-9 110 4-2 111 4-5 113 4-5 y 3-3 47 5-1 48 5-9 T 3-5 50 5-2 52 5-0 54 5-0 57 61 58 50 11 4-7 13 6-1 16 6S HOW TO LEARN THE STARIS. 83 Leo. K 4-6 M 4-1 f 4-0 72 4-9 CO 5-5 y 5-3 54 4-3 •^ 4-5 A 4-4 IT 5-0 58 60 a 4-1 1 5-2 V 3-6 60 4-5 1 4-0 3-8 31 4-6 X 4-7 T 5-1 * 5-7 a 1-4 S 2-7 87 5-0 e 31 f 3-6 9 3-5 V 4-5 22 53 7 2-2 Leo Mmof 10 4-7 21 4-6 /3 4-4 37 4-7 19 5-1 30 5-1 Lepus. 33 5-7 46 3-9 € 3-3 X 4-3 a 2-7 1 3-7 £ 4-7 !< 5-2 y 3-7 17 4-9 M 3-3 8 5-1 C 3-7 4-6 K 4-6 /3 3-0 Libra,. i 3-9 ^ 5-4 , 4-9 1 4-0 A 5-0 a 30 3 2-7 K 50 4-3 1 5-8 C 5'4 1) 5-5 48 4-8 16 4-5 37 4-9 Lynx. 2 4-3 15 4-5 27 4-8 38 3-8 5 5-5 19 5-2 31 4-4 a 3-4 12 4-7 21 4-6 Lyra. 35 5-2 K 4-4 C 4-3 5' 5-3 17 4-9 M 4-9 C^ 5-9 52 4-5 1 5-2 a 0-2 ^1 5-6 7 3-3 ■n 4-5 el 4-6 v'' 51 16 50 e 4-3 €2 4-5 Monoceros. 2 6-1 10 5-0 19 4-8 y 4-2 3 4-8 11 3-9 20 5-1 28 4-9 5 40 13 4-3 22 4-0 29 4-5 8 4-4 17 5-0 34 A NEW STAR ATLAS. OphiucAm. 8 2-8 e 3-4 ^ 4-6 p 4-8 X 50 V 4-6 * 4-4 \ 4-0 ti) 4-7 it' 3-3 ■71^ 4-4 ir= 4-0 e> 5-4 ir= 8-9 IT* 4-8 o^ 4-3 If* 4-7 11 4-7 14 5-4 15 4-8 P 4-5 7 3-0 1 4-3 2 4-8 5 6-2 e 2-4 9 4-4 n 4-2 14 5-0 16 50 20 6-5 1 5-5 4 4-9 12 4-9 e 4-2 V 3-9 16 4-4 17 4-8 T 4-0 20 5-4 i 2-8 19 6-1 20 4-7 t 4-4 K 3'4 V 2-6 36 4-7 41 4-9 1 4-5 i8 0-3 T 3-6 23 5-0 29 4-3 ■n 3-5 y 1-9 r 4-6 V 4-7 31 4-9 32 4-3 33 6-5 S 2-4 V 4-8 1 4-0 e 3-8 »* 5-7 T» 4-4 30 5-2 31 5-0 32 60 38 6-0 37 B-3 V 4-7 7 3-1 I 41 K 3-9 to 4-7 31 5-0 a 1-9 34 4-8 Pegasiis. Perseus. e 3-4 44 4-5 45 4-4 tr 4-4 51 4-9 a 2-2 h 4-7 58 50 |8 2-9 V 4-7 *' 4-4 X 3-5 fl' 4-4 8^ 4-9 42 4-6 i 30 e 1-8 r 4-4 a 3-7 49 5-0 f 1-9 i 3-6 1 3-1 1 4-2 \ 4-2 V- 3-7 a 53 9 4-9 /3 2-6 a 2-6 55 4-6 0- 4-4 'I' 4-2 S 3-2 40 V 40 c 3-1 43 5-5 6 30 7 3-8 p 3-5 66 4-8 67 4-0 68 4-4 T 4-9 70 4-1 72 3-8 52 5-3 K 2-2 56 5-0 X* 4-6 ^ 4-3 X' 5-1 x^ 4-8 y 4-4 i 4-2 71 51 74 51 CK 56 4-9 58 5-3 T 4-7 64 5-4 u 4-6 70 4-6 71 5-4 72 5-2 •I- 4-6 J 4-1 \ 4-5 48 4-3 /» 4-2 52 4-9 b' 4-6 53 4-9 58 4-4 1 4-8 2 4-7 p 4-0 TT 31 5 2-5 I 4-1 5 5-1 t' 5-5 10 5-1 S 4-0 T" 6-9 Y 61 fi^OJT TO LEARN- THE STARS. 35 Pisces. 8 4'6 T 4-7 IT 5-6 7 38 64 5-3 * 4-6 V 4-7 k' 5-0 66 5-8 c 5-0 4-4 9 4-4 ;' 6-0 1^ 5-2 5 5-5 ft; 4-2 X 4-9 V 3-7 Sagitta. 2 60 j8 4-1 C 4-9 1 5-3 e 5-6 S 3-7 7 3-6 e 6-1 u 4-3 Sagittarius. 4 4-6 '1' 3-B IT 31 52 4-6 t" 3-0 v^ 50 'I' 6-2 54 5-6 /u 4-1 r' 51 43 4-9 55 5-0 1) 8-0 (T 2-8 P' 3'9 a) 4'9 5 2-8 e 3-6 P' 6-1 59 4-7 € 2-1 ( 2-9 V 4-7 61 5-0 21 4-9 3-9 X 5-1 62 4-7 A 3-1 T 3-5 Soorpio. $ 2-9 0)1 4-1 a.'^ 4-6 11 5-6 13 4-7 V 4-2 ')' 4-8 X 5-6 19 4-7 9 3-0 Serpens. 4-8 ( 4-5 € 3-7 a 2-7 36 5-2 /3 3-8 P 4-8 X 4-3 7 4-0 IT 4-2 ir 5'0 M 3-5 Sextans. a 4-8 8 5-3 15 •4-5 11 2-9 2-1 2-8 1-7 V 4-4 \ 3-8 4-4 i 4-5 V 3-8 e 41 36 A NEW STAB ATLAS. Taurus. 3-8 37 4-4 71 4-6 97 61 i 3-8 -f- 5-2 TT 4-9 1 4.7 5 4-3 47 50 e 3-7 104 5-1 7 60 h 4-3 6' 3-9 P 1-9 10 4-3 CO 4-6 92 3-6 114 4-8 17 3-8 f 51 P 4-8 119 4-6 19 4-4 y 3-9 a 1-0 f 30 20 4-0 X 5-5 88 4-5 126 4-9 23 4-2 51 40 90 4-3 132 5-1 V 30 82 4-7 (> 4-4 ■f- 3-1 S 3-4 15 4-4 TIrsa Mmor, 2 4-5 ;8 2-1 f 4-5 6 4-5 a 2-1 11 5-1 19 5-5 s 4-3 4 4-9 7 3-2 1) 60 24 5-9 5 4-3 5-3 Virgo. f 4-9 P 5-1 a 1-2 K 4-3 V 4-3 31 5-6 68 5-5 1 4-2 (3 3-7 '(' 5-0 69 4-8 X 4-6 7 5-2 S 3-7 78 4-9 • 5-2 IT 4-4 6 30 f 3-6 p 50 4'3 e 4-4 82 5-3 !>■ 39 V 4-0 53 6-1 84 5-7 109 3-7 X 4-7 (T 5-0 89 5-2 110 4-6 7 2-8 61 4-8 T 4-4 Spottiswoode &> Co. Ltd., Printers, New-street Square., London. MAP I STAR MAGNITUDES O _ /ua-f o Srrond . riiird _ Fourth • imh • Sivih (iirid iduier) NeJ^iiltL RA.h.-.rr>.r.j:d \ ^x o O. '-<^K^^ - ._^ -•■V ; j«,X :,„.....) :rf\ ^-^-'-r-j- .. -.-A ' »ii / ■° °'oib ^- / / ."0 ,-. • y -■ .oA ANNO 1880 The.AiY'oivs mdicati'j the/ fre/Li/.-isinnal n wtwn for 300 Yiiars o • I '♦-s- ^^ ^- o!^ f / ^t ©■' ■# y», ..^ ^ .\ -,o' ■'A ^r"' Qa, «r\ •>' 6" ¥a^V u '■■v*^\^ 1&" ■" 7 •■ ^ ^T'^o*' •f - W' • ,'l«i- --m V . *— ■ — — '^■'^ 2. /A' AB B R EVI ATIO NS R or Ru - Bfd Tr - Trinary ij^Vv/^ V or Va - Voj-iahle 1' - 21 Piizii Dor Du- Doiihlc H - 57>- KHerschel T ^Triphi h = :>ir .1 Hersdu^l a = QanyirupUt I — Strijvc Q i " (liiintuple A - Vurdop B = Binary Kci! -^^tLi■pa.■.0^inxjj"j' R u ? = ^vspeatcdi Redi ■ = SuspectaJj Biruxry (tochStoj-) ^MuLdpla (to a AffJi'iiJa.' •= MassicJ" 'ehuJ^Lh H V. 10. MAP 3 STAR MAGNITUDES \ \ *i A o _ First X \^ o Second, o = Third = Fourth «< = Fim, • SvxHi i and under) . Nebula. RA Proctor. Del ANNO 1880 Tfie.Arroi*'s mBicat& tfie PrecessioTuil motinrh for 100 Years AB B R EVl AT!0 NS R or Ru = Redi Tr " TrijuiTy V or Va - Variabl/i i' = 21 Piazzv D or D u - Double H = iV WSerschel T Qa Qi B " Triple h ■= ^iJ" J. BcrscheZ = QunJi'uple T- ■=■ Strove = Quintuple A = DunJjyp = Binary R u^ =SiLspectGct Red. B^ =■ Suspected, Binary M fwcbStar) = Multiple M fw cbJ^ebuZsbl '^ Messier \Q^ftoa.NebulzH H.V, 10. ' K'We, ' MAP 4 —^ t" •Z3 A • ,ffl" •16" a f-'.e '-> • 9° •o .* .1713" STAR MAGNITUDES O - First o o o Second Tliird. Fifth Sixdi (ojidundcrj Nehitla, B.A Procto. NO 1880 FrexxssioTwl rruytwn, for loo Tears AB B R EVl ATIO NS R or Ru = Redy Tr = Trinary V or Va - Vai-iable 1' - 2 1 Pinzzi D or Du - DoiihU W^Sir WHaschel T " Triple h ^ Sii- J. Hasctiel Q a = QuaJj-uple X =- Struye Q i = Qiiintuple. A — Dunlop B = Binary R u? = Suspected, Red^ B^ - Swspeci£xi Bijuuy M (tocbStai-) ^ MuhiplG lO^ffjycbNeluULl- H.V. 10. MAP 5 STAR MAGNITUDES O _ First o SecOTui o Third o ^ Fovriti • Fifilt • (und. under) Nehidcb i Froccor- ANNO 1880 The. Arrows in^icat£' fhe- PrecessionalnwliorL for 200 7ea^■s ABBREVIATIONS, R orRu = I{e a,Star I - Vubdpla aNchuhul-Mcssitr a,Jlabala.l- H.V. 10. Yon MAP 9 STAR MAGNITUDES \ \ o = First V^ o ^ Snnid ^^ \ o Third o FaurA • FiAh • _ SiTth (ojul under} ^ Nebvlo R-AProcinr.Lel (HERCULES^ V-~~~~~""^"^^^^ ANNO 1880 'rh£-Arrow,i injdicat& th& PrecesswniH rtwtiori, for 100 Years ABB R EVI ATIONS RorRu -ife■ W.Herschel T - Triple h ■= Sir J. HerscJiel a. = Quadruple I ■" Struye Qi " QuinUiple A = DimJop B = Biiixiry ^]x^= Suspected Red' B - SuspectcrZ Binary M ^wcLStar) '"Multiple. M iWcbMehuli. "Messier lOVwftT^iitZa,;- H.V. 10. NORTHERN INDEX MAP 1880 On thte Stereographac Proiectiorv On the giohe the circLzs I, 2. 4, 6. 8. and 10 are equal to sach other, and. also to those circles in which. the overlaps. 3.5.7.9 and Jl heloi RAh-octor.Del Shewing all the spojc^ covered/ hy the sioc Nor^terv^ mccps , and. tliose parts of tJxe Southern, maps which he North ofJI "South Dec ?• The dates round, the map are those on, wJzich the corresporuhzuj mer-iAums come to they SoiLth firhNortherrL Ix^titiiBjes ) at midjiighi'' iji, ife/w'SfTk,Sofn-b(^&Calcm^iCU. SOUTHERN ND EX MAP 1880 Ort the glohe tht^ cwclf^ IC S, 5, 7 ^9 and 11 are equnl ui encK ether ajxd. also to those at'cles to which the. o\ e'-ln.p.-r 2,4 h, S, cxnd W he^^mci B A Pronar Deh^ Sh^wiiu^ all the space^ covered' by the- sir Southern, maps, And, those parts of ihe. 'Nor-ihttrn. rruxps wht*^ Ue SouthofWNbi^Dcc"- . L "" • A '?. Sols anal // <: Colore ^ // ^•-•Il • c . H ^^ I '■ ° \ // --^./ "~^X*s^ / / 1 ! ■- ■• / The. dates roimd the map cLTff, those on which ih£. correspon^jnq mcruiuuis come t'J the. South l^uzNortitem, lahtiLd^es ) at nyitimght T^cw T"'-!'- fiiini]yajv <& I'niciiJlu