12 



C. V. L. Clmrlier 



For transforming equatorial coordinates directly into anti-centre coordinates we 

 have the relations: 



If 4, -q, C or Tj', C' are multiplied by the distance r of the cluster from the 

 sun we get the rectangular galactic coordinates of the cluster. 



6. Treating the clusters observed by Melotte according to the scheme given 

 above I first deduced the galactic longitude (/) and latitude [b] of each clusters. 

 These numbers are given in the columns 8 and 9 of table 1. From these coor 

 dinates we get directly the apparent distribution of the clusters in the galactic 

 system. I have for convenience in statistical researches divided the heaven into 

 48 galactic squares, similarly defined in respect to the Milky Way as the equatorial 

 squares in regard to the celestial equator. Consequently I introduce such squares, 

 all of the same area (= 859.4 square-degi-ees) and denote them by the same desig- 

 nations as the equatorial ones, only with a G (= galactic) prefixed. Thus GA^ 

 and G A.-, denote the squares round the north pole of the Milky Way, GC^, GC^, 

 (tCj2 denote the 12 squares between the Milky Way and -f 30° galactic latitude etc. 



The longitudes are, as usually, reckoned from the ascending node {Ü) of the 

 Milky Way on the equator (a = 280°). Thus GC, stretches from / = 0° to ^ = 30" 

 and from = 0" to = + 30«, the square GC, from / = 30" to 1 = 60" between 

 the same parallels etc. 



The values of I and b for the clusters are also given by Melotte, though he 

 uses a galactic plane somewhat different from that here used. 



The apparent distribution of the clusters is shown in the figure 2 of plate I. 

 The adherence of the clusters to the Milky Way is still better shown than in the 

 equatorial projection. In the polar squares there is only a single cluster, and with- 

 out the parallels at b — ± 30" there are besides only two clusters, all the other 140 

 being between the parallels b == ± 30" and generally close to the galactic equator. 



Among the 143 clusters in table 1 there are 6 which are denoted by Melotte 

 as globular clusters, though I have treated them here together with the ordinary 

 clusters. The reason is that these clusters are denoted as ordinary clusters in the 

 N. G. C. and are not named in the catalogue of globular clusters issued by Bailey 

 in H. A. 76. Moreover I have examined the Franklin-Adams charts regarding these 

 objects and generally found no reason to confirm the classification of Melotte. It 

 must, however, be remarked that the latter has based his description on the plates 

 which are much superior to the charts. Owing to the great importance of every 

 new discovery of globular clusters the cases noted by Melotte ought to be minu- 

 tely scrutinized. 



(11) 



i" 0.5446 -^- Tj" 0.3938 + C" 0.7405, 

 i" 0.8387 + ïj" 0,2657 -f C" 0.4808, 

 — -q" 0.8829 -f C" 0.4695. 



