141 



CHAP. XVII. THE RESULT OF THE INQUIRY. 



WE are finally in a position to make a general summary of the dis- 

 tribution of the various chemical groups of stars not only in relation 

 to their direction in space, as seen from the solar system, a direction 

 most conveniently considered in relation to galactic latitudes and 

 longitudes, but also in relation to their distance from us. 



The results arrived at in the two previous chapters may be sum- 

 marized as follows. First we will consider the stars studied by their 

 absorption phenomena. 



Group. 



Kelation to Milkv Way. 



Proper motion. 



Gaseous stars 

 Proto-metallic 



Metallic 



Metallic flutings. 

 Carbon . 



Condensed in Milky Way 



(Pickering and McClean) 

 Brighter ones not notably 



condensed in Milky Way 



(McClean) 

 Tend to collect in Milky Way 



more especially the fainter 



stars (Pickering) 

 Not condensed in Milky Way 



(Pickering and McClean) 

 Collected in Milky Way 



(Kapteyn) 



Smallest* (Monck). 

 Intermediate (Monck). 



Div. 1. Greatest (Kapteyn). 

 Div. 2. Small (Kapteyn). 



We find that the gaseous stars are chiefly in the Milky Way and 

 are far away from us ; that the proto-metallic stars are not so confined 

 to the Milky Way, and they are not so far away from us. But when 

 we come to the metallic stars and the carbon stars they have not much 

 obvious connection with the Milky Way, and they are close to us. 

 Unfortunately, with regard to the metallic fluting stars the informa- 

 tion is not so complete. Mr. McClean has dealt with a very small 

 number, and he shows that they, like Duner's stars, the carbon stars, 

 have very little relation to the Milky Way. We thus obtain a tre- 

 mendous separation between the hot stars with their great distance 

 and the cooler stars with their smaller distance. 



* Kapteyn finds small proper motions for gaseous and proto -metallic stars, but 

 does not separate them into two groups. 



