stellar clusters 



41 



of the Galaxy. Determining the srale in tliis manner we conclude that the globular 

 clusters have the same dispersion perpendicular to the XY-plane of the Galaxy as 

 the B-stars and the ordinary clusters, a result coutirming the value of the scale. 

 In the XF-plane of the Galaxy, against the negative F-axis [Sagittarius), it reaches 

 to a distance of some 10Ü siriometers. 



The value obtained for the scale is, however, subject to considerable uncertainty, 

 all the more as other considerations lead to much higher (10 times as high) value 

 of the scale. It is to be expected that tlie variable stars of short period, so abundant 

 in tlie globulars, will give material for a surer determination of the scale. 



The relation of the globulars to the great star cloud in Sagittarius, shown on 

 plate VII, gives rise to interesting cosmological consequences. 



6 



