Stellar velocity distribution 



39 



36. From the above results it may be established that the three axial velocity 

 distribution of the stars as derived from radial velocity observations is closely re- 

 lated to the galactic system, and further that the longest and shortest axes of the 



4.5 

 4.0 

 3.5 

 3.0 

 2.5 

 2.0 



1 



ß, B 2 /»:,. B, Bs Bi B 7 B 3 A\ B /0 B z .<% 



Fig. 14. 



Graphical comparison between observed and computed dispersion in the line of sight 

 for stars of magnitudes 5^4.9. Squares B 1 to B l0 . 

















< 







































































5.0 < 



) 





















< 



1 





l.t 





























Z.o 





























C c t C 3 C+ C? C 4 c 7 c g c f c M C C, C c 2 



Fig. 15. 



Graphical comparison between observed and computed dispersion in the line 

 of sight for stars of magnitudes 5S4.9. Squares C\ to C 10 . 



ellipsoids are both coincident with the plane of the Milky Way. It is true that the 

 directions of the axes of the ellipsoid from the different groups are diverging, but 

 this divergence is surely due to the small number of observations. In each case 

 the arrangement of the three axes is the same. 



