387 
1908-9.] The Systematic Motions of the Stars. 
their random distribution similar, it follows that the stream velocities are 
in the ratio — 
*957 : ’G06 or 1 : ‘63. 
If the stars within 30° of the directions of the two apices are con- 
sidered, we find — 
8in (dist.). 
I. 
II. 
•957 
111*2 
57-6 
•818 
80-5 
46-7 
•606 
57-5 
21*1 
•404 
24-3 
14-0 
And the number of stars of Stream I distant sin 1 *404 from A agrees 
o 
sufficiently well with the number of Stream II distant sin -1 ’606 from B 
to confirm this result, but the weight of this determination is small. 
The interest of this determination lies in the difference between 
this result of approximately 3:2 in the relative stream velocities 
with that of 3 or 4 : 1 found by Eddington using stars of all proper 
motions. 
11. The value of the method here employed depends on the uniformity 
with which the stars are distributed. It is therefore of interest to 
examine whether the distribution of magnitude of proper motion 
varies with the distances from A and B in the two streams. Confining 
our attention to stars moving within 30° of the directions of A and B 
respectively, i.e. those stars whose velocities are largely determined by 
the stream velocities, we find between the distances 65° and 115° from A 
and B the following table for the number of stars whose proper motions 
are above certain limits : * — 
Proper 
Motion. 
I. 
II. 
>100" 
24 
14 
> 60 
67 
35 
> 50 
97 
56 
o 
A 
158 
84 
> 35 
208 
96 
> 30 
267 
130 
> 27 
315 
159 
> 24 
388 
182 
> 22 
445 
224 
> 20 
478 
248 
* As a p.m. of >994" is called 100", the limits 100", 60", etc. are more strictly 992", 
•59A, etc. 
