( 224 ) 
considered as chance-errors of observation, and hence are left out 
of consideration. 
Now eae ue cas 
e= — ayy = — (54) 4 — Go)? 
braan Ge ). 400 G). ir 
and negleeting small quantities of higher order we can put: 
Tj S= 5 sin ho \- (32). dA — (4). dD 7 
ru A is h ; ( oA OA ) 
Vo = sin Ay + hls Ao) (5a) a4 -+ Go)? Me 
‘ 
ae) Oe h 
Here we assume as unknown quantities i == dl ant “dD,and 
So al g 
obtain from the equations for «, the two following normal equations: 
ro) hal = ie Asi a} —_dd + (54) Gee as) = —dD 
(B) 
ripe) (ren a [ea 
From the equation for vo we derive three normal equations, of 
which the first is: 
vo i | = sin” ho |= + sin Ay cos ho (=) | = dA + 
+ sin Ay cos Ag 5). Ie : dD 
The two other equations are left out of consideration on account 
of their small weight. 
For stars, distributed symmetrically with regard to the Apex 
and the Antapex, both sin Ay cos NEN and | sin Ay cos Ag (5). | 
