In this way we find 
from all observations AZ=+1"5 +1".2 
from those of 1911 only +1.0+1 4 
The value of AZ is fairly small and almost equal to its mean 
error. The 3 partial results Jidda 1910, Jidda 1911 and Mecca have, 
however, the same sign. In order to correct one-sided observations 
we have employed the value deduced from 1911, Jidda and Mecca 
together, + 1".0. 
In the second place we shall consider the differences between the 
results from the North and the Southstar. Except on one night in 
1910 the zenith-distances of the observed stars lie between 10° and 
45° and the mean z is about 30°. The py—gs therefore contain 
twice the flexure for a zenith-distance of about 30° and the influence 
of the systematic division-errors on an are of about 60°, 
We now find: 
Jidda 1910 py — gp; == +1".7 weight 5.5 
OL KEN, a ee | 
Mecca s +04 „ 8 
from which follows for 
all observations together + 3.0 + 1.7 
for the observations in 1911 +3 4+41.9 
So the differences are not great. That the flexure of the telescope 
would be small was to be expected, but our results prove also that 
the systematic division-errors of the circle cannot be great. For the 
reduction of the incomplete observations we always employed (even 
in 1910), according to the results for 1911 
Hey 5) = 417 
In this manner we deduced for all observation-nights values for 
(py fs), and the means taken from these, giving half weight to 
the nights on which only one star had been observed, were considered 
our final results. Moreover mean values have been formed from the 
results in the separate positions and from the separate stars, again 
giving half weight to incomplete observations. 
So we found : 
] 
Northstar Southstar Nih sth 
Te an hits Mean Tok. Tele Mean 
Jidda AES 
Eek CA Gee kond 13"0 1673 1477 29 145 
2 sf) BO. 0 LS As 20:9 tot. 16.5, 160 29 18.5 
