( 283 ) 
etc. A regular variation of the zenith-point during the observation 
will then reveal itself in the differences between the separate results. 
Contrary to the expectation an almost equal value was found for the 
mean error in the two series, namely : 
Ist series Mean error of 2 pointings + 1.51 
gd = 1,59 
Hence the influence of a variation of the zenith-point is not at all 
perceptible. Yet after all I thought better to assign a smaller weight 
to the observations of the 1st series, considering that for this series 
the uncertainty originating from the level may be greater, and that 
less attention had been paid to the equality of the zenith distances 
for the different observations. Thus I assigned to the mean result 
of the positions 0° and 180° together in the 1st series, the same 
weight as to the position 0° in the 24, to 90° and 270° in the 
Ist series the same weight as to 90° in the 2d, and lastly to 225° 
in the first series half of that of 45° in the 2d, When two 
observations made under the same circumstances had to be combined, 
the number of pointings was not considered, except with the obser- 
vations of /? and @, Centauri on June 15, of which the results were 
combined with weights 2 and 1. Lastly the observation of /} Ursae 
majoris on May 2 was rejected owing to the diverging zenith 
distance. 
In this manner the results, given in the following table, were 
obtained. In this table column 2 and 3 give the mean zenith distance 
for the northern and the southern stars, column 4 and 5 the results 
derived for the Jatitude from these two groups, column 6 their diffe- 
rence and column 7 their half sum. 
ZEN. P. | 2. N. | 2.8. | NORTH | SOUTH | N—S | Nek 
Selen gett syne 
0° Bie | 542 6843 57/68 | — 10775 | 12 3706 
15 56 52 63.78 65.37 | 4 1.59 4.58 
90 54 52 60.86 67.99 | + 7.43 4.42 
135 55 54 64.90 63.07 | — 1.83 3.98 
