110 I. P. Косн. 
circumstance that as our first approximation we considered the time 
of the transit as being equal to the right ascensions of the corre- 
sponding stars, that is, we assumed that the hour angles of the 
equatorial stars at the moment of transit was zero. Now, however, 
the preliminary computation proves 
i, = + 12929 and ft, = + 112175. 
We might thus have made a fresh computation with the values: 
f} — 226380385 + 12™29s — 11260495 — about 21h24m and 
Ё — 23822093 4 11017: — 15260495 — “ahout 22507™ 
and the moments of transit calculated in this manner would then 
have been identical with those observed. A fresh computation of 
this kind is, however, superfluous; even a difference of a whole 
minute between the time of transit calculated a priori and the one 
observed offers no practical difficulties. 
To the preliminary computation further belongs an estimate of 
the readings of the horizontal circle corresponding to the various 
observations of Polaris. As we had no meridian mark, the meridian 
point of the circle had to be known within a few minutes. By means 
of this and the values for a! and af found in the course of the 
preliminary computation we computed the reading of the corresponding 
divisions of the horizontal circle. As regards the other two observa- 
tions of Polaris we simply estimated in the course of the observa- 
tion itself. 
Before mentioning the method of observation the contents of 
the observation journal will be quoted as regards the former star 
group, i.e. 1) the result of the preliminary computations, 2) the 
observations themselves, and 3) the calculations made in the ob- 
servation journal. 
Determination for time 24/XI 1907. 
Observer: KocH; Assistant: WEGENER. 
| Mag. | 57203 AL Et 
| | | circle 
Polaris | 2.1 21h25m 1298 30013 
n Pegasi 3.1 21 31.5 47 .1 
и Pegasi пи 217385 52 Л 
у Piscium 3.8 22 04.5 74 0 
х Piscium 5.0 22 13,8 76 .0 34°25’ 
