Observer Z. 
List of results for y, obtained and arranged in the same way as 
for observer H. 
1920 March22 Bo 50 
/ kebr, 23 KN 
„ May 12 Moos 
» Febr. 18 14°.0 
» May 15 18°.4 
7 eee! 18°.4 
l 
1920 Febr. 12 | 22°.4 
d ; 52326 
ve Oet. 28") 25256 
es Nov. 19 28° .0 
i ij 8/01 28900 | 
174 
0° .00159 
+0.00167 
—0.00013 
+0.00077 
+0.00095 
0.00041 
—0.00275 
+0.00377 
+0.00288 
+0.00209 
| +-0.00505 
1920 June 
1920 June 
” 
y saf, 
Febr. 
June 
Aug. 
Febr. 
The separate results give the following means: 
Zone 
” 
>” 
” 
0°— 20° 
20°— 30° 
30°—40° 
40°— zenith 
13°,0 
25°,6 
33°,3 
41°,8 
+ 05,00088 
+ 05,00221 
+ 0s,00324 
+ 0s,00696 
31°.2 | +0 .00339 
32°.2 +0.00222 
32°.5 +0.00314 
32°.6 +0.00547 
34°.3 —0.00017 
36°.8 +0.00535 
40°.0 +0.00132 
42°.0 +0.00315 
42° .2 +0.01195 
43°.2 +0.01142 
a=) 20 
eer 133 
a2 086 
a 271.6 
Owing to the smaller number of nights, the mean error is much 
greater, although the same influence is fairly marked. 
Treated as above, y can be represented by the formula: 
y = + 08.00497 tan d sec d. 
The residuals O—C for the four zones are: 
—0s,00030, 
—05,00043, 
The correction z becomes: 
z == + 05.285 (sec d; — see d). 
—0s,00068, + 0s,00100 
For observer Z. we find the same phenomenon, that stars of high 
deel. are registered too early, those with small decl. too late. 
Observer G. 
List of the separate results, arranged as before. 
