[ 3i ] 
Altho’ I have taken no Observation of T c Perfei 
ftnce the 2 2d Day of January 1740; yet, as this 
Star is very near the Zenith, and a Sufficient Num- 
ber were made about the Times when the Equation, 
refulting from the Hypothefis, was at its Maximum 
1 judged it proper to infert fome of them in the 
next Table 5 the lad Column .of which (hews, how 
much the Star’s mean Didance was South of 3S 0 . 
2o ; . on the 27th Day of March 172 7. Among 
near 60 Observations I meet with two only, that 
differ from the mean of thefe fo much as 2" 5 and 
thofe differ almoft as much from the mean of others, 
that were taken near the fame time: fo that the 
Hypothefts feems to correfpond, in general, with the 
Obfervations of this Star as well, as with either of 
the foregoing. 
t Verfei . 
South ot 
0 
38. 20 
Precel- 
iion. 
Aberra- 
ration. 
Nuta- 
tion. 
Mean 
Dift. 
South. 
1727 September 16 
December 29 
1728 December 21 
[729 December 2 
; 
60.1 
39-7 
22.5 
3 . 9.2 
+ ; 4 
IT. 9 
27.2 
4.2.0 
// 
7 
+ 12 9 
12.8 
1 1.5 
// 
+ 6-7 
7.2 
8.7 
9.0 
~li " 
7 T .0 
7 i -7 
71.2 
71.7 
1731 January 3 
1732 January 8 
1733 January 21 
1738 December 23 
1740 January 22 
N. 8.2 
22.0 
34.6 
117.0 
132.5 
59.0 
74.8 
91.0 
1834 
200.2 
12.8 
12.7 
11. 7 
128 
1I -7 
8.3 
6.7 
+ 4-3 
— 9 ° 
8.6 
71.9 
72.2 
72 4 
70.2 
70.8 
After the lad recited Observations, it may per- 
haps Seem needlefs to add thofe of a Terfei, which 
is farther from the Zenith j but however, as this 
Star lies very nearly at an equal Didance from the 
Equinottial 
