462 W. MM. Harrington Brief Study of Vesta. 
each body was taken and is entered as the datum in the follow: 
ing table. The variations in these numbers for the stars are 
probably due to sources of photometric error, but I took especial 
pains to have these errors the same for all three of rei pe 
observed so that they would be eliminated in a comparison of 
the three. I cannot hope that I have entirely presi “ it 
was my special study to do so. 
of observation: | 16 | Vesta, | ate. | MURS Or 
ee 1883. 
. m 8. 8. § 
Sr iT 50°8 39°6 31°6 q°34 
ie xi Si 46°4 3T6 25°65 619 
38°3 32°4 19-2 6°38 
Vg 36°2 29'0 16°7 6°59 
16 xu 38 44:7 36°0 24°0 647 
xu 19 46°8 38-7 25°8 6°65 
43 41°5 33°9 21°7 6°55 
1G = 47°38 38-1 22 6°95 
x1. «66 46°4 BY fa | 25°6 
26 47-2 38°8 25°8 6°66 
55 46°9 36-6 25°7 5-00 
xin 24 44°3 35°2 24-5 6°91 
xii 49 44°8 35°1 24°9 701 
xiv 18 43°4 32°6 TOL 
at IS) 29 44 36°0 23°6 6°16 
& RN Bf 49°5 39°9 28°2 671 
> ieee: 48°47 40°1 27:5 6°72 
pa Seas 475 317 27°1 6°98 
i, 29 46:7 387°9 25°4 6°75 
xr 50 46°8 379 25°4 6'T6 
93 sd 2 45°2 36°1 24°5 5°84 
Xi 31 45°5 37-0 26°2 6°85 
19 xn 41 45'3 35°8 24°8 6°92 
98 xn <8 47°6 36°5 26°6 q-12 
1 58 48°3 36°9 26°7 7-15 
26 xi. «565 507 39°2 30°2 7°25 
25 Xi 27 52°0 40°7 31°2 7-20 
In the first column are given the Ann Arbor sidereal times 
of the middle of the set of observations on the three 1€8. 
from entrance on the wedge to extinction. Argelander give 
as the magnitude of the first comparison star 5°38 and 0 
second 8°8. If we adopt these magnitudes and assume that th 
stars do not vary during the course of the observations, U 
can easily determine the magnitude of the asteroid at the 
of observation. As the magnitude of the star and the ced 
extinction in the wedge change as the logarithm of the hight : : 
they can be sot rhgy directly. The fifth column was fo 
by the proportion 
