128 
The stars which I have used for comparison with R Vulpe- 
culse are shown in the small chart which accompanies this 
paper, and their magnitudes are as follow, the numbers in the 
cases of <z, b, c, d, g , l, m, n being- the means between my 
own values and those assigned by Mr. Baxendell : — 
a = 7-1 
<7=10-0 
6 = 7-3± 
/t=10-5 
c = 8-3 
k= 10-9 
<2=9-1 
2=11-4 
e - 9-5 
wi = 1 1 -9 
<J* 
II 
n = 12-6 
i 
56m. 58m. Om. 
20hrs. 21hrs. 
The star b is variable to the extent of some few tenths of a 
magnitude, and may therefore with advantage be rejected as 
a comparison star ; g is a double star, the magnitude assigned 
above being that of the two components seen as one star. 
I cannot close this communication without gratefully 
acknowledging the courtesy and kindness of Mr. Baxendell in 
freely communicating to me his own methods, and in affording 
me all necessary explanations in cases of doubt or difficulty. 
It is to be hoped that the time is not far distant when the 
best methods of procedure in this branch of the science will 
lind a place in our textbooks of practical astronomy. 
