[ 3 6 3 3 
Through the great cloudinefs of the fkies at St. 
Helena, I could obferve the moon only one night, 
namely January 8, 1762, near her limits of decli- 
nation ; on the other nights, I endeavoured to com. 
pare her with as many flars as came within the field 
of the telefcope, trufling to determine afterwards the 
difference of right afeenfion of the flars, with which 
(he was compared in the former and latter obferva- 
tions of the fame night. This defign I have fince 
completed, by procuring a great many tranfits of 
thefe flars, to be obferved on the meridian, at the 
Royal Obfervatory, in the latter end of the year 
1762, and beginning of the year 1763; many alfo 
1 made there myfelf. An account of them is given 
at the end of the other obfervations. 
An ufeful remark here offers itfelf to our notice j 
that the moon’s parallax may be very well deter- 
mined, in a fixed obfervatory, at any period of her 
declination, by obferving the difference of right afeen- 
fion of her limb, and any flar near her parallel, at a 
confiderable diflance from the meridian, either to 
the eaft or wefl, with the parallactic telefcope, and 
alfo on the meridian with the tranfit inflrument. 
But, in purfuing this method, the parallactic 
telefcope ought to be nearly of equal goodnefs with 
the tranfit telefcope ; elfe the moon s diameter might 
appear greater by fome feconds through one and the 
other, and confequently the parallax fo deduced 
would not be exadt. It is true, that, by a proper 
method of comparing the obfervations, this fmall 
error might be obviated, though the telefcopes dif- 
fered ever fo much in the degree of diflindtnefs, 
namely, by taking a mean of the refults found by 
A a a 2 the 
