[ in ] 
fradlion, it may be found to great exadnefs ; this line 
once fettled will lave trouble aftei wards, and is indeed 
the foundation of all aflronomical obfervations. 
' 'To find a known Star or Planet at aiiy propofed infiant 
oj timey whether in the day or night. 
The inflrument remaining redified as in the laft 
obfervation ; fet the declination femicircle to the 
declination of the planet, at the propofed infiant, 
and bring the index of the equatorial plate, to point 
to the meridian difl^nce of the flar or planet, at the 
propofed infiant if weflward, or to the complement of 
the meridian diflance if eaflward of the meridian. 
(This diftance is found by adding together the right 
afcenfion of the Sun in time, and the apparent time 
ol the day, and taking the difference between the 
fum and the flar’s right afcenfion in time^ when the 
flar’s ri<iht afcenfion in time is greater than the above 
fum, the meridian diflance will be Eaft ; when the 
flar’s right afcenfion is lefs than the fum, the meri- 
dian diflance is Wefl,) Having thus fet the Inflrument, 
look through the telefcope, you will fee the flar or 
planet j and if it fliould afterwards get out of the 
field, you will eafily recover it, by moving the equa- 
torial handle onlv, provided the flar is above the 
horizon, becauie the diurnal motion of a flar is par- 
aliel to the ^equator. 
By this inflrument mofl of the flars of the firfl and 
fecond magnitude may be feen even at midday, and 
the Sun finning bright, as alio Mercury, Venus, and 
Jupiter ; Saturn and Mars are not fo eafy to be feen, 
in the day time, upon account of the ftintnefs of 
their 
