356 An Analysis of Mr. Baily’s Astronomical Tables 
computed from the tables recently published by M. Besse in. 
the fifth part of his Asfronomische Beobachtungen, published at 
Konigsberg in 1820. Mr. Barty properly observes with respect 
to this table, * that it is difficult to account for the general con- - 
sent which seems to have existed amongst astronomers, to ob- 
serve more particularly those 36 stars, and which have thus ac- 
quired the name of fundamental stars; because they by no 
means furnish the best arrangement that might be made; some 
others might have been selected, more generally distributed over 
the heavens.”” Both M. Besser, and our own AsTRONOMER 
Roya, now make daily observations on every star above the 
fifth magnitude, a practice which immortalized the names of 
BraD_ey and Pazzi. 
Table the eighth contains four pages devoted to the apparent 
place of the pole star, for every day of the year, at the time of 
its upper culmination. This table was computed by Dr. Struve, 
the director of the Observatory at Dorpat in Livonia, from the 
tables of M. Besse before alluded to. 
The ninth table contains a comparison of the mean right 
ascensions of the 36 principal stars given in the sixth table. Of 
the five columns which compose this table, the first contains the 
latest observations of Dr. MasKELYNE, with the old transit in- 
strument, and the remaining columns contain the results of 
Mr. Ponp’s observations, with the new transit instrument. 
Dr. MaskELYNE’s observations correspond with those of 
Mr. Ponp, for the year 1816, with singular accuracy ; but those 
for 1817, 1818, and 1819 present some remarkable variations. 
The tenth table contains a comparison of the mean north 
polar distances of 34, principal stars, on January 1, 1822, as 
deduced from the observations of the ASTRONOMER RoyaL, with 
the mural circle, during the years 1812, 13, 14, 15, 16, 19, 
and 20. Columns are also added, to exhibit the differences Le- 
tween these different years. 
In the eleventh table will be found a list of all the eclipses of 
Jupiter’s satellites visible at Greenwich. This table has been 
deduced by Mr. Batty, from the Connaissance des Tems for 
_ 1822, by, allowing for the difference of the meridians. The 
computers of the latter work deduced the same from the tables 
of DELAMBRE, published in 1817, There is a column also in 
this table, to denote the distance of the satellite from Juprrer’s 
limb, at the moment of its reappearance, in terms of the planet’s 
diameter, which is regarded as unity; the distance bemg mea- 
sured, either in a line with the planet’s equator, or ina line pa- 
rallel thereto, 
In the twelfth table, the apparent obliquity of the ecliptic and 
the equation of the equinoxes are given, for the first day of every 
month 
