326 Mr. South’s re-examination of the apparent distances 
No. VIII. R. A. 8 h 2 m ; Decl. 18 0 11' N. 
f Cancri ; I. 24 and III. 19 ; H. and S. 90. 
continued. 
Passy ; April 4 , 1825 ; Seven-feet Equatorial. 
7th and 8th magnitudes. 
Position = 67° 14' sf\ 7 Obs. | Diff. = i° 30'. Very difficult. 
Observed with 413, when a few minutes west of the meridian; but the unstea- 
diness of the stars renders it impossible to procure any observations of distance. 
Passy ; April 5 , 1825 ; Seven-feet Equatorial. 
7th and 8th magnitudes. 
Position = 68° 49' 
Distance = 5".6 i6 
7 Obs. 
5 Obs. 
Diff. = i° 27' I 
Diff. = o".6 73 1 Ver ^ 
difficult. 
Observed a few minutes west of the meridian with 413 ; stars well defined, but very 
unsteady. 
Mean Result. 
of A B. Position 32°i o' 72/(43 Obs.); Distance T.o 86 (i 50 bs); 
of AC. 67 0 55 ' s f (27 Obs.) ; /.436 (i 1 Obs.) ; 
Epoch 1825.27. 
Note. The observations of A C, when the star A was only 
seen as a single star, are rejected. 
This star presents the hitherto unique combination of three 
individuals, forming, if not a system connected by the agency 
of attractive forces, at least one in which all the parts are in 
a state of relative motion. To begin with the two nearer 
stars A and B. Sir W. Herschel’s measure of their posi- 
tion Nov. 28, 1781 (1781.90) was 86° 32' nf. and it will be 
remarked, that a position so nearly perpendicular to the diur- 
nal motion carries in some measure its own verification with 
it, as not liable to gross error. This differs no less than 
54° 22' from the present angle in the same quadrant, giving 
a mean annual motion of -f i °.254 or direct [nf s p). The 
distance remains as it was, so close as to be barely separable. 
In 1802 it was so also ; but at that time, though observed by 
