G-OTiE — A Catalogue of Binary Stars, 8fc. 
591 
45. 70 (y) Ophiuclii = 5 2272, More tlian a complete revolution 
of this well-known binary star has now been described since its dis- 
covery by Sir W. Herschel in 1779. Numerous orbits have been 
computed, but my elements represent recent measures better than 
others. 
Some recent measures are : — 
1886-528 : 
13°-8 
1" 
•98, Hall. 
1886-657 : 
14 
-08 : 
I 
•814, Schiaparelli. 
1886-67 
14 
•86 
1 
•88, Engelmann. 
1886-67 
13 
•7 
2 
•01, Jedrzejewicz. 
1886-76 
14 
•53 
2 
•07, Tarrant. 
1887-611 
3 .6 
1 
•93, Hall. 
1887-631 
4 
•36 
. 1 
•89, Schiaparelli. 
1887-812 
: 3 
•49 
: 1 
•91, Tarrant 2898). 
1887-86 
2 
•50 
2 
•35, Young. 
*1888-619 
• 350 
•47 
1 
•78, Tarrant. 
*1888-650 
352 
•4 
2 
•14, Leavenworth. 
*1889-30 
. 348 
•7 
: 2 
•16, Eurnham (36-inch refrac- 
tor) . ' ' Both stars single 
with 36-inch." 
The measures marked with an asterisk were made since my orbit 
was published {Mon. Notices, E. A. S., March, 1888). My elements 
give for these epochs : — 
1888-619 : 353°-63 : r'-86. 
1888- 650 : 353 -27 : 1 -87. 
1889- 30 : 346 -05 : 1 ^92. 
My elements, combined with Kriiger's parallax of 0"^162, give for 
the combined mass of the components = 2-777 times the sun's mass, 
and a mean distance of 27-77 times the sun's mean distance from the 
earth. The mass is, therefore, about the same as that of the Sirian 
system. 
I find that the plane of my orbit is at right angles to the plane of 
the Milky Way. 
46. ^ Sagittarii. Eecent measures seem to show that my elements 
are not far from the truth, but indicate that the period is slightly 
E.I. A. PEOC, SEK. III. VOL. I. 2 U 
