200 Use of the Zenith Telescope in Determining Latitudes. 
> Z—EZ1=2 41" for 17 pairs. 
PD. | A+A' 2-2 2D. 
Pair, Star. [N.or8.| Mag. | Auta. AR. | N. 
| hee: ms. 8.422 > tA! Pas 
6109 | N | 5 3 17 55 39 | 44 29 23 92° 1° 46! 
I Time, yp! Sagittarii at| 18 04 46 
6203 | S | Vi | x | 18 10 59 | 47 53 21 | 2944" |=—6 16 "1 38 
yre. 18 31 51 
Time, < 6599 ....... II 
6 Aquile ..| 19 17 58 
2 1| N | VIs{ 3 | 19 23 0f | 32 16 29 13 iz 
6740; 8 IV 3 | 19 33 27 | 60 17 24 [27 53!/—1 OF} 1 y 
3 | 67713 | S Vv 3 | 19 38 53 | 53 00 19 45 
6865 | N | VI 1 | 19 52 38 | 39 30 00 |30 19/1 19) 6 45 
4| 6937| S Vv 3°} 20 03 51 |°53 35 56 ES 
6959 | Nj V I | 20 08 22 | 38-59 12 |35 o8|+6 08 7 16 
5 | 7001 | S VI 1 | 2013 29 | 51 27 51 . 5 12 
7062 | N vi 2 | 20 22 27.| 41 06 48 |34 39/45 39) 5 09 
Time, 61', Cygni,.. 21 00 11 
= 7398 | S | 4 e Ir 31 | 51-13 58 Be 
ALI I at 14 18 | 41 07 25 | 21 23/—7 37] 5 
Time, 8 Aquarii,... 21 23 39 
7 | 7598 3 | 21 41 15 | 41 23 03 4 52 
7614 VI 1 | 21 44 52 | 51 09 32 59/43 59 4 54 
3 ad 1 | 22 15 38 | 47 00 37 —- 
3 | 22 31 48 | 45 35 50 | 36 27|+7 27} 0 40 
9 733 i WW t.3 28 38 | 36 55 50 ,*, 
158 VI | 3 | 00 29 20 | 55 25 43 | a1 34|/—7 26 aie 
I 226 | N | VI oo 41 13 | 43 03 18 i 
283 VI 3 | 00 54 29} 49 27 54 | 3 12\-+4+2, 12) 3 12 
II 318 oo 5g 28 46 51 35 o 36 
352 y o1 03 54 | 45 27 50 | 19 25|-9 35| 0 47 
12 487 i oe 1 28 48 | 42 08 06 f ‘ a 
102 1 31 44 }|-50 11 13 |19 19|- Ing 
13 a Va 1 59 27 | 52 51 20 sacks eis 6 36 
67 ‘i Vi 2 29 27 +o 27) 6 37 
14 706 Vv : 2 09 37 18 55 cd Bad 
727 ¥ 2 13 31 | 49 17 18 |36 13/47 13) 3 02 
15{ 819} N | VI I 2 32 26 | 37 07 08 ee 
Va | 3| 24216 | 55 33 47 | fo 55/411 55] 9 18 
16 | 915 V4 | 2] 249 45 | 55 25 27 i a 
94 V } Wig} 3 | 2 53 57 | 37 05 11 |30 38/41. 38 ae 
17 | 953 3 | 2 55-341 51 44 Ae 
1043 II 4 | 3 13-37} 40 4o 42} 25 26/-3 34 5 3 
Som + 47/ 57" 
: ie 14, 16!" 
DZ—IZl = 2! Ault 
ES Se eee 
The places of the stars are next accurately worked up by the 
method laid down in the preface to the B, A. C.. ; 
he forms used for computing the observations with the zenith 
telescope are shown, in the annexed tables. There are brieler 
methods; but this one has the advantage that all the quantities 
are spread out in the table, so that a second computer (the office 
computer) who differs from the first (the field computer) may 
trace, readily, the source of discrepancy. 05 
y a» Poe: Sy F pen 
a 
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