Astro-Photographic Catalogue Plates. 



109 







From Meridian observations. 





From the Plate. 



star 



Rig 



ht Ascension 



(1900.0) Declination 



Xsec 6 



Y 



I 



h 

 O 



m 



59 



31-38 



24 



25 



18.2 



— 267!483 



+ 1517-35 



2 



O 



59 



59-37 



23 



56 



5I-I 



— 240.496 



— 191.70 



3 





I 



1.05 



24 



22 



9-7 



—178.289 



+ 1320.37 



4 





I 



41.71 



24 



18 



22.6 



—137-815 



+ 1093.05 



5 





2 



4.61 



24 



26 



21.5 



—114.790 



+ 1569.09 



6 





3 



52.92 



23 



55 



30.1 



— 6.941 



— 283.20 



7 





4 



14.86 



23 



15 



42.1 



+ 15-246 



—2671.86 



8 





4 



16.12 



23 



59 



5-7 



+ 16.262 



— 68.32 



9 





6 



57-04 



24 







2.9 



+ 177-143 



— 5-19 



lO 





7 



55-00 



24 



55 



49.6 



+233.493 



+3347-08 



II 





8 



7.14 



24 



28 



32.3 



,+246.422 



+1710.60 



From Table I, we find the following values of the refraction 

 coefficients : 



Mx = +.000226 



My = .00010 



iVx = .0000000 



Ny = +.000345 



The next step towards the determination of p, r, k and is the 

 computation of x sec d and y from the above values of the stars' 

 right ascensions and declinations. This is done by the aid of 

 Tables II and III, and the computation is here given in exten- 

 so for the first and last stars : 



Star. 



Aa 

 (Tab. II a) 

 (Tab. II B) 



X sec f5 



AS 

 + (Tab. Ill A 

 + (Tab. Ill b] 

 ± (Tab. lit D) 



y 



AS 

 1000 



AS 

 1000 



+ 



24 



+ 



+ 



+ 



59 



31-38 



I 



8 



7.14 



4 



0.00 



I 



4 



0.00 





268.62 



+ 





247.14 





.882 



— 





•913 





.026 



+ 





.020 





267.764 



+ 





246.247 



25 



18.2 



24 



28 



32^3 





1518.2 



+ 





1712.37 





14.62 



+ 





12.3 





.20 



+ 





•19 





-03 



+ 





.04 





1533-05 



+ 





1724.90 



We' now proceed to the computation of Ux and n by means of 

 equations (2). We have : 



