studies in Stellar Statistics 



47 



A glance on the table, eventually seconded by a graphical representation on 

 a globe, shows immediately that the right ascention of the apex must be about + 270". 

 The values of 31{x) and Jf(//) hence point to the classical value for the position of 

 this point. It is now known, from the researches of Kobold and others, that this 

 question cannot be satisfactory discussed without taking into account the systematic 

 motions of the stars themselves. As I intend to consider this problem in the next 

 term I here confine myself to the above remarks. 



25. Though it may not be impossible to determine rather accurately from 

 the dispersions of x and it is often connected with great difficulty and not free 

 from subjectivity to decide whether a certain star shall be excluded or not in the 

 computation of a. As, generally, the large deviations influence less the value of 

 the mean than that of the dispersion, it seems hence adviseable to use M{x) and 

 M{i/) for the determination of though these quantities are in other respects less 

 satisfactory. It seems indeed, as far as I have had opportunity to discuss the 

 problem, not appropriate to determine except in connection with a discussion of 

 the systematic motions of the stars. The following determination of X^^, as well as 

 that in the 23th §, must hence be considered as only provisional. I have even 

 confined myself to the use of M(y) only in the computation of X^, the values of 

 M{x) being indeed more affected by the systematic raotitms of the stars. 



Tab. 10. 





4 



Vi 





b 



m 



6'" 



Number of 



stars 





M{x) 



M[y) 



M{x) 



M(y) 



M{y) 







gm 





+ Ü.23 



— 0.43 



+ 0.74 



— 0.39 



— 0.42 



15 



38 



43 





+ 1.30 



— 0.75 



+ 0.75 



— 0.68 



- 1.11 



lö . 



65 



33 





+ 0 52 



— 0.71 



+ 0.66 



— 0.47 



— 0.46 



43 



94 



28 



% 



— 0.15 



— 0.68 





-0.29 



— 0.54 



— 0.29 



17 



71 



31 





— 0.86 



— 1.36 





- 0.59 



— 0.76 



— 0.70 



14 



43 



52 





— 1.00 



— Ü.83 





- 1.30 



— 0.73 



— 0.54 



12 



39 



36 





— 0.79 



— 0.17 





-0.85 



— 0.40 



— 0.86 



14 



40 



26 





— 1.03 



— 0.91 





-0.74 



— 0.57 



— 0.53 



17 



42 



10 





— 0.42 



- 0.27 





-0.3t 



— 0.35 



— 0.44 



IH 



61 



17 





+ 0.11 



— 0.07 



+ 0.14 



— 0.32 



— 0.21 



23 



73 



10 





+ 0.44 



— 1.11 



H 



L0.37 



— 0.44 



+ 0.22 



18 



54 



19 





+ 0.88 



— 0.31 



+ 0.67 



— 0.16 



— 0.55 



16 



38 



27 



Dr 



+ 0.72 



— 0.50 



- 



- 0.55 



— 0,20 



— 0.36 



9 



40 



29 



A 



+ 0 25 



— 0.56 



H 



- 1 35 



— 0.87 



+ 0.01 



16 



46 



18 





+ 0.15 



— 0.37 



+ 0.22 



— 0.23 



— 0.10 



23 



60 



11 





— 0.31 



— 0.00 





-0.25 



+ 0.04 



— 0.16 



82 



100 



8 



D. 



— 0.08 



— 0.50 





-0.85 



— 0.19 



— 0.38 



19 



52 



17 



A 



— 1.41 



— 0.41 





-0.89 



— 0.02 



— 0.13 



11 



31 



34 



D. 



(— 0.90 



— 0.30) 





-0.83 



— 0.52 



— 0.44 



5 



46 



37 





— 0.74 



— 0.55 





-0.74 



— 0.74 



— 0.74 



21 



51 



36 



A 



— 0.07 



— 1.14 





-0.23 



— 0.82 



— 0.56 



28 



37 



39 



Ao 



+ 0.62 



— 0.19 





-0.75 



— 0.55 



— 0.37 



16 



76 



38 



At 



+ 0.56 



— 0.61 





-0.66 



— 0.70 



- 0.57 



18 



50 



61 



A. 



+ 0.81 



— 0.92 





-0.73 



— 0.40 



— 0.32 



19 



51 



53 



