Stellar velocity distribution 



57 



TABLE XVIII. 

 The parallaxes of stars brighter than magn 4.9. 















Results of 







Number 

 of stars 











Campbei. 



L 



Kapteyn 





Spectral type 







all magnitudes 



computed for 

 m agn. 5.0 















Number 





Remarks 



Number 



it 





B 



197 



0".0075 



+ 



0".0003 



312 



90 



0".0061 

 0.0129 



B0—Bb 

 BS—Bd 



440 



0".0068 





A 



192 



0.0162 



± 



O.ooio 



172 



0.0166 





1088 



0.0008 





F 



128 



0 0270 



+ 



0.C031 



180 



0.0354 









VI 



G 



107 



0.0127 



± 



0.0016 



118 



0.0223 





1036 



0.0224 



îl- 

 es 



K 



338 



0.0170 



+ 



0.00:12 



346 



0.0146 











M 



63 



0.0144 



± 



0.0023 



71 



0.0106 





101 



0.0111 





All spectral types 



1028 



0.0161! 



+ 



0.0005 













In the table XVIII the values of $ l are given for each spectral class. It may 

 be observed that, when using the units Sirioineter and Stellar year in connection 

 with angular measure, the values of i> L will be equal to the parallaxes. 



For a comparison with other results, I give the values of the parallaxes derived 

 by Campbell and Kapteyn. None of these results, however, are comparable with 

 the present ones, since here the stars are limited to the magnitude 5.0. On the 

 other hand Campbell has determined the parallaxes in a special way. The average 

 values of the components of the proper motion after a reduction for the sun's velo- 

 city he directly compares with the average radial velocity and thus derives the 

 parallaxes. This method, only applicable when the stars in each spectral class are 

 at the same distance, is surely a rough approximation. 



The agreement between the present results and those of Campbell seems to 

 be satisfactory with the exception of the parallaxes of the F and G class stars. It 

 must however be noted that Campbell only rejected very few stars, whose proper 

 motions were extremely large b 



52. In order to examine whether the parallax is a function of galactic lati- 

 tude I have for the group magnitude < 4.9 in the way described on page 19 divided 

 the sky into two groups of squares surrounding the plane and the pole of the 



1 See Lick Obs. Bulletin VI page 131. 



Lunds Universitets Årsskrift. N. F. Afd. 2. Bd 11. 



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