Stellar velocity distribution 



65 



3. Concerning the moments of higher order for stars brighter than 5,0 the 

 characteristics of the third and fourth orders in the three main directions in the 

 galactic system were found to be very small. However, a distinct negative skewness 

 was found in the direction of the principal vertex, and, furthermore, a positive 

 excess in the other two directions. 



4. A comparison between proper motion and radial velocity of the stars, the 

 mean parallaxes were derived for the different spectral classes including stars of 

 magn < 4,9. 



5. A comparison between the moments of the second order from proper motion 

 and radial velocity observations led to the unexpected small value 4- 0.50 of the 

 constant q . This value is, however, strongly influenced by the parallax assumed. 



Observatory Lund jan. 1915. 



In concluding I desire to express to Prof. C. V. L. Charlier my hearty thanks 

 for the interest he has taken in my work and for the valuable advice and direc- 

 tions he has given me during its progress. I also take this opportunity of thanking 

 my colleague, Mr S. D. Wicksell for pleasant and profitable collaboration ; our common 

 discussions on stellar astronomical problems have, especially in the case of the pre- 

 sent paper, been of extremely great use to me. 



To the Royal Physiographic Society I am indebted for monetary assistance. 



Errata : 



In the table X page 30 the lines indicated by K and M are to be exchanged. 



Lnnds Universitets Årsskrift. N. F. Avd. 2. Bd 11. 



9 



