Stellar velocity distribution 29 

 TABLE IX. 



The mean velocities of the different spectral classes, computed after the combination 

 of the diametrically situated squares. 









ß 





A 





F 







G 





K 





M 



Sc 



a a re 































































/z 



G 



n 





n 





n 







n 





" 







+ F 2 



2 



+ O.90 



6 



+ 3.38 



- 



+ 3.26 



4 





h 3.27 



22 



+ 4.06 



5 



+ 2.60 



A 2 



+ F, 



7 



+ 1.62 





+ 2.94 



10 



+ 4.14 



1 1 





- 3.74 



31 



+ 4.56 



3 



+ 5.14 



Bi 



+ £„ 



32 



+ 1.97 



12 



+ 2.79 



lo 



+ 5.30 



9 



+ 3.09 



21 



+ 4.38 



5 



+ 3.74 



B 2 





2!) 



-f- 2.14 



3 



+ 2.33 



13 



+ 2.90 



13 



+ 4.41 



19 



+ 4.32 



4 



-1- 4 47 



Bs 



+ £« 



L2 



-f 2.02 



12 



+ 3 19 



9 



+ 4.22 



s 



+ 5.87 



24 



+ 4.69 



4 



+ 3.35 



Bi 



+ £« 



1; 



+ 0.96 



15 



+ 2 35 



11 



+ 3.79 



9 



+ 3 62 



20 



+ 3.91 



2 



+ 5.5.Ï 



ß 5 



+ £ 10 



2 



+ 1.71 



Hi 



+ 3.17 



10 



+ 3.57 



9 



+ 4 55 



23 



+ 4^36 



5 



+ 2 40 



B« 



+ £1 



4 



+ 2.28 



1 7 



+ 2.04 



12 



+ 2.41 



8 



+ 3.59 



13 



+ 3.95 



5 



+ 3.65 



B, +E 2 



6 



+ 1-92 



10 



+ 3.07 



L3 



+ 3 61 



in 



+ 3.77 



19 



+ 3.67 



4 



+ 4.70 



B K + E S 



13 



+ 1.35 



12 



+ 1.99 



13 



+ 2.79 



8 



+ 4.20 



26 



+ 3.88 



6 



+ 2.88 



ß, +£ 4 



2 s 



+ 1.63 



12 



+ 2.11 



16 



+ 2.50 



1 ( ) 



+ 2.46 



36 



+ 3.68 





+ 0.85 



B 1 



+ £, 



20 



+ 2.28 



14 



+ 3.33 



11 



+ 3.98 



10 



+ 2.35 



27 



+ 3.53 



3 



+ 10.93 



C, 



+ o 7 



3 



+ 1.13 



8 



+ 1.51 



4 



+ 2.28 







h 3.08 



13 



+ 4.30 



3 



+ 5.26 



c 2 



+ Dh 



11 



+ 1.32 



9 



+ 4.24 



5 



+ 3.69 



4 



+ 4.04 



20 



+ 4.39 





+ 6.00 



c 3 



+ D, 



17 



+ 1.38 



23 



+ 4.49 



18 



+ 4.65 



9 





-3.46 



16 



+ 2.88 



4 



+ 1 36 



Ci 



+ ö,o 



6 



+ 2.32 



8 



+ 3.96 



8 



+ 3.57 



15 





-3.60 



22 



+ 5.59 



3 



+ 5.08 



c 5 



+ D U 



2 



+ 2.07 



13 



+ 3.63 



9 



+ 4.54 



11 





- 4 79 



13 



+ 2.28 



4 



+ 4.77 



c 6 



+ A« 







11 



+ 2.89 



8 



+ 3.83 



5 





-1.84 



11 



+ 4.62 



4 



+ 5.13 



c 7 





1 



+ 0.17 



8 



+ 3.91 



5 



+ 3.37 



8 





-3,57 



20 



+ 3.99 



5 



+ 4.28 



c 8 



+ D 2 





+ 1.95 



10 



+ 2.42 



11 



+ 4.54 



6 





- 7.69 



20 



+ 4 81 



3 



+ 6.66 



c 9 



+ Ds 



16 



+ 1 34 



9 



+ 3.59 



8 



+ 4.50 



6 



+ 7.89 



18 



+ 3.73 



2 



+ 9.13 



c 10 



+ Ü4 



18 



+ 2.43 



12 



+ 3.03 



9 



+ 5.03 



11 





h 3.74 



22 



+ 4.46 



2 



+ 3.50 



c„ 



+ ö 5 



4 



+ 1.27 



9 



+ 2.08 



11 



+ 4.05 



13 





-4.46 



14 



+ 4.63 



2 



+ 1.17 



c„ 



+ D 8 



4 



+ 1.80 



9 



+ 2.36 



6 



+ 2.15 



4 



+ 3.42 



16 



+ 4.52 



3 



+ 3.12 



26. Let us start with an examination of the mean velocities of the stars in 

 relation to their spectral classes. For this purpose all squares have to be combined. 

 The dispersion being computed about a fixed point in every square, the formula takes 

 the simple form 



No; = + n 2 a\ + . . . + n 2i T 2i . 



Here N denotes the total number of stars, », and a, : are referred to the individual squares. 



The table X contains these mean velocities v s for the spectral classes and for 

 two groups of magnitudes. 



For every value the mean error is added, computed from the usual formula 



The column designated with x> contains the average velocity, and is related with 

 the former through 



(H) 



