48 



Hans Henie 



In the table the indices C signifies the squares, into which the zone between 

 equator and the circle of decHnation + 30" is divided. In Stellar Statistics this 

 zone is divided into twelve squares and in nine of these the characteristics Ic and 

 are computed. As can be seen, h, which is the dispersion in the frequency 

 curve of stellar magnitudes, is comparatively constant. The quantity however, 

 varies and has its maximum i i. e. in the Milky Way, and signifies the magni- 

 tude which includes the maximal number of stars. By the help of this little table 

 I calculate the reduction R[m) for each square, giving m the values 9,0 9,5 ... 12,0 12,5, 

 In this way I get the following values. 





i?(9,0) 



Ev!),5) 



Z?(U),0) 



ß(10,5 



E(ll) 



ß(ii,5: 



ß(12,0^ 



sa 2,5) 





7,895 



4,412 



2,632 



],G13 



1 



0,641 



0,423 



0,281 



Ci 



G,667 



4,211 



2,500 



1,569 



1 



0,650 



0,432 



0,293 



Cs 



6,944 



4,167 



2,551 



1,582 



1 



0,648 



0,430 



0,291 



Ci 



9,C00 



5,143 



2,7C9 



1,636 



1 



0,6C0 



0,371 



0,237 



c. 





4,553 



2,075 



1,609 



1 



0,6t3 



0,414 



0,278 



c. 



7^000 



4,109 



2.487 



1,549 



1 



0,6C0 



0,415 



0,312 



c, 



5,947 



3,G85 



2,822 



1,507 



1 



0,078 



0,470 



0,384 



c. 



(;,103 



3,778 



2,356 



1,516 



1 



0,672 



0,459 



0,319 



c. 



8,250 



4,714 



2,700 



1,623 



1 



0,636 



0,417 



0,282 



These series show, that the reduction is not the same in all regions of the 

 heavens, but that it is influenced by the distance from the Milky Way. 1 there- 

 fore combine the squares having nearly the same star density and get the follo- 

 wing average values for small star density, I; for average, II; and for great star 

 density, III. 





5(9,0) 





R[,10,0) 





B(ll,o; 



ß(ll,5; 



R(12,0) 



ß(12,5) 



I 



6,350 



3,857 



2,888 



1,524 



1 



0,670 



0,460 



0,322 



II 



7,535 



4,411 



2,012 



1,599 



1 



0,640 



0,423 



0,286 



,1, 



9,000 



5,143 



2,709 



1,630 



1 



0,602 



0,371 



0,287 



These values are to be used for the reduction of the star density from any limi- 

 ting magnitude to the eleventh. For this purpose I interpolate the following table 

 in which I II III refer to the groups of density. 



