1 332 



of cognate methods. The inegiilar coiii-se of the iimiibei'S n^" n," n^" 

 (hilt make up our mateiial, renders it doiil)tfnl whetlier the value 

 found is accurate up to 0,1. If we take the average 1,0J, and for 

 A^ and .1, 13,71 and 12,70, we find for all limiting magnitudes 

 (expressed in the provisional scale): 



^14,66; .1^13.71: .1 J 2,70; .4,11,66; yl, 10,50; A.'^A^. 

 When reduced to the real magnitudes, the limiting magnitude is 

 therefore : 



^14,30; .4,13,46; .4,12,57; .43 11,65; .4,10,62; ^,9,66 

 and the differences in limiting magnitude become: 



0,84 0,89 0,92 1,03 0,96 magn. 



4. lifsults. In tjie square that was examined the stars are not 

 regularly distributed. The greatest density is found on the N. and W. 

 sides; it seems as if two stai'-clouds, one from above, and one from 

 the right, stretch into this I'egion, divided by a region of less density, 

 reaching towards the S.El. Below lies a triangular, very poor region. 

 Herein as a kind of core, lie.* the three-armed void, which in the 

 pliotographs of the Galaxy taken by M.ax Wolf and Barnard, shows 

 like a black spot or hole ^). On dividing the field into 5 regions of 

 equal size, each of 20 stpiares, (the outlines of which have been 

 indicated on Table I by means of thicker lines), .so that 1 and II 

 comprise the densest. III and IV the niedium, and V the poorest 

 region, we find for the numbers of stars: 



III 



IV 



Sum 

 total 



logN 



m 



dlogN 

 dm 



0.52 

 0.36 

 0.43 

 0.39 

 0.63 



The values resulting hei-etVom for log N, the amount per square 

 degree, and for the gradient, are to be found foi- the entire square 

 in the last columns, for the five minor regions in the following list. 



The gradients for the entire region |»resent a few irregularities. 

 The differences between the last 3 values can be attributed to acci- 



') Compare e.g. Max Wolf, Die Milchslrasse, Fig. 33 and 34. 



