fp, = 4,25 () = 7,25 61 = 10,25 
m. = 3 
eo} Se e=4 | ¢=1 Se e=4 | 2=l Si e=4 
2 | | 
0,093 | 0,105 | 0,105 [0,006 | 0,006 | 0,006 
>| 135 155 158 | 012 013 013 
ae 221 226 | 021 023 023 
> | 939 301 311 | 035 039 039 
© | 20 396 417 | 057 | 064 065 [0,003 | 0,003 | 0,003 
TT 345 500 543 | 085 ~ 099 100 | 006 006 | 006 
° | 383 605 689 | 122 | 146 150 | O11 012 | 012 
"| 404 697 854 | 164 206 214 | 019 021 021 
mel doe fet. | 1,033 |= 210. | — 279 204 | 032 036 | 036 
Es 399 188 | 1,214 | 253 | 361 393 | 051 059 | 060 
= 382 780 | 1,375 | 289 | 448 509 | 075 091 093 
Ne ae 149 | 1,479 | 312 527 641 | 106 133 138 
ele 705 | 1,500 | 320 | 587 785 | 140 186 196 
Pel Bia 657 | 1,448 | 315 | 617 933 | 174 247 269 
2 286 605 | 1,354 | 295 | 610 | 1,060 | 200 | 308 | 350 
oe Sea | 560 | 1,254 | 277 | 586 | 1,153 | 224 313 | 452 
a 255 546 | 1,179 | 236 426 563 
k 233 | 500 | 1,140 | 235 456 | 676 
: 212 | 454 | 1,059 | 225 460 778 
| | 
6. For fainter stars the logarithmic defect strongly increases at 
first, until a maximum is reached (about proportional to the absorp- 
tion), and the values again decrease. This is due to the fact that 
for the faint magnitudes an ever greater majority of the stars lies 
behind the nebula, so that the logarithmic defect approaches ever 
more to the difference log Nn—log N,,-:; for fainter magnitudes, 
however, this difference decreases. 
c. For the bright stars, where the influence of the absorption 
begins to be felt, the logarithmic defect changes but little with the 
absorption-coefficient. The reason is that here the obscured stars 
behind the screen play hardly any part at all. The decrease in the 
number of stars is almost entirely a result of the falling off of the 
