THE APPAKENT POSITION OF TIIE ZODIACAL LIGIIT. 



149 



midway between cr and <j> Leoms, and afterwards to Coma Berenices. The other 

 columns are divided into groups of three for the successive hours of right ascen- 

 sion. In each group the 

 by the line, the declinati 



first column gives the number 



of square degrees crossed 



of 



southern border of 



fir. 



squai 



I tal 



degree. 



The vacant 



if negative, and the mean number of stars to the square 



spaces show that the course of the lines sometimes carries them beyond the 



adopted limits of declination. 



TABLE V. 





^ * _ ■ ". > 



No. Of 



Line. 



No. 



Decl. 



Mean. 



19 



o 



14 



13.1 



22 



17 



13.5 



22 



20 



15.9 



19 



23 



16.2 



21 



26 



16.7 



14.0 

 11.0 

 11.0 



No. 



Decl. 



Mean. 



12 



o 



3 



11.2 



22 



6 



10.7 



21 



9 



10.2 



19 



12 



9.6 



21 



15 



11.0 



19 



17 



12.9 



21 



20 



12.6 



19 



23 



11.3 



20 



26 



11.1 



15 



27 



10.5 



11 



27 



10.9 



6 



27 



7.3 



No. 



Decl. 



Mean. I No. 



10.0 

 10.4 



u\ 



Decl. 



o 



io.r> 



10.1 



Mean. I No. 



Decl. 



Mean 



10.3 



In 8 



9\ and 10 h there is a 



maximum 



of stars, which appears later in 

 in each successive hour. If the position of the lines is exam- 



the series of lines 



ined, it will appear that the maximum approximately folio 



the course of 



pt 



The lines run northward in ll h and 12\ so that for these hours no in- 



dication is given in Table V. of the relative frequency of 



d it 



ly appears that the 



the course of the supposed band. If other observ 



of the Durchmusterung are 



*rs should 



ar the ecliptic, 

 ively few upon 

 sider that any 



band 



of faint light occurs there, the possibility of a diffused nebulosity in 



this 



part of the sky (which abounds in telescop 



nebulae), might be suggested 



Another faint band of light 



i 



appear 



to me to be situated south of /3 and 



1 



Vi 



irgmis. 



This 



g 



too near the southern limit of the Durchmusterung to 



the distribution of stars in it to be well studied from that catalogue. 



But 



so far as evidence can be obtained from it by the method above explained, it 

 would seem that along the line 



passing 



pproximately through /? and rj Virg 



1 Astronomische Nachrichten, CIX. 262. 



