DR. W. HUGGINS ON THE PHOTOGRAPHIC SPECTRA OF STARS. 
G83 
I incline to believe that they would be detected probably in a more perfect spectrum. 
It may be, however, that e, £, 77, 0, l are really absent in the spectrum of Sirius. 
W.L. 
H 
4340 
h 
4101 
W 
3968 
K 
probably absent. 
Lines. 
W.L. 
« 3887-5 
/3 3834 
7 3795 
3 3767-5 
[See Addendum.] 
§ XI. 77 Ursce Majoris. 
The spectrum of this star is very similar to the typical spectrum of Vega. When 
the two spectra are seen together on the same plate it is at once perceived that the 
lines are rather less winged and broad than those of Vega. Eleven lines have been 
measured. The existence of a twelfth line 1 is doubtful, and therefore I have not 
inserted it in the map. As to K, any suspicion of a line here is far too doubtful to 
justify its insertion. As the spectrum is beautifully defined in the photograph, I 
think there is a strong presumption that it is absent. 
A strong continuous spectrum extends beyond S. In this star we may mark a 
first step in the direction of a spectrum containing fine lines in the photographic 
portion of the spectrum. Four fine lines are inserted in the map. 
Liner. 
H 
4340 
ft 
3820 very thin. 
4087-5 
thin and faint. 
7 
3795 
4137-5 
thin, but distinct. 
3 
3767-5 
h 
4101 
G 
3745-5 
4021 
thin, distinct. 
£ 
3730' 
3968 
V 
3717-5 
K 
probably absent. 
0 
3707-5 
CL 
3887-5 
L 
probably present. 
ft 
3834 
§ XII. a 
Virginis. 
In this spectrum we find ourselves advancing towards a condition in which the 
twelve lines are narrower and defined at the edges. At the same time a greater 
number of fine lines have appeared. I suspect a thin line at the position of K, and 
I have indicated this probability by a dotted line in the map. There is no doubt of 
line between H and K. In this spectrum I have not been able to measure lines 
beyond 77, though the continuous spectrum is strong and extends to about S. 
