266 PROFESSOR L. BECKER ON 
Table VII. further contains the hydrogen spectrum observed by Wrtsineé and the — 
spectrum of Nova Aurigee by VocEL, both copied from the table in Wisine’s memoir 
Untersuchungen ueber das Spectrum der Nova Auriga. I ought to mention here 
that during the progress of my work I did not consult any previous researches or ; 
observations on new stars, and that I arrived at the result A without bias. Between 
4067 and 4341 the wave-length , of the zeros of the bands agree well with the waye- 
lengths measured in the spectrum of Nova Aurigee, and the two lines 4922 and 5016 | 
are also present in both. On the other hand, there are marked differences between 
H, and H,, the region which, owing to the large interval between two identifiable bands, 
presented the greatest difficulty to division into bands. Thesame remarks apply to the — 
hydrogen spectrum. It is of no moment that some of the lines, as 4388, 4472, etc., are 
found intensely bright, because, in accordance with the above, each might be split into 
two or more fainter lines. The fact that the hydrogen line 4581 is the only bright line 
of intensity above 6 which is not represented in the spectrum of Nova Persei, while it 
occurs in the spectrum of Nova Aurigze, appears to suggest that the observed maximum 
4560 to 4589 is not due to the band A, = 4570, which is one of those used in subdividing 
the spectrum. 
B. I therefore repeated the work between H, and H,, and subdivided the spectrum — 
as before, but chose 4581 instead of 4570; 4634 instead of 4637; and 4684 instead of 
4687. I further introduced the condition that as few lines as possible should be chosen, 
and that where the wave-length of the zero of a band fell near that of a hydrogen line, 
the wave-length of the H-line should be taken. The introduction of the line 4581 
instead of 4570 as zero of a band changed the position of all the bands as far as the 
H,-band; 4570 being the mean of 4559 and 4581, the two bands belonging to them 
share almost equally in producing the maximum formerly ascribed to 4570. Each band 
entails the introduction of a series of bands fitting into one another, and there are thus 
14 bands required to represent the intensity curve compared with 7 bands before. In 
other regions I altered some of the wave-lengths slightly to make them agree with 
those of hydrogen. The band ,=4768, which does not occur in the hydrogen 
spectrum, is perhaps due to a series of faint limes. The result of this new analysis is 
given in Table VIL, B, and the intensity curve calculated at intervals of 2 tenth-metres 
is drawn on Plates I. and II. under B. It is remarkable that the lines of the hydrogen __ 
spectrum, which I have been forced to take from Wus1ne’s table as being within 3 t.m. 
of the zeros of bands actually obtained, include all the hydrogen lines whose intensities | 
exceed 2 between 434] and 4861, though no heed was taken of their intensity. The — 
spectrum as defined by \, agrees well with that of Nova Aurigze. In the same table 1 | 
have further entered all the lines of helium except those of the two second subordinate 
series. All of them have corresponding lines in the Nova spectrum. 
(On the me of the additive rule, the brightest lines of the hydrogen and 2 
to Table V. and Sent 1; and I consider ie conjecture that inde actually pro-— 
