extra Lines in the Spectra of the Helium Stars, fyc. 419 



it as a helium star. It contains two crucial lines of helium. The 

 Wolf-Rayet stars, of which it is the principal example, are thus 

 classified as helium stars. There are also some coincidences between 

 the bright lines of 7 Argus and the spectrum of oxygen, which 

 suggest a possible connection. 



The spectrum of /x Centauri is also given as a bright line helium 

 star. The bright lines in this case are due to hydrogen, and the 

 spectrum resembles that of 7 Cassiopeia?. The spectrum of 8 Centauri 

 is similar. 



I take this opportunity of presenting a summary of the spectra of 

 116 stars to the 3-s- magnitude in the Southern Hemisphere. They 

 were photographed between May and October last by means of my 

 own object-glass prism, mounted in front of the Cape astrographic 

 telescope. This instrument, which is similar to my own telescope at 

 Rusthall, with which the spectra of the northern stars were photo- 

 graphed, was kindly placed at my disposal by H.M. Astronomer, 

 Dr. Gill. It may be a little time before the actual photographs of 

 the stellar spectra are ready for presentation, and meanwhile the 

 results are of interest. 



In my previous paper I divided the sphere into eight equal areas 

 consisting or two galactic equatorial areas and two galactic polar 

 areas, situated on either side of the galactic equator. The northern 

 stars already given occupy the upper or northerly lateral areas A, 

 B, C, and D, also the southerly area AA. The southern stars now 

 given occupy the lower or southerly lateral areas BB, CC, and DD. 

 Their photographic spectra are distributed into these areas, and are 

 classified on the same system as in the previous pa.per. The table of 

 distribution for the whole sphere by areas and classes is given below. 



There are in all 89 helium stars (Division I), distributed 71 in the 

 galactic zones and 18 in the galactic polar areas, the areas being 

 equal. There are 29 in the upper galactic zone (B and BB), and 42 

 in the lower galactic zone (C and CC). There are 9 in the upper 

 polar areas (A and AA), and 9 in the lower polar areas (D and DD). 

 There are 23 in the northerly halves of the two galactic zones (B 

 and C) and 48 in the southerly halves (BB and CC). 



The 81 stars in Division II, the Sirian stars, and Division III, the 

 Procyon stars (which along with Division I constitute Secchi's 

 Type I) are rather irregularly distributed throughout the sphere. 

 There are 40 in the galactic zones and 41 in the galactic polar areas. 

 There are 18 in the upper galactic zone (B and BB) and 22 in the 

 lower (C and CC). There are 29 in the upper polar areas (A and 

 AA) and 12 in the lower (D and DD). To the extent of the obser- 

 vations there is no condensation of stars of Divisions II and III in 

 the galactic zones as there is in the case of stars of Division I. 



The 106 3tars in Divisions IV and V (II and III of Secchi's types) 



