748 



TABLE 852.— PERCENTAGE OF STARS OF VARIOUS SPECTRAL CLASSES* 



The data are taken from the publications of the Harvard, McCormick, and Bergedorf Observ- 

 atories. The discontinuity in trend appearing between the visual and photographic groupings is 

 in the sense to be expected. Ninety-nine percent of the stars brighter than magnitude 8.5 belong 

 to the six classes listed ; less than one percent have spectra of classes P , WR, O, R, N, S, and 

 Peculiar, and such stars are even more uncommon among the fainter groupings. 



Among stars brighter than sixth magnitude the percentages of dwarfs are as follows (Opik 

 et al.) : 



F5 



75 



F8 

 60 



GO 

 50 



G5 

 15 



KQ 



5 



3 



K5 

 2 



M 

 



A limited sampling in the Milky Way yields the following percentages of dwarfs among 

 fainter stars (Nassau and McCrae) : 



Photographic 

 magnitude 



8 to 10 



10 to 11 



11 to 12 



F 8 to G 2 

 75 



77 

 82 



(75 

 23 

 31 



42 



G 8 to K 3 



7 



8 



10 



In higher galactic latitudes the percentages of dwarfs are higher; thus in latitudes 31° to 90° 

 dwarfs constitute about 17 percent of the K0 and K2 stars of visual magnitude 10.4 (Janssen 

 and Vyssotsky). Among the M0 and M8 stars of all latitudes between visual magnitudes 8.5 

 and 10.5 3 percent are dwarfs (Dyer and Vyssotsky). 



* Prepared by A. N. Vyssotsky, University of Virginia. 



TABLE 853.— THE LOCAL FAMILY OF GALAXIES 275 



Member Type 



Our galaxy Sb 



M 31 Sb 



LMC / 



M 33 Sc 



SMC / 



M 32 E 2 



Fornax system E 



NGC 205 E5p 



NGC 6822 / 



IC 1613 / 



Sculptor system E 



NGC 185 E 



NGC 147 E 



275 Baade, Walter, Astrophys. Journ., vol. 100, 

 t Modulus in stellar magnitude is m — M = 5 

 absolute magnitude. 



p. 150, 1944. 



(log d — 1), where d is distance in parsecs and M is 



SMITHSONIAN PHYSICAL TABLES 



