756 



TABLE 863.— LOG (NO. STARS)/(SQ. DEGREE) BRIGHTER THAN PHOTO- 

 GRAPHIC MAGNITUDE, m , AT STATED GALACTIC LATITUDES* 



(Characteristic 8. or 9. means, of course, —2. or — 1.) 



For values averaged over all galactic longitudes see reference, footnote 281. An excess 

 of stars, relative to the averages, between longitudes 230° and 50°, and a deficit elsewhere, 

 reflect the eccentric position of the sun within the stellar system, which, in a first approxi- 

 mation, may be regarded as a greatly flattened spheroid. For more detailed values for both 

 longitude and latitude see references, footnote 282. The Groningen numbers are generally 

 larger than the Mount Wilson values, notably so in low galactic latitudes. This defference 

 arises partly from the irregular influence of the highly complex structure of the stellar 

 system and especially of the obscuring dust clouds in and near the Milky Way. Mount 

 Wilson results were derived from counts of stars in small areas at and north of declination 

 — 15° ; Groningen results from sample counts over the whole sky. The Groningen magni- 

 tude scale for faint stars south of declination — 15° is, however, somewhat in doubt and 

 may also affect the totals. 



* Prepared by F. H. Seares, Mount Wilson Observatory. 



^vanRhijn, Groningen Publ. No. 43, Table 6, 1929. 



282 vanRhijn, Groningen Publ. No. 43, Table 10; Seares and Joyner, Mount Wilson Contributions 

 Nos. 346, 347; Astrophys. Journ., vol. 67, p. 24, 123, 1928; Puhl. Astron. Soc. Pacific, vol. 40, p. 303, 

 1928. 



TABLE 864.— STARS OF LARGE PROPER MOTION * 



Star m 



+ 4 : 3561 9.4 



—44:612 9.0 



+38:2285 6.4 



—36:9694 7.3 



—37:9435 8.5 



R 619 12.6 



61 Cygni 5.6 



+36:2147 7.5 



W 359 13.8 



e Indi 4.7 



+44:2051 8.7 



o 2 Eridani 4.5 



m = magnitude, Sp = spectrum, M =: proper motion, = position angle. 



Stars have been identified with their B.D. or C.P.D. numbers. In case of multiple stars the 

 magnitudes and spectra of the brightest component are given. For further information on stars 

 possessing large proper motions see references, footnote 283. 



* Prepared by W. Luyten, University of Minnesota. 



ssoLick Obs. Bull. No. 344; Harvard Circ. 283; Publ. Cincinnati Obs. LO 18; Publ. Astronomical Obs. 

 Univ. Minnesota, vol. 3, No. 1. 



SMITHSONIAN PHYSICAL TABLES 



