The important assumption of constancy in the relative proportions of stars of different luminosities at all points in the galactic plane makes possible an analysis of galactic structure based upon general star counts. It is admitted, however, that there are serious fluctuations in this luminosity function from point to point and even over comparatively small distance ranges. In an attempt to evaluate systematically these variations, observations based on spectral types, colors and star counts are being made in eleven regions of the galactic plane from 1 = 120 to 1 = 2000. The spectral classifications are complete to mpg = 12.25. Analyses have been completed for two regions LFI at 19h27m, +6?9 in Aquila and LF2 at I9h36m, +300 in Cygnus. Color excesses for the early type stars in each region indicate moderate interstellar absorption. Densities for individual spectral groups have been computed and used to derive by summation a general luminosity function at 100, 200, 400, and 600 parsecs in each region. Comparison of these functions with the standard luminosity function generally used in star count analyses indicates: (a)At 100 parsecs an excess of 0.3 in log ~(M) for M ~ 2; for 3 ~ M ~ 6 there is a corresponding deficiency compared to the standard van Rhijn function. (b)The values of log ~(M) decrease on the average by 0.7 in the distance interval 100 to 600 parsecs in LFI, while the shape of the (M, log ~(M)) curves remains sensibly the same. (c)At M = 0 in LF2 a small excess over the standard function is present at distances 200, 400, and 600 parsecs. For I ~ M ~ 5 the observed functions are deficient by about 0.4 in log ~(M). Details of the investigation will be published elsewhere. Warner and Swasey Observatory, Case School of Applied Science, Cleveland, Ohio.