부산대학교 도서관

We have analyzed the data on field galaxies presented in a previous paper, as well as other published data. Dropping the usual assumption of uniform space distribution, we find that the luminosity function of field galaxies can be fit by the function proposed by Schechter with faint end slope, ..cap alpha..=-1.10 +- 0.15, and characteristic magnitude, M/sup asterisk//sub B/T=-21.00 +- 0.11 (assuming H/sub 0/=50 km s/sup -1/ Mpc/sup -1/), values not significantly different from those of the cluster galaxy luminosity function. The space density of galaxies in the south galactic cap is fairly constant with distance, out to our survey limit of about 200 h/sup -1/ Mpc. In the north galactic cap there are large density fluctuations, including the local supercluster and an even larger feature, 50 h/sup -1/ Mpc deep, centered at v/sub r/approx.8000 km s/sup -1/. Galaxy counts and the distribution of rich clusters confirm this analysis and suggest that the second feature subtends a large fraction of the north galactic polar cap. The large density fluctuations over our survey volume make it difficult to determine accurately the mean space density of galaxies. We estimate the mean luminosity density of the universe to be 10/sup 8/L/sub sun/ Mpc/sup -3/, but the uncertainty is large. A spatial covariance function analysis of our sample suggests power on scales up to 30 h/sup -1/ Mpc, with no evidence of the break in xi (r) at approx.10 h/sup -1/ found by Groth and Peebles in the projected galaxy distribution.