  Using a nearest neighbor analysis, we construct a sample of void galaxies
from the Sloan Digital Sky Survey (SDSS) and compare the photometric properties
of these galaxies to the population of non-void (wall) galaxies. We trace the
density field of galaxies using a volume-limited sample with z_{max}=0.089.
Galaxies from the flux-limited SDSS with z\leq z_{max} and fewer than three
volume-limited neighbors within 7h^{-1}Mpc are classified as void galaxies.
This criterion implies a density contrast \delta \rho/ \rho < -0.6 around void
galaxies. From 155,000 galaxies, we obtain a sub-sample of 13,742 galaxies with
z\leq z_{max}, from which we identify 1,010 galaxies as void galaxies. To
identify an additional 194 faint void galaxies from the SDSS in the nearby
universe, r~ 72 h^{-1}Mpc, we employ volume-limited samples extracted from the
Updated Zwicky Catalog and the Southern Sky Redshift Survey with z_{max}=0.025
to trace the galaxy distribution. Our void galaxies span a range of absolute
magnitude from M_r=-13.5 to M_r=-22.5. Using SDSS photometry, we compare the
colors, concentration indices, and Sersic indices of the void and wall samples.
Void galaxies are significantly bluer than galaxies lying at higher density.
The population of void galaxies with M_r ~ M* +1 and brighter is on average
bluer and more concentrated (later type) than galaxies outside of voids. The
latter behavior is only partly explained by the paucity of luminous red
galaxies in voids. These results generally agree with the predictions of
semi-analytic models for galaxy formation in cold dark matter models, which
indicate that void galaxies should be relatively bluer, more disklike, and have
higher specific star formation rates.
