  The large-scale structure (LSS) of the Universe is comprised of galaxy
filaments, tendrils, and voids. The majority of the Universe's volume is taken
up by these voids, which exist as underdense, but not empty, regions. The
galaxies found inside these voids are expected to be some of the most isolated
objects in the Universe. This study, using the Galaxy and Mass Assembly (GAMA)
and Galaxy Zoo surveys, aims to investigate basic physical properties and
morphology of void galaxies versus field (filament and tendril) galaxies. We
use void galaxies with stellar masses of $9.35 < log(M/M_\odot) < 11.25$, and
this sample is split by identifying two redshift-limited regions, 0 < z <
0.075, and, $0.075 < z < 0.15$. To find comparable objects in the sample of
field galaxies from GAMA and Galaxy Zoo, we identify "twins" of void galaxies
as field galaxies within $\pm$0.05 dex and $\pm$0.15 dex of M and specific star
formation rate. We determine the statistical significance of our results using
the Kolmogorov-Smirnov (KS) test. We see that void galaxies, in contrast with
field galaxies, seem to be disk-dominated and have predominantly round bulges
(with > 50 percent of the Galaxy Zoo citizen scientists agreeing that bulges
are present).
