  We study the morphologies and structures of 57 dwarf galaxies that are
representative of the general population of dwarf galaxies, and compare their
demographics to a sample of dwarf galaxies hosting optically-selected AGNs. The
two samples span the same galaxy stellar mass ($10^9 \lesssim M_\star/M_\odot
\lesssim 10^{9.5}$) and color range, and the observations are well-matched in
physical resolution. The fractions of irregular galaxies (14\%) and
early-types/ellipticals ($\sim 18\%$) are nearly identical among the two
samples. However, among galaxies with disks (the majority of each sample), the
AGN hosts almost always have a detectable (pseudo)bulge, while a large fraction
of the non-AGN hosts are pure disk galaxies with no detectable (pseudo)bulge.
Central point sources of light consistent with nuclear star clusters are
detected in many of the non-AGN hosts. In contrast, central point sources
detected in the AGN hosts are on average more than two orders of magnitude more
luminous, suggesting the point sources in these objects are dominated by AGN
light. The preference for (pseudo)bulges in dwarf AGN hosts may inform searches
for massive black holes in dwarf galaxies and attempts to constrain the black
hole occupation fraction, which in turn has implications for our understanding
of black hole seeding mechanisms.
