  We present detailed image analysis of rest-frame optical images of 235
low-redshift ($z \leq$ 0.35) type 1 active galactic nuclei (AGNs) observed with
the Hubble Space Telescope. The high-resolution images enable us to perform
rigorous two-dimensional image modeling to decouple the luminous central point
source from the host galaxy, which, when warranted, is further decomposed into
its principal structural components (bulge, bar, and disk). In many cases, care
must be taken to account for structural complexities such as spiral arms, tidal
features, and overlapping or interacting companion galaxies. We employ Fourier
modes to characterize the degree of asymmetry of the light distribution of the
stars, as a quantitative measure of morphological distortion due to
interactions or mergers. We examine the dependence of the physical parameters
of the host galaxies on the properties of the AGNs, namely radio-loudness and
the width of the broad emission lines. In accordance with previous studies,
narrow-line (H$\beta$ FWHM $\leq 2000$ km~s$^{-1}$) type 1 AGNs, in contrast to
their broad-line (H$\beta$ FWHM $> 2000$ km~s$^{-1}$) counterparts, are
preferentially hosted in later type, lower luminosity galaxies, which have a
higher incidence of pseudo-bulges, are more frequently barred, and are less
morphologically disturbed. This suggests narrow-line type 1 AGNs experienced a
more quiescent evolutionary history driven primarily by internal secular
evolution instead of external dynamical perturbations. The fraction of AGN
hosts showing merger signatures is larger for more luminous sources. Radio-loud
AGNs generally preferentially live in earlier type (bulge-dominated), more
massive hosts, although a minority of them appears to contain a significant
disk component. We do not find convincing evidence for enhanced merger
signatures in the radio-loud population.
