The Carnegie Supernova Project-I: Correlation Between Type Ia Supernovae
  and Their Host Galaxies from Optical to Near-Infrared Bands
  We present optical and near-infrared ($ugriYJH$) photometry of host galaxies
of Type Ia supernovae (SN~Ia) observed by the \textit{Carnegie Supernova
Project-I}. We determine host galaxy stellar masses and, for the first time,
study their correlation with SN~Ia standardized luminosity across optical and
near-infrared ($uBgVriYJH$) bands. In the individual bands, we find that SNe~Ia
are more luminous in more massive hosts with luminosity offsets ranging between
$-0.07 \pm0.03$ mag to $-0.15\pm0.04$ mag after light-curve standardization.
The slope of the SN~Ia Hubble residual-host mass relation is negative across
all $uBgVriYJH$ bands with values ranging between $-0.036\pm 0.025$ mag/dex to
$-0.097\pm 0.027$ mag/dex -- implying that SNe~Ia in more massive galaxies are
brighter than expected. The near-constant observed correlations across optical
and near-infrared bands indicate that dust may not play a significant role in
the observed luminosity offset--host mass correlation. We measure projected
separations between SNe~Ia and their host centers, and find that SNe~Ia that
explode beyond a projected 10 kpc have a $\rm 30\% \ to \ 50\%$ reduction of
the dispersion in Hubble residuals across all bands -- making them a more
uniform subset of SNe~Ia. Dust in host galaxies, peculiar velocities of nearby
SN~Ia, or a combination of both may drive this result as the color excesses of
SNe~Ia beyond 10 kpc are found to be generally lower than those interior, but
there is also a diminishing trend of the dispersion as we exclude nearby
events. We do not find that SN~Ia average luminosity varies significantly when
they are grouped in various host morphological types. Host galaxy data from
this work will be useful, in conjunction with future high-redshift samples, in
constraining cosmological parameters.
