The Dependence of Type Ia Supernova Luminosities on their Host Galaxies
  (Abridged) Precision cosmology with Type Ia supernovae (SNe Ia) makes use of
the fact that SN Ia luminosities depend on their light-curve shapes and
colours. Using Supernova Legacy Survey (SNLS) and other data, we show that
there is an additional dependence on the global characteristics of their host
galaxies: events of the same light-curve shape and colour are, on average,
0.08mag (~4.0sigma) brighter in massive host galaxies (presumably metal-rich)
and galaxies with low specific star-formation rates (sSFR). SNe Ia in galaxies
with a low sSFR also have a smaller slope ("beta") between their luminosities
and colours with ~2.7sigma significance, and a smaller scatter on SN Ia Hubble
diagrams (at 95% confidence), though the significance of these effects is
dependent on the reddest SNe. SN Ia colours are similar between low-mass and
high-mass hosts, leading us to interpret their luminosity differences as an
intrinsic property of the SNe and not of some external factor such as dust. If
the host stellar mass is interpreted as a metallicity indicator, the luminosity
trends are in qualitative agreement with theoretical predictions. We show that
the average stellar mass, and therefore the average metallicity, of our SN Ia
host galaxies decreases with redshift. The SN Ia luminosity differences
consequently introduce a systematic error in cosmological analyses, comparable
to the current statistical uncertainties on parameters such as w. We show that
the use of two SN Ia absolute magnitudes, one for events in high-mass
(metal-rich) galaxies, and one for events in low-mass (metal-poor) galaxies,
adequately corrects for the differences. Cosmological fits incorporating these
terms give a significant reduction in chi^2 (3.8-4.5sigma). We conclude that
future SN Ia cosmological analyses should use a correction of this (or similar)
form to control demographic shifts in the galaxy population.
