  Brighter Type Ia supernovae (SNe Ia) prefer less massive host galaxies and
regions of higher star formation, but the dependence on host property
measurement technique on this bias is not known. Using the PISCO IFS sample of
SN host galaxies alongside SDSS, GALEX, and 2MASS photometry, we compared host
galaxy stellar mass and star formation rate (SFR) estimates using different
observation methods and fitting techniques. Mass estimates were consistent
regardless of fitting technique. For optical wavelengths, the magnitude
correction size ("magnitude step") for mass estimates varied from -0.04 mag for
FAST++ and STARLIGHT to -0.02 mag for ZPEG. Including UV information for mass
estimates results in a mass-dependent shift in estimates of the individual
galaxies but had no effect on measured mass step size or location. Regardless
of technique, the measured magnitude step for global specific SFR (sSFR) was
~0.1 mag; UV-calibrated SFR estimates were consistent with those from
H{\alpha}. Only 49 hosts were used to measure the sSFR step as opposed to 76
FAST++ mass estimates or 97 STARLIGHT mass estimates to measure the mass step.
Local sSFR step model fits were inconclusive due to a diminished sample size of
38 SNe Ia. Stronger correlation between GALEX UV photometry global and local
sSFR estimates relative H{\alpha}estimates due to a large GALEX PSF inhibits
its use to measure local UV 1 kpc flux. Overall, observation method and fitting
technique had little influence on host bias detection. Instead, of importance
is the property used to measure the host bias.
