SNIa Host Galaxy Properties and the Dust Extinction Distribution

TL;DR

This study analyzes how host galaxy properties influence the dust extinction distribution for Type Ia supernovae, providing a refined model to improve supernova lightcurve fitting and cosmological measurements.

Contribution

It introduces a detailed analysis of the dependence of extinction distribution on galaxy inclination, radial position, and star formation, proposing a tailored prior for supernova lightcurve fitting.

Findings

Extinction distribution follows an exponential with τ=0.4 or 0.33.

Inclination correction with an infinitely thin disk suffices.

Star formation level affects the width of the extinction distribution.

Abstract

Supernovae Type Ia display a complex relation with their host galaxies. An important prior to the fit of the supernovae's lightcurve is the distribution of host galaxy extinction values that can be encountered. The SDSS-SN project has published light curve fits using both MLCS2k2 and SALT2. We use the former fits extinction parameter ($A_V$) to map this distribution of extinction values. We explore the dependence of this distribution on four observables; the inclination of the host galaxy disk, radial position of the supernova, redshift of the supernova and host, and the level of star-formation in the host galaxy. The distribution of $A_V$ values encountered by supernovae is typically characterised by: $\rm N_0 ~ e^{-A_V/\tau}$, with $\tau$= 0.4 or 0.33. We find that the inclination correction using an infinitely thin disk for the SNIa is sufficient, resulting in similar exponential $A_V$ distributions for high- and low-inclination disks. The $A_V$ distribution also depends on the radial position in the disk, consistent with previous results on the transparency of spiral disks. The distribution of $A_V$ values narrows with increased star-formation, possibly due to the destruction or dispersion of the dusty ISM by stellar winds prior to the ignition of the supernova. In future supernova searches, certainly the inclination of the host galaxy disk, should be considered in the construction of the \av \ prior with $\tau=0.4/cos(i)$ as the most likely prior in each individual host galaxy's case.