Spatially Resolved Properties of Supernova Host Galaxies in SDSS-IV MaNGA

TL;DR

This study analyzes the properties and environments of supernova host galaxies from SDSS-IV MaNGA, revealing differences in galaxy morphology and local stellar populations associated with different supernova types.

Contribution

It provides a detailed statistical comparison of supernova host galaxy properties, highlighting differences in morphology and local environments for Type Ia and CC supernovae.

Findings

Type Ia SNe occur in both star-forming and quiescent galaxies.

Type CC SNe are exclusively in star-forming galaxies.

SN locations have lower metallicity and younger stars than galaxy centers.

Abstract

We crossmatch galaxies from Mapping Nearby Galaxies at Apache Point Observatory with the Open Supernova Catalog, obtaining a total of 132 SNe within MaNGA bundle. These 132 SNe can be classified into 67 Type Ia and 65 Type CC. We study the global and local properties of supernova host galaxies statistically. Type Ia SNe are distributed in both star-forming galaxies and quiescent galaxies, while Type CC SNe are all distributed along the star-forming main sequence. As the stellar mass increases, the Type Ia/CC number ratio increases. We find: (1) there is no obvious difference in the interaction possibilities and environments between Type Ia SN hosts and a control sample of galaxies with similar stellar mass and SFR distributions, except that Type Ia SNe tend to appear in galaxies which are more bulge-dominated than their controls. For Type CC SNe, there is no difference between their hosts and the control galaxies in galaxy morphology, interaction possibilities as well as environments; (2) the SN locations have smaller velocity dispersion, lower metallicity, and younger stellar population than galaxy centers. This is a natural result of radius gradients of all these parameters. The SN location and the its symmetrical position relative to the galaxy center, as well as regions with similar effective radii have very similar [Mg/Fe], gas-phase metallicity, gas velocity dispersion and stellar population age.