Core-collapse, superluminous, and gamma-ray burst supernova host galaxy populations at low redshift: the importance of dwarf and starbursting galaxies

TL;DR

This study analyzes the properties of 150 nearby core-collapse supernova host galaxies, comparing them to gamma-ray burst and superluminous supernova hosts, highlighting the importance of dwarf and starbursting galaxies in these phenomena.

Contribution

It provides a comprehensive, unbiased analysis of low-redshift CCSN host galaxies and compares their properties with SLSN and LGRB hosts, emphasizing the role of dwarf and starburst galaxies.

Findings

33% of CCSNe occur in dwarf galaxies

2% of CCSNe are in dwarf starburst galaxies

Higher SLSN to CCSN rate in low-mass and high sSFR galaxies

Abstract

We present a comprehensive study of an unbiased sample of 150 nearby (<z> = 0.014) core-collapse supernova (CCSN) host galaxies drawn from the All-Sky Automated Survey for Supernovae (ASAS-SN) for direct comparison to the nearest LGRB and SLSN hosts. We use public imaging surveys to gather multi-wavelength photometry for all CCSN host galaxies and fit their spectral energy distributions (SEDs) to derive stellar masses and integrated star formation rates. CCSNe populate galaxies across a wide range of stellar masses, from blue and compact dwarf galaxies to large spiral galaxies. We find 33(+4,-4) per cent of CCSNe are in dwarf galaxies (M < 10^9 M_Sun) and 2(+2,-1) per cent are in dwarf starburst galaxies (sSFR > 10^-8 yr^-1). We reanalyse low-redshift SLSN and LGRB hosts from the literature (out to $z<0.3$) in a homogeneous way and compare against the CCSN host sample. The relative SLSN to CCSN supernova rate is increased in low-mass galaxies and at high specific star-formation rates. These parameters are strongly covariant and we cannot break the degeneracy between them with our current sample, although there is some evidence that both factors may play a role. Larger unbiased samples of CCSNe from projects such as ZTF and LSST will be needed to determine whether host-galaxy mass (a proxy for metallicity) or specific star-formation rate (a proxy for star-formation intensity and potential IMF variation) is more fundamental in driving the preference for SLSNe and LGRBs in unusual galaxy environments.