Physical Properties of the Host Galaxies of Ca-rich Transients

TL;DR

This study analyzes the host galaxies of Ca-rich transients using multiwavelength data to understand their stellar populations and progenitor origins, suggesting a predominantly white dwarf origin with possible contributions from massive stars.

Contribution

It provides a comprehensive multiwavelength characterization of Ca-rich transient host galaxies and estimates progenitor probabilities, advancing understanding of their origins.

Findings

Ca-rich transients are likely from white dwarf stars or a mixed population.

Host galaxy properties suggest a connection to older stellar populations.

Progenitor origin is not exclusively from core-collapse explosions.

Abstract

Calcium-rich (Ca-rich) transients are a new class of supernovae (SNe) that are known for their comparatively rapid evolution, modest peak luminosities, and strong nebular calcium emission lines. Currently, the progenitor systems of Ca-rich transients remain unknown. Although they exhibit spectroscopic properties not unlike core-collapse Type Ib/c SNe, nearly half are found in the outskirts of their host galaxies that are predominantly elliptical, suggesting a closer connection to the older stellar populations of SNe Ia. In this paper, we present a compilation of publicly available multiwavelength observations of all known and/or suspected host galaxies of Ca-rich transients ranging from FUV to IR, and use these data to characterize their stellar populations with prospector. We estimate several galaxy parameters including integrated star formation rate, stellar mass, metallicity, and age. For nine host galaxies, the observations are sensitive enough to obtain nonparametric star formation histories, from which we recover SN rates and estimate probabilities that the Ca-rich transients in each of these host galaxies originated from a core-collapse vs. Type Ia-like explosion. Our work supports the notion that the population of Ca-rich transients do not come exclusively from core-collapse explosions, and must either be only from white dwarf stars or a mixed population of white dwarf stars with other channels, potentially including massive star explosions. Additional photometry and explosion site spectroscopy of larger samples of Ca-rich host galaxies will improve these estimates and better constrain the ratio of white dwarf vs. massive star progenitors of Ca-rich transients.