The Observed Phase Space of Mass-loss History from Massive Stars Based on Radio Observations of a Large Supernova Sample

Itai Sfaradi*, Assaf Horesh, Rob Fender, Lauren Rhodes, Joe Bright, David Williams-Baldwin, Dave A. Green

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

Abstract

In this work, we study the circumstellar material (CSM) around massive stars, and the mass-loss rates depositing this CSM, using a large sample of radio observations of 325 core-collapse supernovae (CCSNe; only ~22% of them being detected). This sample comprises both archival data and our new observations of 99 CCSNe conducted with the AMI-LA radio array in a systematic approach devised to constrain the mass loss at different stages of stellar evolution. In the supernova (SN)-CSM interaction model, observing the peak of the radio emission of an SN provides the CSM density at a given radius (and therefore the mass-loss rate that deposited this CSM). On the other hand, limits on the radio emission, and/or on the peak of the radio emission provide a region in the CSM phase space that can be ruled out. Our analysis shows a discrepancy between the values of mass-loss rates derived from radio-detected and radio-nondetected SNe. Furthermore, we rule out mass-loss rates in the range of 2 × 10−6-10−4 M yr−1 for different epochs during the last 1000 yr before the explosion (assuming wind velocity of 10 km s−1) for the progenitors of ~80% of the Type II supernovae (SNe II) in our sample. In addition, we rule out the ranges of mass-loss rates suggested for red supergiants for ~50% of the progenitors of SNe II in our sample. We emphasize here that these results take a step forward in constraining mass loss in winds from a statistical point of view.

Original languageEnglish
Article number189
JournalAstrophysical Journal
Volume979
Issue number2
DOIs
StatePublished - 1 Feb 2025

Bibliographical note

Publisher Copyright:
© 2025. The Author(s). Published by the American Astronomical Society.

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