Constraining the gravitational-wave emission of core-collapse supernovae with ground-based detectors

TL;DR

This paper sets new upper limits on gravitational-wave emissions from core-collapse supernovae using advanced detectors, and evaluates future detection prospects with next-generation observatories.

Contribution

It provides the first constraints on CCSNe gravitational-wave energy emission from third-generation detector data and assesses future detection capabilities.

Findings

Upper limit of 0.01 solar masses c^2 on GW energy from CCSNe

Constraints improve previous limits by about two orders of magnitude

Future detectors may detect individual CCSNe before the GWB

Abstract

A gravitational-wave background (GWB) arising from the superposition of numerous unresolved gravitational-wave signals has yet to be detected. Potential contributing sources to such a background include compact binary coalescences (CBCs) and core-collapse supernovae (CCSNe). In this work, we place upper limits on the gravitational-wave energy emitted by CCSNe using cross-correlation measurements made with Advanced LIGO and Advanced Virgo detectors during their third observing run. Specifically, we obtain a $95\%$ credibility upper limit of $0.01~ {M_\odot c^2}$ while accounting for the contribution from CBC sources to a GWB. This result improves on previous constraint obtained from initial LIGO data by approximately two orders of magnitude. We also explore the detection prospects of third-generation ground-based detectors such as the Einstein Telescope and Cosmic Explorer for both individual CCSNe events and the GWB. Our results show that single events are likely to be detected prior to the GWB.