Observational upper limits on the gravitational wave production of core collapse supernovae

Abstract

The upper limit on the energy density of a stochastic gravitational wave (GW) background obtained from the two-year science run (S5) of the Laser Interferometer Gravitational-wave Observatory (LIGO) is used to constrain the average GW production of core collapse supernovae (ccSNe). We assume that the ccSNe rate tracks the star formation history of the universe and show that the stochastic background energy density depends only weakly on the assumed average source spectrum. Using the ccSNe rate for $z\le 10$, we scale the generic source spectrum to obtain an observation-based upper limit on the average GW emission. We show that the mean energy emitted in GWs can be constrained within $<(0.49-1.98)1mm{M}_{\odot }{c}^2$ depending on the average source spectrum. While these results are higher than the total available gravitational energy in a core collapse event, second and third generation GW detectors will enable tighter constraints to be set on the GW emission from such systems.

accepted for publication in MNRAS letters

References in corpus (8)

• The gravitational wave burst signal from core collapse of rotating stars
• The Total Merger Rate of Compact Object Binaries In The Local Universe
• Challenging the paradigm of singularity excision in gravitational collapse
• A New Mechanism for Gravitational Wave Emission in Core-Collapse Supernovae
• Search for Gravitational Wave Bursts from Soft Gamma Repeaters
• On the gravitational radiation from the collapse of neutron stars to rotating black holes
• Searching for prompt signatures of nearby core-collapse supernovae by a joint analysis of neutrino and gravitational-wave data
• Joint searches between gravitational-wave interferometers and high-energy neutrino telescopes: science reach and analysis strategies