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Published February 15, 2016 | Published + Submitted
Journal Article Open

Observing gravitational waves from core-collapse supernovae in the advanced detector era


The next galactic core-collapse supernova (CCSN) has already exploded, and its electromagnetic (EM) waves, neutrinos, and gravitational waves (GWs) may arrive at any moment. We present an extensive study on the potential sensitivity of prospective detection scenarios for GWs from CCSNe within 5 Mpc, using realistic noise at the predicted sensitivity of the Advanced LIGO and Advanced Virgo detectors for 2015, 2017, and 2019. We quantify the detectability of GWs from CCSNe within the Milky Way and Large Magellanic Cloud, for which there will be an observed neutrino burst. We also consider extreme GW emission scenarios for more distant CCSNe with an associated EM signature. We find that a three-detector network at design sensitivity will be able to detect neutrino-driven CCSN explosions out to ∼5.5  kpc, while rapidly rotating core collapse will be detectable out to the Large Magellanic Cloud at 50 kpc. Of the phenomenological models for extreme GW emission scenarios considered in this study, such as long-lived bar-mode instabilities and disk fragmentation instabilities, all models considered will be detectable out to M31 at 0.77 Mpc, while the most extreme models will be detectable out to M82 at 3.52 Mpc and beyond.

Additional Information

© 2016 American Physical Society. Received 9 November 2015; published 5 February 2016. The authors thank Alan Weinstein, Peter Kalmus, Lucia Santamaria, Viktoriya Giryanskaya, Valeriu Predoi, Scott Coughlin, James Clark, Michał Wąs, Marek Szczepanczyk, Beverly Berger, and Jade Powell for many fruitful discussions that have benefitted this paper greatly. We thank the CCSN simulation community for making their gravitational waveform predictions available for this study. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation, and operates under cooperative agreement No. PHY-0757058. Advanced LIGO was built under Award No. PHY-0823459. C. D. O. is partially supported by National Science Foundation Grants No. PHY-1404569 and No. CAREER PHY-1151197 and by the Sherman Fairchild Foundation. This paper carries LIGO Document No. LIGO-P1400233.

Attached Files

Published - PhysRevD.93.042002.pdf

Submitted - 1511.02836v1.pdf


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