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1811068885033549824
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MIT
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© 2019. The American Astronomical Society. All rights reserved.. One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity.
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2024-09-23T08:02:29Z
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Article
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mit-1721.1/132415
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Massachusetts Institute of Technology
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English
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2024-09-23T08:02:29Z
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2021
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American Astronomical Society
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dspace
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| spelling |
mit-1721.1/1324152022-09-30T01:53:33Z Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817 © 2019. The American Astronomical Society. All rights reserved.. One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity. 2021-09-20T18:22:17Z 2021-09-20T18:22:17Z 2019 2020-10-21T16:40:58Z Article http://purl.org/eprint/type/JournalArticle https://hdl.handle.net/1721.1/132415 en 10.3847/1538-4357/AB0F3D Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf American Astronomical Society The American Astronomical Society
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| spellingShingle |
Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817
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| title |
Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817
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| title_full |
Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817
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| title_fullStr |
Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817
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| title_full_unstemmed |
Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817
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| title_short |
Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817
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| title_sort |
search for gravitational waves from a long lived remnant of the binary neutron star merger gw170817
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| url |
https://hdl.handle.net/1721.1/132415
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