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Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817

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Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817. / LIGO Scientific Collaboration and Virgo Collaboration.

In: The Astrophysical Journal, Vol. 875, No. 2, 160, 25.04.2019.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

LIGO Scientific Collaboration and Virgo Collaboration 2019, 'Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817', The Astrophysical Journal, vol. 875, no. 2, 160. https://doi.org/10.3847/1538-4357/ab0f3d

APA

LIGO Scientific Collaboration and Virgo Collaboration (2019). Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817. The Astrophysical Journal, 875(2), [160]. https://doi.org/10.3847/1538-4357/ab0f3d

Vancouver

LIGO Scientific Collaboration and Virgo Collaboration. Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817. The Astrophysical Journal. 2019 Apr 25;875(2). 160. https://doi.org/10.3847/1538-4357/ab0f3d

Author

LIGO Scientific Collaboration and Virgo Collaboration. / Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817. In: The Astrophysical Journal. 2019 ; Vol. 875, No. 2.

Bibtex

@article{a4147838d25840a6a7f776e08b25a073,
title = "Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817",
abstract = "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.",
keywords = "gravitational waves, methods: data analysis, stars: neutron, General Relativity and Quantum Cosmology, Astrophysics - High Energy Astrophysical Phenomena",
author = "{LIGO Scientific Collaboration and Virgo Collaboration} and M. Pitkin",
year = "2019",
month = apr,
day = "25",
doi = "10.3847/1538-4357/ab0f3d",
language = "English",
volume = "875",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",
number = "2",

}

RIS

TY - JOUR

T1 - Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817

AU - LIGO Scientific Collaboration and Virgo Collaboration

AU - Pitkin, M.

PY - 2019/4/25

Y1 - 2019/4/25

N2 - 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.

AB - 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.

KW - gravitational waves

KW - methods: data analysis

KW - stars: neutron

KW - General Relativity and Quantum Cosmology

KW - Astrophysics - High Energy Astrophysical Phenomena

U2 - 10.3847/1538-4357/ab0f3d

DO - 10.3847/1538-4357/ab0f3d

M3 - Journal article

VL - 875

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 160

ER -