Journal
ASTROPHYSICAL JOURNAL
Volume 875, Issue 2, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/1538-4357/ab0f3d
Keywords
gravitational waves; methods: data analysis; stars: neutron
Categories
Funding
- Australian Research Council
- EGO consortium
- Council of Scientific and Industrial Research of India
- Department of Science and Technology, India
- Science AMP
- Engineering Research Board (SERB), India
- Ministry of Human Resource Development, India
- Spanish Agencia Estatal de Investigacion
- Vicepresidencia i Conselleria d'Innovacio Recerca i Turisme
- Conselleria d'Educacio i Universitat del Govern de les Illes Balears
- Conselleria d'Educacio Investigacio Cultura i Esport de la Generalitat Valenciana
- National Science Centre of Poland
- Swiss National Science Foundation (SNSF)
- Russian Foundation for Basic Research
- Russian Science Foundation
- European Commission
- European Regional Development Funds (ERDF)
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- Hungarian Scientific Research Fund (OTKA)
- Lyon Institute of Origins (LIO)
- Paris Ile-de-France Region
- National Research, Development and Innovation Office Hungary (NKFI)
- National Research Foundation of Korea
- Industry Canada
- Province of Ontario through the Ministry of Economic Development and Innovation
- Natural Science and Engineering Research Council Canada
- Canadian Institute for Advanced Research
- Brazilian Ministry of Science, Technology, Innovations, and Communications
- International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR)
- Research Grants Council of Hong Kong
- National Natural Science Foundation of China (NSFC)
- Leverhulme Trust
- Research Corporation
- Ministry of Science and Technology (MOST), Taiwan
- Kavli Foundation
- STFC [ST/H002006/1, ST/L000954/1, ST/J00166X/1, ST/N000072/1, ST/K005014/1, Gravitational Waves, PPA/G/S/2002/00652, ST/N00003X/1, ST/M005844/1, 1802894, 1945971, ST/V001396/1, ST/K005014/2, ST/N005406/1, ST/R00045X/1, ST/N005406/2, 1802888, ST/N000633/1, ST/I006269/1, 1653089, 1654298, ST/N005430/1, ST/T000147/1, ST/K000845/1, ST/N005422/1, 2142081, ST/S000305/1] Funding Source: UKRI
Ask authors/readers for more resources
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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