Characterization of low-significance gravitational-wave compact binary sources
Advanced LIGO and Virgo have so far detected gravitational waves from 10 binary black hole mergers (BBH) and 1 binary neutron star merger (BNS). In the future, we expect the detection of many more marginal sources, since compact binary coalescences detectable by advanced ground-based instruments are...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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American Physical Society
2019
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| Online Access: | http://hdl.handle.net/1721.1/120005 https://orcid.org/0000-0003-2700-0767 |
| _version_ | 1811001866649075712 |
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| author | Huang, Yiwen Middleton, Hannah Ng, Ken K. Y. Vitale, Salvatore Veitch, John |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Huang, Yiwen Middleton, Hannah Ng, Ken K. Y. Vitale, Salvatore Veitch, John |
| author_sort | Huang, Yiwen |
| collection | MIT |
| description | Advanced LIGO and Virgo have so far detected gravitational waves from 10 binary black hole mergers (BBH) and 1 binary neutron star merger (BNS). In the future, we expect the detection of many more marginal sources, since compact binary coalescences detectable by advanced ground-based instruments are roughly distributed uniformly in comoving volume. In this paper we simulate weak signals from compact binary coalescences of various morphologies and optimal network signal-to-noise ratios (henceforth SNRs), and analyze if and to which extent their parameters can be measured by advanced LIGO and Virgo in their third observing run. We show that subthreshold binary neutron stars, with SNRs below 12 (10) yield uncertainties in their sky position larger than 400 (700) deg^{2} (90% credible interval). The luminosity distance, which could be used to measure the Hubble constant with standard sirens, has relative uncertainties larger than 40% for BNSs and neutron star black hole mergers. For sources with SNRs below 8, it is not uncommon that the extrinsic parameters, sky position and distance, cannot be measured. Next, we look at the intrinsic parameters, masses and spins. We show that the detector-frame chirp mass can sometimes be measured with uncertainties below 1% even for sources at SNRs of 6, although multimodality is not uncommon and can significantly broaden the posteriors. The effective inspiral spin is best measured for neutron star black hole mergers, for which the uncertainties can be as low as ∼0.08 (∼0.2) at SNR 12 (8). The uncertainty is higher for systems with comparable component masses or lack of spin precession. |
| first_indexed | 2024-09-23T15:39:27Z |
| format | Article |
| id | mit-1721.1/120005 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T15:39:27Z |
| publishDate | 2019 |
| publisher | American Physical Society |
| record_format | dspace |
| spelling | mit-1721.1/1200052022-10-02T03:11:33Z Characterization of low-significance gravitational-wave compact binary sources Huang, Yiwen Middleton, Hannah Ng, Ken K. Y. Vitale, Salvatore Veitch, John Massachusetts Institute of Technology. Department of Physics LIGO (Observatory : Massachusetts Institute of Technology) MIT Kavli Institute for Astrophysics and Space Research Huang, Yiwen Ng, Ken K. Y. Vitale, Salvatore Advanced LIGO and Virgo have so far detected gravitational waves from 10 binary black hole mergers (BBH) and 1 binary neutron star merger (BNS). In the future, we expect the detection of many more marginal sources, since compact binary coalescences detectable by advanced ground-based instruments are roughly distributed uniformly in comoving volume. In this paper we simulate weak signals from compact binary coalescences of various morphologies and optimal network signal-to-noise ratios (henceforth SNRs), and analyze if and to which extent their parameters can be measured by advanced LIGO and Virgo in their third observing run. We show that subthreshold binary neutron stars, with SNRs below 12 (10) yield uncertainties in their sky position larger than 400 (700) deg^{2} (90% credible interval). The luminosity distance, which could be used to measure the Hubble constant with standard sirens, has relative uncertainties larger than 40% for BNSs and neutron star black hole mergers. For sources with SNRs below 8, it is not uncommon that the extrinsic parameters, sky position and distance, cannot be measured. Next, we look at the intrinsic parameters, masses and spins. We show that the detector-frame chirp mass can sometimes be measured with uncertainties below 1% even for sources at SNRs of 6, although multimodality is not uncommon and can significantly broaden the posteriors. The effective inspiral spin is best measured for neutron star black hole mergers, for which the uncertainties can be as low as ∼0.08 (∼0.2) at SNR 12 (8). The uncertainty is higher for systems with comparable component masses or lack of spin precession. Solomon Buchsbaum AT&T Research Fund National Science Foundation (U.S.) Laser Interferometer Gravitational Wave Observatory 2019-01-11T19:34:52Z 2019-01-11T19:34:52Z 2018-12 2018-09 2018-12-27T18:00:19Z Article http://purl.org/eprint/type/JournalArticle 2470-0010 2470-0029 http://hdl.handle.net/1721.1/120005 Huang, Yiwen, et al. “Characterization of Low-Significance Gravitational-Wave Compact Binary Sources.” Physical Review D, vol. 98, no. 12, Dec. 2018. © 2018 American Physical Society https://orcid.org/0000-0003-2700-0767 en http://dx.doi.org/10.1103/PhysRevD.98.123021 Physical Review D 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. American Physical Society application/pdf American Physical Society American Physical Society |
| spellingShingle | Huang, Yiwen Middleton, Hannah Ng, Ken K. Y. Vitale, Salvatore Veitch, John Characterization of low-significance gravitational-wave compact binary sources |
| title | Characterization of low-significance gravitational-wave compact binary sources |
| title_full | Characterization of low-significance gravitational-wave compact binary sources |
| title_fullStr | Characterization of low-significance gravitational-wave compact binary sources |
| title_full_unstemmed | Characterization of low-significance gravitational-wave compact binary sources |
| title_short | Characterization of low-significance gravitational-wave compact binary sources |
| title_sort | characterization of low significance gravitational wave compact binary sources |
| url | http://hdl.handle.net/1721.1/120005 https://orcid.org/0000-0003-2700-0767 |
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