GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M
On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible i...
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| Veröffentlicht in: | Astrophysical journal. Letters 2020-03, Vol.892 (1), p.L3, Article 3 |
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| creator | Abbott, R. Abraham, S. Amato, A. Ballmer, S. W. Basti, A. Beniwal, D. Bhandare, R. Briggs, J. H. Buonanno, A. Cabero, M. Cao, J. Caudill, S. Chan, M. Cheong, C. K. Chincarini, A. Chung, S. Ciolfi, R. Corban, P. Corsi, A. Cortese, S. Costa, C. A. Cowart, M. J. Croquette, M. D'Antonio, S. Datrier, L. E. H. Dent, T. Dhurandhar, S. Palma, I. Di Downes, T. P. Estevez, D. Fan, X. Fiori, I. Fittipaldi, R. Fiumara, V. Freise, A. Fulda, P. Gabbard, H. A. Gammaitoni, L. Gayathri, V. George, R. González, G. Haegel, L. Hannam, M. D. Hannuksela, O. A. Harms, J. Hendry, M. Hild, S. Hoy, C. G. Idzkowski, B. Junker, J. Kim, W. Kozak, D. B. Laghi, D. Lane, B. B. Levin, Y. Losurdo, G. Lough, J. D. Lower, M. E. Martelli, F. Meadors, G. D. Mehmet, M. Mercer, R. A. Mereni, L. Michel, C. Mills, J. C. Milovich-Goff, M. C. Moreno, G. Page, M. A. Pang, P. T. H. Paoletti, F. Phukon, K. S. Pirello, M. Porter, E. K. Prajapati, A. K. Prestegard, T. Punturo, M. Pürrer, M. Razzano, M. Richardson, C. J. Rosofsky, S. G. Rüdiger, A. Samajdar, A. Scheel, M. Schreiber, E. Schutz, B. F. Shukla, K. ShyamSundar, S. Somala, S. Sunil, S. Tapia, A. Toland, K. Trovato, A. Tsang, K. W. Vass, S. Venugopalan, G. Verkindt, D. Wang, S. Ward, R. L. Williamson, A. R. Wittel, H. |
| description | On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from to ( - if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250-2810 . |
| doi_str_mv | 10.3847/2041-8213/ab75f5 |
| format | Article |
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A. ; Gammaitoni, L. ; Gayathri, V. ; George, R. ; González, G. ; Haegel, L. ; Hannam, M. D. ; Hannuksela, O. A. ; Harms, J. ; Hendry, M. ; Hild, S. ; Hoy, C. G. ; Idzkowski, B. ; Junker, J. ; Kim, W. ; Kozak, D. B. ; Laghi, D. ; Lane, B. B. ; Levin, Y. ; Losurdo, G. ; Lough, J. D. ; Lower, M. E. ; Martelli, F. ; Meadors, G. D. ; Mehmet, M. ; Mercer, R. A. ; Mereni, L. ; Michel, C. ; Mills, J. C. ; Milovich-Goff, M. C. ; Moreno, G. ; Page, M. A. ; Pang, P. T. H. ; Paoletti, F. ; Phukon, K. S. ; Pirello, M. ; Porter, E. K. ; Prajapati, A. K. ; Prestegard, T. ; Punturo, M. ; Pürrer, M. ; Razzano, M. ; Richardson, C. J. ; Rosofsky, S. G. ; Rüdiger, A. ; Samajdar, A. ; Scheel, M. ; Schreiber, E. ; Schutz, B. F. ; Shukla, K. ; ShyamSundar, S. ; Somala, S. ; Sunil, S. ; Tapia, A. ; Toland, K. ; Trovato, A. ; Tsang, K. W. ; Vass, S. ; Venugopalan, G. ; Verkindt, D. ; Wang, S. ; Ward, R. L. ; Williamson, A. R. ; Wittel, H. ; Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><description>On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from to ( - if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250-2810 .</description><identifier>ISSN: 2041-8205</identifier><identifier>ISSN: 2041-8213</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/ab75f5</identifier><language>eng</language><publisher>BRISTOL: The American Astronomical Society</publisher><subject>Astronomy & Astrophysics ; ASTRONOMY AND ASTROPHYSICS ; Binary stars ; Black holes ; Coalescence ; Coalescing ; Gravitational waves ; Neutron stars ; Neutrons ; Parameter estimation ; Physical Sciences ; Science & Technology ; Signal to noise ratio</subject><ispartof>Astrophysical journal. Letters, 2020-03, Vol.892 (1), p.L3, Article 3</ispartof><rights>2020. The Author(s). 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C.</creatorcontrib><creatorcontrib>Moreno, G.</creatorcontrib><creatorcontrib>Page, M. A.</creatorcontrib><creatorcontrib>Pang, P. T. H.</creatorcontrib><creatorcontrib>Paoletti, F.</creatorcontrib><creatorcontrib>Phukon, K. S.</creatorcontrib><creatorcontrib>Pirello, M.</creatorcontrib><creatorcontrib>Porter, E. K.</creatorcontrib><creatorcontrib>Prajapati, A. K.</creatorcontrib><creatorcontrib>Prestegard, T.</creatorcontrib><creatorcontrib>Punturo, M.</creatorcontrib><creatorcontrib>Pürrer, M.</creatorcontrib><creatorcontrib>Razzano, M.</creatorcontrib><creatorcontrib>Richardson, C. J.</creatorcontrib><creatorcontrib>Rosofsky, S. G.</creatorcontrib><creatorcontrib>Rüdiger, A.</creatorcontrib><creatorcontrib>Samajdar, A.</creatorcontrib><creatorcontrib>Scheel, M.</creatorcontrib><creatorcontrib>Schreiber, E.</creatorcontrib><creatorcontrib>Schutz, B. F.</creatorcontrib><creatorcontrib>Shukla, K.</creatorcontrib><creatorcontrib>ShyamSundar, S.</creatorcontrib><creatorcontrib>Somala, S.</creatorcontrib><creatorcontrib>Sunil, S.</creatorcontrib><creatorcontrib>Tapia, A.</creatorcontrib><creatorcontrib>Toland, K.</creatorcontrib><creatorcontrib>Trovato, A.</creatorcontrib><creatorcontrib>Tsang, K. W.</creatorcontrib><creatorcontrib>Vass, S.</creatorcontrib><creatorcontrib>Venugopalan, G.</creatorcontrib><creatorcontrib>Verkindt, D.</creatorcontrib><creatorcontrib>Wang, S.</creatorcontrib><creatorcontrib>Ward, R. L.</creatorcontrib><creatorcontrib>Williamson, A. R.</creatorcontrib><creatorcontrib>Wittel, H.</creatorcontrib><creatorcontrib>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><title>GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>ASTROPHYS J LETT</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from to ( - if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic BNS population. 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R.</creator><creator>Wittel, H.</creator><general>The American Astronomical Society</general><general>IOP Publishing Ltd</general><general>IOP Publishing</general><general>Institute of Physics (IOP)</general><scope>O3W</scope><scope>TSCCA</scope><scope>AOWDO</scope><scope>BLEPL</scope><scope>DTL</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>OIOZB</scope><scope>OTOTI</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0003-4955-6280</orcidid><orcidid>https://orcid.org/0000-0003-4534-4619</orcidid><orcidid>https://orcid.org/0000-0002-6960-8538</orcidid><orcidid>https://orcid.org/0000-0002-8069-8490</orcidid><orcidid>https://orcid.org/0000-0003-1613-3142</orcidid><orcidid>https://orcid.org/0000-0002-5552-7681</orcidid><orcidid>https://orcid.org/0000-0001-5116-6789</orcidid><orcidid>https://orcid.org/0000-0001-9557-651X</orcidid><orcidid>https://orcid.org/0000-0002-0456-2452</orcidid><orcidid>https://orcid.org/0000-0003-3870-7215</orcidid><orcidid>https://orcid.org/0000-0002-1451-1368</orcidid><orcidid>https://orcid.org/0000-0002-8648-0767</orcidid><orcidid>https://orcid.org/0000-0003-0482-5942</orcidid><orcidid>https://orcid.org/0000-0002-4341-2860</orcidid><orcidid>https://orcid.org/0000-0003-2771-8816</orcidid><orcidid>https://orcid.org/0000-0002-4991-8213</orcidid><orcidid>https://orcid.org/0000-0003-3103-3473</orcidid><orcidid>https://orcid.org/0000-0001-8553-7904</orcidid><orcidid>https://orcid.org/0000-0001-7852-7484</orcidid><orcidid>https://orcid.org/0000-0003-3611-3042</orcidid><orcidid>https://orcid.org/0000-0003-3726-6016</orcidid><orcidid>https://orcid.org/0000-0001-8193-5825</orcidid><orcidid>https://orcid.org/0000-0001-8171-6833</orcidid><orcidid>https://orcid.org/0000-0002-5288-1351</orcidid></search><sort><creationdate>20200320</creationdate><title>GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M</title><author>Abbott, R. ; Abraham, S. ; Amato, A. ; Ballmer, S. W. ; Basti, A. ; Beniwal, D. ; Bhandare, R. ; Briggs, J. H. ; Buonanno, A. ; Cabero, M. ; Cao, J. ; Caudill, S. ; Chan, M. ; Cheong, C. K. ; Chincarini, A. ; Chung, S. ; Ciolfi, R. ; Corban, P. ; Corsi, A. ; Cortese, S. ; Costa, C. A. ; Cowart, M. J. ; Croquette, M. ; D'Antonio, S. ; Datrier, L. E. H. ; Dent, T. ; Dhurandhar, S. ; Palma, I. Di ; Downes, T. P. ; Estevez, D. ; Fan, X. ; Fiori, I. ; Fittipaldi, R. ; Fiumara, V. ; Freise, A. ; Fulda, P. ; Gabbard, H. A. ; Gammaitoni, L. ; Gayathri, V. ; George, R. ; González, G. ; Haegel, L. ; Hannam, M. D. ; Hannuksela, O. A. ; Harms, J. ; Hendry, M. ; Hild, S. ; Hoy, C. G. ; Idzkowski, B. ; Junker, J. ; Kim, W. ; Kozak, D. B. ; Laghi, D. ; Lane, B. B. ; Levin, Y. ; Losurdo, G. ; Lough, J. D. ; Lower, M. E. ; Martelli, F. ; Meadors, G. D. ; Mehmet, M. ; Mercer, R. A. ; Mereni, L. ; Michel, C. ; Mills, J. C. ; Milovich-Goff, M. C. ; Moreno, G. ; Page, M. A. ; Pang, P. T. H. ; Paoletti, F. ; Phukon, K. S. ; Pirello, M. ; Porter, E. K. ; Prajapati, A. K. ; Prestegard, T. ; Punturo, M. ; Pürrer, M. ; Razzano, M. ; Richardson, C. J. ; Rosofsky, S. G. ; Rüdiger, A. ; Samajdar, A. ; Scheel, M. ; Schreiber, E. ; Schutz, B. F. ; Shukla, K. ; ShyamSundar, S. ; Somala, S. ; Sunil, S. ; Tapia, A. ; Toland, K. ; Trovato, A. ; Tsang, K. W. ; Vass, S. ; Venugopalan, G. ; Verkindt, D. ; Wang, S. ; Ward, R. L. ; Williamson, A. R. ; Wittel, H.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c403t-ceccc0cfee64b07b4f161083a270c17e054e8f5afac61935d434a161176523de3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Astronomy & Astrophysics</topic><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>Binary stars</topic><topic>Black holes</topic><topic>Coalescence</topic><topic>Coalescing</topic><topic>Gravitational waves</topic><topic>Neutron stars</topic><topic>Neutrons</topic><topic>Parameter estimation</topic><topic>Physical Sciences</topic><topic>Science & Technology</topic><topic>Signal to noise ratio</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Abbott, R.</creatorcontrib><creatorcontrib>Abraham, S.</creatorcontrib><creatorcontrib>Amato, A.</creatorcontrib><creatorcontrib>Ballmer, S. 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F.</creatorcontrib><creatorcontrib>Shukla, K.</creatorcontrib><creatorcontrib>ShyamSundar, S.</creatorcontrib><creatorcontrib>Somala, S.</creatorcontrib><creatorcontrib>Sunil, S.</creatorcontrib><creatorcontrib>Tapia, A.</creatorcontrib><creatorcontrib>Toland, K.</creatorcontrib><creatorcontrib>Trovato, A.</creatorcontrib><creatorcontrib>Tsang, K. W.</creatorcontrib><creatorcontrib>Vass, S.</creatorcontrib><creatorcontrib>Venugopalan, G.</creatorcontrib><creatorcontrib>Verkindt, D.</creatorcontrib><creatorcontrib>Wang, S.</creatorcontrib><creatorcontrib>Ward, R. L.</creatorcontrib><creatorcontrib>Williamson, A. R.</creatorcontrib><creatorcontrib>Wittel, H.</creatorcontrib><creatorcontrib>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><collection>Institute of Physics Open Access Journal Titles</collection><collection>IOPscience (Open Access)</collection><collection>Web of Science - Science Citation Index Expanded - 2020</collection><collection>Web of Science Core Collection</collection><collection>Science Citation Index Expanded</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><collection>DOAJ Directory of Open Access Journals</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Abbott, R.</au><au>Abraham, S.</au><au>Amato, A.</au><au>Ballmer, S. W.</au><au>Basti, A.</au><au>Beniwal, D.</au><au>Bhandare, R.</au><au>Briggs, J. H.</au><au>Buonanno, A.</au><au>Cabero, M.</au><au>Cao, J.</au><au>Caudill, S.</au><au>Chan, M.</au><au>Cheong, C. K.</au><au>Chincarini, A.</au><au>Chung, S.</au><au>Ciolfi, R.</au><au>Corban, P.</au><au>Corsi, A.</au><au>Cortese, S.</au><au>Costa, C. A.</au><au>Cowart, M. J.</au><au>Croquette, M.</au><au>D'Antonio, S.</au><au>Datrier, L. E. H.</au><au>Dent, T.</au><au>Dhurandhar, S.</au><au>Palma, I. Di</au><au>Downes, T. P.</au><au>Estevez, D.</au><au>Fan, X.</au><au>Fiori, I.</au><au>Fittipaldi, R.</au><au>Fiumara, V.</au><au>Freise, A.</au><au>Fulda, P.</au><au>Gabbard, H. A.</au><au>Gammaitoni, L.</au><au>Gayathri, V.</au><au>George, R.</au><au>González, G.</au><au>Haegel, L.</au><au>Hannam, M. D.</au><au>Hannuksela, O. A.</au><au>Harms, J.</au><au>Hendry, M.</au><au>Hild, S.</au><au>Hoy, C. G.</au><au>Idzkowski, B.</au><au>Junker, J.</au><au>Kim, W.</au><au>Kozak, D. B.</au><au>Laghi, D.</au><au>Lane, B. B.</au><au>Levin, Y.</au><au>Losurdo, G.</au><au>Lough, J. D.</au><au>Lower, M. E.</au><au>Martelli, F.</au><au>Meadors, G. D.</au><au>Mehmet, M.</au><au>Mercer, R. A.</au><au>Mereni, L.</au><au>Michel, C.</au><au>Mills, J. C.</au><au>Milovich-Goff, M. C.</au><au>Moreno, G.</au><au>Page, M. A.</au><au>Pang, P. T. H.</au><au>Paoletti, F.</au><au>Phukon, K. S.</au><au>Pirello, M.</au><au>Porter, E. K.</au><au>Prajapati, A. K.</au><au>Prestegard, T.</au><au>Punturo, M.</au><au>Pürrer, M.</au><au>Razzano, M.</au><au>Richardson, C. J.</au><au>Rosofsky, S. G.</au><au>Rüdiger, A.</au><au>Samajdar, A.</au><au>Scheel, M.</au><au>Schreiber, E.</au><au>Schutz, B. F.</au><au>Shukla, K.</au><au>ShyamSundar, S.</au><au>Somala, S.</au><au>Sunil, S.</au><au>Tapia, A.</au><au>Toland, K.</au><au>Trovato, A.</au><au>Tsang, K. W.</au><au>Vass, S.</au><au>Venugopalan, G.</au><au>Verkindt, D.</au><au>Wang, S.</au><au>Ward, R. L.</au><au>Williamson, A. R.</au><au>Wittel, H.</au><aucorp>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><stitle>ASTROPHYS J LETT</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2020-03-20</date><risdate>2020</risdate><volume>892</volume><issue>1</issue><spage>L3</spage><pages>L3-</pages><artnum>3</artnum><issn>2041-8205</issn><issn>2041-8213</issn><eissn>2041-8213</eissn><abstract>On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from to ( - if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250-2810 .</abstract><cop>BRISTOL</cop><pub>The American Astronomical Society</pub><doi>10.3847/2041-8213/ab75f5</doi><tpages>24</tpages><orcidid>https://orcid.org/0000-0003-4955-6280</orcidid><orcidid>https://orcid.org/0000-0003-4534-4619</orcidid><orcidid>https://orcid.org/0000-0002-6960-8538</orcidid><orcidid>https://orcid.org/0000-0002-8069-8490</orcidid><orcidid>https://orcid.org/0000-0003-1613-3142</orcidid><orcidid>https://orcid.org/0000-0002-5552-7681</orcidid><orcidid>https://orcid.org/0000-0001-5116-6789</orcidid><orcidid>https://orcid.org/0000-0001-9557-651X</orcidid><orcidid>https://orcid.org/0000-0002-0456-2452</orcidid><orcidid>https://orcid.org/0000-0003-3870-7215</orcidid><orcidid>https://orcid.org/0000-0002-1451-1368</orcidid><orcidid>https://orcid.org/0000-0002-8648-0767</orcidid><orcidid>https://orcid.org/0000-0003-0482-5942</orcidid><orcidid>https://orcid.org/0000-0002-4341-2860</orcidid><orcidid>https://orcid.org/0000-0003-2771-8816</orcidid><orcidid>https://orcid.org/0000-0002-4991-8213</orcidid><orcidid>https://orcid.org/0000-0003-3103-3473</orcidid><orcidid>https://orcid.org/0000-0001-8553-7904</orcidid><orcidid>https://orcid.org/0000-0001-7852-7484</orcidid><orcidid>https://orcid.org/0000-0003-3611-3042</orcidid><orcidid>https://orcid.org/0000-0003-3726-6016</orcidid><orcidid>https://orcid.org/0000-0001-8193-5825</orcidid><orcidid>https://orcid.org/0000-0001-8171-6833</orcidid><orcidid>https://orcid.org/0000-0002-5288-1351</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 2041-8205 |
| ispartof | Astrophysical journal. Letters, 2020-03, Vol.892 (1), p.L3, Article 3 |
| issn | 2041-8205 2041-8213 2041-8213 |
| language | eng |
| recordid | cdi_crossref_primary_10_3847_2041_8213_ab75f5 |
| source | Institute of Physics Open Access Journal Titles; Institute of Physics IOPscience extra; Web of Science - Science Citation Index Expanded - 2020<img src="https://exlibris-pub.s3.amazonaws.com/fromwos-v2.jpg" />; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Astronomy & Astrophysics ASTRONOMY AND ASTROPHYSICS Binary stars Black holes Coalescence Coalescing Gravitational waves Neutron stars Neutrons Parameter estimation Physical Sciences Science & Technology Signal to noise ratio |
| title | GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M |
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