GW190521: A Binary Black Hole Merger with a Total Mass of 150 Mꙩ
On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 i...
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| Veröffentlicht in: | Physical review letters 2020-09, Vol.125 (10) |
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| creator | Acernese, F. Adams, C. Ansoldi, S. Barish, B. C. Barone, F. Barr, B. Belahcene, I. Bhandari, A. V. Carbognani, F. Cavalier, F. Cella, G. Chaibi, O. Chan, C. Cho, M. Davier, M. Del´eglise, S. Lillo, N. De Doravari, S. Dwyer, S. E. Edo, T. B. Fazio, M. Fittipaldi, R. Gaonkar, S. G. Gaudio, S. Ghosh, Abhirup Gibson, D. R. Gossan, S. E. Grant, A. Griggs, H. L. Guo, Y. Hanks, J. Healy, J. Hui, V. Huxford, R. Inchauspe, H. Isac, J.-M. Johns, G. R. Jones, J. D. Kaufer, S. Key, J. S. Khetan, N. Khursheed, M. King, P. J. Laghi, D. Lanza, R. K. Lecoeuche, Y. K. Linker, S. D. Littenberg, T. B. Loriette, V. Lück, H. Macfoy, S. Mantovani, M. Márka, S. Martin, I.W. Mastrogiovanni, S. Matas, A. Merzougui, M. Meylahn, F. Miao, H. Milano, L. Mo, G. Nissanke, S. Nitz, A. Oganesyan, G. Osthelder, C. Ottaway, D. J. Pai, S. A. Paoletti, F. Pascucci, D. Pasqualetti, A. Penn, S. Perego, A. Perigois, C. Petermann, J. Pinard, L. Pirello, M. Prajapati, A. K. Principe, M. Razzano, M. Read, J. Sadecki, T. Saleem, M. Sawant, D. Schmidt, J. Scheuer 14 P. Shawhan, P. Siellez, K. Srivastava, V. Steinlechner, S. Suresh, J. Tait, S. C. Tao, D. Tapia, A. Tripathee, A. Trovato, A. Vahlbruch, H. Vitale, S. Vocca, H. S.Walsh, S.Walsh R.Weiss, R.Weiss Zendri, J.-P. |
| description | On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85 (+21,−14) Mꙩ and 66 (+17,−18) Mꙩ (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65 M⊙. We calculate the mass of the remnant to be 142 (+28,−16) Mꙩ, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3 (+2.4,−2.6) Gpc, corresponding to a redshift of 0.82 (+0.28,−0.34) . The inferred rate of mergers similar to GW190521 is 0.13 (+0.30,−0.11) Gpc^(−3) per yr. |
| doi_str_mv | 10.1103/PhysRevLett.125.101102 |
| format | Article |
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C. ; Barone, F. ; Barr, B. ; Belahcene, I. ; Bhandari, A. V. ; Carbognani, F. ; Cavalier, F. ; Cella, G. ; Chaibi, O. ; Chan, C. ; Cho, M. ; Davier, M. ; Del´eglise, S. ; Lillo, N. De ; Doravari, S. ; Dwyer, S. E. ; Edo, T. B. ; Fazio, M. ; Fittipaldi, R. ; Gaonkar, S. G. ; Gaudio, S. ; Ghosh, Abhirup ; Gibson, D. R. ; Gossan, S. E. ; Grant, A. ; Griggs, H. L. ; Guo, Y. ; Hanks, J. ; Healy, J. ; Hui, V. ; Huxford, R. ; Inchauspe, H. ; Isac, J.-M. ; Johns, G. R. ; Jones, J. D. ; Kaufer, S. ; Key, J. S. ; Khetan, N. ; Khursheed, M. ; King, P. J. ; Laghi, D. ; Lanza, R. K. ; Lecoeuche, Y. K. ; Linker, S. D. ; Littenberg, T. B. ; Loriette, V. ; Lück, H. ; Macfoy, S. ; Mantovani, M. ; Márka, S. ; Martin, I.W. ; Mastrogiovanni, S. ; Matas, A. ; Merzougui, M. ; Meylahn, F. ; Miao, H. ; Milano, L. ; Mo, G. ; Nissanke, S. ; Nitz, A. ; Oganesyan, G. ; Osthelder, C. ; Ottaway, D. J. ; Pai, S. 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L. ; Guo, Y. ; Hanks, J. ; Healy, J. ; Hui, V. ; Huxford, R. ; Inchauspe, H. ; Isac, J.-M. ; Johns, G. R. ; Jones, J. D. ; Kaufer, S. ; Key, J. S. ; Khetan, N. ; Khursheed, M. ; King, P. J. ; Laghi, D. ; Lanza, R. K. ; Lecoeuche, Y. K. ; Linker, S. D. ; Littenberg, T. B. ; Loriette, V. ; Lück, H. ; Macfoy, S. ; Mantovani, M. ; Márka, S. ; Martin, I.W. ; Mastrogiovanni, S. ; Matas, A. ; Merzougui, M. ; Meylahn, F. ; Miao, H. ; Milano, L. ; Mo, G. ; Nissanke, S. ; Nitz, A. ; Oganesyan, G. ; Osthelder, C. ; Ottaway, D. J. ; Pai, S. A. ; Paoletti, F. ; Pascucci, D. ; Pasqualetti, A. ; Penn, S. ; Perego, A. ; Perigois, C. ; Petermann, J. ; Pinard, L. ; Pirello, M. ; Prajapati, A. K. ; Principe, M. ; Razzano, M. ; Read, J. ; Sadecki, T. ; Saleem, M. ; Sawant, D. ; Schmidt, J. Scheuer 14 P. ; Shawhan, P. ; Siellez, K. ; Srivastava, V. ; Steinlechner, S. ; Suresh, J. ; Tait, S. C. ; Tao, D. ; Tapia, A. ; Tripathee, A. ; Trovato, A. ; Vahlbruch, H. ; Vitale, S. ; Vocca, H. ; S.Walsh, S.Walsh ; R.Weiss, R.Weiss ; Zendri, J.-P.</creatorcontrib><description>On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85 (+21,−14) Mꙩ and 66 (+17,−18) Mꙩ (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65 M⊙. We calculate the mass of the remnant to be 142 (+28,−16) Mꙩ, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3 (+2.4,−2.6) Gpc, corresponding to a redshift of 0.82 (+0.28,−0.34) . 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Scheuer 14 P.</creatorcontrib><creatorcontrib>Shawhan, P.</creatorcontrib><creatorcontrib>Siellez, K.</creatorcontrib><creatorcontrib>Srivastava, V.</creatorcontrib><creatorcontrib>Steinlechner, S.</creatorcontrib><creatorcontrib>Suresh, J.</creatorcontrib><creatorcontrib>Tait, S. C.</creatorcontrib><creatorcontrib>Tao, D.</creatorcontrib><creatorcontrib>Tapia, A.</creatorcontrib><creatorcontrib>Tripathee, A.</creatorcontrib><creatorcontrib>Trovato, A.</creatorcontrib><creatorcontrib>Vahlbruch, H.</creatorcontrib><creatorcontrib>Vitale, S.</creatorcontrib><creatorcontrib>Vocca, H.</creatorcontrib><creatorcontrib>S.Walsh, S.Walsh</creatorcontrib><creatorcontrib>R.Weiss, R.Weiss</creatorcontrib><creatorcontrib>Zendri, J.-P.</creatorcontrib><title>GW190521: A Binary Black Hole Merger with a Total Mass of 150 Mꙩ</title><title>Physical review letters</title><description>On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85 (+21,−14) Mꙩ and 66 (+17,−18) Mꙩ (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65 M⊙. We calculate the mass of the remnant to be 142 (+28,−16) Mꙩ, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3 (+2.4,−2.6) Gpc, corresponding to a redshift of 0.82 (+0.28,−0.34) . The inferred rate of mergers similar to GW190521 is 0.13 (+0.30,−0.11) Gpc^(−3) per yr.</description><subject>Astrophysics</subject><subject>Physics Of Elementary Particles And Fields</subject><issn>0031-9007</issn><issn>1079-7114</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><sourceid>CYI</sourceid><recordid>eNqFjU0KgkAYQIcoyH5uEPFdQPu-8b9dRuUiIUJoKUOMaYmCMxQepSN0tU5Ri_atHry3eIzNCS0itBeHolNHed9LrS3irkX41bzHDEI_NH0ip88MRJvMENEfspFSV0Qk7gUGi3YnCtHltIQVRGUt2g6iSpxvEDeVhES2F9nCo9QFCEgbLSpIhFLQ5EAuQvJ-viZskItKyemPYzbbbtJ1bNZCiazWrco4cvoeHS9A-0_-AP7uOSI</recordid><startdate>20200902</startdate><enddate>20200902</enddate><creator>Acernese, F.</creator><creator>Adams, C.</creator><creator>Ansoldi, S.</creator><creator>Barish, B. C.</creator><creator>Barone, F.</creator><creator>Barr, B.</creator><creator>Belahcene, I.</creator><creator>Bhandari, A. 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L. ; Guo, Y. ; Hanks, J. ; Healy, J. ; Hui, V. ; Huxford, R. ; Inchauspe, H. ; Isac, J.-M. ; Johns, G. R. ; Jones, J. D. ; Kaufer, S. ; Key, J. S. ; Khetan, N. ; Khursheed, M. ; King, P. J. ; Laghi, D. ; Lanza, R. K. ; Lecoeuche, Y. K. ; Linker, S. D. ; Littenberg, T. B. ; Loriette, V. ; Lück, H. ; Macfoy, S. ; Mantovani, M. ; Márka, S. ; Martin, I.W. ; Mastrogiovanni, S. ; Matas, A. ; Merzougui, M. ; Meylahn, F. ; Miao, H. ; Milano, L. ; Mo, G. ; Nissanke, S. ; Nitz, A. ; Oganesyan, G. ; Osthelder, C. ; Ottaway, D. J. ; Pai, S. A. ; Paoletti, F. ; Pascucci, D. ; Pasqualetti, A. ; Penn, S. ; Perego, A. ; Perigois, C. ; Petermann, J. ; Pinard, L. ; Pirello, M. ; Prajapati, A. K. ; Principe, M. ; Razzano, M. ; Read, J. ; Sadecki, T. ; Saleem, M. ; Sawant, D. ; Schmidt, J. Scheuer 14 P. ; Shawhan, P. ; Siellez, K. ; Srivastava, V. ; Steinlechner, S. ; Suresh, J. ; Tait, S. C. ; Tao, D. ; Tapia, A. ; Tripathee, A. ; Trovato, A. ; Vahlbruch, H. ; Vitale, S. ; Vocca, H. ; S.Walsh, S.Walsh ; R.Weiss, R.Weiss ; Zendri, J.-P.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-nasa_ntrs_202100146803</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Astrophysics</topic><topic>Physics Of Elementary Particles And Fields</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Acernese, F.</creatorcontrib><creatorcontrib>Adams, C.</creatorcontrib><creatorcontrib>Ansoldi, S.</creatorcontrib><creatorcontrib>Barish, B. C.</creatorcontrib><creatorcontrib>Barone, F.</creatorcontrib><creatorcontrib>Barr, B.</creatorcontrib><creatorcontrib>Belahcene, I.</creatorcontrib><creatorcontrib>Bhandari, A. V.</creatorcontrib><creatorcontrib>Carbognani, F.</creatorcontrib><creatorcontrib>Cavalier, F.</creatorcontrib><creatorcontrib>Cella, G.</creatorcontrib><creatorcontrib>Chaibi, O.</creatorcontrib><creatorcontrib>Chan, C.</creatorcontrib><creatorcontrib>Cho, M.</creatorcontrib><creatorcontrib>Davier, M.</creatorcontrib><creatorcontrib>Del´eglise, S.</creatorcontrib><creatorcontrib>Lillo, N. De</creatorcontrib><creatorcontrib>Doravari, S.</creatorcontrib><creatorcontrib>Dwyer, S. E.</creatorcontrib><creatorcontrib>Edo, T. B.</creatorcontrib><creatorcontrib>Fazio, M.</creatorcontrib><creatorcontrib>Fittipaldi, R.</creatorcontrib><creatorcontrib>Gaonkar, S. G.</creatorcontrib><creatorcontrib>Gaudio, S.</creatorcontrib><creatorcontrib>Ghosh, Abhirup</creatorcontrib><creatorcontrib>Gibson, D. R.</creatorcontrib><creatorcontrib>Gossan, S. E.</creatorcontrib><creatorcontrib>Grant, A.</creatorcontrib><creatorcontrib>Griggs, H. 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B.</creatorcontrib><creatorcontrib>Loriette, V.</creatorcontrib><creatorcontrib>Lück, H.</creatorcontrib><creatorcontrib>Macfoy, S.</creatorcontrib><creatorcontrib>Mantovani, M.</creatorcontrib><creatorcontrib>Márka, S.</creatorcontrib><creatorcontrib>Martin, I.W.</creatorcontrib><creatorcontrib>Mastrogiovanni, S.</creatorcontrib><creatorcontrib>Matas, A.</creatorcontrib><creatorcontrib>Merzougui, M.</creatorcontrib><creatorcontrib>Meylahn, F.</creatorcontrib><creatorcontrib>Miao, H.</creatorcontrib><creatorcontrib>Milano, L.</creatorcontrib><creatorcontrib>Mo, G.</creatorcontrib><creatorcontrib>Nissanke, S.</creatorcontrib><creatorcontrib>Nitz, A.</creatorcontrib><creatorcontrib>Oganesyan, G.</creatorcontrib><creatorcontrib>Osthelder, C.</creatorcontrib><creatorcontrib>Ottaway, D. J.</creatorcontrib><creatorcontrib>Pai, S. A.</creatorcontrib><creatorcontrib>Paoletti, F.</creatorcontrib><creatorcontrib>Pascucci, D.</creatorcontrib><creatorcontrib>Pasqualetti, A.</creatorcontrib><creatorcontrib>Penn, S.</creatorcontrib><creatorcontrib>Perego, A.</creatorcontrib><creatorcontrib>Perigois, C.</creatorcontrib><creatorcontrib>Petermann, J.</creatorcontrib><creatorcontrib>Pinard, L.</creatorcontrib><creatorcontrib>Pirello, M.</creatorcontrib><creatorcontrib>Prajapati, A. K.</creatorcontrib><creatorcontrib>Principe, M.</creatorcontrib><creatorcontrib>Razzano, M.</creatorcontrib><creatorcontrib>Read, J.</creatorcontrib><creatorcontrib>Sadecki, T.</creatorcontrib><creatorcontrib>Saleem, M.</creatorcontrib><creatorcontrib>Sawant, D.</creatorcontrib><creatorcontrib>Schmidt, J. Scheuer 14 P.</creatorcontrib><creatorcontrib>Shawhan, P.</creatorcontrib><creatorcontrib>Siellez, K.</creatorcontrib><creatorcontrib>Srivastava, V.</creatorcontrib><creatorcontrib>Steinlechner, S.</creatorcontrib><creatorcontrib>Suresh, J.</creatorcontrib><creatorcontrib>Tait, S. C.</creatorcontrib><creatorcontrib>Tao, D.</creatorcontrib><creatorcontrib>Tapia, A.</creatorcontrib><creatorcontrib>Tripathee, A.</creatorcontrib><creatorcontrib>Trovato, A.</creatorcontrib><creatorcontrib>Vahlbruch, H.</creatorcontrib><creatorcontrib>Vitale, S.</creatorcontrib><creatorcontrib>Vocca, H.</creatorcontrib><creatorcontrib>S.Walsh, S.Walsh</creatorcontrib><creatorcontrib>R.Weiss, R.Weiss</creatorcontrib><creatorcontrib>Zendri, J.-P.</creatorcontrib><collection>NASA Scientific and Technical Information</collection><collection>NASA Technical Reports Server</collection><jtitle>Physical review letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Acernese, F.</au><au>Adams, C.</au><au>Ansoldi, S.</au><au>Barish, B. C.</au><au>Barone, F.</au><au>Barr, B.</au><au>Belahcene, I.</au><au>Bhandari, A. V.</au><au>Carbognani, F.</au><au>Cavalier, F.</au><au>Cella, G.</au><au>Chaibi, O.</au><au>Chan, C.</au><au>Cho, M.</au><au>Davier, M.</au><au>Del´eglise, S.</au><au>Lillo, N. De</au><au>Doravari, S.</au><au>Dwyer, S. E.</au><au>Edo, T. B.</au><au>Fazio, M.</au><au>Fittipaldi, R.</au><au>Gaonkar, S. G.</au><au>Gaudio, S.</au><au>Ghosh, Abhirup</au><au>Gibson, D. R.</au><au>Gossan, S. E.</au><au>Grant, A.</au><au>Griggs, H. L.</au><au>Guo, Y.</au><au>Hanks, J.</au><au>Healy, J.</au><au>Hui, V.</au><au>Huxford, R.</au><au>Inchauspe, H.</au><au>Isac, J.-M.</au><au>Johns, G. R.</au><au>Jones, J. D.</au><au>Kaufer, S.</au><au>Key, J. S.</au><au>Khetan, N.</au><au>Khursheed, M.</au><au>King, P. J.</au><au>Laghi, D.</au><au>Lanza, R. K.</au><au>Lecoeuche, Y. K.</au><au>Linker, S. D.</au><au>Littenberg, T. B.</au><au>Loriette, V.</au><au>Lück, H.</au><au>Macfoy, S.</au><au>Mantovani, M.</au><au>Márka, S.</au><au>Martin, I.W.</au><au>Mastrogiovanni, S.</au><au>Matas, A.</au><au>Merzougui, M.</au><au>Meylahn, F.</au><au>Miao, H.</au><au>Milano, L.</au><au>Mo, G.</au><au>Nissanke, S.</au><au>Nitz, A.</au><au>Oganesyan, G.</au><au>Osthelder, C.</au><au>Ottaway, D. J.</au><au>Pai, S. A.</au><au>Paoletti, F.</au><au>Pascucci, D.</au><au>Pasqualetti, A.</au><au>Penn, S.</au><au>Perego, A.</au><au>Perigois, C.</au><au>Petermann, J.</au><au>Pinard, L.</au><au>Pirello, M.</au><au>Prajapati, A. K.</au><au>Principe, M.</au><au>Razzano, M.</au><au>Read, J.</au><au>Sadecki, T.</au><au>Saleem, M.</au><au>Sawant, D.</au><au>Schmidt, J. Scheuer 14 P.</au><au>Shawhan, P.</au><au>Siellez, K.</au><au>Srivastava, V.</au><au>Steinlechner, S.</au><au>Suresh, J.</au><au>Tait, S. C.</au><au>Tao, D.</au><au>Tapia, A.</au><au>Tripathee, A.</au><au>Trovato, A.</au><au>Vahlbruch, H.</au><au>Vitale, S.</au><au>Vocca, H.</au><au>S.Walsh, S.Walsh</au><au>R.Weiss, R.Weiss</au><au>Zendri, J.-P.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>GW190521: A Binary Black Hole Merger with a Total Mass of 150 Mꙩ</atitle><jtitle>Physical review letters</jtitle><date>2020-09-02</date><risdate>2020</risdate><volume>125</volume><issue>10</issue><issn>0031-9007</issn><eissn>1079-7114</eissn><abstract>On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85 (+21,−14) Mꙩ and 66 (+17,−18) Mꙩ (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65 M⊙. We calculate the mass of the remnant to be 142 (+28,−16) Mꙩ, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3 (+2.4,−2.6) Gpc, corresponding to a redshift of 0.82 (+0.28,−0.34) . The inferred rate of mergers similar to GW190521 is 0.13 (+0.30,−0.11) Gpc^(−3) per yr.</abstract><cop>Goddard Space Flight Center</cop><pub>American Physical Society</pub><doi>10.1103/PhysRevLett.125.101102</doi></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0031-9007 |
| ispartof | Physical review letters, 2020-09, Vol.125 (10) |
| issn | 0031-9007 1079-7114 |
| language | eng |
| recordid | cdi_nasa_ntrs_20210014680 |
| source | American Physical Society Journals; NASA Technical Reports Server; EZB-FREE-00999 freely available EZB journals |
| subjects | Astrophysics Physics Of Elementary Particles And Fields |
| title | GW190521: A Binary Black Hole Merger with a Total Mass of 150 Mꙩ |
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