GW190521: A Binary Black Hole Merger with a Total Mass of 150M⊙

verfasst von: The LIGO Scientific Collaboration , Virgo Collaboration , R. Abbott, T. D. Abbott, S. Abraham, F. Acernese, K. Ackley, C. Adams, R. X. Adhikari, V. B. Adya, C. Affeldt, M. Agathos, K. Agatsuma, N. Aggarwal, O. D. Aguiar, A. Aich, L. Aiello, A. Ain, P. Ajith, S. Akcay, G. Allen, A. Allocca, P. A. Altin, A. Amato, S. Anand, A. Ananyeva, S. B. Anderson, W. G. Anderson, S. V. Angelova, S. Ansoldi, S. Antier, S. Appert, K. Arai, M. C. Araya, J. S. Areeda, M. Arène, N. Arnaud, S. M. Aronson, K. G. Arun, Y. Asali, S. Ascenzi, G. Ashton, S. M. Aston, S. L. Danilishin, K. Danzmann, M. Heurs, H. Lück, D. Steinmeyer, H. Vahlbruch, D. M. Wilken, B. Willke, H. Wittel, Sukanta Bose, D. D. Brown, Y. H. Chen, J. Gniesmer, M. M. Hanke, J. Hennig, M. T. Hübner, Sanjeev Kumar, R. N. Lang, C. H. Lee, H. M. Lee, H. W. Lee, J. Lee, K. Lee, X. Li, C. A. Rose, D. Rose, J. R. Sanders, Patricia Schmidt, L. Sun, D. S. Wu, R. Zhang, H. Zhang, X. J. Zhu, M. Zhou, Fabio Bergamin, A. Bisht, Nina Bode, P. Booker, M. Brinkmann, M. Cabero, N. Gohlke, J. Heinze, O. de Varona, S. Hochheim, J. Junker, W. Kastaun, Stefan Kaufer, S. Khan, P. Koch, N. Koper, S. M. Köhlenbeck, V. Kringel, G. Kuehn, S. Leavey, J. Lehmann, J. Liu, J. D. Lough, M. Mehmet, Fabian Meylahn, N. Mukund, M. Nery, F. Ohme, P. Oppermann, E. Schreiber, B. W. Schulte, Y. Setyawati, M. Steinke, M. Weinert, F. Wellmann, Peter Weßels, W. Winkler, J. Woehler, M. Standke, M. Phelps, Peter Aufmuth, Gerald Bergmann, R. Kirchhoff, Alexander H. Nitz, Li-Wei Wei
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 85-14+21 Mm and 66-18+17 Mm (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 Mm. We calculate the mass of the remnant to be 142-16+28 Mm, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3-2.6+2.4 Gpc, corresponding to a redshift of 0.82-0.34+0.28. The inferred rate of mergers similar to GW190521 is 0.13-0.11+0.30 Gpc-3 yr-1.
Organisationseinheit(en): QUEST Leibniz Forschungsschule
Institut für Gravitationsphysik
QuantumFrontiers
Externe Organisation(en): Washington State University Pullman
Inter-University Centre for Astronomy and Astrophysics India
University of Adelaide
Universität Hamburg
Monash University
Tata Institute of Fundamental Research (TIFR HYD)
LIGO Laboratory
Inje University
Stanford University
California Institute of Technology (Caltech)
California State University Fullerton
The California State University
Radboud Universität Nijmegen (RU)
University of Melbourne
University of Florida (UF)
Fudan University
National Taiwan Normal University
Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav)
Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut)
University of Glasgow
Laser Zentrum Hannover e.V. (LZH)
Typ: Artikel
Journal: Physical review letters
Band: 125
Anzahl der Seiten: 17
ISSN: 0031-9007
Publikationsdatum: 04.09.2020
Publikationsstatus: Veröffentlicht
ASJC Scopus Sachgebiete: Allgemeine Physik und Astronomie
Elektronische Version(en): https://arxiv.org/abs/2009.01075 (Zugang: Offen)
https://doi.org/10.1103/physrevlett.125.101102 (Zugang: Offen)
https://doi.org/10.15488/10650 (Zugang: Offen)
: Details im Forschungsportal „Research@Leibniz University“

BibTeX

@article{0cab9914cc5f4779b95f01e5375dea80,
title = "GW190521: A Binary Black Hole Merger with a Total Mass of 150M⊙",
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 85-14+21 Mm and 66-18+17 Mm (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 Mm. We calculate the mass of the remnant to be 142-16+28 Mm, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3-2.6+2.4 Gpc, corresponding to a redshift of 0.82-0.34+0.28. The inferred rate of mergers similar to GW190521 is 0.13-0.11+0.30 Gpc-3 yr-1.",
author = "{The LIGO Scientific Collaboration} and {The Virgo Collaboration} and R. Abbott and T. D. Abbott and S. Abraham and F. Acernese and K. Ackley and C. Adams and R. X. Adhikari and V. B. Adya and C. Affeldt and M. Agathos and K. Agatsuma and N. Aggarwal and O. D. Aguiar and A. Aich and L. Aiello and A. Ain and P. Ajith and S. Akcay and G. Allen and A. Allocca and P. A. Altin and A. Amato and S. Anand and A. Ananyeva and S. B. Anderson and W. G. Anderson and S. V. Angelova and S. Ansoldi and S. Antier and S. Appert and K. Arai and M. C. Araya and J. S. Areeda and M. Ar{\`e}ne and N. Arnaud and S. M. Aronson and K. G. Arun and Y. Asali and S. Ascenzi and G. Ashton and S. M. Aston and S. L. Danilishin and K. Danzmann and M. Heurs and H. L{\"u}ck and D. Steinmeyer and H. Vahlbruch and D. M. Wilken and B. Willke and H. Wittel and Sukanta Bose and Brown, {D. D.} and Chen, {Y. H.} and J. Gniesmer and Hanke, {M. M.} and J. Hennig and H{\"u}bner, {M. T.} and Sanjeev Kumar and Lang, {R. N.} and Lee, {C. H.} and Lee, {H. M.} and Lee, {H. W.} and J. Lee and K. Lee and X. Li and Rose, {C. A.} and D. Rose and Sanders, {J. R.} and Patricia Schmidt and L. Sun and Wu, {D. S.} and R. Zhang and H. Zhang and Zhu, {X. J.} and M. Zhou and Fabio Bergamin and A. Bisht and Nina Bode and P. Booker and M. Brinkmann and M. Cabero and N. Gohlke and J. Heinze and {de Varona}, O. and S. Hochheim and J. Junker and W. Kastaun and Stefan Kaufer and S. Khan and P. Koch and N. Koper and K{\"o}hlenbeck, {S. M.} and V. Kringel and G. Kuehn and S. Leavey and J. Lehmann and J. Liu and Lough, {J. D.} and M. Mehmet and Fabian Meylahn and N. Mukund and M. Nery and F. Ohme and P. Oppermann and E. Schreiber and Schulte, {B. W.} and Y. Setyawati and M. Steinke and M. Weinert and F. Wellmann and Peter We{\ss}els and W. Winkler and J. Woehler and M. Standke and M. Phelps and Peter Aufmuth and Gerald Bergmann and R. Kirchhoff and Nitz, {Alexander H.} and Li-Wei Wei",
note = "Funding Information: The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Netherlands Organization for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigaci{\'o}n, the Vicepresid{\`e}ncia i Conselleria d{\textquoteright}Innovaci{\'o}, Recerca i Turisme and the Conselleria d{\textquoteright}Educaci{\'o} i Universitat del Govern de les Illes Balears, the Conselleria d{\textquoteright}Innovaci{\'o}, Universitats, Ci{\`e}ncia i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concert{\'e}es (ARC) and Fonds Wetenschappelijk Onderzoek—Vlaanderen (FWO), Belgium, the Paris {\^I}le-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN, and CNRS for provision of computational resources. We thank the referees for useful comments that have improved the manuscript. In addition to the software cited earlier, pesummary was used to produce the publicly released samples and matplotlib was used for plotting.",
year = "2020",
month = sep,
day = "4",
doi = "10.1103/physrevlett.125.101102",
language = "English",
volume = "125",
journal = "Physical review letters",
issn = "0031-9007",
publisher = "American Physical Society",
number = "10",
}

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