Properties and Astrophysical Implications of the 150 M o˙Binary Black Hole Merger GW190521

Research output: Contribution to journal › Article › Research › peer review

Authors

  • The Virgo Collaboration
  • The LIGO Scientific Collaboration
  • C. Affeldt
  • S. L. Danilishin
  • K. Danzmann
  • M. Heurs
  • H. Lück
  • D. Steinmeyer
  • H. Vahlbruch
  • L. W. Wei
  • D. M. Wilken
  • B. Willke
  • H. Wittel
  • Sukanta Bose
  • D. D. Brown
  • Y. H. Chen
  • Hai-Ping Cheng
  • J. Gniesmer
  • Manuela 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
  • H. Zhang
  • X. J. Zhu
  • Minchuan 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
  • R. Kirchhoff
  • 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. Phelps
  • M. Standke
  • M. Weinert
  • F. Wellmann
  • Peter Weßels
  • W. Winkler
  • J. Woehler
  • Peter Aufmuth
  • Gerald Bergmann

Research Organisations

External Research Organisations

  • California Institute of Caltech (Caltech)
  • Louisiana State University
  • Inter-University Centre for Astronomy and Astrophysics India
  • Universita di Salerno
  • Monte S. Angelo University Federico II
  • Monash University
  • Australian National University
  • University of Cambridge
  • University of Birmingham
  • Northwestern University
  • Instituto Nacional de Pesquisas Espaciais
  • University of Texas Rio Grande Valley
  • Gran Sasso Science Institute
  • Istituto Nazionale di Fisica Nucleare (INFN)
  • Tata Institute of Fundamental Research (TIFR HYD)
  • University of Illinois at Urbana-Champaign
  • Sezione di Pisa
  • Université de Lyon
  • University of Wisconsin Milwaukee
  • University of Strathclyde
  • University of Udine
  • Observatoire de Paris (OBSPARIS)
  • California State University Fullerton
  • Universite Paris-Sud XI
  • European Gravitational Observatory (EGO)
  • University of Florida
  • Chennai Mathematical Institute
  • Columbia University
  • Carson College of Business
  • University of Adelaide
  • Massachusetts Institute of Technology
  • Universität Hamburg
  • LIGO Laboratory
  • Inje University
  • Stanford University
  • The California State University
  • Radboud University Nijmegen (RU)
  • University of Melbourne
  • National Taiwan Normal University
  • Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
  • Friedrich Schiller University Jena
  • University of Glasgow
  • Laser Zentrum Hannover e.V. (LZH)
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Details

Original languageEnglish
Article numberL13
JournalAstrophysical Journal Letters
Volume900
Issue number1
Publication statusPublished - 2 Sept 2020

Abstract

The gravitational-wave signal GW190521 is consistent with a binary black hole (BBH) merger source at redshift 0.8 with unusually high component masses, 85-14+21 M o˙ and 66-18+17 M o˙, compared to previously reported events, and shows mild evidence for spin-induced orbital precession. The primary falls in the mass gap predicted by (pulsational) pair-instability supernova theory, in the approximate range 65-120 M o˙. The probability that at least one of the black holes in GW190521 is in that range is 99.0%. The final mass of the merger (142-16+28 M o˙) classifies it as an intermediate-mass black hole. Under the assumption of a quasi-circular BBH coalescence, we detail the physical properties of GW190521's source binary and its post-merger remnant, including component masses and spin vectors. Three different waveform models, as well as direct comparison to numerical solutions of general relativity, yield consistent estimates of these properties. Tests of strong-field general relativity targeting the merger-ringdown stages of the coalescence indicate consistency of the observed signal with theoretical predictions. We estimate the merger rate of similar systems to be 0.13-0.11+0.30 Gpc-3 yr-1. We discuss the astrophysical implications of GW190521 for stellar collapse and for the possible formation of black holes in the pair-instability mass gap through various channels: via (multiple) stellar coalescences, or via hierarchical mergers of lower-mass black holes in star clusters or in active galactic nuclei. We find it to be unlikely that GW190521 is a strongly lensed signal of a lower-mass black hole binary merger. We also discuss more exotic possible sources for GW190521, including a highly eccentric black hole binary, or a primordial black hole binary.

ASJC Scopus subject areas

Cite this

Properties and Astrophysical Implications of the 150 M o˙Binary Black Hole Merger GW190521. / The Virgo Collaboration; The LIGO Scientific Collaboration; Affeldt, C. et al.
In: Astrophysical Journal Letters, Vol. 900, No. 1, L13, 02.09.2020.

Research output: Contribution to journal › Article › Research › peer review

The Virgo Collaboration, The LIGO Scientific Collaboration, Affeldt, C, Danilishin, SL, Danzmann, K, Heurs, M, Lück, H, Steinmeyer, D, Vahlbruch, H, Wei, LW, Wilken, DM, Willke, B, Wittel, H, Bose, S, Brown, DD, Chen, YH, Cheng, H-P, Gniesmer, J, Hanke, M, Hennig, J, Hübner, MT, Kumar, S, Lang, RN, Lee, CH, Lee, HM, Lee, HW, Lee, J, Lee, K, Li, X, Rose, CA, Rose, D, Sanders, JR, Schmidt, P, Sun, L, Wu, DS, Zhang, H, Zhu, XJ, Zhou, M, Bergamin, F, Bisht, A, Bode, N, Booker, P, Brinkmann, M, Cabero, M, Gohlke, N, Heinze, J, de Varona, O, Hochheim, S, Junker, J, Kastaun, W, Kaufer, S, Khan, S, Kirchhoff, R, Koch, P, Koper, N, Köhlenbeck, SM, Kringel, V, Kuehn, G, Leavey, S, Lehmann, J, Liu, J, Lough, JD, Mehmet, M, Meylahn, F, Mukund, N, Nery, M, Ohme, F, Oppermann, P, Schreiber, E, Schulte, BW, Setyawati, Y, Steinke, M, Phelps, M, Standke, M, Weinert, M, Wellmann, F, Weßels, P, Winkler, W, Woehler, J, Aufmuth, P & Bergmann, G 2020, 'Properties and Astrophysical Implications of the 150 M o˙Binary Black Hole Merger GW190521', Astrophysical Journal Letters, vol. 900, no. 1, L13. https://doi.org/10.48550/arXiv.2009.01190, https://doi.org/10.3847/2041-8213/aba493
The Virgo Collaboration, The LIGO Scientific Collaboration, Affeldt, C., Danilishin, S. L., Danzmann, K., Heurs, M., Lück, H., Steinmeyer, D., Vahlbruch, H., Wei, L. W., Wilken, D. M., Willke, B., Wittel, H., Bose, S., Brown, D. D., Chen, Y. H., Cheng, H.-P., Gniesmer, J., Hanke, M., ... Bergmann, G. (2020). Properties and Astrophysical Implications of the 150 M o˙Binary Black Hole Merger GW190521. Astrophysical Journal Letters, 900(1), Article L13. https://doi.org/10.48550/arXiv.2009.01190, https://doi.org/10.3847/2041-8213/aba493
The Virgo Collaboration, The LIGO Scientific Collaboration, Affeldt C, Danilishin SL, Danzmann K, Heurs M et al. Properties and Astrophysical Implications of the 150 M o˙Binary Black Hole Merger GW190521. Astrophysical Journal Letters. 2020 Sept 2;900(1):L13. doi: 10.48550/arXiv.2009.01190, 10.3847/2041-8213/aba493
The Virgo Collaboration ; The LIGO Scientific Collaboration ; Affeldt, C. et al. / Properties and Astrophysical Implications of the 150 M o˙Binary Black Hole Merger GW190521. In: Astrophysical Journal Letters. 2020 ; Vol. 900, No. 1.
Download
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title = "Properties and Astrophysical Implications of the 150 M o˙Binary Black Hole Merger GW190521",
abstract = "The gravitational-wave signal GW190521 is consistent with a binary black hole (BBH) merger source at redshift 0.8 with unusually high component masses, 85-14+21 M o˙ and 66-18+17 M o˙, compared to previously reported events, and shows mild evidence for spin-induced orbital precession. The primary falls in the mass gap predicted by (pulsational) pair-instability supernova theory, in the approximate range 65-120 M o˙. The probability that at least one of the black holes in GW190521 is in that range is 99.0%. The final mass of the merger (142-16+28 M o˙) classifies it as an intermediate-mass black hole. Under the assumption of a quasi-circular BBH coalescence, we detail the physical properties of GW190521's source binary and its post-merger remnant, including component masses and spin vectors. Three different waveform models, as well as direct comparison to numerical solutions of general relativity, yield consistent estimates of these properties. Tests of strong-field general relativity targeting the merger-ringdown stages of the coalescence indicate consistency of the observed signal with theoretical predictions. We estimate the merger rate of similar systems to be 0.13-0.11+0.30 Gpc-3 yr-1. We discuss the astrophysical implications of GW190521 for stellar collapse and for the possible formation of black holes in the pair-instability mass gap through various channels: via (multiple) stellar coalescences, or via hierarchical mergers of lower-mass black holes in star clusters or in active galactic nuclei. We find it to be unlikely that GW190521 is a strongly lensed signal of a lower-mass black hole binary merger. We also discuss more exotic possible sources for GW190521, including a highly eccentric black hole binary, or a primordial black hole binary.",
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TY - JOUR

T1 - Properties and Astrophysical Implications of the 150 M o˙Binary Black Hole Merger GW190521

AU - The Virgo Collaboration

AU - The LIGO Scientific Collaboration

AU - Abbott, R.

AU - Abbott, T. D.

AU - Abraham, S.

AU - Acernese, F.

AU - Ackley, K.

AU - Adams, C.

AU - Adhikari, R. X.

AU - Adya, V. B.

AU - Affeldt, C.

AU - Agathos, M.

AU - Agatsuma, K.

AU - Aggarwal, N.

AU - Aguiar, O. D.

AU - Aich, A.

AU - Aiello, L.

AU - Ain, A.

AU - Ajith, P.

AU - Akcay, S.

AU - Allen, G.

AU - Allocca, A.

AU - Altin, P. A.

AU - Amato, A.

AU - Anand, S.

AU - Ananyeva, A.

AU - Anderson, S. B.

AU - Anderson, W. G.

AU - Angelova, S. V.

AU - Ansoldi, S.

AU - Antier, S.

AU - Appert, S.

AU - Arai, K.

AU - Araya, M. C.

AU - Areeda, J. S.

AU - Arène, M.

AU - Arnaud, N.

AU - Aronson, S. M.

AU - Arun, K. G.

AU - Asali, Y.

AU - Ascenzi, S.

AU - Ashton, G.

AU - Danilishin, S. L.

AU - Danzmann, K.

AU - Heurs, M.

AU - Lück, H.

AU - Steinmeyer, D.

AU - Vahlbruch, H.

AU - Wei, L. W.

AU - Wilken, D. M.

AU - Willke, B.

AU - Wittel, H.

AU - Bose, Sukanta

AU - Brown, D. D.

AU - Chen, Y. H.

AU - Cheng, Hai-Ping

AU - Gniesmer, J.

AU - Hanke, Manuela

AU - Hennig, J.

AU - Hübner, M. T.

AU - Kumar, Sanjeev

AU - Lang, R. N.

AU - Lee, C. H.

AU - Lee, H. M.

AU - Lee, H. W.

AU - Lee, J.

AU - Lee, K.

AU - Li, X.

AU - Rose, C. A.

AU - Rose, D.

AU - Sanders, J. R.

AU - Schmidt, Patricia

AU - Sun, L.

AU - Wu, D. S.

AU - Zhang, H.

AU - Zhu, X. J.

AU - Zhou, Minchuan

AU - Bergamin, Fabio

AU - Bisht, A.

AU - Bode, Nina

AU - Booker, P.

AU - Brinkmann, M.

AU - Cabero, M.

AU - Gohlke, N.

AU - Heinze, J.

AU - de Varona, O.

AU - Hochheim, S.

AU - Junker, J.

AU - Kastaun, W.

AU - Kaufer, Stefan

AU - Khan, S.

AU - Kirchhoff, R.

AU - Koch, P.

AU - Koper, N.

AU - Köhlenbeck, S. M.

AU - Kringel, V.

AU - Kuehn, G.

AU - Leavey, S.

AU - Lehmann, J.

AU - Liu, J.

AU - Lough, J. D.

AU - Mehmet, M.

AU - Meylahn, Fabian

AU - Mukund, N.

AU - Nery, M.

AU - Ohme, F.

AU - Oppermann, P.

AU - Schreiber, E.

AU - Schulte, B. W.

AU - Setyawati, Y.

AU - Steinke, M.

AU - Phelps, M.

AU - Standke, M.

AU - Weinert, M.

AU - Wellmann, F.

AU - Weßels, Peter

AU - Winkler, W.

AU - Woehler, J.

AU - Aufmuth, Peter

AU - Bergmann, Gerald

PY - 2020/9/2

Y1 - 2020/9/2

N2 - The gravitational-wave signal GW190521 is consistent with a binary black hole (BBH) merger source at redshift 0.8 with unusually high component masses, 85-14+21 M o˙ and 66-18+17 M o˙, compared to previously reported events, and shows mild evidence for spin-induced orbital precession. The primary falls in the mass gap predicted by (pulsational) pair-instability supernova theory, in the approximate range 65-120 M o˙. The probability that at least one of the black holes in GW190521 is in that range is 99.0%. The final mass of the merger (142-16+28 M o˙) classifies it as an intermediate-mass black hole. Under the assumption of a quasi-circular BBH coalescence, we detail the physical properties of GW190521's source binary and its post-merger remnant, including component masses and spin vectors. Three different waveform models, as well as direct comparison to numerical solutions of general relativity, yield consistent estimates of these properties. Tests of strong-field general relativity targeting the merger-ringdown stages of the coalescence indicate consistency of the observed signal with theoretical predictions. We estimate the merger rate of similar systems to be 0.13-0.11+0.30 Gpc-3 yr-1. We discuss the astrophysical implications of GW190521 for stellar collapse and for the possible formation of black holes in the pair-instability mass gap through various channels: via (multiple) stellar coalescences, or via hierarchical mergers of lower-mass black holes in star clusters or in active galactic nuclei. We find it to be unlikely that GW190521 is a strongly lensed signal of a lower-mass black hole binary merger. We also discuss more exotic possible sources for GW190521, including a highly eccentric black hole binary, or a primordial black hole binary.

AB - The gravitational-wave signal GW190521 is consistent with a binary black hole (BBH) merger source at redshift 0.8 with unusually high component masses, 85-14+21 M o˙ and 66-18+17 M o˙, compared to previously reported events, and shows mild evidence for spin-induced orbital precession. The primary falls in the mass gap predicted by (pulsational) pair-instability supernova theory, in the approximate range 65-120 M o˙. The probability that at least one of the black holes in GW190521 is in that range is 99.0%. The final mass of the merger (142-16+28 M o˙) classifies it as an intermediate-mass black hole. Under the assumption of a quasi-circular BBH coalescence, we detail the physical properties of GW190521's source binary and its post-merger remnant, including component masses and spin vectors. Three different waveform models, as well as direct comparison to numerical solutions of general relativity, yield consistent estimates of these properties. Tests of strong-field general relativity targeting the merger-ringdown stages of the coalescence indicate consistency of the observed signal with theoretical predictions. We estimate the merger rate of similar systems to be 0.13-0.11+0.30 Gpc-3 yr-1. We discuss the astrophysical implications of GW190521 for stellar collapse and for the possible formation of black holes in the pair-instability mass gap through various channels: via (multiple) stellar coalescences, or via hierarchical mergers of lower-mass black holes in star clusters or in active galactic nuclei. We find it to be unlikely that GW190521 is a strongly lensed signal of a lower-mass black hole binary merger. We also discuss more exotic possible sources for GW190521, including a highly eccentric black hole binary, or a primordial black hole binary.

UR - http://www.scopus.com/inward/record.url?scp=85094168773&partnerID=8YFLogxK

U2 - 10.48550/arXiv.2009.01190

DO - 10.48550/arXiv.2009.01190

M3 - Article

AN - SCOPUS:85094168773

VL - 900

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

SN - 2041-8205

IS - 1

M1 - L13

ER -

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