Details
| Originalsprache | Englisch |
|---|---|
| Aufsatznummer | L13 |
| Fachzeitschrift | Astrophysical Journal Letters |
| Jahrgang | 900 |
| Ausgabenummer | 1 |
| Publikationsstatus | Veröffentlicht - 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 Sachgebiete
- Physik und Astronomie (insg.)
- Astronomie und Astrophysik
- Erdkunde und Planetologie (insg.)
- Astronomie und Planetologie
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in: Astrophysical Journal Letters, Jahrgang 900, Nr. 1, L13, 02.09.2020.
Publikation: Beitrag in Fachzeitschrift › Artikel › Forschung › Peer-Review
}
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 -