R. Abbott, California Institute of Technology
T. D. Abbott, Louisiana State University
S. Abraham, Inter-University Centre for Astronomy and Astrophysics India
F. Acernese, Università di Salerno
K. Ackley, Monash University
C. Adams, LIGO Livingston
R. X. Adhikari, California Institute of Technology
V. B. Adya, The Australian National University
C. Affeldt, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
M. Agathos, Friedrich Schiller Universität Jena
K. Agatsuma, University of Birmingham
N. Aggarwal, Northwestern University
O. D. Aguiar, Instituto Nacional de Pesquisas Espaciais
A. Aich, University of Texas Rio Grande Valley
L. Aiello, Gran Sasso Science Institute
A. Ain, Inter-University Centre for Astronomy and Astrophysics India
P. Ajith, Tata Institute of Fundamental Research, Mumbai
S. Akcay, Friedrich Schiller Universität Jena
G. Allen, University of Illinois at Urbana-Champaign
A. Allocca, Istituto Nazionale di Fisica Nucleare, Sezione di Pisa
P. A. Altin, The Australian National University
A. Amato, Université de Lyon
S. Anand, California Institute of Technology
A. Ananyeva, California Institute of Technology
S. B. Anderson, California Institute of Technology
W. G. Anderson, University of Wisconsin-Milwaukee
S. V. Angelova, University of Strathclyde
S. Ansoldi, Università degli Studi di Udine
S. Antier, APC - AstroParticule et Cosmologie
S. Appert, California Institute of Technology
K. Arai, California Institute of Technology
Tiffany Z. Summerscales, Andrews UniversityFollow

Document Type


Publication Date



© 2020 authors. Published by the American Physical Society. 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.

Journal Title

Physical Review Letters







First Department



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