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GW190521: A Binary Black Hole Merger with a Total Mass of 150  M_{⊙}.

  • Author(s): Abbott, R;
  • Abbott, TD;
  • Abraham, S;
  • Acernese, F;
  • Ackley, K;
  • Adams, C;
  • Adhikari, RX;
  • Adya, VB;
  • Affeldt, C;
  • Agathos, M;
  • Agatsuma, K;
  • Aggarwal, N;
  • Aguiar, OD;
  • Aich, A;
  • Aiello, L;
  • Ain, A;
  • Ajith, P;
  • Akcay, S;
  • Allen, G;
  • Allocca, A;
  • Altin, PA;
  • Amato, A;
  • Anand, S;
  • Ananyeva, A;
  • Anderson, SB;
  • Anderson, WG;
  • Angelova, SV;
  • Ansoldi, S;
  • Antier, S;
  • Appert, S;
  • Arai, K;
  • Araya, MC;
  • Areeda, JS;
  • Arène, M;
  • Arnaud, N;
  • Aronson, SM;
  • Arun, KG;
  • Asali, Y;
  • Ascenzi, S;
  • Ashton, G;
  • Aston, SM;
  • Astone, P;
  • Aubin, F;
  • Aufmuth, P;
  • AultONeal, K;
  • Austin, C;
  • Avendano, V;
  • Babak, S;
  • Bacon, P;
  • Badaracco, F;
  • Bader, MKM;
  • Bae, S;
  • Baer, AM;
  • Baird, J;
  • Baldaccini, F;
  • Ballardin, G;
  • Ballmer, SW;
  • Bals, A;
  • Balsamo, A;
  • Baltus, G;
  • Banagiri, S;
  • Bankar, D;
  • Bankar, RS;
  • Barayoga, JC;
  • Barbieri, C;
  • Barish, BC;
  • Barker, D;
  • Barkett, K;
  • Barneo, P;
  • Barone, F;
  • Barr, B;
  • Barsotti, L;
  • Barsuglia, M;
  • Barta, D;
  • Bartlett, J;
  • Bartos, I;
  • Bassiri, R;
  • Basti, A;
  • Bawaj, M;
  • Bayley, JC;
  • Bazzan, M;
  • Bécsy, B;
  • Bejger, M;
  • Belahcene, I;
  • Bell, AS;
  • Beniwal, D;
  • Benjamin, MG;
  • Bentley, JD;
  • Bergamin, F;
  • Berger, BK;
  • Bergmann, G;
  • Bernuzzi, S;
  • Berry, CPL;
  • Bersanetti, D;
  • Bertolini, A;
  • Betzwieser, J;
  • Bhandare, R;
  • Bhandari, AV;
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  • Biscoveanu, S;
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  • Blair, DG;
  • Blair, RM;
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  • George, J;
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  • Ghosh, Archisman;
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  • et al.
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}  M_{⊙} and 66_{-18}^{+17}  M_{⊙} (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_{-16}^{+28}  M_{⊙}, 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}.

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