Статья

Candidate Electromagnetic Counterpart to the Binary Black Hole Merger Gravitational-Wave Event S190521g

M. J. GrahamCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USAK. E. Saavik FordDepartment of Astrophysics, American Museum of Natural History, Central Park West, New York, New York 10028, USABarry McKernanDepartment of Astrophysics, American Museum of Natural History, Central Park West, New York, New York 10028, USANicholas P. RossInstitute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3 HJ, United KingdomDaniel SternJet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USAKevin B. BurdgeCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USAM. W. CoughlinDivision of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, California 91125, USAS. G. DjorgovskiCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USAA. J. DrakeCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USADmitry A. DuevCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USAM. M. KasliwalCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USAAshish A MahabalCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USASjoert van VelzenCenter for Cosmology and Particle Physics, New York University, New York, New York 10003, USAJustin BeleckiCaltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USAE. BellmDIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, Washington 98195, USARick BurrussCaltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USAS. B. CenkoAstrophysics Science Division, NASA Goddard Space Flight Center, MC 661, Greenbelt, Maryland 20771, USAVirginia CunninghamDepartment of Astronomy, University of Maryland, College Park, Maryland 20742, USAG. HelouIPAC, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USAS. R. KulkarniCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USAFrank J. MasciIPAC, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USAThomas A. PrinceCahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USADan ReileyCaltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USAH. RodriguezCaltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USABen RusholmeIPAC, California Institute of Technology, 1200 E. California Boulevard, Pasadena, California 91125, USARoger M. SmithCaltech Optical Observatories, California Institute of Technology, Pasadena, California 91125, USAMaayane T. SoumagnacDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel

2020en

ABI

Аннотация

We report the first plausible optical electromagnetic counterpart to a (candidate) binary black hole merger. Detected by the Zwicky Transient Facility, the electromagnetic flare is consistent with expectations for a kicked binary black hole merger in the accretion disk of an active galactic nucleus [B. McKernan, K. E. S. Ford, I. Bartos et al., Astrophys. J. Lett. 884, L50 (2019)AJLEEY2041-821310.3847/2041-8213/ab4886] and is unlikely [<O(0.01%))] due to intrinsic variability of this source. The lack of color evolution implies that it is not a supernova and instead is strongly suggestive of a constant temperature shock. Other false-positive events, such as microlensing or a tidal disruption event, are ruled out or constrained to be <O(0.1%). If the flare is associated with S190521g, we find plausible values of total mass M_{BBH}∼100 M_{⊙}, kick velocity v_{k}∼200 km s^{-1} at θ∼60° in a disk with aspect ratio H/a∼0.01 (i.e., disk height H at radius a) and gas density ρ∼10^{-10} g cm^{-3}. The merger could have occurred at a disk migration trap (a∼700r_{g}; r_{g}≡GM_{SMBH}/c^{2}, where M_{SMBH} is the mass of the active galactic nucleus supermassive black hole). The combination of parameters implies a significant spin for at least one of the black holes in S190521g. The timing of our spectroscopy prevents useful constraints on broad-line asymmetry due to an off-center flare. We predict a repeat flare in this source due to a reencountering with the disk in ∼1.6 yr(M_{SMBH}/10^{8} M_{⊙})(a/10^{3}r_{g})^{3/2}.

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Идентификаторы

DOI: 10.1103/physrevlett.124.251102

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Цитирований: 3Использованных источников: 0

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