A noninteracting low-mass black hole-giant star binary system

Todd A Thompson^{1

2

3}, Christopher S Kochanek^{4

2}, Krzysztof Z Stanek^{4

2}, Carles Badenes^{5

6}, Richard S Post⁷, Tharindu Jayasinghe^{4

2}, David W Latham⁸, Allyson Bieryla⁸, Gilbert A Esquerdo⁸, Perry Berlind⁸, Michael L Calkins⁸, Jamie Tayar^{4

9}, Lennart Lindegren¹⁰, Jennifer A Johnson^{4

2}, Thomas W-S Holoien¹¹, Katie Auchettl^{2

12

13}, Kevin Covey¹⁴

Affiliations

¹ Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA. thompson.1847@osu.edu.
² Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA.
³ Institute for Advanced Study, 1 Einstein Dr., Princeton, NJ 08540, USA.
⁴ Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA.
⁵ Department of Physics and Astronomy and Pittsburgh Particle Physics, Astrophysics and Cosmology Center, University of Pittsburgh, 3941 O'Hara St., Pittsburgh, PA 15260, USA.
⁶ Institut de Ciències del Cosmos, Universitat de Barcelona, Martí Franqués 1, E08028 Barcelona, Spain.
⁷ Post Observatory, Lexington, MA 02421, USA.
⁸ Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA.
⁹ Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr., Honolulu, Hawaii 96822, USA.
¹⁰ Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden.
¹¹ The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA.
¹² Department of Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA.
¹³ Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Lyngbyvej 2, 2100 Copenhagen, Denmark.
¹⁴ Department of Physics and Astronomy, Western Washington University, Mail Stop 9164, Bellingham, WA, 98225, USA.

PMID: 31672898
DOI: 10.1126/science.aau4005

A noninteracting low-mass black hole-giant star binary system

Todd A Thompson et al. Science. 2019.

. 2019 Nov 1;366(6465):637-640.

doi: 10.1126/science.aau4005.

Authors

Affiliations

¹ Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA. thompson.1847@osu.edu.
² Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA.
³ Institute for Advanced Study, 1 Einstein Dr., Princeton, NJ 08540, USA.
⁴ Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA.
⁵ Department of Physics and Astronomy and Pittsburgh Particle Physics, Astrophysics and Cosmology Center, University of Pittsburgh, 3941 O'Hara St., Pittsburgh, PA 15260, USA.
⁶ Institut de Ciències del Cosmos, Universitat de Barcelona, Martí Franqués 1, E08028 Barcelona, Spain.
⁷ Post Observatory, Lexington, MA 02421, USA.
⁸ Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA.
⁹ Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr., Honolulu, Hawaii 96822, USA.
¹⁰ Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden.
¹¹ The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA.
¹² Department of Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA.
¹³ Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Lyngbyvej 2, 2100 Copenhagen, Denmark.
¹⁴ Department of Physics and Astronomy, Western Washington University, Mail Stop 9164, Bellingham, WA, 98225, USA.

PMID: 31672898
DOI: 10.1126/science.aau4005

Abstract

Black hole binary systems with companion stars are typically found via their x-ray emission, generated by interaction and accretion. Noninteracting binaries are expected to be plentiful in the Galaxy but must be observed using other methods. We combine radial velocity and photometric variability data to show that the bright, rapidly rotating giant star 2MASS J05215658+4359220 is in a binary system with a massive unseen companion. The system has an orbital period of ~83 days and near-zero eccentricity. The photometric variability period of the giant is consistent with the orbital period, indicating star spots and tidal synchronization. Constraints on the giant's mass and radius imply that the unseen companion is [Formula: see text] solar masses, indicating that it is a noninteracting low-mass black hole or an unexpectedly massive neutron star.

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Comment on "A noninteracting low-mass black hole-giant star binary system".
van den Heuvel EPJ, Tauris TM. van den Heuvel EPJ, et al. Science. 2020 May 8;368(6491):eaba3282. doi: 10.1126/science.aba3282. Science. 2020. PMID: 32381688

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A noninteracting low-mass black hole-giant star binary system

Affiliations

A noninteracting low-mass black hole-giant star binary system

Authors

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Abstract

Comment in

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