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A black hole hiding in a binary star

As material falls toward a black hole, it heats up and emits x-rays. Almost all black holes are discovered by this x-ray emission. Thompson et al. observed light from a giant star that is Doppler shifted, indicating an orbit around a binary companion. The companion object must weigh more than 2.6 solar masses, but it emits no light, including x-rays. This indicates the presence of a black hole that is not currently consuming any material. There may be a population of similarly hidden black holes that have been missed by x-ray observations.
Science, this issue p. 637

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 3.30.7+2.8 solar masses, indicating that it is a noninteracting low-mass black hole or an unexpectedly massive neutron star.
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Supplementary Material

Summary

Materials and Methods
Figs. S1 to S9
Tables S1 to S8
References (3489)

Resources

File (aau4005_thompson_sm.pdf)

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Volume 366Issue 64651 November 2019
Pages: 637 - 640
PubMed: 31672898

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Received: 7 June 2018
Accepted: 10 October 2019

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Acknowledgments

We thank J. Choi for making MIST models available and C. Jordi and C. Fabricius for discussions. We thank the Ohio State University College of Arts and Sciences Technology Services for setting up the ASAS-SN Sky Patrol light curve server, which was critically useful during this work. T.A.T. thanks J. Zinn, T. Sukhbold, S. Gaudi, O. Pejcha, K. Stassun, M. Pinsonneault, A. Brown, C. Gammie, E. Rossi, J. Fuller, S. Phinney, A.-C. Eilers, D. Hogg, K. Cunha, and R. Poleski for discussions, and K. A. Byram for encouragement and support. Full facility acknowledgments are provided in the supplementary materials. Funding: T.A.T. acknowledges support from Scialog Scholar grant 24216 from the Research Corporation; a Simons Foundation Fellowship; and an IBM Einstein Fellowship from the Institute for Advanced Study, Princeton. C.B. acknowledges support from PHY 14-30152: Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the National Science Foundation. C.S.K. and K.Z.S. are supported in part by NSF grants AST-1515927 and AST-1515876. J.T. acknowledges support from NASA Hubble Fellowship grant 51424 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Author contributions: T.A.T. led the project, conceived of the search strategy, led the analysis, and led the writing of the text. C.S.K. analyzed the SED and the ASAS-SN photometry and fitted the observational data with evolutionary models. K.Z.S. analyzed the Post and ASAS-SN photometry and interpreted the system. R.S.P. provided the Post photometry. C.B. provided APOGEE RV analysis and interpretation of the system. T.J. carried out the time-series analysis of the ASAS-SN photometry. D.W.L., A.B., G.A.E., P.B., and M.L.C. obtained the TRES data and carried out the RV analysis. J.T. provided the rotation measurement from the APOGEE spectrum. L.L. provided the Gaia parallax bias analysis. J.A.J. consulted on the APOGEE spectra. T.W.-S.H. and K.A. obtained and analyzed the Swift data. K.C. participated in preparing the text and discussions of the APOGEE RV data. Competing interests: There are no competing interests to declare. Data and materials availability: The ASAS-SN light curve data are available at https://asas-sn.osu.edu/photometry/166c0f1c-2502-5e10-b5aa-38d31dddb398. The APOGEE observations, including all individual spectra, the combined spectrum, and analysis results are available at https://dr14.sdss.org/infrared/spectrum/view/stars?id=68401. Photometry for J05215658 is listed in table S8. X-ray and ultraviolet observations from the Neil Gehrels Swift Observatory (18) are available at https://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/swift.pl under target id 10442. The code used to calculate the parallax bias in the Gaia observations is available at https://github.com/chargedcurrent/Gaia_parallax_J05215658.

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Affiliations

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

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*Corresponding author. Email: [email protected]

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Volume 366|Issue 6465
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