Black hole masses of tidal disruption event host galaxies II

Author:

Wevers Thomas1,Stone Nicholas C2ORCID,van Velzen Sjoert34,Jonker Peter G56,Hung Tiara4,Auchettl Katie789,Gezari Suvi4,Onori Francesca5ORCID,Mata Sánchez Daniel10,Kostrzewa-Rutkowska Zuzanna56,Casares Jorge1112ORCID

Affiliation:

1. Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK

2. Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA

3. Center for Cosmology and Particle Physics, New York University, New York, NY 10003, USA

4. Department of Astronomy, University of Maryland, College Park, MD 20742, USA

5. SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, NL-3584CA Utrecht, the Netherlands

6. Department of Astrophysics/IMAPP, Radboud University, PO Box 9010, NL-6500GL Nijmegen, the Netherlands

7. Center for Cosmology and Astro-Particle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USA

8. Department of Physics, The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USA

9. Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, DK-2100 Copenhagen, Denmark

10. Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UK

11. Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain

12. Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain

Abstract

ABSTRACT We present new medium resolution, optical long-slit spectra of a sample of six ultraviolet (UV)/optical and 17 X-ray-selected tidal disruption event candidate host galaxies. We measure emission line ratios from the optical spectra, finding that the large majority of hosts are quiescent galaxies, while those displaying emission lines are generally consistent with star formation dominated environments; only three sources show clear evidence of nuclear activity. We measure bulge velocity dispersions using absorption lines and infer host black hole (BH) masses using the M – σ relation. While the optical and X-ray host BH masses are statistically consistent with coming from the same parent distribution, the optical host distribution has a visible peak near $M_{\rm BH} \sim 10^6 \, \mathrm{M}_\odot$, whereas the X-ray host distribution appears flat in MBH. We find a subset of X-ray-selected candidates that are hosted in galaxies significantly less luminous (Mg ∼ −16) and less massive (stellar mass ∼ 108.5–9 M⊙) than those of optical events. Using statistical tests we find suggestive evidence that, in terms of BH mass, stellar mass, and absolute magnitude, the hard X-ray hosts differ from the UV/optical and soft X-ray samples. Similar to individual studies, we find that the size of the emission region for the soft X-ray sample is much smaller than the optical emission region, consistent with a compact accretion disc. We find that the typical Eddington ratio of the soft X-ray emission is ∼ 0.01, as opposed to the optical events which have LBB ∼ LEdd. The latter seems artificial if the radiation is produced by self-intersection shocks, and instead suggests a connection to the supermassive black hole.

Funder

European Research Council

European Commission

National Science Foundation

National Aeronautics and Space Administration

Horizon 2020

Ministerio de Economía y Competitividad

California Institute of Technology

University of California

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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