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Multimessenger signatures of massive black holes in dwarf galaxies
Bellovary, Jillian M.; Cleary, Colleen E.; Munshi, Ferah; Tremmel, Michael; Christensen, Charlotte R.; Brooks, Alyson; Quinn, Thomas R.
AA(Department of Physics, Queensborough Community College, City University of New York, 222-05 56th Ave, Bayside, NY 11364, USA; Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024, USA 0000-0001-7596-8372), AB(Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024, USA; Department of Physics, Hunter College, City University of New York, New York, NY 10007, USA), AC(Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN, 37212, USA; Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks St, Norman, OK, 73019, USA), AD(Department of Astronomy, Yale University, 52 Hillhouse Ave, New Haven, CT 06511, USA), AE(Department of Physics, Grinnell College, 1115 8th Ave, Grinnel, IA, 50112, USA), AF(Department of Physics & Astronomy, Rutgers University, 136 Frelinghuysen Rd., Piscataway, NJ 08854, USA), AG(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98122, USA)
Monthly Notices of the Royal Astronomical Society, Volume 482, Issue 3, p.2913-2923 (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
black hole physics, gravitational waves, galaxies: dwarf
Abstract Copyright:
2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
Bibliographic Code:


Recent discoveries of massive black holes (MBHs) in dwarf galaxies suggest that they may have a more common presence than once thought. Systematic searches are revealing more candidates, but this process could be accelerated by predictions from simulations. We perform a study of several high-resolution, cosmological, zoom-in simulations focusing on dwarf galaxies that host massive black holes at z = 0, with the aim of determining when the black holes are most observable. Larger dwarf galaxies are more likely to host MBHs than those of lower mass. About 50 per cent of the MBHs in dwarfs are not centrally located, but rather are wandering within a few kpc of the galaxy centre. The accretion luminosities of MBHs in dwarfs are low throughout cosmic time, rendering them extremely difficult to detect. However, the merger history of these MBHs is optimal for gravitational wave detection by LISA.
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