Intermediate-Mass Black Holes

Author:

Greene Jenny E.1,Strader Jay2,Ho Luis C.3

Affiliation:

1. Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544, USA;

2. Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA

3. Kavli Institute for Astronomy and Astrophysics, and Department of Astronomy, School of Physics, Peking University, Beijing 100871, China

Abstract

We describe ongoing searches for intermediate-mass black holes with MBH≈ 10–105M. We review a range of search mechanisms, both dynamical and those that rely on accretion signatures. We find the following conclusions: ▪  Dynamical and accretion signatures alike point to a high fraction of 109–1010Mgalaxies hosting black holes with MBH∼ 105M. In contrast, there are no solid detections of black holes in globular clusters. ▪  There are few observational constraints on black holes in any environment with MBH≈ 100–104M. ▪  Considering low-mass galaxies with dynamical black hole masses and constraining limits, we find that the MBH–σ*relation continues unbroken to MBH∼105M, albeit with large scatter. We believe the scatter is at least partially driven by a broad range in black hole masses, because the occupation fraction appears to be relatively high in these galaxies. ▪  We fold the observed scaling relations with our empirical limits on occupation fraction and the galaxy mass function to put observational bounds on the black hole mass function in galaxy nuclei. ▪  We are pessimistic that local demographic observations of galaxy nuclei alone could constrain seeding mechanisms, although either high-redshift luminosity functions or robust measurements of off-nuclear black holes could begin to discriminate models.

Publisher

Annual Reviews

Subject

Space and Planetary Science,Astronomy and Astrophysics

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