Intermediate - mass black holes

  title={Intermediate - mass black holes},
  author={M. Coleman Miller and Edward James McBride Colbert},
  journal={International Journal of Modern Physics D},
The mathematical simplicity of black holes, combined with their links to some of the most energetic events in the universe, means that black holes are key objects for fundamental physics and astrophysics. Until recently, it was generally believed that black holes in nature appear in two broad mass ranges: stellar-mass (M ∼ 3 − 20 M⊙), which are produced by the core collapse of massive stars, and supermassive (M ∼ 10 6 − 10 10 M⊙), which are found in the centers of galaxies and are produced by a… 

Probing General Relativity with Mergers of Supermassive and Intermediate-Mass Black Holes

Recent observations and stellar dynamics simulations suggest that ~103 M☉ black holes can form in compact massive young star clusters. Any such cluster in the bulge of its host galaxy will, within a

A symbiotic scenario for the rapid formation of supermassive black holes

The most massive black holes, lurking at the centres of large galaxies, must have formed less than a billion years after the big bang, as they are visible today in the form of bright quasars at


If binaries consisting of two ∼100 M☉ black holes exist, they would serve as extraordinarily powerful gravitational-wave sources, detectable to redshifts of z ∼ 2 with the advanced LIGO/Virgo

Intermediate-mass black holes from stellar mergers in young star clusters

Intermediate-mass black holes (IMBHs) in the mass range $10^2\!-\!10^5\, \mathrm{M_{\odot }}$ bridge the gap between stellar black holes (BHs) and supermassive BHs. Here, we investigate the

Measuring the spins of accreting black holes

A typical galaxy is thought to contain tens of millions of stellar-mass black holes, the collapsed remnants of once massive stars, and a single nuclear supermassive black hole. Both classes of black

Investigating the retention of intermediate-mass black holes in star clusters using N-body simulations

Context. Contrary to supermassive and stellar-mass black holes (SBHs), the existence of intermediate-mass black holes (IMBHs) with masses ranging between 10 2−5 M⊙ has not yet been confirmed. The

Searching for intermediate-mass black holes in galaxies with low-luminosity AGN: a multiple-method approach

Aims. This work is the first stage of a campaign to search for intermediate-mass black holes (IMBHs) in low-luminosity active galactic nuclei (LLAGN) and dwarf galaxies. An additional and equally

Intermediate-Mass Black Hole Induced Quenching of Mass Segregation in Star Clusters

In many theoretical scenarios it is expected that intermediate-mass black holes (IMBHs, with masses M ∼ 102–104 M☉) reside at the centers of some globular clusters. However, observational evidence

Dark matter annihilation around intermediate mass black holes: an update

The formation and evolution of black holes (BHs) inevitably affects the distribution of dark and baryonic matter in the neighborhood of the BH. These effects may be particularly relevant around

Probing the formation of the seeds of supermassive black holes with gravitational waves

  • M. Colpi
  • Physics
    Formation of the First Black Holes
  • 2019
The existence of black holes in the intermediate mass interval between one hundred and ten thousand solar masses, filling the gap between the stellar and the supermassive black holes is a key



Production of intermediate-mass black holes in globular clusters

The discovery of numerous non-nuclear X-ray point sources with luminosities L>1039 erg s−1 in several starburst galaxies has stimulated speculation about their nature and origin. The strong

Gravitational Radiation from Intermediate-Mass Black Holes

Recent X-ray observations of galaxies with ROSAT, ASCA, and Chandra have revealed numerous bright off-center point sources that, if isotropic emitters, are likely to be intermediate-mass black holes,

Dynamics of massive black holes as a possible candidate of Galactic dark matter

If the dark halo of the Galaxy is comprised of massive black holes (MBHs), then those within approximately 1 kpc will spiral to the center, where they will interact with one another, forming binaries

Primordial black holes in globular clusters

IT HAS recently been recognized1 that significant numbers of medium-mass black holes (of order 10 solar masses) should form in globular clusters during the early stages of their evolution. Here we

Stellar black holes in globular clusters

FOLLOWING the discovery of X-ray sources in globular clusters, the accretion of matter onto a central massive black hole was suggested1–3 as a possible explanation. Subsequently, it was found4,5 that

Black Hole Mergers in the Universe

This Letter explores the possibility that black holes become members of close binaries via dynamical interactions with other stars in dense stellar systems, implying gravity-wave detection rates substantially greater than the corresponding rates from neutron star mergers.

Theoretical Black Hole Mass Distributions

We derive the theoretical distribution function of black hole masses by studying the formation processes of black holes. We use the results of recent two-dimensional simulations of stellar core

Mass Limits For Black Hole Formation

We present a series of two-dimensional core-collapse supernova simulations for a range of progenitor masses and different input physics. These models predict a range of supernova energies and compact

The Need for a Second Black Hole at the Galactic Center

Deep infrared observations and long-term monitoring programs have provided dynamical evidence of a supermassive black hole of mass 3 × 106 M☉ associated with the radio source Sagittarius A* at the

Massive black hole remnants of the first stars in galactic haloes

We investigate the possibility that present-day galactic haloes contain a population of massive black holes (MBHs) that form by hierarchical merging of the BH remnants of the first stars. Some of the