Black Holes, Galaxy Formation, and the MBH-σ Relation

  title={Black Holes, Galaxy Formation, and the MBH-$\sigma$ Relation},
  author={Andrew King},
  journal={The Astrophysical Journal Letters},
  pages={L27 - L29}
  • A. King
  • Published 20 August 2003
  • Physics
  • The Astrophysical Journal Letters
Recent X-ray observations of intense high-speed outflows in quasars suggest that supercritical accretion on to the central black hole may have an important effect on a host galaxy. I revisit some ideas of Silk & Rees and assume that such flows occur in the final stages of building up the black hole mass. It is now possible to model explicitly the interaction between the outflow and the host galaxy. This is found to resemble a momentum-driven stellar wind bubble, implying a relation MBH = (fgκ/2… 

Accretion and Outflow in Active Galaxies

  • A. King
  • Physics
    Proceedings of the International Astronomical Union
  • 2009
Abstract I review accretion and outflow in active galactic nuclei. Accreti4on appears to occur in a series of very small-scale, chaotic events, whose gas flows have no correlation with the

A 10,000-solar-mass black hole in the nucleus of a bulgeless dwarf galaxy

The motions of gas and stars in the nuclei of nearby galaxies have demonstrated that massive black holes are common1 and that their masses correlate with the stellar velocity dispersion σ★ of the

The evolution of black hole mass and spin in active galactic nuclei

It is concluded that supermassive black holes (SMBH) should on average spin moderately, with the mean value a decreasing slowly as the mass increases; SMBH coalescences leave little long-term effect on a; rare examples of massive holes with larger spin parameters could result from prograde coalescence withSMBHs of similar mass, and are most likely to be found in giant ellipticals.

Black hole feedback in the luminous quasar PDS 456

A signature in x-ray spectra of a strong persistent outflow in the quasar PDS 456 is seen, estimating a broad solid angle spanned by the wind that enables a far greater impact on the host galaxy than narrower jet outflows.

Black hole starvation and bulge evolution in a Milky Way-like galaxy

We present a new zoom-in hydrodynamical simulation, `ErisBH', which features the same initial conditions, resolution, and sub-grid physics as the close Milky Way-analogue `Eris' (Guedes et al. 2011),

Black Hole Outflows

I show that Eddington accretion episodes in active galactic nuclei (AGN) are likely to produce winds with velocities υ ~ 0.1c and ionization parameters up to ξ ~ 10 4 (cgs), implying the presence of

Radiative feedback from quasars and the growth of massive black holes in stellar spheroids

We discuss the importance of feedback via photoionization and Compton heating on the co-evolution of massive black holes (MBHs) at the centre of spheroidal galaxies, and their stellar and gaseous

Probing the Growth of Massive Black Holes with Black Hole–Host Galaxy Spin Correlations

Supermassive black holes are commonly found at the centers of their host galaxies, but their formation still remains an open question. In light of the tight correlation between the black hole (BH)

Correlations between supermassive black holes and hot gas atmospheres in IllustrisTNG and X-ray observations

Recent X-ray observations have revealed remarkable correlations between the masses of central supermassive black holes (SMBHs) and the X-ray properties of the hot atmospheres permeating their host

Correlations between supermassive black holes, hot atmospheres, and the total masses of early-type galaxies

We present a study of relations between the masses of the central supermassive black holes (SMBHs) and the atmospheric gas temperatures and luminosities measured within a range of radii between Re



High-redshift galaxies, their active nuclei and central black holes

We demonstrate that the luminosity function of the recently detected population of actively star-forming galaxies at redshift z = 3 and the B-band luminosity function of quasi-stellar objects (QSOs)


The mass density of massive black holes observed locally is consistent with the hard X-ray background provided that most of the radiation produced during their growth was absorbed by surrounding gas.

A Relationship between Nuclear Black Hole Mass and Galaxy Velocity Dispersion

We describe a correlation between the mass Mbh of a galaxy's central black hole and the luminosity-weighted line-of-sight velocity dispersion σe within the half-light radius. The result is based on a

Observational constraints on growth of massive black holes

We study the observational constraints on the growth of massive black holes (BHs) in galactic nuclei. We use the velocity dispersions of early-type galaxies obtained by the Sloan Digital Sky Survey

Cooling Flows and Quasars. II. Detailed Models of Feedback-modulated Accretion Flows

Most elliptical galaxies contain central black holes (BHs), and most also contain significant amounts of hot gas capable of accreting on to the central BH as a result of having cooling times that are

Cooling Flows and Quasars: Different Aspects of the Same Phenomenon? I. Concepts

We present a new class of solutions for the gas flows in elliptical galaxies containing massive central black holes (BHs). Modified King model galaxies are assumed. Two source terms operate: mass

A Fundamental Relation between Supermassive Black Holes and Their Host Galaxies

The masses of supermassive black holes correlate almost perfectly with the velocity dispersions of their host bulges, Mbh ∝ σα, where α = 4.8 ± 0.5. The relation is much tighter than the relation

The Slope of the Black Hole Mass versus Velocity Dispersion Correlation

Observations of nearby galaxies reveal a strong correlation between the mass of the central dark object MBH and the velocity dispersion σ of the host galaxy, of the form log(MBH/M☉) = α + β

Collisional dark matter and the origin of massive black holes

  • Ostriker
  • Physics
    Physical review letters
  • 2000
If the cosmological dark matter is primarily in the form of an elementary particle which has mass m(p) and cross section for self-interaction sigma, then seed black holes will grow in a Hubble time t(H) due to accretion of the dark matter to a mass, which produces massive black holes in the (10(6)-10(9) range observed.

Introduction to Stellar Winds

Preface 1. Historical overview 2. Observations of stellar winds 3. Basic concepts: isothermal winds 4. Basic concepts: non-isothermal winds 5. Coronal winds 6. Sound wave driven winds 7. Dust driven