Do massive black holes reside in elliptical galaxies?

Nature ◽  
1988 ◽  
Vol 333 (6176) ◽  
pp. 829-831 ◽  
Author(s):  
A. C. Fabian ◽  
C. R. Canizares
Keyword(s):  
Black Holes ◽  
Elliptical Galaxies ◽  
Massive Black Holes

scholarly journals Gaseous Disks in the Nuclei of Elliptical Galaxies

1997 ◽  
Vol 163 ◽  
pp. 620-625 ◽  
Author(s):  
H. Ford ◽  
Z. Tsvetanov ◽  
L. Ferrarese ◽  
G. Kriss ◽  
W. Jaffe ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Accretion Disks ◽  
Large Scale ◽  
Elliptical Galaxies ◽  
Central Mass ◽  
Massive Black Holes ◽  
Radio Jets

AbstractHST images have led to the discovery that small (r ~ 1″ r ~ 100 – 200 pc), well-defined, gaseous disks are common in the nuclei of elliptical galaxies. Measurements of rotational velocities in the disks provide a means to measure the central mass and search for massive black holes in the parent galaxies. The minor axes of these disks are closely aligned with the directions of the large–scale radio jets, suggesting that it is angular momentum of the disk rather than that of the black hole that determines the direction of the radio jets. Because the disks are directly observable, we can study the disks themselves, and investigate important questions which cannot be directly addressed with observations of the smaller and unresolved central accretion disks. In this paper we summarize what has been learned to date in this rapidly unfolding new field.

scholarly journals JD8 - Hot Interstellar Matter in Elliptical Galaxies

2009 ◽  
Vol 5 (H15) ◽  
pp. 269-270
Author(s):  
Dong-Woo Kim ◽  
Silvia Pellegrini
Keyword(s):  
Black Holes ◽  
Star Formation ◽  
Analytical Modeling ◽  
Elliptical Galaxies ◽  
Theoretical Studies ◽  
Interstellar Matter ◽  
Significant Progress ◽  
Massive Black Holes ◽  
X Ray ◽  
Formation And Evolution

The physical properties of the hot interstellar matter in elliptical galaxies are directly related with the formation and evolution of elliptical galaxies via star formation episodes, environmental effects such as stripping, infall, and mergers, and growth of super-massive black holes. The recent successful Chandra and XMM-Newton X-ray space missions have provided a large amount of high spatial/spectral resolution observational data on the hot ISM in elliptical galaxies. At the same time, theoretical studies with numerical simulations and analytical modeling of the dynamical and chemical evolution of elliptical galaxies have made a significant progress and start to predict various observable quantities.

scholarly journals Central Black Holes and Dark Halos in Elliptical Galaxies

1995 ◽  
Vol 164 ◽  
pp. 215-225
Author(s):  
P.T. De Zeeuw
Keyword(s):  
Black Holes ◽  
Dark Matter ◽  
Recent Work ◽  
Stellar Populations ◽  
Elliptical Galaxies ◽  
Massive Black Holes ◽  
Area Of Interest

Studies of the mass–to–light ratio M/L as a function of radius in a galaxy usually focus on: a) the existence of dark matter in and around galaxies, and b) the presence of massive black holes in their nuclei. Here we concentrate on elliptical galaxies, and summarize some recent work in both areas. We refer to more extensive reviews for earlier developments (Schwarzschild, 1954; Trimble, 1987; Ashman, 1992; Kormendy, 1993). A third area of interest is the behavior of the stellar populations as a function of radius, and its effect on M/L (e.g., Peletier, 1989). We will not discuss this here.

scholarly journals Relics of Nuclear Activity: Do All Galaxies Have Massive Black Holes?

1999 ◽  
Vol 186 ◽  
pp. 333-340
Author(s):  
Roeland P. van der Marel
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Growth Models ◽  
Elliptical Galaxies ◽  
Large Scatter ◽  
Nuclear Activity ◽  
Massive Black Holes ◽  
The Core ◽  
Kinematic Studies ◽  
Kinematical Data

The distribution of black hole (BH) masses M• in galaxies is constrained by photometric and kinematic studies of individual galaxies, and by the properties of the quasar population. I review our understanding of these topics, present new results of adiabatic BH growth models for HST photometry of elliptical galaxies with brightness profiles of the ‘core’ type, and discuss the implications of ground-based stellar kinematical data. It is not yet possible to uniquely determine the BH mass distribution, but the available evidence is not inconsistent with a picture in which: (i) a majority of galaxies has BHs; (ii) there is a correlation (with large scatter) between M• and spheroid luminosity Lsph of the form M• ≈ 10−2Lsph (solar B-band units); and (iii) the BHs formed in a quasar phase through mass accretion with efficiency ε ≈ 0.05.

scholarly journals The Masses of Nuclear Black Holes in Luminous Elliptical Galaxies and Implications for the Space Density of the Most Massive Black Holes

2007 ◽  
Vol 662 (2) ◽  
pp. 808-834 ◽  
Author(s):  
Tod R. Lauer ◽  
S. M. Faber ◽  
Douglas Richstone ◽  
Karl Gebhardt ◽  
Scott Tremaine ◽  
...  
Keyword(s):  
Black Holes ◽  
Elliptical Galaxies ◽  
Space Density ◽  
Massive Black Holes ◽  
The Masses

scholarly journals X-ray properties of reverberation-mapped AGNs with super-Eddington accreting massive black holes

2019 ◽  
Vol 15 (S356) ◽  
pp. 143-143
Author(s):  
Jaya Maithil ◽  
Michael S. Brotherton ◽  
Bin Luo ◽  
Ohad Shemmer ◽  
Sarah C. Gallagher ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Accretion Rate ◽  
Time Lags ◽  
Black Hole Mass ◽  
Host Galaxies ◽  
Massive Black Holes ◽  
X Ray ◽  
Photon Index ◽  
The Impact

AbstractActive Galactic Nuclei (AGN) exhibit multi-wavelength properties that are representative of the underlying physical processes taking place in the vicinity of the accreting supermassive black hole. The black hole mass and the accretion rate are fundamental for understanding the growth of black holes, their evolution, and the impact on the host galaxies. Recent results on reverberation-mapped AGNs show that the highest accretion rate objects have systematic shorter time-lags. These super-Eddington accreting massive black holes (SEAMBHs) show BLR size 3-8 times smaller than predicted by the Radius-Luminosity (R-L) relationship. Hence, the single-epoch virial black hole mass estimates of highly accreting AGNs have an overestimation of a factor of 3-8 times. SEAMBHs likely have a slim accretion disk rather than a thin disk that is diagnostic in X-ray. I will present the extreme X-ray properties of a sample of dozen of SEAMBHs. They indeed have a steep hard X-ray photon index, Γ, and demonstrate a steeper power-law slope, ασx.

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