scholarly journals Co-evolution of bulges and black holes

2007 ◽  
Vol 3 (S245) ◽  
pp. 223-226 ◽  
Author(s):  
Jong-Hak Woo ◽  
Tommaso Treu ◽  
Matthew A. Malkan ◽  
Roger D. Blandford
Keyword(s):  
Black Holes ◽  
Galaxy Evolution ◽  
Velocity Dispersion ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Host Galaxies ◽  
Nuclear Activity ◽  
The Past ◽  
Global Properties ◽  
Direct Measurements

AbstractIn the present-day universe, the global properties of bulges and early-type galaxies correlate with the mass of their central black holes, indicating a connection between galaxy evolution and nuclear activity. Understanding the origin of this relation is a major challenge for cosmological models. Using Keck spectra and HST images, we present direct measurements of the correlations between black hole mass and host spheroid luminosity and velocity dispersion at z=0.36, showing that the relations evolved significantly in the past 4 billion years. It appears that black holes of a few 108M⊙completed their growth before their host galaxies, and that the current scaling relations are only the final point of the co-evolution of galaxies and black holes.

scholarly journals Coevolution (or not) of supermassive black holes and host galaxies: Black hole scaling relations are not biased by selection effects

2019 ◽  
Vol 14 (S353) ◽  
pp. 186-198
Author(s):  
John Kormendy
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Velocity Dispersion ◽  
Stellar Mass ◽  
Supermassive Black Holes ◽  
Scaling Relations ◽  
Selection Effects ◽  
Host Galaxies ◽  
Scatter Plots ◽  
Host Properties

AbstractThe oral version of this paper summarized Kormendy & Ho 2013, ARA&A, 51, 511. However, earlier speakers at this Symposium worried that selection effects bias the derivation of black hole scaling relations. I therefore added – and this proceedings paper emphasizes – a discussion of why we can be confident that selection effects do not bias the observed correlations between BH mass M• and the luminosity, stellar mass, and velocity dispersion of host ellipticals and classical bulges. These are the only galaxy components that show tight BH-host correlations. The scatter plots of M• with host properties for pseudobulges and disks are upper envelopes of scatter that does extend to lower BH masses. BH correlations are most consistent with a picture in which BHs coevolve only with classical bulges and ellipticals. Four physical regimes of coevolution (or not) are suggested by Kormendy & Ho 2013 and are summarized here.

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.

An accreting < 105M⊙ black hole at the center of dwarf galaxy IC750

2019 ◽  
Vol 15 (S356) ◽  
pp. 376-376
Author(s):  
Ingyin Zaw
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dwarf Galaxies ◽  
Dwarf Galaxy ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Host Galaxies ◽  
Seed Formation ◽  
Maser Emission ◽  
Water Masers

AbstractNuclear black holes in dwarf galaxies are important for understanding the low end of the supermassive black hole mass distribution and the black hole-host galaxy scaling relations. IC 750 is a rare system which hosts an AGN, found in ˜0.5% of dwarf galaxies, with circumnuclear 22 GHz water maser emission, found in ˜3–5% of Type 2 AGNs. Water masers, the only known tracer of warm, dense gas in the center parsec of AGNs resolvable in position and velocity, provide the most precise and accurate mass measurements of SMBHs outside the local group. We have mapped the maser emission in IC 750 and find that it traces a nearly edge-on warped disk, 0.2 pc in diameter. The central black hole has an upper limit mass of ˜1 × 105 M⊙ and a best fit mass of ˜8 × 104 M⊙, one to two orders of magnitude below what is expected from black hole-galaxy scaling relations. This has implications for models of black hole seed formation in the early universe, the growth of black holes, and their co-evolution with their host galaxies.

A LOCAL BASELINE OF THE BLACK HOLE MASS SCALING RELATIONS FOR ACTIVE GALAXIES. II. MEASURING STELLAR VELOCITY DISPERSION IN ACTIVE GALAXIES

2012 ◽  
Vol 201 (2) ◽  
pp. 29 ◽  
Author(s):  
Chelsea E. Harris ◽  
Vardha N. Bennert ◽  
Matthew W. Auger ◽  
Tommaso Treu ◽  
Jong-Hak Woo ◽  
...  
Keyword(s):  
Black Hole ◽  
Velocity Dispersion ◽  
Active Galaxies ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Mass Scaling ◽  
Stellar Velocity

scholarly journals Galaxy Scaling Relations as a Result of Secular Evolution

2004 ◽  
Vol 220 ◽  
pp. 417-418
Author(s):  
Xiaolei Zhang
Keyword(s):  
Galaxy Evolution ◽  
Morphological Evolution ◽  
Evolution Process ◽  
Scaling Relations ◽  
Secular Evolution ◽  
The Past

The secular evolution process which slowly transforms the morphology of a given galaxy over its lifetime through mostly internal dynamical mechanisms could naturally account for most of the observed properties of physical galaxies (Zhang 2003a). As an emerging paradigm for galaxy evolution, its dynamical foundations had been established in the past few years (Zhang 1996, 1998, 1999). in this paper, we explore further implications of the secular morphological evolution process in reproducing the well-known scaling relations of galaxies.

scholarly journals C iv black hole mass measurements with the Australian Dark Energy Survey (OzDES)

2019 ◽  
Vol 487 (3) ◽  
pp. 3650-3663 ◽  
Author(s):  
J K Hoormann ◽  
P Martini ◽  
T M Davis ◽  
A King ◽  
C Lidman ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dark Energy ◽  
Emission Line ◽  
Galaxy Evolution ◽  
Supermassive Black Holes ◽  
Black Hole Mass ◽  
Mass Measurements ◽  
Dark Energy Survey ◽  
Energy Survey

ABSTRACT Black hole mass measurements outside the local Universe are critically important to derive the growth of supermassive black holes over cosmic time, and to study the interplay between black hole growth and galaxy evolution. In this paper, we present two measurements of supermassive black hole masses from reverberation mapping (RM) of the broad C iv emission line. These measurements are based on multiyear photometry and spectroscopy from the Dark Energy Survey Supernova Program (DES-SN) and the Australian Dark Energy Survey (OzDES), which together constitute the OzDES RM Program. The observed reverberation lag between the DES continuum photometry and the OzDES emission line fluxes is measured to be $358^{+126}_{-123}$ and $343^{+58}_{-84}$ d for two quasars at redshifts of 1.905 and 2.593, respectively. The corresponding masses of the two supermassive black holes are 4.4 × 109 and 3.3 × 109 M⊙, which are among the highest redshift and highest mass black holes measured to date with RM studies. We use these new measurements to better determine the C iv radius−luminosity relationship for high-luminosity quasars, which is fundamental to many quasar black hole mass estimates and demographic studies.

scholarly journals The extended gas halo of QSO host galaxies

2012 ◽  
Vol 8 (S295) ◽  
pp. 56-56 ◽  
Author(s):  
R. Falomo ◽  
E. P. Farina ◽  
R. Decarli ◽  
A. Treves ◽  
J. Kotilainen
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Significant Enhancement ◽  
Line Of Sight ◽  
Host Galaxies ◽  
Nuclear Activity ◽  
Massive Galaxies ◽  
Gas Accretion ◽  
Absorption Features

AbstractWe investigate the MgII 2800 and CIV 1540 absorption features of the gas in the halo of a foreground QSO through the absorption imprinting on the spectra of a background QSO that is closely aligned with the nearest quasar. We present the results for 13 QSO pairs (0.7 < z < 2.2) that allow us to probe the gas at distances between 60 kpc and 120 kpc from the QSO nucleus. We identify absorption features associated with the foreground QSO in 7 out of 10 systems for MgII, and one out of 3 for CIV (see example in Fig. 1). At variance with the case of inactive and less massive galaxies we find that relatively strong (EW ~ 1 Ang) absorption features are present out to a radius of 100 kpc. This suggests that a large extended halo is associated with massive galaxies.The comparison of these results with those for inactive (not hosting active black holes) galaxies (see e.g. Chen et al. 2010a) shows that the halo of QSOs is similar to that of inactive galaxies. In the observed sample we do not detect a significant enhancement of the absorption strengths, as it could be expected if the QSO nuclear activity were driven by intense gas accretion onto the black hole. Moreover along the line of sight of the QSO we do not detect any Mg II absorbers of the same strength of the transverse one. These results are in agreement with models that consider a non-isotropic emission of the QSO, which are hosted by massive gaseous halos.

scholarly journals A FUNDAMENTAL EQUATION FOR SUPERMASSIVE BLACK HOLES

2011 ◽  
Vol 20 (12) ◽  
pp. 2305-2315 ◽  
Author(s):  
ANTONIO FEOLI ◽  
LUIGI MANCINI
Keyword(s):  
Black Holes ◽  
Angular Momentum ◽  
Scaling Laws ◽  
Velocity Dispersion ◽  
Fundamental Equation ◽  
Supermassive Black Holes ◽  
Host Galaxies ◽  
Starting Point ◽  
Interstellar Material ◽  
Energy And Momentum

We developed a theoretical model that is able to give a common origin to the correlations between the mass M• of supermassive black holes and the mass, velocity dispersion, kinetic energy and momentum parameter of the corresponding host galaxies. Our model is essentially based on the transformation of the angular momentum of the interstellar material, which falls into the black hole, into the angular momentum of the radiation emitted in this process. In this framework, we predict the existence of a relation of the form M• ∝ R e σ3, which is confirmed by the experimental data and can be the starting point to understand the other popular scaling laws too.

scholarly journals Time-average properties of z ∼ 0.6 major mergers: mergers significantly scatter high-z scaling relations

2019 ◽  
Vol 488 (1) ◽  
pp. 876-893 ◽  
Author(s):  
M Puech ◽  
H Flores ◽  
M Rodrigues ◽  
F Hammer ◽  
Y B Yang
Keyword(s):  
Velocity Dispersion ◽  
Scaling Relations ◽  
Gas Velocity ◽  
The Past ◽  
Gravitational Perturbations ◽  
Self Consistent ◽  
Major Merger ◽  
Consistent Picture ◽  
Time Average ◽  
Kinematic Properties

Abstract Interpreting the scaling relations measured by recent large kinematic surveys of z ≲ 1 galaxies has remained hampered by large observational scatter. We show that the observed ISM and morpho-dynamical properties along the average z ∼ 0.6 major merger describe a very self-consistent picture in which star formation is enhanced during first passage and fusion as a result of gravitational perturbations due to the interaction, while the gas velocity dispersion is simultaneously enhanced through shocks that convert kinematic energy associated with bulk orbital motions into turbulence at small scales. Angular momentum and rotation support in the disc are partly lost during the most perturbing phases, resulting in a morphologically compact phase. The fractions of present-day E/S0 versus later type galaxies can be predicted within only a few per cent, confirming that roughly half of local discs were reformed in the past 8–9 Gyr after gas-rich major mergers. Major mergers are shown to strongly scatter scaling relations involving kinematic quantities (e.g. the Tully–Fisher or Fall relations). Selecting high-z discs relying only on V/σ turns out to be less efficient than selecting discs from multiple criteria based on their morpho-kinematic properties, which can reduce the scatter of high-z scaling relations down to the values measured in local galaxy samples.

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