scholarly journals AGN feedback in numerical simulations

2009 ◽  
Vol 5 (H15) ◽  
pp. 293-293
Author(s):  
Luca Ciotti
Keyword(s):  
Black Hole ◽  
Numerical Simulations ◽  
Stellar Population ◽  
Cosmic Time ◽  
Elliptical Galaxies ◽  
Stellar Mass ◽  
Feedback Effects ◽  
Supermassive Black Hole ◽  
Physically Based ◽  
Continuous Source

AbstractThe passively evolving stellar population in elliptical galaxies (Es) provides a continuous source of fuel for accretion on the central supermassive black hole (SMBH), which is 1) extended over the entire galaxy life (but declining with cosmic time), 2) linearly proportional to the stellar mass of the host spheroid, 3) summing up to a total gas mass that is > 100 times larger than the currently observed SMBH masses, 4) available independently of merging events. The main results of numerical simulations of Es with central SMBH, in which a physically based implementation of radiative and mechanical feedback effects is considered, are presented.

scholarly journals Evolution of Merger Remnants with Supermassive Black Holes

2003 ◽  
Vol 208 ◽  
pp. 455-456
Author(s):  
Jeremy Tinker ◽  
Barbara Ryden
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Numerical Simulations ◽  
Spiral Galaxies ◽  
Elliptical Galaxies ◽  
Supermassive Black Holes ◽  
Host Galaxies ◽  
Supermassive Black Hole

We present results of numerical simulations of mergers of spiral galaxies using GADGET (Springel, Yoshida, & White 2001). In three of these simulations one of the progenitor galaxies contained a central supermassive black hole (BH), as well as one simulation which did not contain a BH. The merger remnants were evolved to an age of ∼ 13 Gyr to examine the evolution of the shape of each merger remnant. The results of these simulations were compared to observations of elliptical galaxies, which show that older galaxies appear rounder than younger ones (Ryden, Forbes, & Terlevich 2001).We found that the simulations in which the BH mass was fixed throughout the evolution influence the shape of their host galaxies on timescales less than 3 Gyr. These simulations show little trend of shape with age beyond this time. In the simulations in which the BH mass increased linearly over the duration of the simulation, there is a significant evolution of the shape of the remnant throughout its lifetime, comparable to the observational trend.

scholarly journals SUPERMASSIVE BLACK HOLE GROWTH IN STARBURST GALAXIES OVER COSMIC TIME: CONSTRAINTS FROM THE DEEPESTCHANDRAFIELDS

2011 ◽  
Vol 742 (1) ◽  
pp. 3 ◽  
Author(s):  
D. A. Rafferty ◽  
W. N. Brandt ◽  
D. M. Alexander ◽  
Y. Q. Xue ◽  
F. E. Bauer ◽  
...  
Keyword(s):  
Black Hole ◽  
Cosmic Time ◽  
Starburst Galaxies ◽  
Time Constraints ◽  
Supermassive Black Hole ◽  
Black Hole Growth ◽  
Hole Growth

scholarly journals The supermassive black hole coincident with the luminous transient ASASSN-15lh

2018 ◽  
Vol 610 ◽  
pp. A14 ◽  
Author(s):  
T. Krühler ◽  
M. Fraser ◽  
G. Leloudas ◽  
S. Schulze ◽  
N. C. Stone ◽  
...  
Keyword(s):  
Black Hole ◽  
Stellar Population ◽  
Physical Nature ◽  
Central Component ◽  
Narrow Line ◽  
Host Galaxies ◽  
Ionization Source ◽  
Supermassive Black Hole ◽  
Gas Kinematics ◽  
Spatially Resolved

The progenitors of astronomical transients are linked to a specific stellar population and galactic environment, and observing their host galaxies hence constrains the physical nature of the transient itself. Here, we use imaging from the Hubble Space Telescope, and spatially resolved, medium-resolution spectroscopy from the Very Large Telescope obtained with X-shooter and MUSE to study the host of the very luminous transient ASASSN-15lh. The dominant stellar population at the transient site is old (around 1 to 2 Gyr) without signs of recent star formation. We also detect emission from ionized gas, originating from three different, time invariable, narrow components of collisionally excited metal and Balmer lines. The ratios of emission lines in the Baldwin-Phillips-Terlevich diagnostic diagram indicate that the ionization source is a weak active galactic nucleus with a black hole mass of M• = 5-3+8 × 108 M⊙, derived through the M•-σ relation. The narrow line components show spatial and velocity offsets on scales of 1 kpc and 500 km s-1, respectively; these offsets are best explained by gas kinematics in the narrow-line region. The location of the central component, which we argue is also the position of the supermassive black hole, aligns with that of the transient within an uncertainty of 170 pc. Using this positional coincidence as well as other similarities with the hosts of tidal disruption events, we strengthen the argument that the transient emission observed as ASASSN-15lh is related to the disruption of a star around a supermassive black hole, most probably spinning with a Kerr parameter a• ≳ 0.5.

scholarly journals A black hole fundamental plane

2007 ◽  
Vol 3 (S245) ◽  
pp. 219-222
Author(s):  
Philip F. Hopkins
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Elliptical Galaxies ◽  
Simple Relation ◽  
Host Galaxies ◽  
Fundamental Plane ◽  
Supermassive Black Hole ◽  
The Masses

AbstractWe study observed correlations between supermassive black hole (BHs) and the properties of their host galaxies, and show that the observations define a BH “fundamental plane” (BHFP), of the form $\mbh\propto\sigma^{3.0\pm0.3}\,\re^{0.43\pm0.19}$ or $\mbh\propto\mstar^{0.54\pm0.17}\,\sigma^{2.2\pm0.5}$, analogous to the FP of elliptical galaxies. The BHFP is preferred over a simple relation between MBH and any of σ, M*, Mdyn, or Re alone at > 3 σ (99.9%) significance. The existence of this BHFP has important implications for the formation of supermassive BHs and the masses of the very largest black holes, and immediately resolves several apparent conflicts between the BH masses expected and measured for outliers in both the MBH − σ and MBH − M* relations.

scholarly journals Feedback in the Dark Domain

2009 ◽  
Vol 5 (S267) ◽  
pp. 362-369
Author(s):  
Keiichi Wada
Keyword(s):  
Black Hole ◽  
High Resolution ◽  
Interstellar Medium ◽  
Numerical Simulations ◽  
Dynamical Effect ◽  
Theoretical Knowledge ◽  
X Ray ◽  
Supermassive Black Hole

AbstractIn order to clarify the physics of AGN feedback and feeding, we need to understand the interstellar medium (ISM) in the central several tens of parsecs in galaxies where our observational and theoretical knowledge is relatively poor. Here we discuss feedback processes due to strong far UV and X-ray radiation, as well as the dynamical effect of a supermassive black hole (SMBH) based on new high-resolution numerical simulations of the ISM in the central R ≤ 32 pc region around a SMBH at the center of a galaxy.

scholarly journals Star formation history and isophotal shapes of fossil central galaxies

2007 ◽  
Vol 3 (S245) ◽  
pp. 81-82
Author(s):  
Habib G. Khosroshahi ◽  
Louisa A. Nolan
Keyword(s):  
Star Formation ◽  
Numerical Simulations ◽  
Stellar Population ◽  
Stellar Populations ◽  
Elliptical Galaxies ◽  
Star Formation History ◽  
Spectral Fitting ◽  
Stellar Component ◽  
Formation History ◽  
Two Component

AbstractWe study the structure and stellar populations of the luminous elliptical galaxies dominating fossil groups and compare them with the brightest galaxies in ordinary groups. Despite being over-luminous, the fossil central galaxies do not show boxy stellar isophotes which are usually associated with luminous elliptical galaxies. Boxy isophotes, according to the numerical simulations, are produced in gas poor mergers. The isophotal shapes of the fossil central galaxies, therefore, suggest a gas rich merger for fossil central galaxies. Using a two-component spectral fitting, we show that the dominant stellar population of the fossil and non-fossil galaxies is old and the second population is either old or intermediate age. However, the second stellar component (recently-formed stars) in fossil central galaxies is significantly more metal poor than that in the brightest galaxies of non-fossil groups.

scholarly journals The supermassive black hole mass–Sérsic index relations for bulges and elliptical galaxies

2013 ◽  
Vol 434 (1) ◽  
pp. 387-397 ◽  
Author(s):  
G. Savorgnan ◽  
A. W. Graham ◽  
A. Marconi ◽  
E. Sani ◽  
L. K. Hunt ◽  
...  
Keyword(s):  
Black Hole ◽  
Elliptical Galaxies ◽  
Black Hole Mass ◽  
Supermassive Black Hole
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