Radiative feedback of low-Lbol/LEdd AGNs

2019 ◽  
Vol 15 (S356) ◽  
pp. 189-193
Author(s):  
Fu-Guo Xie
Keyword(s):  
Black Hole ◽  
Crucial Role ◽  
Radiative Heating ◽  
Host Galaxy ◽  
Radiative Feedback ◽  
Supermassive Black Hole ◽  
Kinetic Mode

AbstractAGN feedback, through either radiation or kinematics by expelled medium, plays a crucial role in the coevolution of supermassive black hole (SMBH) and its host galaxy. The nuclei spend most of their time as low-luminosity AGNs (LLAGNs), whose spectra are distinctive to bright AGNs, and the feedback is the hot mode (also named kinetic mode). We thus investigate the radiative heating in the hot mode. We calculate the value of “Compton temperature” Tc, which defines the heating capability of the radiation at given flux, and find that Tc∼(5−15)×107 K, depending on the spectrum of individual LLAGNs. This work provides a cheap way to include the radiative heating of LLAGNs in the study of AGN feedback.

scholarly journals Supermassive black hole mass regulated by host galaxy morphology

2009 ◽  
Vol 400 (4) ◽  
pp. 1803-1807 ◽  
Author(s):  
Y. Watabe ◽  
N. Kawakatu ◽  
M. Imanishi ◽  
T. T. Takeuchi
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Supermassive Black Hole ◽  
Galaxy Morphology

scholarly journals Study of central intensity ratio of early-type galaxies from low-density environment

2020 ◽  
Vol 500 (1) ◽  
pp. 1343-1349
Author(s):  
K Sruthi ◽  
C D Ravikumar
Keyword(s):  
Black Hole ◽  
Intensity Ratio ◽  
Velocity Dispersion ◽  
Host Galaxy ◽  
Low Density ◽  
Early Type ◽  
Central Intensity ◽  
Supermassive Black Hole

ABSTRACT We present correlations involving central intensity ratio (CIR) of 52 early-type galaxies, including 24 ellipticals and 28 lenticulars, selected from low-density environment in the nearby (<30 Mpc) universe. CIR is found to be negatively and significantly correlated with the mass of the central supermassive black hole, central velocity dispersion, absolute B-band magnitude, stellar bulge mass, and central Mg2 index of the host galaxy. The study proposes the use of CIR as a simple, fast, and efficient photometric tool for exploring the co-evolution scenario existing in galaxies.

scholarly journals Quasars, Feedback, and Galaxy Formation

2009 ◽  
Vol 5 (S267) ◽  
pp. 421-428
Author(s):  
Philip F. Hopkins
Keyword(s):  
Black Hole ◽  
Galaxy Evolution ◽  
Galaxy Formation ◽  
Theoretical Models ◽  
Light Curves ◽  
Host Galaxy ◽  
Host Galaxies ◽  
Supermassive Black Hole ◽  
Analytic Models ◽  
Black Hole Masses

AbstractRecent observations of tight correlations between supermassive black hole masses and the properties of their host galaxies demonstrate that black holes and bulges are co-eval and have motivated theoretical models in which feedback from AGN activity regulates the black hole and host galaxy evolution. Combining simulations, analytic models, and recent observations, answers to a number of questions are starting to take shape: how do AGN get triggered? How long do they live? What are typical light curves and what sets them? Is feedback necessary and/or sufficient to regulate BH growth? What effects does that feedback have on the host galaxy? On the host halo? All of this also highlights questions that remain wide open: how does gas get from a few pc to the AGN? What are the actual microphysical mechanisms of feedback? What is the tradeoff between stellar and AGN feedback? And, if there are different “modes” of feedback, where/when are each important?

scholarly journals Understanding the environment around the intermediate mass black hole candidate ESO 243-49 HLX-1

2017 ◽  
Vol 602 ◽  
pp. A103 ◽  
Author(s):  
N. A. Webb ◽  
A. Guérou ◽  
B. Ciambur ◽  
A. Detoeuf ◽  
M. Coriat ◽  
...  
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Intermediate Mass ◽  
Rotating Disc ◽  
Large Variability ◽  
Black Hole Candidate ◽  
Supermassive Black Hole ◽  
Flux Variability ◽  
The Galaxy ◽  
Multi Wavelength

Aims. ESO 243-49 HLX-1, otherwise known as HLX-1, is an intermediate mass black hole (IMBH) candidate located 8′′ (3.7 Kpc) from the centre of the edge-on S0 galaxy ESO 243-49. How the black hole came to be associated with this galaxy, and the nature of the environment in which it resides, remain unclear. Using multi-wavelength observations we aim to investigate the nature of the medium surrounding HLX-1, search for evidence of past mergers with ESO 243-49 and constrain parameters of the galaxy, including the mass of the expected central supermassive black hole, essential for future modelling of the interaction of the IMBH and ESO 243-49. Methods. We have reduced and analysed integral field unit observations of ESO 243-49 that were taken with the MUSE instrument on the VLT. Using complementary multi-wavelength data, including X-shooter, HST, Swift, Chandra and ATCA data, we have further examined the vicinity of HLX-1. We additionally examined the nature of the host galaxy and estimate the mass of the central supermassive black hole in ESO 243-49 using (black hole mass)–(host spheroid) scaling relations and the fundamental plane of black hole activity. Results. No evidence for a recent minor-merger that could result in the presence of the IMBH is discerned, but the data are compatible with a scenario in which minor mergers may have occurred in the history of ESO 243-49. The MUSE data reveal a rapidly rotating disc in the centre of the galaxy, around the supermassive black hole. The mass of the supermassive black hole at the centre of ESO 243-49 is estimated to be 0.5−23 × 107M⊙. Studying the spectra of HLX-1, that were taken in the low and hard state, we determine Hα flux variability to be at least a factor 6, compared to observations taken during the high and soft state. This Hα flux variability over one year indicates that the line originates close to the intermediate mass black hole, excluding the possibility that the line emanates from a surrounding nebula or a star cluster. The large variability associated with the X-ray states of HLX-1 confirms that the Hα line is associated with the object and therefore validates the distance to HLX-1.

scholarly journals Host Galaxy Bulge Predictors of Supermassive Black Hole Mass

2007 ◽  
Vol 665 (1) ◽  
pp. 120-156 ◽  
Author(s):  
M. C. Aller ◽  
D. O. Richstone
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Supermassive Black Hole

scholarly journals CO-EVOLUTION OF SUPERMASSIVE BLACK HOLE AND HOST GALAXY FROMz∼ 1 TOz= 0

2009 ◽  
Vol 696 (1) ◽  
pp. 1051-1062 ◽  
Author(s):  
Gaku Kiuchi ◽  
Kouji Ohta ◽  
Masayuki Akiyama
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Supermassive Black Hole

scholarly journals Constraining astrophysical observables of galaxy and supermassive black hole binary mergers using pulsar timing arrays

2019 ◽  
Vol 488 (1) ◽  
pp. 401-418 ◽  
Author(s):  
Siyuan Chen ◽  
Alberto Sesana ◽  
Christopher J Conselice
Keyword(s):  
Black Hole ◽  
Mass Function ◽  
Host Galaxy ◽  
Supermassive Black Hole ◽  
Pulsar Timing ◽  
Upper Limits ◽  
Binary Mergers ◽  
Black Hole Binary ◽  
Merger Rate ◽  
The Universe

ABSTRACT We present an analytic model to describe the supermassive black hole binary (SMBHB) merger rate in the Universe with astrophysical observables: galaxy stellar mass function, pair fraction, merger time-scale, and black hole–host galaxy relations. We construct observational priors and compute the allowed range of the characteristic spectrum hc of the gravitational wave background (GWB) to be 10−16 < hc < 10−15 at a frequency of f = 1 yr−1. We exploit our parametrization to tackle the problem of astrophysical inference from pulsar timing array (PTA) observations. We simulate a series of upper limits and detections and use a nested sampling algorithm to explore the parameter space. Corroborating previous results, we find that the current PTA non-detection does not place significant constraints on any observables; however, either future upper limits or detections will significantly enhance our knowledge of the SMBHB population. If a GWB is not detected at a level of hc(f = 1 yr−1) = 10−17, our current understanding of galaxy and SMBHB mergers is disfavoured at a 5σ level, indicating a combination of severe binary stalling, overestimating of the SMBH–host galaxy relations, and extreme dynamical properties of merging SMBHBs. Conversely, future detections of a Square Kilometre Array (SKA)-type instrument will allow to constrain the normalization of the SMBHB merger rate in the Universe, the time between galaxy pairing and SMBHB merging, the normalization of the SMBH–host galaxy relations and the dynamical binary properties, including their eccentricity and density of stellar environment.

Feeding and feedback in the nucleus of NGC 613

2019 ◽  
Vol 15 (S359) ◽  
pp. 364-365
Author(s):  
Patrícia da Silva ◽  
J. E. Steiner ◽  
R. B. Menezes
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Hii Regions ◽  
Stellar Populations ◽  
Host Galaxy ◽  
Molecular Gas ◽  
X Rays ◽  
Supermassive Black Hole ◽  
Feeding Process

AbstractActive Galactic Nuclei (AGN) are objects in which a supermassive black hole is fed by gas and, as this generates energy, can ionise the environment and interact with it by jets and winds. This work is focused on the processes of feeding and feedback in the nucleus of NGC 613. This object is a case in which both phenomena can be studied in some detail. The kinematics and morphology of the molecular gas trace the feeding process while the ionization cone, seen in [O iii]λ5007 and soft X-rays, as well as the radio jet and wind/outflows are associated with feedback processes. In addition, we see 10 HII regions, associated with nuclear and circumnuclear young stellar populations, dominant in the optical, that makes the analysis complicated, though more interesting. For all these phenomena, NGC 613 nucleus is a vibrant example of the interplay between the AGN and the host galaxy.

scholarly journals AGN mass estimates in large spectroscopic surveys: the effect of host galaxy light

2018 ◽  
Vol 618 ◽  
pp. A127 ◽  
Author(s):  
Ludovica Varisco ◽  
Tullia Sbarrato ◽  
Giorgio Calderone ◽  
Massimo Dotti
Keyword(s):  
Black Hole ◽  
Spectroscopic Analysis ◽  
Host Galaxy ◽  
Host Galaxies ◽  
Analysis Software ◽  
Supermassive Black Hole ◽  
Virial Mass ◽  
Fitting In ◽  
Black Hole Masses ◽  
Line Fitting

Virial–based methods for estimating active supermassive black hole masses are now commonly used on extremely large spectroscopic quasar catalogs. Most spectral analyses, though, do not pay enough attention to the detailed continuum decomposition. To understand how this affects virial mass estimates, we test the influence of host galaxy light on them, along with a Balmer continuum component. A detailed fit with the new spectroscopic analysis software QSFIT demonstrates that the presence or absence of continuum components does not significantly affect the virial-based results for our sample. Taking a host galaxy component into consideration or not, instead, affects the emission line fitting in a more pronounced way at lower redshifts, where in fact we observe dimmer quasars and more visible host galaxies.

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