scholarly journals The fundamental relation between supermassive black holes and their host galaxies

2019 ◽  
Vol 490 (1) ◽  
pp. 600-612 ◽  
Author(s):  
Stefano de Nicola ◽  
Alessandro Marconi ◽  
Giuseppe Longo
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
Fundamental Relation ◽  
Host Galaxies ◽  
Fundamental Plane ◽  
Secular Evolution ◽  
Spatially Resolved ◽  
Effective Velocity ◽  
Novel Approach ◽  
Natural Outcome

ABSTRACT We study the correlations between supermassive black holes (BHs) and their host galaxies, using a sample of 83 BH masses collected from the most recent and reliable spatially resolved estimates available from the literature. We confirm the mono- and bivariate correlations between SMBHs and the bulges of their host galaxies, confirming that the correlation with the effective velocity dispersion is not significantly improved by higher dimensionality. Instead, pseudo-bulges do not seem to correlate with their SMBHs, probably because their secular evolution is often unable to trigger accretion onto the central BH. We then present a novel approach aimed at finding the fundamental relation between SMBHs and their host galaxies. For the first time, we analytically combine BH masses with the Fundamental Plane (FP), showing that MBH–σe appears to be the fundamental relation rather than a putative ‘BH Fundamental Plane’ of the kind MBH–σe–Re. These results can be explained by a picture which sees the MBH–σe relation as a natural outcome of the change in AGN feedback from momentum-driven to energy-driven. The other scaling relations are then established through the FP.

scholarly journals A Fundamental Relation between Compact Stellar Nuclei, Supermassive Black Holes, and Their Host Galaxies

2006 ◽  
Vol 644 (1) ◽  
pp. L21-L24 ◽  
Author(s):  
Laura Ferrarese ◽  
Patrick Côté ◽  
Elena Dalla Bontà ◽  
Eric W. Peng ◽  
David Merritt ◽  
...  
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
Fundamental Relation ◽  
Host Galaxies

scholarly journals The ALMA view of the high-redshift relation between supermassive black holes and their host galaxies

2020 ◽  
Vol 637 ◽  
pp. A84 ◽  
Author(s):  
A. Pensabene ◽  
S. Carniani ◽  
M. Perna ◽  
G. Cresci ◽  
R. Decarli ◽  
...  
Keyword(s):  
Black Holes ◽  
High Redshift ◽  
Line Emission ◽  
Supermassive Black Holes ◽  
Host Galaxies ◽  
Local Universe ◽  
Dynamical Mass ◽  
Gas Kinematics ◽  
Spatially Resolved ◽  
Galaxy Masses

Context. The existence of tight correlations between supermassive black holes (BHs) and their host galaxies’ properties in the local Universe suggests a closely linked evolution. Investigating these relations up to the high redshifts (z ≳ 6) is crucial in order to understand the interplay between star formation and BH growth across the cosmic time and to set constraints on galaxy formation and evolution models. In this work, we focus on the relation between BH mass (MBH) and the dynamical mass (Mdyn) of the host galaxy. Aims. Previous works suggest an evolution of the MBH−Mdyn relation with redshift indicating that BH growth precedes the galaxy mass assembly during their co-evolution at z >  3. However, dynamical galaxy masses at high redshift are often estimated through the virial theorem, thus introducing significant uncertainties. Within the scope of this work, our aim is to study the MBH−Mdyn relation of a sample of 2 <  z <  7 quasars by constraining their galaxy masses through a full kinematical modelling of the cold gas kinematics, thus avoiding all possible biases and effects introduced by the rough estimates usually adopted so far. Methods. For this purpose, we retrieved public observations of 72 quasar host galaxies observed in [CII]158 μm or CO transitions with the Atacama Large Millimeter Array (ALMA). We then selected those quasars whose line emission is spatially resolved, and performed a kinematic analysis on ALMA observations. We estimated the dynamical mass of the systems by modelling the gas kinematics with a rotating disc, taking into account geometrical and instrumental effects. Our dynamical mass estimates, combined with MBH obtained from literature and our own new CIVλ1550 observations allowed us to investigate the MBH/Mdyn in the early Universe. Results. Overall, we obtained a sample of ten quasars at z ∼ 2−7, in which line emission is detected with high S/N (≳5−10) and the gas kinematics are spatially resolved and dominated by ordered rotation. The estimated dynamical masses place six out of ten quasars above the local relation yielding to MBH/Mdyn ratios ∼10× higher than those estimated in low-z galaxies. On the other hand, we found that four quasars at z ∼ 4−6 have dynamical-to-BH-mass ratios consistent with what is observed in early-type galaxies in the local Universe.

scholarly journals Nuclear star clusters

2009 ◽  
Vol 5 (S266) ◽  
pp. 58-63 ◽  
Author(s):  
Torsten Böker
Keyword(s):  
Black Holes ◽  
Structural Properties ◽  
Galaxy Evolution ◽  
Globular Clusters ◽  
Star Clusters ◽  
Supermassive Black Holes ◽  
Subsequent Growth ◽  
Local Universe ◽  
Fundamental Plane ◽  
Evolutionary Connection

AbstractThe centers of most galaxies in the local Universe are occupied by compact, barely resolved sources. Based on their structural properties, position in the Fundamental Plane, and integrated spectra, these sources clearly have a stellar origin. They are therefore called ‘nuclear star clusters’ (NCs) or ‘stellar nuclei’. NCs are found in galaxies of all Hubble types, suggesting that their formation is intricately linked to galaxy evolution. Here, I review some recent studies of NCs, describe ideas for their formation and subsequent growth, and touch on their possible evolutionary connection with both supermassive black holes and globular clusters.

scholarly journals Feedback from supermassive black holes transforms centrals into passive galaxies by ejecting circumgalactic gas

2019 ◽  
Vol 491 (2) ◽  
pp. 2939-2952 ◽  
Author(s):  
Benjamin D Oppenheimer ◽  
Jonathan J Davies ◽  
Robert A Crain ◽  
Nastasha A Wijers ◽  
Joop Schaye ◽  
...  
Keyword(s):  
Black Holes ◽  
Binding Energy ◽  
Strong Predictor ◽  
Supermassive Black Holes ◽  
Gas Content ◽  
Hydrodynamic Simulation ◽  
Star Forming ◽  
Secular Evolution ◽  
Gas Accretion ◽  
The Relationship

ABSTRACT Davies et al. established that for L* galaxies the fraction of baryons in the circumgalactic medium (CGM) is inversely correlated with the mass of their central supermassive black holes (BHs) in the EAGLE hydrodynamic simulation. The interpretation is that, over time, a more massive BH has provided more energy to transport baryons beyond the virial radius, which additionally reduces gas accretion and star formation. We continue this research by focusing on the relationship between the (1) BH masses (MBH), (2) physical and observational properties of the CGM, and (3) galaxy colours for Milky Way-mass systems. The ratio of the cumulative BH feedback energy over the gaseous halo binding energy is a strong predictor of the CGM gas content, with BHs injecting significantly higher than the binding energy resulting in gas-poor haloes. Observable tracers of the CGM, including $\rm {C\, \small{IV}}$, $\rm {O\, \small{VI}}$, and ${\rm {H\, \small{I}}}$ absorption line measurements, are found to be effective tracers of the total z ∼ 0 CGM halo mass. We use high-cadence simulation outputs to demonstrate that BH feedback pushes baryons beyond the virial radius within 100 Myr time-scales, but that CGM metal tracers take longer (0.5–2.5 Gyr) to respond. Secular evolution of galaxies results in blue, star-forming or red, passive populations depending on the cumulative feedback from BHs. The reddest quartile of galaxies with M* = 1010.2−10.7 M⊙ (median u − r = 2.28) has a CGM mass that is 2.5 times lower than the bluest quartile (u − r = 1.59). We propose observing strategies to indirectly ascertain fCGM via metal lines around galaxies with measured MBH. We predict statistically detectable declines in $\rm {C\, \small{IV}}$ and $\rm {O\, \small{VI}}$ covering fractions with increasing MBH for central galaxies with M* = 1010.2−10.7M⊙.

scholarly journals Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). VIII. A less biased view of the early co-evolution of black holes and host galaxies

2019 ◽  
Vol 71 (6) ◽  
Author(s):  
Takuma Izumi ◽  
Masafusa Onoue ◽  
Yoshiki Matsuoka ◽  
Tohru Nagao ◽  
Michael A Strauss ◽  
...  
Keyword(s):  
Black Holes ◽  
Far Infrared ◽  
Supermassive Black Holes ◽  
Host Galaxies ◽  
Star Forming ◽  
Wide Range ◽  
The Galaxy ◽  
Order Of Magnitude ◽  
Local Relation ◽  
Almost All

Abstract We present ALMA [C ii] line and far-infrared (FIR) continuum observations of three $z \gt 6$ low-luminosity quasars ($M_{\rm 1450} \gt -25$ mag) discovered by our Subaru Hyper Suprime-Cam (HSC) survey. The [C ii] line was detected in all three targets with luminosities of $(2.4\mbox{--}9.5) \times 10^8\, L_{\odot }$, about one order of magnitude smaller than optically luminous ($M_{\rm 1450} \lesssim -25$ mag) quasars. The FIR continuum luminosities range from $\lt 9 \times 10^{10}\, L_{\odot }$ (3 $\sigma$ limit) to ${\sim } 2 \times 10^{12}\, L_{\odot }$, indicating a wide range in star formation rates in these galaxies. Most of the HSC quasars studied thus far show [C ii]/ FIR luminosity ratios similar to local star-forming galaxies. Using the [C ii]-based dynamical mass ($M_{\rm dyn}$) as a surrogate for bulge stellar mass ($M_{\rm\, bulge}$), we find that a significant fraction of low-luminosity quasars are located on or even below the local $M_{\rm\, BH}$–$M_{\rm\, bulge}$ relation, particularly at the massive end of the galaxy mass distribution. In contrast, previous studies of optically luminous quasars have found that black holes are overmassive relative to the local relation. Given the low luminosities of our targets, we are exploring the nature of the early co-evolution of supermassive black holes and their hosts in a less biased way. Almost all of the quasars presented in this work are growing their black hole mass at a much higher pace at $z \sim 6$ than the parallel growth model, in which supermassive black holes and their hosts grow simultaneously to match the local $M_{\rm\, BH}$–$M_{\rm\, bulge}$ relation at all redshifts. As the low-luminosity quasars appear to realize the local co-evolutionary relation even at $z \sim 6$, they should have experienced vigorous starbursts prior to the currently observed quasar phase to catch up with the relation.

Coevolution of supermassive black holes and their host galaxies

2008 ◽  
Author(s):  
J. K. Kotilainen ◽  
R. Decarli ◽  
R. Falomo ◽  
M. Labita ◽  
R. Scarpa ◽  
...  
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
Host Galaxies

scholarly journals Supermassive black holes: Coevolution (or not) of black holes and host galaxies

2012 ◽  
Vol 8 (S295) ◽  
pp. 241-256
Author(s):  
John Kormendy
Keyword(s):  
Black Holes ◽  
Galaxy Formation ◽  
Globular Clusters ◽  
Hubble Space Telescope ◽  
Supermassive Black Holes ◽  
Host Galaxy ◽  
Late Time ◽  
Host Galaxies ◽  
Energy Feedback ◽  
Negative Effect

AbstractSupermassive black holes (BHs) have been found in 75 galaxies by observing spatially resolved dynamics. The Hubble Space Telescope (HST) revolutionized BH work by advancing the subject from its ‘proof of concept’ phase into quantitative studies of BH demographics. Most influential was the discovery of a tight correlation between BH masses M• and the velocity dispersions σ of stars in the host galaxy bulge components at radii where the stars mostly feel each other and not the BH. Together with correlations between M• and bulge luminosity, with the ‘missing light’ that defines galaxy cores, and with numbers of globular clusters, this has led to the conclusion that BHs and bulges coevolve by regulating each other's growth. This simple picture with one set of correlations for all galaxies dominated BH work in the past decade.New results are now replacing the above, simple story with a richer and more plausible picture in which BHs correlate differently with different kinds of galaxy components. BHs with masses of 105—106M⊙ live in some bulgeless galaxies. So classical (merger-built) bulges are not necessary equipment for BH formation. On the other hand, while they live in galaxy disks, BHs do not correlate with galaxy disks or with disk-grown pseudobulges. They also have no special correlation with dark matter halos beyond the fact that halo gravity controls galaxy formation. This leads to the suggestion that there are two modes of BH feeding, (1) local, secular and episodic feeding of small BHs in largely bulgeless galaxies that involves too little energy feedback to drive BH–host-galaxy coevolution and (2) global feeding in major galaxy mergers that rapidly grows giant BHs in short-duration events whose energy feedback does affect galaxy formation. After these quasar-like phases, maintenance-mode BH feedback into hot, X-ray-emitting gas continues to have a primarily negative effect in preventing late-time star formation when cold gas or gas-rich galaxies get accreted. Finally, the highest-mass galaxies inherit coevolution effects from smaller galaxies; the tightness of their BH correlations is caused mainly by averaging during dissipationless major mergers.

scholarly journals An Observed Fundamental Plane Relation for Supermassive Black Holes

2007 ◽  
Vol 669 (1) ◽  
pp. 67-73 ◽  
Author(s):  
Philip F. Hopkins ◽  
Lars Hernquist ◽  
Thomas J. Cox ◽  
Brant Robertson ◽  
Elisabeth Krause
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
Fundamental Plane
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