SUPERMASSIVE BLACK HOLES AND THEIR HOST GALAXIES. I. BULGE LUMINOSITIES FROM DEDICATED NEAR-INFRARED DATA

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.

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Coevolution of supermassive black holes and their host galaxies

10.1063/1.3009487 ◽

2008 ◽

Author(s):

J. K. Kotilainen ◽

R. Decarli ◽

R. Falomo ◽

M. Labita ◽

R. Scarpa ◽

...

Keyword(s):

Black Holes ◽

Supermassive Black Holes ◽

Host Galaxies

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

Proceedings of the International Astronomical Union ◽

10.1017/s174392131300495x ◽

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.

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A FUNDAMENTAL EQUATION FOR SUPERMASSIVE BLACK HOLES

International Journal of Modern Physics D ◽

10.1142/s0218271811020330 ◽

2011 ◽

Vol 20 (12) ◽

pp. 2305-2315 ◽

Cited By ~ 7

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.

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Correlations between supermassive black holes and hot gas atmospheres in IllustrisTNG and X-ray observations

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3880 ◽

2020 ◽

Vol 501 (2) ◽

pp. 2210-2230

Author(s):

Nhut Truong ◽

Annalisa Pillepich ◽

Norbert Werner

Keyword(s):

Black Holes ◽

Supermassive Black Holes ◽

High Mass ◽

Mass Relation ◽

Host Galaxies ◽

X Ray ◽

Hierarchical Assembly ◽

Hot Gas ◽

The Masses

ABSTRACT Recent X-ray observations have revealed remarkable correlations between the masses of central supermassive black holes (SMBHs) and the X-ray properties of the hot atmospheres permeating their host galaxies, thereby indicating the crucial role of the atmospheric gas in tracing SMBH growth in the high-mass regime. We examine this topic theoretically using the IllustrisTNG cosmological simulations and provide insights to the nature of this SMBH – gaseous halo connection. By carrying out a mock X-ray analysis for a mass-selected sample of TNG100 simulated galaxies at $z$ = 0, we inspect the relationship between the masses of SMBHs and the hot gas temperatures and luminosities at various spatial and halo scales – from galactic (∼Re) to group/cluster scales (∼R500c). We find strong SMBH-X-ray correlations mostly in quenched galaxies and find that the correlations become stronger and tighter at larger radii. Critically, the X-ray temperature (kBTX) at large radii (r ≳ 5Re) traces the SMBH mass with a remarkably small scatter (∼0.2 dex). The relations emerging from IllustrisTNG are broadly consistent with those obtained from recent X-ray observations. Overall, our analysis suggests that, within the framework of IllustrisTNG, the present-time MBH–kBTX correlations at the high-mass end (MBH ≳ 108M⊙) are fundamentally a reflection of the SMBH mass–halo mass relation, which at such high masses is set by the hierarchical assembly of structures. The exact form, locus, and scatter of those scaling relations are, however, sensitive to feedback processes such as those driven by star formation and SMBH activity.

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The Parallel Lives of Supermassive Black Holes and~their Host Galaxies

ESO Astrophysics Symposia - Relativistic Astrophysics Legacy and Cosmology – Einstein’s ◽

10.1007/978-3-540-74713-0_36 ◽

2007 ◽

pp. 158-162 ◽

Cited By ~ 5

Author(s):

A. Merloni ◽

G. Rudnick ◽

T. Di Matteo

Keyword(s):

Black Holes ◽

Supermassive Black Holes ◽

Host Galaxies ◽

Parallel Lives

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

Proceedings of the International Astronomical Union ◽

10.1017/s1743921319008500 ◽

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.

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AGNs at the cosmic dawn: predictions for future surveys from a ΛCDM cosmological model

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa024 ◽

2020 ◽

Vol 492 (2) ◽

pp. 2535-2552

Author(s):

Andrew J Griffin ◽

Cedric G Lacey ◽

Violeta Gonzalez-Perez ◽

Claudia del P Lagos ◽

Carlton M Baugh ◽

...

Keyword(s):

Black Holes ◽

Galaxy Formation ◽

Near Infrared ◽

Accretion Rate ◽

High Redshift ◽

Host Galaxies ◽

Accretion Rates ◽

Infrared Wavelengths ◽

The Masses ◽

High Redshift Universe

ABSTRACT Telescopes to be launched over the next decade and a half, such as JWST, EUCLID, ATHENA, and Lynx, promise to revolutionize the study of the high-redshift Universe and greatly advance our understanding of the early stages of galaxy formation. We use a model that follows the evolution of the masses and spins of supermassive black holes (SMBHs) within a semi-analytic model of galaxy formation to make predictions for the active galactic nucleus luminosity function at $z$ ≥ 7 in the broadband filters of JWST and EUCLID at near-infrared wavelengths, and ATHENA and Lynx at X-ray energies. The predictions of our model are relatively insensitive to the choice of seed black hole mass, except at the lowest luminosities (Lbol < 1043 erg s−1) and the highest redshifts ($z$ > 10). We predict that surveys with these different telescopes will select somewhat different samples of SMBHs, with EUCLID unveiling the most massive, highest accretion rate SMBHs, Lynx the least massive, lowest accretion rate SMBHs, and JWST and ATHENA covering objects inbetween. At $z$ = 7, we predict that typical detectable SMBHs will have masses, MBH ∼ 105–8 M⊙, and Eddington normalized mass accretion rates, $\dot{M}/\dot{M}_{\mathrm{Edd}}\sim 0.6{-}2$. The SMBHs will be hosted by galaxies of stellar mass M⋆ ∼ 108–10 M⊙, and dark matter haloes of mass Mhalo ∼ 1011–12 M⊙. We predict that the detectable SMBHs at $z$ = 10 will have slightly smaller black holes, accreting at slightly higher Eddington normalized mass accretion rates, in slightly lower mass host galaxies compared to those at $z$ = 7, and reside in haloes of mass Mhalo ∼ 1010–11 M⊙.

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