The Case for the Fundamental MBH-σ Relation

Marsden, Christopher; Shankar, Francesco; Ginolfi, M.; Zubovas, Kastytis

doi:10.3389/fphy.2020.00061

Cited by 30 publications

(24 citation statements)

References 106 publications

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“…Bulge + disc decomposition relies on several aspects/assumptions (each study having its own) and can suffer from lack of information on the inclination, surface brightness limits, spatial resolution, and signal-to-noise ratio (see discussions in Simard et al 2011;Dubois et al 2012;Volonteri et al 2016). It has been shown that the M BH − σ plane could be more fundamental than those with galaxy stellar luminosity or mass, or effective radius (for a review Marsden et al 2020). At relatively low redshift, there is no observational evidence for a redshift evolution of the M BH − σ relation, as demonstrated by Shen et al (2015) using about 90 SDSS quasars at z < 1 and by indirect estimates (Shankar, Bernardi & Haiman 2009a;Zhang, Lu & Yu 2012).…”

Section: Data Ava I L a B I L I T Y S Tat E M E N Tmentioning

confidence: 99%

“…These scaling relations are mostly observed in the local Universe since it is extremely challenging to measure these quantities at higher redshifts. For this reason, we only study the M BH − M relation in this paper (M being easier to measure), even if BH mass scales more tightly with the galaxy velocity dispersion locally (Saglia et al 2016;Shankar et al 2016;de Nicola, Marconi & Longo 2019;Marsden et al 2020). The scaling relations potentially imply the co-evolution of BHs and their host galaxies.…”

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confidence: 99%

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Supermassive black holes in cosmological simulations I: MBH − M⋆ relation and black hole mass function

Habouzit

Somerville

et al. 2021

Monthly Notices of the Royal Astronomical Society

105

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The past decade has seen significant progress in understanding galaxy formation and evolution using large-scale cosmological simulations. While these simulations produce galaxies in overall good agreement with observations, they employ different sub-grid models for galaxies and supermassive black holes (BHs). We investigate the impact of the sub-grid models on the BH mass properties of the Illustris, TNG100, TNG300, Horizon-AGN, EAGLE, and SIMBA simulations, focusing on the MBH − M⋆ relation and the BH mass function. All simulations predict tight MBH − M⋆ relations, and struggle to produce BHs of $M_{\rm BH}\leqslant 10^{7.5}\, \rm M_{\odot }$ in galaxies of $M_{\star }\sim 10^{10.5}-10^{11.5}\, \rm M_{\odot }$. While the time evolution of the mean MBH − M⋆ relation is mild ($\rm \Delta M_{\rm BH}\leqslant 1\, dex$ for 0 ≤ z ≤ 5) for all the simulations, its linearity (shape) and normalization varies from simulation to simulation. The strength of SN feedback has a large impact on the linearity and time evolution for $M_{\star }\leqslant 10^{10.5}\, \rm M_{\odot }$. We find that the low-mass end is a good discriminant of the simulation models, and highlights the need for new observational constraints. At the high-mass end, strong AGN feedback can suppress the time evolution of the relation normalization. Compared with observations of the local Universe, we find an excess of BHs with $M_{\rm BH}\geqslant 10^{9}\, \rm M_{\odot }$ in most of the simulations. The BH mass function is dominated by efficiently accreting BHs (log10 fEdd ≥ −2) at high redshifts, and transitions progressively from the high-mass to the low-mass end to be governed by inactive BHs. The transition time and the contribution of active BHs are different among the simulations, and can be used to evaluate models against observations.

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Section: Data Ava I L a B I L I T Y S Tat E M E N Tmentioning

confidence: 99%

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confidence: 99%

Supermassive black holes in cosmological simulations I: MBH − M⋆ relation and black hole mass function

Habouzit

Somerville

et al. 2021

Monthly Notices of the Royal Astronomical Society

105

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“…Many studies have suggested that the M BH -σ relation may be the most fundamental/universal relation (e.g., Ferrarese & Merritt 2000;Gebhardt et al 2000;Ferrarese & Ford 2005;de Nicola et al 2019;Marsden et al 2020) between a black hole and the host galaxy due to its obvious link with the galaxy's gravitational potential and the appearance of M BH ∝ σ 4−5 relations in theories trying to explain black hole feedback (Silk & Rees 1998;Fabian 1999). These claims are based on past observations (van den Bosch 2016; Saglia et al 2016) which reported a single M BH -σ relation for all galaxy types (including bulge-less galaxies), and also a smaller scatter seen in the M BH -σ diagram relative to the M BH -M * ,sph relation.…”

Section: Fundamental Black Hole Scaling Relationmentioning

confidence: 99%

The (Black Hole Mass)-(Spheroid Stellar Density) Relations: $M_{\rm BH}$--$μ$ (and $M_{\rm BH}$--$Σ$) and $M_{\rm BH}$--$ρ$

Sahu,

Graham,

Davis

2021

Preprint

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This paper is the fourth in a series presenting (galaxy morphology, and thus galaxy formation)dependent black hole mass, M BH , scaling relations. We have used a sample of 119 galaxies with directly-measured M BH and host spheroid parameters obtained from multi-component decomposition of, primarily, 3.6 µm Spitzer images. Here, we investigate the correlations between M BH and the projected luminosity density µ, the projected stellar mass density Σ, and the deprojected (internal) stellar mass density ρ, for various spheroid radii. We discover the predicted M BH -µ 0,sph relation and present the first M BH -µ e,sph and M BH -ρ e,int,sph diagrams displaying slightly different (possibly curved) trends for early-and late-type galaxies (ETGs and LTGs) and an offset between ETGs with (fastrotators, ES/S0) and without (slow-rotators, E) a disk. The scatter about various M BH -Σ R,sph (and ρ r,sph ) relations is shown to systematically decrease as the enclosing aperture (and volume) increases, dropping from 0.69 dex when using the spheroid "compactness", Σ 1kpc,sph , to 0.59 dex when using Σ 5kpc,sph . We also reveal that M BH correlates with the internal density, ρ soi,sph , at the BH's sphere-ofinfluence radius, such that core-Sérsic (high Sérsic index, n) and (low-n) Sérsic galaxies define different relations with total rms scatters 0.21 dex and 0.77 dex, respectively. The M BH -ρ soi,sph relations shall help with direct estimation of tidal disruption event rates, binary BH lifetimes, and together with other BH scaling relations, improve the characteristic strain estimates for long-wavelength gravitational waves pursued with pulsar timing arrays and space-based interferometers.

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“…Kormendy & Ho 2013 and references therein) indicate that controlling the morphology of the AGN hosts is essential when studying the evolution of scaling relations with redshift. Besides this, the stellar velocity dispersion (σ ) is the most fundamental parameter linking galaxies and SMBHs (Shankar et al 2016;Marsden et al 2020). Moreover, only the M BH −σ relation holds to all galaxy types, from dwarfs to the most massive galaxies (e.g.…”

Section: Introductionmentioning

confidence: 99%

HARMONI view of the host galaxies of active galactic nuclei around cosmic noon

García-Lorenzo

Monreal-Ibero

Pereira-Santaella

et al. 2022

A&A

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Context. The formation and evolution of galaxies appear linked to the growth of supermassive black holes, as evidenced by empirical scaling relations in nearby galaxies. Understanding this co-evolution over cosmic time requires the revelation of the dynamical state of galaxies and the measurement of the mass of their central black holes (MBH) at a range of cosmic distances. Bright active galactic nuclei (AGNs) are ideal for this purpose. Aims. The High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph (HARMONI), the first light integral-field spectrograph for the Extremely Large Telescope, will transform visible and near-infrared ground-based astrophysics thanks to its advances in sensitivity and angular resolution. We aim to analyse the capabilities of HARMONI to reveal the stellar morpho-kinematic properties of the host galaxies of AGNs at about cosmic noon. Methods. We made use of the simulation pipeline for HARMONI (HSIM) to create mock observations of representative AGN host galaxies at redshifts around cosmic noon. We used observations taken with the Multi Unit Spectroscopic Explorer of nearby galaxies showing different morphologies and dynamical stages combined with theoretical AGN spectra to create the target inputs for HSIM. Results. According to our simulations, an on-source integration time of three hours should be enough to measure the MBH and to trace the morphology and stellar kinematics of the brightest host galaxies of AGNs beyond cosmic noon. For host galaxies with stellar masses < 1011 M⊙, longer exposure times are mandatory to spatially resolve the stellar kinematics.

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The Case for the Fundamental MBH-σ Relation

Cited by 30 publications

References 106 publications

Supermassive black holes in cosmological simulations I: MBH − M⋆ relation and black hole mass function

Supermassive black holes in cosmological simulations I: MBH − M⋆ relation and black hole mass function

The (Black Hole Mass)-(Spheroid Stellar Density) Relations: $M_{\rm BH}$--$μ$ (and $M_{\rm BH}$--$Σ$) and $M_{\rm BH}$--$ρ$

HARMONI view of the host galaxies of active galactic nuclei around cosmic noon

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