Expanding the Sample: The Relationship between the Black Hole Mass of BCGs and the Total Mass of Galaxy Clusters

Phipps, Frederika; Bogdán, Ákos; Lovisari, Lorenzo; Kovacs, Orsolya; Volonteri, Marta; Dubois, Yohan

doi:10.3847/1538-4357/ab107c

Cited by 21 publications

(15 citation statements)

References 59 publications

(109 reference statements)

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“…Indeed, in their Table 4 they report σ M BH |M BCG = 0.61 and σ M BH |T = 0.38. The values of the scatters increase in the later analysis by Phipps et al (2019) because of the method used to derive M BH , the authors suggest. Despite, also in that case the two intrinsic scatters in M BH are comparable between each other.…”

Section: Discussionmentioning

confidence: 96%

Black hole mass of central galaxies and cluster mass correlation in cosmological hydro-dynamical simulations

Bassini

Rasia

Borgani

et al. 2019

A&A

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Context. The correlations between the properties of the brightest cluster galaxy (BCG) and the mass of its central super-massive black hole (SMBH) have been extensively studied from a theoretical and observational angle. More recently, relations connecting the SMBH mass and global properties of the hosting cluster, such as temperature and mass, were observed. Aims. We investigate the correlation between SMBH mass and cluster mass and temperature, their establishment and evolution. We compare their scatter to that of the classical M BH − M BCG relation. Moreover, we study how gas accretion and BH-BH mergers contribute to SMBH growth across cosmic time. Methods. We employed 135 groups and clusters with a mass range 1.4 × 10 13 M − 2.5 × 10 15 M extracted from a set of 29 zoom-in cosmological hydro-dynamical simulations where the baryonic physics is treated with various sub-grid models, including feedback by active galactic nuclei. Results. In our simulations we find that M BH correlates well with M 500 and T 500 , with the scatter around these relations compatible within 2σ with the scatter around M BH − M BCG at z = 0. The M BH − M 500 relation evolves with time, becoming shallower at lower redshift as a direct consequence of hierarchical structure formation. On average, in our simulations the contribution of gas accretion to the total SMBH mass dominates for the majority of the cosmic time (z > 0.4), while in the last 2 Gyr the BH-BH mergers become a larger contributor. During this last process, substructures hosting SMBHs are disrupted in the merger process with the BCG and the unbound stars enrich the diffuse stellar component rather than increase BCG mass. Conclusions. From the results obtained in our simulations with simple sub-grid models we conclude that the scatter around the M BH − T 500 relation is comparable to the scatter around the M BH − M BCG relation and that, given the observational difficulties related to the estimation of the BCG mass, clusters temperature and mass can be a useful proxy for the SMBHs mass, especially at high redshift.

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Section: Discussionmentioning

confidence: 96%

Black hole mass of central galaxies and cluster mass correlation in cosmological hydro-dynamical simulations

Bassini

Rasia

Borgani

et al. 2019

A&A

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“…Interestingly, a few simulated galaxies were identified in Horizon-AGN with M bulge 10 12.5 M , i.e. more massive than the observed ones (Bogdán et al 2018;Phipps et al 2019), and overmassive with respect to their M 500 . These simulated galaxies could be too massive while providing a good agreement for the mass of their BHs.…”

Section: Bhs In Massive Galaxies Of M 10 12 Mmentioning

confidence: 95%

“…The most massive BHs reside in BCGs with bulge mass up to M bulge < 10 12.5 M . A non-negligible fraction of the BHs residing in BGGs and BCGs are overmassive with respect to the bulge stellar mass or the stellar velocity dispersion of their host galaxies (Bogdán et al 2018;Phipps et al 2019), compared to the scaling relation of McConnell & Ma (2013) for example. In the comparison of Bogdán et al (2018) with the Horizon-AGN simulation, a very good agreement is found in the plane M BH − M 500 (M 500 the mass enclosed in a sphere of mean mass density 500 times the Universe critical density).…”

Section: Bhs In Massive Galaxies Of M 10 12 Mmentioning

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

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102

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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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“…A few rare objects, e.g., NGC4342 and NGC4291, appear to have become overly "enthusiastic", at early epochs, and may have terminated star formation before the stellar mass grew to the characteristic size needed to lie on the stellar mass -SMBH mass relation. New scaling relations (e.g., Bogdán & Goulding 2015;Bogdán et al 2018;Phipps et al 2019, andGaspari et al 2019) suggest that the stellar mass may not be the fundamental driver of SMBH mass. X-ray all-sky surveys from eROSITA will provide large samples of X-ray bright galaxies to fully explore the present epoch population of dark matter halos and their hot gas content.…”

Section: Discussionmentioning

confidence: 99%

Supermassive Black Hole feedback in early type galaxies

Forman¹,

Jones²,

Bogdán³

et al. 2019

Proc. IAU

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Optically luminous early type galaxies host X-ray luminous, hot atmospheres. These hot atmospheres, which we refer to as coronae, undergo the same cooling and feedback processes as are commonly found in their more massive cousins, the gas rich atmospheres of galaxy groups and galaxy clusters. In particular, the hot coronae around galaxies radiatively cool and show cavities in X-ray images that are filled with relativistic plasma originating from jets powered by supermassive black holes (SMBH) at the galaxy centers. We discuss the SMBH feedback using an X-ray survey of early type galaxies carried out using Chandra X-ray Observatory observations. Early type galaxies with coronae very commonly have weak X-ray active nuclei and have associated radio sources. Based on the enthalpy of observed cavities in the coronae, there is sufficient energy to “balance” the observed radiative cooling. There are a very few remarkable examples of optically faint galaxies that are 1) unusually X-ray luminous, 2) have large dark matter halo masses, and 3) have large SMBHs (e.g., NGC4342 and NGC4291). These properties suggest that, in some galaxies, star formation may have been truncated at early times, breaking the simple scaling relations.

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Expanding the Sample: The Relationship between the Black Hole Mass of BCGs and the Total Mass of Galaxy Clusters

Cited by 21 publications

References 59 publications

Black hole mass of central galaxies and cluster mass correlation in cosmological hydro-dynamical simulations

Black hole mass of central galaxies and cluster mass correlation in cosmological hydro-dynamical simulations

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

Supermassive Black Hole feedback in early type galaxies

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