BCG Mass Evolution in Cosmological Hydro-Simulations

Ragone-Figueroa, Cinthia; Granato, G. L.; Ferraro, M. E.; Murante, Giuseppe; Biffi, V.; Borgani, S.; Planelles, S.; Rasia, Elena

doi:10.1093/mnras/sty1639

Cited by 72 publications

(109 citation statements)

References 81 publications

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“…De Lucia & Blaizot 2007) and to several hydrodynamical simulations (e.g. Ragone-Figueroa et al 2018) it has been proposed that star formation occurs very early in BCG history (mostly before z ∼ 3) and is quickly suppressed by AGN feedback (e.g. Croton et al 2006).…”

mentioning

confidence: 90%

Multiwavelength radio observations of a brightest cluster galaxy at z = 1.71: detection of a modest active galactic nucleus and evidence for extended star formation

Trudeau

Webb

Hlavacek-Larrondo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present deep, multiwavelength radio observations of SpARCS104922.6+564032.5, a z = 1.71 galaxy cluster with a starbusting core. Observations were made with the Karl G. Jansky Very Large Array (JVLA) in 3 bands: 1-2 GHz, 4-8 GHz and 8-12 GHz. We detect a radio source coincident with the Brightest Cluster Galaxy (BCG) that has a spectral index of α=0.44±0.29 and is indicative of emission from an Active Galactic Nucleus. The radio luminosity is consistent with the average luminosity of the lower redshift BCG sample, but the flux densities are 6σ below the predicted values of the star-forming Spectral Energy Distribution based on far infrared data. Our new fit fails to simultaneously describe the far infrared and radio fluxes. This, coupled with the fact that no other bright source is detected in the vicinity of the BCG implies that the star formation region, traced by the infrared emission, is extended or clumpy and not located directly within the BCG. Thus, we suggest that the star-forming core might not be driven by a single major wet merger, but rather by several smaller galaxies stripped of their gas or by a displaced cooling flow, although more data are needed to confirm any of those scenarios.

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mentioning

confidence: 90%

Multiwavelength radio observations of a brightest cluster galaxy at z = 1.71: detection of a modest active galactic nucleus and evidence for extended star formation

Trudeau

Webb

Hlavacek-Larrondo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…As such, the BGGs are thought to have experienced numerous mergers and close tidal encounters with other group galaxies over cosmic time. Simulations suggest that such interactions result not only in the growth of the BGGs' total stellar mass but also, induce structural and kinematic transformations (Murante et al, 2007;Dubinski, 1998;De Lucia & Blaizot, 2007;Cooper et al, 2015;Nipoti, 2017;Ragone-Figueroa et al, 2018). Mergers can also potentially transport in cool gas and fuel in-situ star formation in disc-like structures.…”

Section: Brightest Groups Galaxiesmentioning

confidence: 99%

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

et al. 2021

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Galaxy groups are more than an intermediate scale between clusters and halos hosting individual galaxies, they are crucial laboratories capable of testing a range of astrophysics from how galaxies form and evolve to large scale structure (LSS) statistics for cosmology. Cosmological hydrodynamic simulations of groups on various scales offer an unparalleled testing ground for astrophysical theories. Widely used cosmological simulations with ∼(100 Mpc)3 volumes contain statistical samples of groups that provide important tests of galaxy evolution influenced by environmental processes. Larger volumes capable of reproducing LSS while following the redistribution of baryons by cooling and feedback are the essential tools necessary to constrain cosmological parameters. Higher resolution simulations can currently model satellite interactions, the processing of cool (T≈104−5 K) multi-phase gas, and non-thermal physics including turbulence, magnetic fields and cosmic ray transport. We review simulation results regarding the gas and stellar contents of groups, cooling flows and the relation to the central galaxy, the formation and processing of multi-phase gas, satellite interactions with the intragroup medium, and the impact of groups for cosmological parameter estimation. Cosmological simulations provide evolutionarily consistent predictions of these observationally difficult-to-define objects, and have untapped potential to accurately model their gaseous, stellar and dark matter distributions.

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“…a large and robust statistical sample. Moreover, the simulations include subgrid modeling for both hot and cold gas accretion, as well as ejective (quasar-mode) and maintenance (radio-mode) AGN feedback (Ragone-Figueroa et al 2018 for the numerical details). Fig.…”

Section: Smbh Mergersmentioning

confidence: 99%

The X-Ray Halo Scaling Relations of Supermassive Black Holes

Gaspari

Eckert

Ettori

et al. 2019

ApJ

145

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We carry out a comprehensive Bayesian correlation analysis between hot halos and direct masses of supermassive black holes (SMBHs), by retrieving the X-ray plasma properties (temperature, luminosity, density, pressure, masses) over galactic to cluster scales for 85 diverse systems. We find new key scalings, with the tightest relation being the M • − T x , followed by M • − L x . The tighter scatter (down to 0.2 dex) and stronger correlation coefficient of all the X-ray halo scalings compared with the optical counterparts (as the M • − σ e ) suggest that plasma halos play a more central role than stars in tracing and growing SMBHs (especially those that are ultramassive). Moreover, M • correlates better with the gas mass than dark matter mass. We show the important role of the environment, morphology, and relic galaxies/coronae, as well as the main departures from virialization/self-similarity via the optical/X-ray fundamental planes. We test the three major channels for SMBH growth: hot/Bondilike models have inconsistent anti-correlation with X-ray halos and too low feeding; cosmological simulations find SMBH mergers as sub-dominant over most of the cosmic time and too rare to induce a central-limit-theorem effect; the scalings are consistent with chaotic cold accretion (CCA), the rain of matter condensing out of the turbulent X-ray halos that sustains a long-term self-regulated feedback loop. The new correlations are major observational constraints for models of SMBH feeding/feedback in galaxies, groups, and clusters (e.g., to test cosmological hydrodynamical simulations), and enable the study of SMBHs not only through X-rays, but also via the Sunyaev-Zel'dovich effect (Compton parameter), lensing (total masses), and cosmology (gas fractions).

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BCG Mass Evolution in Cosmological Hydro-Simulations

Cited by 72 publications

References 81 publications

Multiwavelength radio observations of a brightest cluster galaxy at z = 1.71: detection of a modest active galactic nucleus and evidence for extended star formation

Multiwavelength radio observations of a brightest cluster galaxy at z = 1.71: detection of a modest active galactic nucleus and evidence for extended star formation

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

The X-Ray Halo Scaling Relations of Supermassive Black Holes

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