Quantifying the Effect of Black Hole Feedback from the Central Galaxy on the Satellite Populations of Groups and Clusters

Martín-Navarro, Ignacio; Burchett, Joseph N.; Mezcua, Mar

doi:10.3847/2041-8213/ab4885

Cited by 13 publications

(8 citation statements)

References 48 publications

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“…The separation between star-forming and quiescent satellites is based on their location with respect to the star formation main sequence (SFMS). In particular, we find that the SFMS in our sample of satellites is well-fitted 31 by log SFR = 0.75 log M − 7.5. As described in the main text, given this definition of the SFMS and having stellar masses and SFR measurements for each satellite, we label as star-forming any satellite departing less than 1 dex from the SFMS.…”

Section: Methods 1 Sample Properties 11 Sloan Digital Sky Server Datasupporting

confidence: 51%

“…For halos hosting under-massive black holes, the observed amplitude in the signal is 0.016 ±0.002. The expected uncertainty in these black hole mass estimates is of ∼ 0.3 dex due the intrinsic scatter in the M • -σ relation 31 . In individual galaxies, this over-massive vs under-massive black hole metric has been now widely used to probe the interplay between black hole activity and star formation 11,41,[43][44][45][46][47][48] , further supporting a black hole-related origin for the observed signal.…”

Section: Dependence On Galaxy Properties In Sdss Datamentioning

confidence: 95%

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Anisotropic satellite galaxy quenching modulated by supermassive black hole activity

Martín-Navarro,

Pillepich,

Nelson

et al. 2021

Preprint

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Section: Methods 1 Sample Properties 11 Sloan Digital Sky Server Datasupporting

confidence: 51%

Section: Dependence On Galaxy Properties In Sdss Datamentioning

confidence: 95%

Anisotropic satellite galaxy quenching modulated by supermassive black hole activity

Martín-Navarro,

Pillepich,

Nelson

et al. 2021

Preprint

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“…Finally, some studies mention the possible role of AGN feedback from the central galaxy in quenching its satellites (e.g., Dashyan et al 2019;Martín-Navarro et al 2019): the lack of quenching in high-redshift satellites could therefore also be the consequence of an imperfect AGN feedback implementation at high redshift, although hydrodynamical simulations show that the activity of SNe in low mass galaxies quench the growth of black holes and their associated AGN feedback (e.g., Dubois et al 2015;Habouzit et al 2017;Anglés-Alcázar et al 2017).…”

mentioning

confidence: 99%

COSMOS2020: Cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to z ∼ 5

Shuntov

McCracken

Gavazzi

et al. 2022

A&A

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We used the COSMOS2020 catalog to measure the stellar-to-halo mass relation (SHMR) divided by central and satellite galaxies from z = 0.2 to z = 5.5. Starting from accurate photometric redshifts, we measured the near-infrared selected two-point angular correlation and stellar mass functions in ten redshift bins. We used a phenomenological model that parametrizes the stellar-to-halo mass relation for central galaxies and the number of galaxies inside each halo to describe our observations. This model qualitatively reproduces our measurements and their dependence on the stellar mass threshold. Surprisingly, the mean halo occupation distribution only shows a mild evolution with redshift suggesting that galaxies occupy halos similarly throughout cosmic time. At each redshift, we measured the ratio of stellar mass to halo mass, M*/Mh, which shows the characteristic strong dependence of halo mass with a peak at Mhpeak ∼ 2 × 1012 M⊙. For the first time, using a joint modeling of clustering and abundances, we measured the evolution of Mhpeak from z = 0.2 to z = 5.5. Mhpeak increases gradually with redshift from log Mhpeak/M⊙ ∼ 12.1 at z ∼ 0.3 to log Mhpeak/M⊙ ∼ 12.3 at z ∼ 2, and up to log Mhpeak/M⊙ ∼ 12.9 at z ∼ 5. Similarly, the stellar mass peak M∗peak increases with redshift from log M∗peak/M⊙ ∼ 10.5 at z ∼ 0.3 to log M∗peak/M⊙ ∼ 10.9 at z ∼ 3. The SHMR ratio at the peak halo mass remains almost constant with redshift. These results are in accordance with the scenario in which the peak of star-formation efficiency moves toward more massive halos at higher redshifts. We also measured the fraction of satellites as a function of stellar mass and redshift. For all stellar mass thresholds, the satellite fraction decreases at higher redshifts. At a given redshift, there is a higher fraction of low-mass satellites and this fraction reaches a plateau at ∼25% at z ∼ 1. The satellite contribution to the total stellar mass budget in halos becomes more important than that of the central at halo masses of about Mh > 1013 M⊙ and always stays below the peak, indicating that quenching mechanisms are present in massive halos that keep the star-formation efficiency low. Finally, we compared our results with three hydrodynamical simulations: HORIZON-AGN, TNG100 of the ILLUSTRISTNG project, and EAGLE. We find that the most significant discrepancy is at the high-mass end, where the simulations generally show that satellites have a higher contribution to the total stellar mass budget than the observations. This, together with the finding that the fraction of satellites is higher in the simulations, indicates that the feedback mechanisms acting in both group- and cluster-scale halos appear to be less efficient in quenching the mass assembly of satellites – and that quenching occurs much later in the simulations.

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“…These conflicting observational results could be explained by the difficulty in detecting the satellites in the neighborhood of a luminous quasar, where the strong AGN feedback can play a fundamental role in shaping their baryonic component. AGN feedback could affect the MBH environment well beyond the host galaxy scale radius and significantly modify the star formation (SF) activity of the orbiting companions (see Martín-Navarro et al 2019, 2021. Dashyan et al (2019) explicitly investigated, in cosmological hydrodynamical simulations, the AGN-driven quenching effect within galactic satellites at low redshift (z < 3).…”

Section: Introductionmentioning

confidence: 99%

Enhanced star formation in $z\sim6$ quasar companions

Zana,

Gallerani,

Carniani

et al. 2022

Preprint

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Quasars powered by supermassive black holes (MBH, > 10 8 M ) at z ∼ 6 are predicted to reside in cosmic over-dense regions. However, observations so far could not confirm this expectation due to limited statistics. The picture is further complicated by the possible effects of quasar outflows (i.e. feedback) that could either suppress or stimulate the star formation rate (SFR) of companion galaxies, thus modifying the expected bias.Here we quantify feedback effects on the properties and detectability of companions by comparing cosmological zoom-in simulations of a quasar in which feedback is either included or turned-off. With respect to the no-feedback case, companions (a) directly impacted by the outflow have their SFR increased by a factor 2 − 3, and (b) tend to be more massive. Both effects shift the [CII]158µm and UV luminosity functions toward brighter magnitudes. This leads us to conclude that quasar feedback slightly increases the effective quasar bias, boosting the number density of observable quasar companions, in agreement with what has been found around the brightest quasars of recent ALMA [CII] surveys. Deeper observations performed with JWST and/or ALMA will improve the statistical significance of this result by detecting a larger number of fainter quasar companions.

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Quantifying the Effect of Black Hole Feedback from the Central Galaxy on the Satellite Populations of Groups and Clusters

Cited by 13 publications

References 48 publications

Anisotropic satellite galaxy quenching modulated by supermassive black hole activity

Anisotropic satellite galaxy quenching modulated by supermassive black hole activity

COSMOS2020: Cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to z ∼ 5

Enhanced star formation in $z\sim6$ quasar companions

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