Exploring the Limits of AGN Feedback: Black Holes and the Star Formation Histories of Low-mass Galaxies

Martín-Navarro, Ignacio; Mezcua, Mar

doi:10.3847/2041-8213/aab103

Cited by 64 publications

(34 citation statements)

References 51 publications

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“…There is now growing evidence suggesting that the baryonic properties of massive galaxies, namely their ages, star formation rates, and chemical composition, are tightly coupled to the masses of their central super-massive black holes , 2018bMartín-Navarro & Mezcua 2018;Terrazas et al 2016Terrazas et al , 2017. The observed relation between black holes and coronal gas temperature described in § 2 provides further observational evidence for a scenario where the star formation in massive galaxies is regulated by the energetic input from the central black hole.…”

Section: Discussionmentioning

confidence: 87%

Black hole feedback and the evolution of massive early-type galaxies

Martín-Navarro

Burchett

Mezcua

2019

Monthly Notices of the Royal Astronomical Society

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Observationally, constraining the baryonic cycle within massive galaxies has proven to be quite difficult. In particular, the role of black hole feedback in regulating star formation, a key process in our theoretical understanding of galaxy formation, remains highly debated. We present here observational evidence showing that, at fixed stellar velocity dispersion, the temperature of the hot gas is higher for those galaxies hosting more massive black holes in their centers. Analyzed in the context of well-established scaling relations, particularly the mass-size plane, the relation between the mass of the black hole and the temperature of the hot gas around massive galaxies provides further observational support to the idea that baryonic processes within massive galaxies are regulated by the combined effects of the galaxy halo virial temperature and black hole feedback, in agreement with the expectations from the EAGLE cosmological numerical simulation.

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Section: Discussionmentioning

confidence: 87%

Black hole feedback and the evolution of massive early-type galaxies

Martín-Navarro

Burchett

Mezcua

2019

Monthly Notices of the Royal Astronomical Society

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“…For this reason, BHs with M • 10 5 M fail to reach the mass dictated by their velocity dispersion and become under-massive. Previous observations (e.g., Martín-Navarro & Mezcua 2018) and simulations (e.g., Anglés-Alcázar et al 2017;Habouzit et al 2017) already suggested that feedback is driven by BH activity for M • 10 5 M and by supernova-driven winds for M • 10 5 M .…”

Section: Observational Predictions For Bh Seeding Modelsmentioning

confidence: 94%

“…Some papers (e.g., Greene & Ho 2006;Mezcua 2017;Martín-Navarro & Mezcua 2018) suggest an alternative scenario for the low-mass regime of the M • − σ relation, predicting a flattening at masses ∼ 10 5 − 10 6 M . Martín-Navarro & Mezcua (2018) explained this putative flattening with a weaker coupling between baryonic cooling and BH feedback, disconnecting the BH from the evolution of the host spheroid.…”

Section: Observational Predictions For Bh Seeding Modelsmentioning

confidence: 99%

Glimmering in the Dark: Modeling the Low-mass End of the M_•–σ Relation and of the Quasar Luminosity Function

Pacucci

Loeb

Mezcua

et al. 2018

ApJL

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The M • − σ relation establishes a connection between central black holes (BHs) and their host spheroids. Supported by observations at M • 10 5 M , there is limited data on its validity at lower masses. Employing a semi-analytical model to simulate the combined evolution of BHs and their host galaxies, we predict the observational consequences of assuming a bimodality in the accretion efficiency of BHs, with low-mass BHs (M • 10 5 M ) accreting inefficiently. We predict a departure from the M • − σ relation at a transitional BH mass ∼ 10 5 M , with lower-mass BHs unable to reach the mass dictated by the relation and becoming disconnected from the evolution of the host galaxy. This prediction is an alternative to previous works suggesting a flattening of the relation at ∼ 10 5 − 10 6 M . Furthermore, we predict a deficit of BHs shining at bolometric luminosities ∼ 10 42 erg s −1 . Joined with a detection bias, this could partly explain the scarce number of intermediate-mass BHs detected. Conversely, we predict an increase in source density at lower bolometric luminosities, < 10 42 erg s −1 . Because our predictions assume a bimodal population of high-redshift BH seeds, future observations of fainter BHs will be fundamental for constraining the nature of these seeds.

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“…ing a connection between the star formation and black hole activity , 2018bTerrazas et al 2016Terrazas et al , 2017Martín-Navarro & Mezcua 2018).…”

Section: Black Hole Plus Halo Quenching?mentioning

confidence: 99%

Star formation quenching imprinted on the internal structure of naked red nuggets

Martín-Navarro

Ven

Yıldırım

2019

Monthly Notices of the Royal Astronomical Society

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The formation and assembly process of massive galaxies is a combination of two phases: an initial in-situ-dominated one followed by an ex-situ-dominated evolution. Separating these two contributions is therefore crucial to understand the baryonic cycle within massive halos. A recently discovered population of so-called naked red nuggets, galaxies that shortcut the ex-situ stage preserving their pristine properties, presents a unique opportunity to study in detail star formation in massive galaxies without the confounding effect of later accretion. We investigate the spatially resolved star formation histories of a sample of 12 naked red nuggets. We measure how their radial light distributions, star formation rates and central densities evolved in time. We find that, while forming stars, red nuggets become gradually more concentrated, reaching a maximum concentration at quenching. After being quenched, they kept forming stars in a more disky-like configuration. Our measurements suggest that supermassive black holes and host galaxies grow their mass in a self-regulated way until a characteristic M • /M halo is reached. Once black holes are massive enough, red nuggets get quenched and depart from the star formation main sequence. While in the main sequence, red nuggets evolve at roughly constant star formation rate. This can explain up to ∼ 0.3 dex of the scatter of the star formation main sequence, as well as its higher normalization observed in the early Universe. Hence, our results suggest that the main sequence is composed of populations of galaxies at different evolutionary stages, and that the scatter is therefore due to secular processes.

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Exploring the Limits of AGN Feedback: Black Holes and the Star Formation Histories of Low-mass Galaxies

Cited by 64 publications

References 51 publications

Black hole feedback and the evolution of massive early-type galaxies

Black hole feedback and the evolution of massive early-type galaxies

Glimmering in the Dark: Modeling the Low-mass End of the M_•–σ Relation and of the Quasar Luminosity Function

Star formation quenching imprinted on the internal structure of naked red nuggets

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Exploring the Limits of AGN Feedback: Black Holes and the Star Formation Histories of Low-mass Galaxies

Cited by 64 publications

References 51 publications

Black hole feedback and the evolution of massive early-type galaxies

Black hole feedback and the evolution of massive early-type galaxies

Glimmering in the Dark: Modeling the Low-mass End of the M•–σ Relation and of the Quasar Luminosity Function

Star formation quenching imprinted on the internal structure of naked red nuggets

Contact Info

Product

Resources

About

Glimmering in the Dark: Modeling the Low-mass End of the M_•–σ Relation and of the Quasar Luminosity Function