The incidence of AGN in galaxies with different stellar population ages

Ni, Quan Xing; Aird, James; Merloni, A.; Birchall, Keir L; Buchner, Johannes; Salvato, M.; Yang, Guang

doi:10.1093/mnras/stad2070

Cited by 5 publications

(1 citation statement)

References 78 publications

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“…Riffel et al (2022Riffel et al ( , 2023 found a correlation of intermediate stellar population with AGN luminosity, which is interpreted as the recycled material from the intermediate-age stellar population triggering the AGN. Ni et al (2023) recently showed that a higher level of AGN activity is observed in galaxies with younger stellar population ages, where more recycled gas is produced. Consistent with these observational findings, our study highlights the substantial contribution of recycled gas in triggering AGNs within a comprehensive cosmological hydrodynamic simulation.…”

Section: The Importance Of Recycled Gasmentioning

confidence: 99%

The Origins of Gas Accreted by Supermassive Black Holes: The Importance of Recycled Gas

Choi,

Somerville,

Ostriker

et al. 2024

ApJ

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We investigate the fueling mechanisms of supermassive black holes (SMBHs) by analyzing 10 zoom-in cosmological simulations of massive galaxies, with stellar masses 1011–12 M ⊙ and SMBH masses 108.9–9.7 M ⊙ at z = 0, featuring various major and minor merger events. By tracing the gas history in these simulations, we categorize the gas accreted by the central SMBHs based on its origin. Gas that belonged to a different galaxy before accretion onto the BH is labeled as (i) “external,” while smoothly accreted cosmic gas is classified as (ii) “smooth.” Gas produced within the primary halo through stellar evolution and subsequently accreted by the SMBH is classified as (iii) “recycled.” Our analysis, which includes stellar feedback, reveals that the primary fuel source for SMBHs is the recycled gas from dying stars. This recycled gas from stars in the inner region of the galaxy readily collapses toward the center, triggering starbursts and simultaneously fueling the SMBH. Galaxy mergers also play a crucial role in fueling SMBHs in massive galaxies, as SMBHs in massive halos tend to accrete a higher fraction of external gas from mergers compared to smoothly accreted gas. However, on average, it takes approximately 1.85 Gyr for external gas to enter the main galaxy and accrete onto the SMBH. Considering the presence of various other gas triggers for active galactic nucleus (AGN) activity alongside this time delay, the association between AGNs and mergers may not always be obvious.

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Section: The Importance Of Recycled Gasmentioning

confidence: 99%

The Origins of Gas Accreted by Supermassive Black Holes: The Importance of Recycled Gas

Choi,

Somerville,

Ostriker

et al. 2024

ApJ

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Cosmic evolution of radio-excess active galactic nuclei in quiescent and star-forming galaxies across 0 < z < 4

Wang,

Liu

et al. 2024

A&A

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Radio-excess active galactic nuclei (radio-AGNs) are essential to our understanding of both the physics of black hole (BH) accretion and the interaction between BHs and host galaxies. Recent deep and wide radio continuum surveys have made it possible to study radio-AGNs down to lower luminosities and up to higher redshifts than previous studies, and are providing new insights into the abundance and physical origin of radio-AGNs. Here we focus on the cosmic evolution, physical properties, and AGN-host galaxy connections of radio-AGNs selected from a total sample of sim 400,000 galaxies at $0 < z < 4$ in the GOODS-N and COSMOS fields. Combining the deep radio continuum data with multi-band, de-blended far-infrared, and submillimeter data, we were able to identify 983 radio-AGNs out of the entire galaxy sample through radio excess relative to the far-infrared--radio relation. We studied the cosmic evolution of 1.4 GHz radio luminosity functions (RLFs) for both star-forming galaxies (SFGs) and radio-AGNs, which can be well described by a pure luminosity evolution of $L_ star z +3.57 $ and a pure density evolution of $ star z +2.69 $, respectively. We derived the turnover luminosity, above which the number density of radio-AGNs surpasses that of SFGs. We show that this crossover luminosity increases with increasing redshifts, from $10^ W Hz $ at $z 0$ to W Hz $ at $z 4$. At the full redshift range of $0 < z < 4$, we further derive the probability radio $) of SFGs and quiescent galaxies (QGs) hosting a radio-AGN, as a function of stellar mass ($M_ star $), radio luminosity ($L_ R $), and redshift ($z$), which yields $p_ radio star R $ for SFGs, and $p_ radio star R $ for QGs, respectively. The quantitative relation for the probabilities of galaxies hosting a radio-AGN indicates that radio-AGNs in QGs prefer to reside in more massive galaxies with higher $L_ R $ than those in SFGs. The fraction of radio-AGN increases toward higher redshift in both SFGs and QGs, with a more rapid increase in SFGs.

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The fundamental plane of black hole activity for low-luminosity radio active galactic nuclei across 0 < z < 4

Wang,

et al. 2024

A&A

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The fundamental plane of black hole activity describes the correlation between radio luminosity ($L_ R $), X-ray luminosity ($L_ X $), and black hole mass ($M_ BH $). It reflects a connection between the accretion disc and the jet. However, the dependence of the fundamental plane on various physical properties of active galactic nuclei (AGNs) and host galaxies remains unclear, especially for low-luminosity AGNs, which is important for understanding the accretion physics in AGNs. Here, we explore the dependence of the fundamental plane on the radio loudness, Eddington-ratio ($ Edd $), redshift, and galaxy star formation properties (star-forming galaxies and quiescent galaxies) across $0.1 < z 4$ for radio AGNs. Based on current deep and large surveys, our studies can extend to lower luminosities and higher redshifts. From the deep and large multi-wavelength surveys in the GOODS-N, GOODS-S, and COSMOS/UltraVISTA fields, we constructed a large and homogeneous radio AGN sample consisting of 208 objects with available estimates for $L_ R $ and $L_ X $. Then we divided the radio AGN sample into 141 radio-quiet AGNs and 67 radio-loud AGNs according to the radio loudness defined by the ratio of $L_ R $ to $L_ X $, and explored the dependence of the fundamental plane on different physical properties of the two populations, separately. The ratio of $L_ R $ to $L_ X $ shows a bimodal distribution that is well described by two single Gaussian models. The cross point between these two Gaussian components corresponds to a radio-loudness threshold of $ R /L_ X ) = -2.73$. The radio-quiet AGNs have a significantly larger Eddington ratio than the radio-loud AGNs. Our radio-quiet and radio-loud AGNs show a significantly different fundamental plane, which indicates a significant dependence of the fundamental plane on the radio loudness. For both radio-quiet and radio-loud AGNs, the fundamental plane shows a significant dependence on $ Edd $, but no dependence on redshift. The fundamental plane shows a significant dependence on the galaxy star formation properties for radio-quiet AGNs, while for radio-loud AGNs this dependence disappears. The fundamental plane sheds important light on the accretion physics and X-ray emission origins of central engines. X-ray emission of radio-quiet AGNs at $0.01 < Edd < 0.1$ are produced by a combination of advection-dominated accretion flow (ADAF) and synchrotron radiation from the jet, while at $0.1 < Edd < 1$ they mainly follow the synchrotron jet model. The origins of X-ray emission of radio-loud AGNs are consistent with a combination of ADAF and the synchrotron jet model at $ Edd < 0.01$, agree with the synchrotron jet model at $0.01 < Edd < 0.1$, and follow a combination of the standard thin disc and a jet model at $ Edd

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The incidence of AGN in galaxies with different stellar population ages

Cited by 5 publications

References 78 publications

The Origins of Gas Accreted by Supermassive Black Holes: The Importance of Recycled Gas

The Origins of Gas Accreted by Supermassive Black Holes: The Importance of Recycled Gas

Cosmic evolution of radio-excess active galactic nuclei in quiescent and star-forming galaxies across 0 < z < 4

The fundamental plane of black hole activity for low-luminosity radio active galactic nuclei across 0 < z < 4

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