Is there a relationship between AGN and star formationin IR-bright AGNs?

Dai, Y. Sophia; Wilkes, B. J.; Bergeron, J.; Kuraszkiewicz, Joanna; Omont, A.; Atanas, Adam; Teplitz, Harry I.

doi:10.1093/mnras/sty1341

Cited by 30 publications

(8 citation statements)

References 144 publications

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“…Our result is in general agreement with the correlation found between AGN activity and star formation, i.e. L AGN ∝ L α IR,SF (α ∼ 1.1 − 1.7; see Netzer 2009;Chen et al 2013;Hickox et al 2014;Duras et al 2017;Dai et al 2018;Izumi et al 2019, and references therein). As noted in previous works (see e.g., Dai et al 2018), the variation of slope might be attributed to different sample compositions and/or methods of analysis.…”

Section: Smbh and Host Galaxy Growthsupporting

confidence: 91%

“…L AGN ∝ L α IR,SF (α ∼ 1.1 − 1.7; see Netzer 2009;Chen et al 2013;Hickox et al 2014;Duras et al 2017;Dai et al 2018;Izumi et al 2019, and references therein). As noted in previous works (see e.g., Dai et al 2018), the variation of slope might be attributed to different sample compositions and/or methods of analysis. However, all these studies including our own reveal a significant trend between the SFR and BH accretion spanning a wide range of luminosity, implying that there may be a direct connection between the AGN and star formation activities over galaxy evolution timescales.…”

Section: Smbh and Host Galaxy Growthmentioning

confidence: 99%

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Resolving the Interstellar Medium in Ultraluminous Infrared QSO Hosts with ALMA

Tan

Gao

Kohno

et al. 2019

ApJ

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We present ALMA observations of the CO(1−0) line and 3-mm continuum emission in eight ultraluminous infrared (IR) quasi-stellar objects (QSOs) at z = 0.06−0.19. All eight IR QSO hosts are clearly resolved in their CO molecular gas emission with a median source size of 3.2 kpc, and seven out of eight sources are detected in 3-mm continuum, which is found to be more centrally concentrated with respect to molecular gas with sizes of 0.4−1.0 kpc. Our observations reveal a diversity of CO morphology and kinematics for the IR QSO systems which can be roughly classified into three categories, rotating gas disk with ordered velocity gradient, compact CO peak with disturbed velocity, and multiple CO distinct sources undergoing a merger between luminous QSO and a companion galaxy separated by a few kpc. The molecular gas in three of IR QSO hosts are found to be rotation-dominated with the ratio of the maximum rotation velocity to the local velocity dispersion of V rot /σ = 4 − 6. Basic estimates of the dynamical masses within the CO-emitting regions give masses between 7.4 × 10 9 and 6.9 × 10 10 M . We find an increasing trend between BH mass accretion rate and star formation rate (SFR) over three orders of magnitude in far-IR luminosity/SFR, in line with the correlation between QSO bolometric luminosity and SF activity, indicative of a likely direct connection between AGN and SF activity over galaxy evolution timescales.

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Section: Smbh and Host Galaxy Growthsupporting

confidence: 91%

Section: Smbh and Host Galaxy Growthmentioning

confidence: 99%

Resolving the Interstellar Medium in Ultraluminous Infrared QSO Hosts with ALMA

Tan

Gao

Kohno

et al. 2019

ApJ

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“…Our results also have important implications for the connection between global SFR and instantaneous black hole accretion. Positive average correlations between global SFR and AGN luminosity have been reported for a number of observations (Netzer 2009;Mullaney et al 2012b;Chen et al 2013;Feltre et al 2013;Azadi et al 2015;Delvecchio et al 2015;Dai et al 2018;Masoura et al 2018), while others suggest that they hold only for bulge-dominated galaxies (Yang et al 2019) or the highest-luminosity systems (Lutz et al 2010;Rosario et al 2012;Rovilos et al 2012;Duras et al 2017). Other studies suggest little or no connection between average SFR and black hole accretion (Harrison et al 2012;Mullaney et al 2012a;Stanley et al 2015) or link luminous AGN activity with a suppression of star formation (Page et al 2012), possibly only for galaxies above the star formation main sequence (Masoura et al 2018).…”

Section: The Sfr-agn Connectionmentioning

confidence: 98%

Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

Anglés-Alcázar

Quataert

Hopkins

et al. 2021

ApJ

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We present cosmological hydrodynamic simulations of a quasar-mass halo (M halo ≈ 10 12.5 M e at z = 2) that for the first time resolve gas transport down to the inner 0.1 pc surrounding the central massive black hole. We model a multiphase interstellar medium including stellar feedback by supernovae, stellar winds, and radiation, and a hyper-Lagrangian refinement technique increasing the resolution dynamically approaching the black hole. We do not include black hole feedback. We show that the subpc inflow rate (1) can reach ∼6 M e yr −1 roughly in steady state during the epoch of peak nuclear gas density (z ∼ 2), sufficient to power a luminous quasar, (2) is highly time variable in the pre-quasar phase, spanning 0.001-10 M e yr −1 on Myr timescales, and (3) is limited to short (∼2 Myr) active phases (0.01-0.1 M e yr −1 ) followed by longer periods of inactivity at lower nuclear gas density and late times (z ∼ 1), owing to the formation of a hot central cavity. Inflowing gas is primarily cool, rotational support dominates over turbulence and thermal pressure, and star formation can consume as much gas as provided by inflows across 1 pc-10 kpc. Gravitational torques from multiscale stellar non-axisymmetries dominate angular momentum transport over gas self-torquing and pressure gradients, with accretion weakly dependent on black hole mass. Subpc inflow rates correlate with nuclear (but decouple from global) star formation and can exceed the Eddington rate by ×10. The black hole can move ∼10 pc from the galaxy center on ∼0.1 Myr. Accreting gas forms pc-scale, rotationally supported, obscuring structures often misaligned with the galaxy-scale disk. These simulations open a new avenue to investigate black hole-galaxy coevolution.

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“…more consistent) connection between more luminous AGNs and star formation than for lower luminosity AGNs (e.g. Rosario et al 2013;Stanley et al 2017;Aird, Coil & Georgakakis 2017Dai et al 2018;Masoura et al 2018): for example, it may be that any luminous AGN activity occurs close in time to the star formation activity while lower luminosity AGN activity can occur when the galaxy is more quiescent (and hence, the broader R MS distribution) in addition to occurring during the periods of star formation activity.…”

Section: Implications Of Our Analysismentioning

confidence: 99%

A binning-free method reveals a continuous relationship between galaxies’ AGN power and offset from main sequence

Grimmett

Mullaney

Bernhard

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Studies investigating the relationship between active galactic nucleus (AGN) power and the star formation rates (SFRs) of their host galaxies often rely on averaging techniques – such as stacking – to incorporate information from non-detections. However, averages, and especially means, can be strongly affected by outliers and can therefore give a misleading indication of the ‘typical’ case. Recently, a number of studies have taken a step further by binning their sample in terms of AGN power (approximated by the 2–10 keV luminosity of the AGN), and investigating how the SFR distribution differs between these bins. These bin thresholds are often weakly motivated, and binning implicitly assumes that sources within the same bin have similar (or even identical) properties. In this paper, we investigate whether the distribution of host SFRs – relative to the locus of the star-forming main sequence (i.e. RMS) – changes continuously as a function of AGN power. We achieve this by using a hierarchical Bayesian model that completely removes the need to bin in AGN power. In doing so, we find strong evidence that the RMS distribution changes with 2–10 keV X-ray luminosity. The results suggest that higher X-ray luminosity AGNs have a tighter physical connection to the star-forming process than lower X-ray luminosity AGNs, at least within the 0.8 < z < 1.2 redshift range considered here.

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Is there a relationship between AGN and star formationin IR-bright AGNs?

Cited by 30 publications

References 144 publications

Resolving the Interstellar Medium in Ultraluminous Infrared QSO Hosts with ALMA

Resolving the Interstellar Medium in Ultraluminous Infrared QSO Hosts with ALMA

Cosmological Simulations of Quasar Fueling to Subparsec Scales Using Lagrangian Hyper-refinement

A binning-free method reveals a continuous relationship between galaxies’ AGN power and offset from main sequence

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