Quasar Feedback in the Ultraluminous Infrared Galaxy F11119+3257: Connecting the Accretion Disk Wind with the Large-scale Molecular Outflow

Veilleux, Sylvain; Bolatto, Alberto D.; Tombesi, Francesco; Meléndez, M.; Sturm, E.; González-Alfonso, E.; Fischer, J.; Rupke, David S. N.

doi:10.3847/1538-4357/aa767d

Cited by 145 publications

(173 citation statements)

References 75 publications

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“…Its kinematic properties reveals the likely presence of a disturbed disk with turbulent molecular gas. This is consistent with the large-scale of a few kpc molecular outflow observed in this galaxy, which is interpreted as likely driven by the strong feedback from the central AGN (Veilleux et al 2017).…”

Section: Discussion 41 Host Galaxy Propertiessupporting

confidence: 89%

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: Discussion 41 Host Galaxy Propertiessupporting

confidence: 89%

Resolving the Interstellar Medium in Ultraluminous Infrared QSO Hosts with ALMA

Tan

Gao

Kohno

et al. 2019

ApJ

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“…In the SB-QSO framework, these systems would be associated with the initial evolutionary stages, before feedback phenomena start to deplete the cold gas. Moreover, massive, powerful multi-phase outflows have been discovered in several local (Feruglio et al 2010;Perna et al 2017a;Sturm et al 2011;Veilleux et al 2017) and high redshift galaxies hosting obscured AGN (Brusa et al 2018;Fan et al 2018;Feruglio et al 2017;Nesvadba et al 2016;Popping et al 2017), demonstrating that luminous AGN are capable of expelling large amounts of gas from the host galaxies, thereby potentially explaining the low gas fraction (and high SFE) of optically luminous QSOs. We note however that from an observational point of view, there is not a clear separation between the two classes of dusty AGN, the first one associated with the prelude of the feedback phase (and therefore with more massive gas reservoirs and higher obscuration) and the second one associated with the feedback stage (and moderate column densities).…”

Section: Sb-qso Evolutionary Sequence Vs Orientation Based Unificatimentioning

confidence: 99%

Molecular gas content in obscured AGN at z > 1

Perna

Sargent

Brusa

et al. 2018

A&A

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Aims. The standard active galactic nuclei (AGN)-galaxy co-evolutionary scenario predicts a phase of deeply "buried" supermassive black hole growth coexisting with a starburst (SB) before feedback phenomena deplete the cold molecular gas reservoir of the galaxy and an optically luminous quasar (QSO) is revealed ("SB-QSO evolutionary sequence"). The aim of this work is to measure the cold gas reservoir of three highly obscured QSOs to test if their gas fraction is similar to that of submillimeter galaxies (SMGs), as expected by some models, and place these measurements in the context of the SB-QSO framework. Methods. We target CO(1-0) transition in BzK4892, a Compton Thick (CT) QSO at z=2.6, CO(1-0) in BzK8608 and CO(2-1) in CDF153, two highly obscured (N H ≈ 6 × 10 23 cm −2 ) QSOs at z = 2.5 and z = 1.5, respectively. For all these targets, we place 3σ upper limits on the CO lines, with L CO < (1.5 ÷ 2.8) × 10 10 K km/s pc 2 . We also compare the molecular gas conditions of our targets with those of other systems at z > 1, considering normal star forming galaxies and SMGs, unobscured and obscured AGN from the literature. For the AGN samples, we provide an updated and (almost) complete collection of targets with CO follow-up at z > 1. Results. BzK4892 displays a high star formation efficiency (SFE = L IR /L CO > 410 L /(K km s −1 pc 2 )) and a gas fraction f gas = M gas /(M star + M gas ) < 10%. Less stringent constraints are derived for the other two targets ( f gas < 0.5 and SFE > 10 L /(K km s −1 pc 2 )). From the comparison with literature data, we found that, on average, i) obscured AGN at z > 1 are associated with higher SFE and lower f gas with respect to normal star forming galaxies and SMGs; ii) mildly and highly obscured active galaxies have comparable gas fractions; iii) the SFE of CT and obscured AGN are similar to those of unobscured AGN.Conclusions. Within the SB-QSO framework, these findings could be consistent with a scenario where feedback can impact the host galaxy already from the early phases of the SB-QSO evolutionary sequence.

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“…In fact, the most conservative estimates derived by Veilleux et al (2017) indicate that the OH and CO molecular outflows may have momentum rates in the rangeṖ out ;1-6 L AGN /c andṖ out ;1.5-3 L AGN /c, respectively. Therefore, even if unlikely, the momentum-conserving regime cannot be fully excluded in this case.…”

Section: Connection With Galaxy-scale Molecular Outflowsmentioning

confidence: 99%

NuSTAR View of the Black Hole Wind in the Galaxy Merger IRAS F11119+3257

Tombesi

Veilleux

Meléndez

et al. 2017

ApJ

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Galactic winds driven by active galactic nuclei (AGNs) have been invoked to play a fundamental role in the coevolution between supermassive black holes and their host galaxies. Finding observational evidence of such feedback mechanisms is of crucial importance and it requires a multi-wavelength approach in order to compare winds at different scales and phases. In Tombesi et al., we reported the detection of a powerful ultra-fast outflow (UFO) in the Suzaku X-ray spectrum of the ultra-luminous infrared galaxy IRASF11119+3257. The comparison with a galaxy-scale OH molecular outflow observed with Herschel in the same source supported the energyconserving scenario for AGN feedback. The main objective of this work is to perform an independent check of the Suzaku results using the higher sensitivity and wider X-ray continuum coverage of NuSTAR. We clearly detect a highly ionized Fe K UFO in the 100 ks NuSTAR spectrum with parameters N H =(3.2±1.5)×10 24 cm −2 , log ξ= - 0.061 . The launching radius is likely at a distance of r16r s from the black hole. The mass outflow rate is in the range ofṀ out ;0.5-2 M e yr −1 . The UFO momentum rate and power areṖ out ;0.5-2 L AGN /c andĖ out ;7%-27% L AGN , respectively. The UFO parameters are consistent between the 2013 Suzaku and the 2015 NuSTAR observations. Only the column density is found to be variable, possibly suggesting a clumpy wind. The comparison with the energetics of molecular outflows estimated in infrared and millimeter wavelengths support a connection between the nuclear and galaxy-scale winds in luminous AGNs.

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Quasar Feedback in the Ultraluminous Infrared Galaxy F11119+3257: Connecting the Accretion Disk Wind with the Large-scale Molecular Outflow

Cited by 145 publications

References 75 publications

Resolving the Interstellar Medium in Ultraluminous Infrared QSO Hosts with ALMA

Resolving the Interstellar Medium in Ultraluminous Infrared QSO Hosts with ALMA

Molecular gas content in obscured AGN at z > 1

NuSTAR View of the Black Hole Wind in the Galaxy Merger IRAS F11119+3257

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