Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy

Vayner, Andrey; Wright, Shelley A.; Murray, Norman; Armus, L.; Larkin, James E.; Mieda, Etsuko

doi:10.3847/1538-4357/aa9c42

Cited by 65 publications

(101 citation statements)

References 93 publications

(120 reference statements)

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“…We want to note that evidence of outflows even in early/intermediate stage merger systems has been collected for several nearby ULIRG/AGN galaxies (e.g. Feruglio et al 2013Feruglio et al , 2015Rupke & Veilleux 2013Saito et al 2017) and in the 3C 298 radio-loud QSO at z = 1.439 (Vayner et al 2017; see also §4.3; footnote 9). These results, together with the fact that SFE of dusty and unobscured QSOs are, on average, comparable, could be consistent with the SB-QSO evolutionary scenario assuming that feedback effects occur early in the evolutionary sequence.…”

Section: Resultsmentioning

confidence: 99%

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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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Section: Resultsmentioning

confidence: 99%

“…Banerji et al 2017;Brusa et al 2018;Coppin et al 2008;Fan et al 2018;Kakkad et al 2017;Yan et al 2010) and/or high column densities (e.g. Bothwell et al 2013;Gilli et al 2014;Polletta et al 2011;Stefan et al 2015;Vayner et al 2017).…”

Section: Appendix C: Smg and Qso Samplesmentioning

confidence: 99%

Molecular gas content in obscured AGN at z > 1

Perna

Sargent

Brusa

et al. 2018

A&A

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“…At a redshift of z ∼ 6.4, the luminous quasar SDSS J1148+5251 shows a strong [C ii] broad component indicating the presence of an outflow with velocities of up to 1400 km s −1 and extending to distances of ∼ 30 kpc Cicone et al 2015). At the lower redshifts of z ∼ 1.4, z ∼ 1.6, and z ∼ 3.9, Vayner et al (2017), Brusa et al (2018), and Feruglio et al (2017) report the detection of a molecular outflow traced with CO. In the first two cases the outflow velocities are 600-700 km s −1 , while in the third case the outflow velocity reaches up to ∼1300 km s −1 .…”

Section: The Presence Of Outflows In High-redshift Quasarsmentioning

confidence: 97%

A spectral stacking analysis to search for faint outflow signatures inz∼ 6 quasars

Stanley

Jolly

König

et al. 2019

A&A

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Aims. Outflows in quasars during the early epochs of galaxy evolution are an important part of the feedback mechanisms potentially affecting the evolution of the host galaxy. However, systematic observations of outflows are only now becoming possible with the advent of sensitive mm telescopes. In this study we use spectral stacking methods to search for faint high velocity outflow signal in a sample of [C ii] detected, z ∼ 6 quasars. Methods. We search for broad emission line signatures from high-velocity outflows for a sample of 26 z ∼ 6 quasars observed with the Atacama Large Millimeter Array (ALMA), with a detection of the [C ii] line. The observed emission lines of the sources are dominated by the host galaxy, and outflow emission is not detected for the individual sources. We use a spectral line stacking analysis developed for interferometric data to search for outflow emission. We stack both extracted spectra and the full spectral cubes. We also investigate the possibility that only a sub-set of our sample contributes to the stacked outflow emission. Results. We find only a tentative detection of a broad emission line component in the stacked spectra. When taking a region of about 2 around the source central position of the stacked cubes, the stacked line shows an excess emission due to a broad component of 1.1-1.5σ, but the significance drops to 0.4-0.7σ when stacking the extracted spectra from a smaller region. The broad component can be characterised by a line width of full width half-max FWHM > 700 km s −1 . Furthermore, we find a sub-sample of 12 sources the stack of which maximises the broad component emission.The stack of this sub-sample shows an excess emission due to a broad component of 1.2-2.5σ. The stacked line of these sources has a broad component of FWHM > 775 km s −1 . Conclusions. We find evidence suggesting the presence of outflows in a sub-sample of 12 out of 26 sources, and have demonstrated the importance of spectral stacking techniques in tracing faint signal in galaxy samples. However, deeper ALMA observations are necessary to confirm the presence of a broad component in the individual spectra.

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“…We also use emission line ratio diagnostics with the BPT diagram (Baldwin et al 1981;Veilleux & Osterbrock 1987) to identify optical AGN. Emission line fluxes are obtained in the procedures described in Section 2.2.…”

Section: Emission Line Measurementsmentioning

confidence: 99%

“…Bennert et al 2002;Schmitt et al 2003;Mullaney et al 2013;Zakamska & Greene 2014;. Moreover, Hβ, [OIII], Hα and [NII] are used in emission line ratio diagnostics of the ionized gas using the BPT diagram (Baldwin et al 1981;Veilleux & Osterbrock 1987). NIR spectroscopic observations are therefore the ideal tool to study ionized AGN outflows at z ∼ 1 − 3.…”

Section: Introductionmentioning

confidence: 99%

The MOSDEF Survey: A Census of AGN-driven Ionized Outflows at z = 1.4–3.8

Leung

Coil

Aird

et al. 2019

ApJ

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Using data from the MOSFIRE Deep Evolution Field (MOSDEF) survey, we present a census of AGN-driven ionized outflows in a sample of 159 AGNs at 1.4 ≤ z ≤ 3.8. The sample spans AGN bolometric luminosities of 10 44−47 erg s −1 and includes both quiescent and star-forming galaxies extending across three orders of magnitude in stellar mass. We identify and characterize outflows from the Hβ, [OIII], Hα and [NII] emission line spectra. We detect outflows in 17% of the AGNs, seven times more often than in a mass-matched sample of inactive galaxies in MOSDEF. The outflows are fast and galaxy-wide, with velocities of ∼ 400 − 3500 km s −1 and spatial extents of 0.3 − 11.0 kpc. The incidence of outflows among AGNs is independent of the stellar mass of the host galaxy, with outflows detected in both star-forming and quiescent galaxies. This suggests that outflows exist across different phases in galaxy evolution. We investigate relations between outflow kinematic, spatial, and energetic properties and both AGN and host galaxy properties. Our results show that AGN-driven outflows are widespread in galaxies along the star-forming main sequence. The mass-loading factors of the outflows are typically 0.1 − 1 and increase with AGN luminosity, capable of exceeding unity at L AGN 10 46.3 erg s −1 . In these more luminous sources the ionized outflow alone is likely sufficient to regulate star formation, and when combined with outflowing neutral and molecular gas may be able to quench star formation in their host galaxies.

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Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy

Cited by 65 publications

References 93 publications

Molecular gas content in obscured AGN at z > 1

Molecular gas content in obscured AGN at z > 1

A spectral stacking analysis to search for faint outflow signatures inz∼ 6 quasars

The MOSDEF Survey: A Census of AGN-driven Ionized Outflows at z = 1.4–3.8

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