Active galactic nuclei winds as the origin of the H2 emission excess in nearby galaxies

Riffel, Rogemar A.; Zakamska, Nadia L.; Riffel, Rogério

doi:10.1093/mnras/stz3137

Cited by 18 publications

(12 citation statements)

References 122 publications

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“…Krug et al 2010;Rupke & Veilleux 2011;Cazzoli et al 2016;Concas et al 2019;Roberts-Borsani 2020), cold molecular gas phase, using different transitions of CO, HCN and [C ii], for instance (e.g. García-Burillo et al 2014;Tadhunter et al 2014;Feruglio et al 2017;Aladro et al 2018;Michiyama et al 2018;Zschaechner et al 2018;Aalto et al 2019;Husemann et al 2019;Cicone et al 2020;Veilleux et al 2020), warm and hot molecular gas phase, using transitions in the mid-to near-infrared (Veilleux et al 2009;Davies et al 2014;Hill & Zakamska 2014;Riffel et al 2015;Emonts et al 2017;May et al 2018;Petric et al 2018;Riffel et al 2020) and ionised gas phase observed using the rest-frame optical emission lines such as the forbidden transitions of [O iii] λ5007 (e.g. Harrison et al 2014;Kakkad et al 2016;Zakamska et al 2016;Fiore et al 2017;Venturi et al 2018;Baron & Netzer 2019;Coatman et al 2019;Förster Schreiber et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Super

Kakkad

Mainieri

Vietri

et al. 2020

A&A

101

109

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Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) aims to trace and characterise ionised gas outflows and their impact on star formation in a statistical sample of X-ray selected active galactic nuclei (AGN) at z ∼ 2. We present the first SINFONI results for a sample of 21 Type 1 AGN spanning a wide range in bolometric luminosity (log Lbol = 45.4–47.9 erg s−1). The main aims of this paper are to determine the extension of the ionised gas, characterise the occurrence of AGN-driven outflows, and link the properties of such outflows with those of the AGN. Methods. We used adaptive optics-assisted SINFONI observations to trace ionised gas in the extended narrow line region using the [O III] λ5007 line. We classified a target as hosting an outflow if its non-parametric velocity of the [O III] line, w80, was larger than 600 km s−1. We studied the presence of extended emission using dedicated point-spread function (PSF) observations, after modelling the PSF from the Balmer lines originating from the broad line region. Results. We detect outflows in all the Type 1 AGN sample based on the w80 value from the integrated spectrum, which is in the range ∼650–2700 km s−1. There is a clear positive correlation between w80 and the AGN bolometric luminosity (> 99% correlation probability), and the black hole mass (98% correlation probability). A comparison of the PSF and the [O III] radial profile shows that the [O III] emission is spatially resolved for ∼35% of the Type 1 sample and the outflows show an extension up to ∼6 kpc. The relation between maximum velocity and the bolometric luminosity is consistent with model predictions for shocks from an AGN-driven outflow. The escape fraction of the outflowing gas increases with the AGN luminosity, although for most galaxies, this fraction is less than 10%.

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Section: Introductionmentioning

confidence: 99%

Super

Kakkad

Mainieri

Vietri

et al. 2020

A&A

101

109

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“…The warm (T ∼ 500 K) molecular gas phase may also be important and carry a significant fraction of the momentum in a galactic outflow (Richings & Faucher-Giguère 2018). In nearby galaxies, Spitzer observations of the warm molecular H 2 gas (T ∼ 500 K) have found a significant amount of gas mass in galactic outflows (Dasyra et al 2014;Beirão et al 2015;Riffel et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Multiphase Outflows in High-redshift Quasar Host Galaxies

Vayner

Zakamska

Wright

et al. 2021

ApJ

Self Cite

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We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of six radio-loud quasar host galaxies at z = 1.4–2.3. We combine the kiloparsec-scale resolution ALMA observations with high spatial resolution adaptive optics integral field spectrograph data of the ionized gas. We detect molecular gas emission in five quasar host galaxies and resolve the molecular interstellar medium using the CO (3–2) or CO (4–3) rotational transitions. Clumpy molecular outflows are detected in four quasar host galaxies and a merger system 21 kpc away from one quasar. Between the ionized and cold molecular gas phases, the majority of the outflowing mass is in a molecular phase, while for three out of four detected multiphase gas outflows, the majority of the kinetic luminosity and momentum flux is in the ionized phase. Combining the energetics of the multiphase outflows, we find that their driving mechanism is consistent with energy-conserving shocks produced by the impact of the quasar jets with the gas in the galaxy. By assessing the molecular gas mass to the dynamics of the outflows, we estimate a molecular gas depletion timescale of a few megayears. The gas outflow rates exceed the star formation rates, suggesting that quasar feedback is a major mechanism of gas depletion at the present time. The coupling efficiency between the kinetic luminosity of the outflows and the bolometric luminosity of the quasar of 0.1%–1% is consistent with theoretical predictions. Studying multiphase gas outflows at high redshift is important for quantifying the impact of negative feedback in shaping the evolution of massive galaxies.

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“…Ellison et al 2019), so if the time-scales for shocked H 2 gas are similar to those of AGN then the statistics of shocked H 2 gas should change with AGN triggering mechanism because different AGN triggering could lead to different gas motions and properties. Riffel et al (2020) use SDSS optical spectra for a subsample of the Lambrides et al (2019) galaxies to suggest that excess of MIR H 2 emission seen in AGN is produced by shocks due to AGN driven outflows in the same clouds that produce [OI] emission. Spatially resolved kinematics would be required to confirm this hypothesis.…”

Section: Discussionmentioning

confidence: 99%

Molecular Gas Heating and Modified Dust Properties in Active Galaxies: Growing Black Holes or Tidal Shocks?

Minsley,

Petric,

Lambrides

et al. 2020

Preprint

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We investigate if and how growing super-massive black holes (SMBH) known as Active Galactic Nuclei (AGN) and gravitational interactions affect the warm molecular gas and dust of galaxies. Our analysis focuses on the morphologies and warm ISM properties of 630 galaxies at z < 0.1. We use grizy images from the Pan-STARRS survey to classify the galaxies into mergers, early mergers, and non-mergers. We use MIR spectroscopic measurements of emission from rotational H 2 transitions, dust and PAH features, and silicate emission or absorption lines at 9.7 µm to study how gravitational interactions impact the warm ISM in AGN and non-AGN hosts.We find that in AGN-hosts, the ISM is warmer, the ratios of H 2 to PAHs are larger, the PAH emission line ratios and silicate strengths have a wider range of values than in non-AGN hosts. We find some statistical differences between the H 2 emission of mergers and non-mergers, but those differences are less statistically significant than those between AGN and non-AGN hosts.Our results do not establish a relation between the rate of BH growth and the warm ISM but point to highly statistically significant differences between AGN hosts and non-AGN hosts, differences that are not present with the same statistical significance between mergers and non-mergers. We speculate that the combination of triggering mechanisms, AGN orientations, and evolutionary stages that allow AGN to be classified as such in the MIR indicate that those AGN are energetically coupled on kpc scales to their host galaxies's warm ISM. Future optical and IR, spatially resolved spectroscopic studies are best suited to characterize this connection.

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Active galactic nuclei winds as the origin of the H2 emission excess in nearby galaxies

Cited by 18 publications

References 122 publications

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Multiphase Outflows in High-redshift Quasar Host Galaxies

Molecular Gas Heating and Modified Dust Properties in Active Galaxies: Growing Black Holes or Tidal Shocks?

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