ERRATUM: “BREAKING THE OBSCURING SCREEN: A RESOLVED MOLECULAR OUTFLOW IN A BURIED QSO” (2013, ApJL, 775, L15)

Rupke, David S. N.; Veilleux, Sylvain

doi:10.3847/2041-8205/827/1/l20

Cited by 12 publications

(42 citation statements)

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“…For all three ULIRGs, the outflow velocity reaches a maximum at roughly 0.5 kpc distance from the core. These properties are similar to those of the conical, nuclear H 2 outflow that was first imaged with near-IR integral-field spectroscopy in QSO F08572+3915 (Rupke & Veilleux 2013b). …”

Section: Geometry and Kinematics Of The Outflowssupporting

confidence: 69%

Outflows of hot molecular gas in ultra-luminous infrared galaxies mapped with VLT-SINFONI

Emonts

Colina

López

et al. 2017

A&A

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We present the detection and morphological characterization of hot molecular gas outflows in nearby ultra-luminous infra-red galaxies (ULIRGs), using the Spectrograph for Integral Field Observations in the Near Infrared (SINFONI) on the Very Large Telescope (VLT). We detect outflows observed in the 2.12µm H 2 1-0 S(1) line for three out of four ULIRGs that we analyzed, namely IRAS 12112+0305, IRAS 14348-1447, and IRAS 22491-1808. The outflows are mapped on scales of 0.7 − 1.6 kpc, show typical outflow velocities of 300−500 km s −1 , and appear to originate from the nuclear region. The outflows comprise hot molecular gas masses of M H 2 (hot) ∼ 6−8 ×10 3 M . Assuming a hot-to-cold molecular gas mass ratio of 6 × 10 −5 , as found in nearby luminous infrared galaxies, the total (hot+cold) molecular gas mass in these outflows is expected to be M H 2 (tot) ∼ 1 × 10 8 M . This translates into molecular mass outflow rates ofṀ H 2 (tot) ∼ 30 − 85 M yr −1 , which is a factor of a few lower than the star formation rate in these ULIRGs. In addition, most of the outflowing molecular gas does not reach the escape velocity of these merger systems, which implies that the bulk of the outflowing molecular gas is re-distributed within the system and thus remains available for future star formation. The fastest H 2 outflow is seen in the Compton-thick AGN of IRAS 14348-1447, reaching a maximum outflow velocity of ∼900 km s −1 . Another ULIRG, IRAS 17208-0014, shows asymmetric H 2 line profiles different from the outflows seen in the other three ULIRGs. We discuss several alternative explanations for the line asymmetries in this system, including a very gentle galactic wind, internal gas dynamics, low-velocity gas outside the disk, or two superposed gas disks. We do not detect the hot molecular counterpart to the outflow previously detected in CO(2-1) in IRAS 17208-0014, but we note that our SINFONI data are not sensitive enough to detect this outflow if it has a small hot-to-cold molecular gas mass ratio of 9 × 10 −6 .

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Section: Geometry and Kinematics Of The Outflowssupporting

confidence: 69%

Outflows of hot molecular gas in ultra-luminous infrared galaxies mapped with VLT-SINFONI

Emonts

Colina

López

et al. 2017

A&A

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“…The latter two are the nearest galaxies in this sample and have deep, high-S/N integrations. The F05189−2524 fits are similar to those previously published (Rupke et al 2005a;Rupke & Veilleux 2015), though here the binning is coarser and the spatially unresolved continuum has been removed to match the treatment of the rest of the sample. The integrated spectrum requires 3 components in absorption, while the spaxel-by-spaxel fit uses 2 components.…”

Section: Absorption Line Fittingsupporting

confidence: 61%

“…For galaxies in which more than one emission line component was fitted, two other panels appear: a map of the flux density at a representative blueshifted velocity, and a map of the velocity that encompasses 98% of the cumulative velocity distribution in each spaxel, v 98% c2 . This convention matches that used in some previous IFS studies (Rupke & Veilleux 2011, 2013a. The cumulative percentages are derived in blueshifted spaxels by integrating from the red side of the velocity distribution, such that v 98% c2 is representative of a "maximum" blueshifted velocity.…”

Section: Emission Line Fittingmentioning

confidence: 74%

“…F07599+6508 and Mrk 231 show broad absorption (Boroson & Meyers 1992;Veilleux et al 2013bVeilleux et al , 2016. F05189−2524 (Rupke & Veilleux 2015), F13342+3932, and PG1411+442 (Hamann et al 2017, in prep. ) show narrow absorption.…”

Section: Absorption Line Fittingmentioning

confidence: 97%

“…The properties of quasar-mode AGN outflows (velocity, mass outflow rate) correlate with bolometric AGN luminosity (Sturm et al 2011;Spoon et al 2013;Veilleux et al 2013a;Rupke & Veilleux 2013b;Cicone et al 2014;Stone et al 2016;González-Alfonso et al 2017;Sun et al 2017;Fiore et al 2017). The gas depletion timescales are short in the most luminous AGN, suggesting that feedback is most effective in these systems (Cicone et al 2014;González-Alfonso et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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Quasar-mode Feedback in Nearby Type 1 Quasars: Ubiquitous Kiloparsec-scale Outflows and Correlations with Black Hole Properties

Rupke

Gültekin

Veilleux

2017

ApJ

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170

195

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The prevalence and properties of kiloparsec-scale outflows in nearby Type 1 quasars have been the subject of little previous attention. This work presents Gemini integral field spectroscopy of ten Type 1 radio-quiet quasars at z < 0.3. The excellent image quality, coupled with a new technique to remove the point spread function using spectral information, allow the fitting of the underlying host on a spaxel-by-spaxel basis. Fits to stars, line-emitting gas, and interstellar absorption show that 100% of the sample host warm ionized and/or cool neutral outflows with spatially-averaged velocities ( v 98% ≡ v + 2σ ) of 200-1300 km s −1 and peak velocities (maximum v 98% ) of 500-2600 km s −1 . These minor-axis outflows are powered primarily by the central AGN, reach scales of 3-12 kpc, and often fill the field of view. Including molecular data and Type 2 quasar measurements, nearby quasars show a wide range in mass outflow rates (dM/dt = 1 to >1000 M yr −1 ) and momentum boosts [(c dp/dt)/L AGN = 0.01 − 20]. After extending the mass scale to Seyferts, dM/dt and dE/dt correlate with black hole mass (dM/dt ∼ M 0.7±0.3 BHand dE/dt ∼ M 1.3±0.5 BH). Thus, the most massive black holes in the local universe power the most massive and energetic quasar-mode winds.

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Massive molecular outflows and evidence for AGN feedback from CO observations

Cicone

Maiolino

Sturm

et al. 2014

A&A

888

126

1,224

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We study the properties of massive, galactic-scale outflows of molecular gas and investigate their impact on galaxy evolution. We present new IRAM PdBI CO(1-0) observations of local ULIRGs and QSO hosts: clear signature of massive and energetic molecular outflows, extending on kpc scales, is found in the CO(1-0) kinematics of four out of seven sources, with measured outflow rates of several 100 M yr −1 . We combine these new observations with data from the literature, and explore the nature and origin of massive molecular outflows within an extended sample of 19 local galaxies. We find that starburst-dominated galaxies have an outflow rate comparable to their SFR, or even higher by a factor of ∼2-4, implying that starbursts can indeed be effective in removing cold gas from galaxies. Nevertheless, our results suggest that the presence of an AGN can boost the outflow rate by a large factor, which is found to increase with the L AGN /L bol ratio. The gas depletion time-scales due to molecular outflows are anti-correlated with the presence and luminosity of an AGN in these galaxies, and range from a few hundred million years in starburst galaxies, down to just a few million years in galaxies hosting powerful AGNs. In quasar hosts the depletion time-scales due to the outflow are much shorter than the depletion time-scales due to star formation. We estimate the outflow kinetic power and find that, for galaxies hosting powerful AGNs, it corresponds to about 5% of the AGN luminosity, as expected by models of AGN feedback. Moreover, we find that momentum rates of about 20 L AGN /c are common among the AGN-dominated sources in our sample. For "pure" starburst galaxies our data tentatively support models in which outflows are mostly momentum-driven by the radiation pressure from young stars onto dusty clouds. Overall, our results indicate that, although starbursts are effective in powering massive molecular outflows, the presence of an AGN may strongly enhance such outflows and, therefore, have a profound feedback effect on the evolution of galaxies, by efficiently removing fuel for star formation, hence quenching star formation.

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ERRATUM: “BREAKING THE OBSCURING SCREEN: A RESOLVED MOLECULAR OUTFLOW IN A BURIED QSO” (2013, ApJL, 775, L15)

Cited by 12 publications

References 0 publications

Outflows of hot molecular gas in ultra-luminous infrared galaxies mapped with VLT-SINFONI

Outflows of hot molecular gas in ultra-luminous infrared galaxies mapped with VLT-SINFONI

Quasar-mode Feedback in Nearby Type 1 Quasars: Ubiquitous Kiloparsec-scale Outflows and Correlations with Black Hole Properties

Massive molecular outflows and evidence for AGN feedback from CO observations

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