High-velocity extended molecular outflow in the star-formation dominated luminous infrared galaxy ESO 320-G030

Pereira-Santaella, M.; Colina, L.; García‐Burillo, S.; Alonso‐Herrero, A.; Arribas, S.; Cazzoli, S.; Emonts, Bjorn; López, Javier Piqueras; Planesas, P.; Storchi‐Bergmann, Thaisa; Usero, A.; Villar-Martı́n, M.

doi:10.1051/0004-6361/201628875

Cited by 50 publications

(83 citation statements)

References 91 publications

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“…The emission feature appears to have a weak counterpart in OH119 as well. In addition, the high-lying OH84 line shows hints of a blueshifted line wing in absorption, possibly indicating the coexistence of an outflow in the nuclear region, as observed in CO (Pereira-Santaella et al 2016). In IRAS 15250+3609, the observed OH119, OH79, and OH65 doublets are also redshifted relative to [C ii], and OH119 shows a broad emission feature between ∼ −300 and −1000 km s −1 .…”

Section: Inflowsmentioning

confidence: 79%

Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis

González-Alfonso

Fischer

Spoon

et al. 2017

ApJ

146

204

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We report on the energetics of molecular outflows in 14 local Ultraluminous Infrared Galaxies (ULIRGs) that show unambiguous outflow signatures (P-Cygni profiles or high-velocity absorption wings) in the far-infrared lines of OH measured with the Herschel/PACS spectrometer. All sample galaxies are gas-rich mergers at various stages of the merging process. Detection of both ground-state (at 119 and 79 µm) and one or more radiatively-excited (at 65 and 84 µm) lines allows us to model the nuclear gas ( 300 pc) as well as the more extended components using spherically symmetric radiative transfer models. Reliable models and the corresponding energetics are found in 12 of the 14 sources. The highest molecular outflow velocities are found in buried sources, in which slower but massive expansion of the nuclear gas is also observed. With the exception of a few outliers, the outflows have momentum fluxes of (2 − 5) × L IR /c and mechanical luminosities of (0.1 − 0.3)% of L IR . The moderate momentum boosts in these sources ( 3) suggest that the outflows are mostly momentum-driven by the combined effects of AGN and nuclear starbursts, as a result of radiation pressure, winds, and supernovae remnants. In some sources (∼ 20%), however, powerful (10 10.5−11 L ⊙ ) AGN feedback and (partially) energy-conserving phases are required, with momentum boosts in the range 3 − 20. These outflows appear to be stochastic, strong-AGN feedback events that occur throughout the merging process. In a few sources, the outflow activity in the innermost regions has subsided in the last ∼ 1 Myr. While OH traces the molecular outflows at sub-kpc scales, comparison of the masses traced by OH with those previously inferred from tracers of more extended outflowing gas suggests that most mass is loaded (with loading factors ofṀ /SFR = 1 − 10) from the central galactic cores (a few × 100 pc), qualitatively consistent with an ongoing inside-out quenching of star formation. Outflow depletion timescales are < 10 8 yr, shorter than the gas consumption timescales by factors of 1.1 − 15, and are anti-correlated with the AGN luminosity.

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Section: Inflowsmentioning

confidence: 79%

Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis

González-Alfonso

Fischer

Spoon

et al. 2017

ApJ

146

204

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“…(PL12). ‡ Based on a hot-to-cold molecular gas mass ratio of 6 × 10 −5 (Emonts et al 2014;Pereira-Santaella et al 2016). …”

Section: H 2 Mass Of the Outflowsmentioning

confidence: 99%

“…These studies focused on the coldest phase of molecular outflows, by using strong tracers like CO andOH 119µm (e.g., Feruglio et al 2010, 2015;Fischer et al 2010;Chung et al 2011;Sturm et al 2011;Spoon et al 2013;Veilleux et al 2013;Dasyra & Combes 2012;Dasyra et al 2014;Cicone et al 2014;Sakamoto et al 2014;García-Burillo et al 2015;Aalto et al 2015;Pereira-Santaella et al 2016;González-Alfonso et al 2017). Direct measurements of molecular hydrogen in outflows rely on detecting warm and hot H 2 emission in the mid-to near-IR (e.g., Valentijn & van der Article number, page 1 of 11 arXiv:1708.09503v1 [astro-ph.GA] 30 Aug 2017 A&A proofs: manuscript no.…”

Section: Introductionmentioning

confidence: 99%

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

Emonts

Colina

López

et al. 2017

A&A

Self Cite

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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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“…Most of the cold outflowing material is likely falling back to the disk (fountain scenario). We studied in detail the neutral, ionized and molecular phases of the outflow in the LIRG IRAS F11506-3851 (Cazzoli et al, 2014;Pereira-Santaella et al, 2016). The outflow (a galactic fountain) is ejecting a significant amount of gas from the central regions at a rate of 1.4 times larger than the ongoing SF.…”

Section: Discussionmentioning

confidence: 99%

“…SC contributed also the analysis and interpretation of SINFONI and X-shooter observations (Cazzoli et al, 2014 andMaiolino et al, 2017, respectively). SC contributed also to interpretation of ALMA data (Pereira-Santaella et al, 2016). This manuscript is partially based on the PhD thesis of SC (available online at http://hdl.handle.net/10486/676308, in line with Universidad Autonoma de Madrid policies).…”

Section: Author Contributionsmentioning

confidence: 96%

Negative and Positive Outflow-Feedback in Nearby (U)LIRGs

Cazzoli

2017

Front. Astron. Space Sci.

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The starburst-AGN coexistence in local (U)LIRGs makes these galaxies excellent laboratories for the study of stellar and AGN outflows and feedback. Outflows regulate star formation and AGN activity, redistributing gas, dust and metals over large scales in the interstellar and intergalactic media (negative feedback) being also considered to be able to undergo vigorous star formation (positive feedback). In this contribution, I will summarize the results from a search for outflows in a sample of nearby 38 local (U)LIRG systems observed with VIMOS/VLT integral field unit. For two galaxies of the sample I will detail the outflow properties and discuss the observational evidence for negative and positive outflow-feedback. The assessment of both negative and positive feedback effects represent a novel approach toward a comprehensive understanding of the impact of outflow feedback in the galaxy evolution.

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High-velocity extended molecular outflow in the star-formation dominated luminous infrared galaxy ESO 320-G030

Cited by 50 publications

References 91 publications

Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis

Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis

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

Negative and Positive Outflow-Feedback in Nearby (U)LIRGs

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