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Qizhou Zhang - One of the best experts on this subject based on the ideXlab platform.
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hot core Outflows and magnetic fields in w43 mm1 g30 79 fir 10
The Astrophysical Journal, 2014Co-Authors: T K Sridharan, Ramprasad Rao, Keping Qiu, Paulo C Cortes, Thushara Pillai, N A Patel, Qizhou ZhangAbstract:We present submillimeter spectral line and dust continuum polarization observations of a remarkable hot core and multiple Outflows in the high-mass, star-forming region W43-MM1 (G30.79 FIR 10), obtained using the Submillimeter Array. A temperature of ~400 K is estimated for the hot core using CH_(3)CN (J = 19–18) lines, with detections of 11 K-ladder components. The high temperature and the mass estimates for the Outflows indicate high-mass star formation. The continuum polarization pattern shows an ordered distribution, and its orientation over the main Outflow appears to be aligned with the Outflow. The derived magnetic field indicates slightly super-critical conditions. While the magnetic and Outflow energies are comparable, the B-field orientation appears to have changed from parsec scales to ~0.1 pc scales during the core/star formation process.
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hot core Outflows and magnetic fields in w43 mm1 g30 79 fir 10
arXiv: Astrophysics of Galaxies, 2013Co-Authors: T K Sridharan, Ramprasad Rao, Keping Qiu, Paulo C Cortes, Thushara Pillai, N A Patel, Qizhou ZhangAbstract:We present submillimeter spectral line and dust continuum polarization observations of a remarkable hot core and multiple Outflows in the high-mass star-forming region W43-MM1 (G30.79 FIR 10), obtained using the Submillimeter Array (SMA). A temperature of $\sim$ 400 K is estimated for the hot-core using CH$_3$CN (J=19-18) lines, with detections of 11 K-ladder components. The high temperature and the mass estimates for the Outflows indicate high-mass star-formation. The continuum polarization pattern shows an ordered distribution, and its orientation over the main Outflow appears aligned to the Outflow. The derived magnetic field indicates slightly super-critical conditions. While the magnetic and Outflow energies are comparable, the B-field orientation appears to have changed from parsec scales to $\sim$ 0.1 pc scales during the core/star-formation process.
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discovery of extremely high velocity molecular bullets in the hh 80 81 high mass star forming region
The Astrophysical Journal, 2009Co-Authors: Keping Qiu, Qizhou ZhangAbstract:We present Submillimeter Array 1.3 mm waveband continuum and molecular line observations of the HH 80-81 high-mass star-forming region. The dust continuum emission reveals two dominant peaks, MM1 and MM2, and line emission from high-density tracers suggests the presence of another core, MC. Molecular line emission from MM1, which harbors the exciting source of the HH 80-81 radio jet, yields a hot molecular core at a gas temperature of 110 K. The two younger cores, MM2 and MC, both appear to power collimated CO Outflows. In particular, the Outflow arising from MM2 exhibits a jet-like morphology and a broad velocity range of 190 km s{sup -1}. The Outflow contains compact and fast moving molecular clumps, known as 'molecular bullets', first discovered in low-mass class 0 protostellar Outflows. These 'bullets' cannot be locally entrained or swept up from the ambient gas, but are more likely ejected from the close vicinity of the central protostar. The discovery of this remarkable Outflow manifests an episodic, disk-mediated accretion for massive star formation.
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discovery of extremely high velocity molecular bullets in the hh 80 81 high mass star forming region
arXiv: Astrophysics of Galaxies, 2009Co-Authors: Keping Qiu, Qizhou ZhangAbstract:We present Submillimter Array 1.3 mm waveband continuum and molecular line observations of the HH 80-81 high-mass star-forming region. The dust continuum emission reveals two dominant peaks MM1 and MM2, and line emission from high-density tracers suggests the presence of another core MC. Molecular line emission from MM1, which harbors the exciting source of the HH 80-81 radio jet, yields a hot molecular core at a gas temperature of 110 K. The two younger cores MM2 and MC both appear to power collimated CO Outflows. In particular, the Outflow arising from MM2 exhibits a jet-like morphology and a broad velocity range of 190 km/s. The Outflow contains compact and fast moving molecular clumps, known as "molecular bullets" first discovered in low-mass class 0 protostellar Outflows. These "bullets" cannot be locally entrained or swept up from the ambient gas, but are more likely ejected from the close vicinity of the central protostar. The discovery of this remarkable Outflow manifests an episodic, disk-mediated accretion for massive star formation.
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search for co Outflows toward a sample of 69 high mass protostellar candidates frequency of occurrence
The Astrophysical Journal, 2001Co-Authors: Qizhou Zhang, T R Hunter, J Brand, T K Sridharan, S Molinari, Mark A Kramer, R CesaroniAbstract:A survey for molecular Outflows was carried out by mapping the CO J = 2-1 line toward a sample of 69 luminous IRAS point sources. Sixty objects have IRAS luminosities from 103 to 105 L☉ and are associated with dense gas traced by NH3, identifying them as high-mass star-forming regions. Among 69 sources, 65 sources have data that are suitable for Outflow identification. Thirty-nine regions show spatially confined high-velocity wing emission in CO, indicative of molecular Outflows. Most objects without identifiable Outflows lie within 0° < l < 50° where Outflow signatures are confused by multiple cloud components along the line of sight. Excluding 26 sources with 0° < l < 50°, we found 35 Outflows out of 39 sources, which yields an Outflow detection rate of 90%. Many of the Outflows contain masses of more than 10 M☉ and have momenta of a few hundred M☉ km s-1, at least 2 orders of magnitude larger than those in typical low-mass Outflows. This class of massive and energetic Outflows is most likely driven by high-mass young stellar objects. The high detection rate indicates that molecular Outflows are common toward high-mass young stars. Given the connection between Outflows and accretion disks in low-mass stars, we suggest that high-mass stars may form via an accretion-Outflow process, similar to their low-mass counterparts.
Keping Qiu - One of the best experts on this subject based on the ideXlab platform.
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hot core Outflows and magnetic fields in w43 mm1 g30 79 fir 10
The Astrophysical Journal, 2014Co-Authors: T K Sridharan, Ramprasad Rao, Keping Qiu, Paulo C Cortes, Thushara Pillai, N A Patel, Qizhou ZhangAbstract:We present submillimeter spectral line and dust continuum polarization observations of a remarkable hot core and multiple Outflows in the high-mass, star-forming region W43-MM1 (G30.79 FIR 10), obtained using the Submillimeter Array. A temperature of ~400 K is estimated for the hot core using CH_(3)CN (J = 19–18) lines, with detections of 11 K-ladder components. The high temperature and the mass estimates for the Outflows indicate high-mass star formation. The continuum polarization pattern shows an ordered distribution, and its orientation over the main Outflow appears to be aligned with the Outflow. The derived magnetic field indicates slightly super-critical conditions. While the magnetic and Outflow energies are comparable, the B-field orientation appears to have changed from parsec scales to ~0.1 pc scales during the core/star formation process.
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hot core Outflows and magnetic fields in w43 mm1 g30 79 fir 10
arXiv: Astrophysics of Galaxies, 2013Co-Authors: T K Sridharan, Ramprasad Rao, Keping Qiu, Paulo C Cortes, Thushara Pillai, N A Patel, Qizhou ZhangAbstract:We present submillimeter spectral line and dust continuum polarization observations of a remarkable hot core and multiple Outflows in the high-mass star-forming region W43-MM1 (G30.79 FIR 10), obtained using the Submillimeter Array (SMA). A temperature of $\sim$ 400 K is estimated for the hot-core using CH$_3$CN (J=19-18) lines, with detections of 11 K-ladder components. The high temperature and the mass estimates for the Outflows indicate high-mass star-formation. The continuum polarization pattern shows an ordered distribution, and its orientation over the main Outflow appears aligned to the Outflow. The derived magnetic field indicates slightly super-critical conditions. While the magnetic and Outflow energies are comparable, the B-field orientation appears to have changed from parsec scales to $\sim$ 0.1 pc scales during the core/star-formation process.
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discovery of extremely high velocity molecular bullets in the hh 80 81 high mass star forming region
The Astrophysical Journal, 2009Co-Authors: Keping Qiu, Qizhou ZhangAbstract:We present Submillimeter Array 1.3 mm waveband continuum and molecular line observations of the HH 80-81 high-mass star-forming region. The dust continuum emission reveals two dominant peaks, MM1 and MM2, and line emission from high-density tracers suggests the presence of another core, MC. Molecular line emission from MM1, which harbors the exciting source of the HH 80-81 radio jet, yields a hot molecular core at a gas temperature of 110 K. The two younger cores, MM2 and MC, both appear to power collimated CO Outflows. In particular, the Outflow arising from MM2 exhibits a jet-like morphology and a broad velocity range of 190 km s{sup -1}. The Outflow contains compact and fast moving molecular clumps, known as 'molecular bullets', first discovered in low-mass class 0 protostellar Outflows. These 'bullets' cannot be locally entrained or swept up from the ambient gas, but are more likely ejected from the close vicinity of the central protostar. The discovery of this remarkable Outflow manifests an episodic, disk-mediated accretion for massive star formation.
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discovery of extremely high velocity molecular bullets in the hh 80 81 high mass star forming region
arXiv: Astrophysics of Galaxies, 2009Co-Authors: Keping Qiu, Qizhou ZhangAbstract:We present Submillimter Array 1.3 mm waveband continuum and molecular line observations of the HH 80-81 high-mass star-forming region. The dust continuum emission reveals two dominant peaks MM1 and MM2, and line emission from high-density tracers suggests the presence of another core MC. Molecular line emission from MM1, which harbors the exciting source of the HH 80-81 radio jet, yields a hot molecular core at a gas temperature of 110 K. The two younger cores MM2 and MC both appear to power collimated CO Outflows. In particular, the Outflow arising from MM2 exhibits a jet-like morphology and a broad velocity range of 190 km/s. The Outflow contains compact and fast moving molecular clumps, known as "molecular bullets" first discovered in low-mass class 0 protostellar Outflows. These "bullets" cannot be locally entrained or swept up from the ambient gas, but are more likely ejected from the close vicinity of the central protostar. The discovery of this remarkable Outflow manifests an episodic, disk-mediated accretion for massive star formation.
Hector G Arce - One of the best experts on this subject based on the ideXlab platform.
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molecular Outflows driven by low mass protostars i correcting for underestimates when measuring Outflow masses and dynamical properties
The Astrophysical Journal, 2014Co-Authors: Amelia M Stutz, Hector G Arce, Michael M Dunham, Diego Mardones, Brenda C Matthews, Jonathan WilliamsAbstract:We present a survey of 28 molecular Outflows driven by low-mass protostars, all of which are sufficiently isolated spatially and/or kinematically to fully separate into individual Outflows. Using a combination of new and archival data from several single-dish telescopes, 17 Outflows are mapped in 12CO (2-1) and 17 are mapped in 12CO (3-2), with 6 mapped in both transitions. For each Outflow, we calculate and tabulate the mass (M flow), momentum (P flow), kinetic energy (E flow), mechanical luminosity (L flow), and force (F flow) assuming optically thin emission in LTE at an excitation temperature, T ex, of 50 K. We show that all of the calculated properties are underestimated when calculated under these assumptions. Taken together, the effects of opacity, Outflow emission at low velocities confused with ambient cloud emission, and emission below the sensitivities of the observations increase Outflow masses and dynamical properties by an order of magnitude, on average, and factors of 50-90 in the most extreme cases. Different (and non-uniform) excitation temperatures, inclination effects, and dissociation of molecular gas will all work to further increase Outflow properties. Molecular Outflows are thus almost certainly more massive and energetic than commonly reported. Additionally, Outflow properties are lower, on average, by almost an order of magnitude when calculated from the 12CO (3-2) maps compared to the 12CO (2-1) maps, even after accounting for different opacities, map sensitivities, and possible excitation temperature variations. It has recently been argued in the literature that the 12CO (3-2) line is subthermally excited in Outflows, and our results support this finding.
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molecular Outflows driven by low mass protostars i correcting for underestimates when measuring Outflow masses and dynamical properties
arXiv: Astrophysics of Galaxies, 2014Co-Authors: Amelia M Stutz, Hector G Arce, Michael M Dunham, Diego Mardones, Jeongeun Lee, Brenda C Matthews, Jonathan WilliamsAbstract:We present a survey of 28 molecular Outflows driven by low-mass protostars, all of which are sufficiently isolated spatially and/or kinematically to fully separate into individual Outflows. Using a combination of new and archival data from several single-dish telescopes, 17 Outflows are mapped in CO (2-1) and 17 are mapped in CO (3-2), with 6 mapped in both transitions. For each Outflow, we calculate and tabulate the mass, momentum, kinetic energy, mechanical luminosity, and force assuming optically thin emission in LTE at an excitation temperature of 50 K. We show that all of the calculated properties are underestimated when calculated under these assumptions. Taken together, the effects of opacity, Outflow emission at low velocities confused with ambient cloud emission, and emission below the sensitivities of the observations increase Outflow masses and dynamical properties by an order of magnitude, on average, and factors of 50-90 in the most extreme cases. Different (and non-uniform) excitation temperatures, inclination effects, and dissociation of molecular gas will all work to further increase Outflow properties. Molecular Outflows are thus almost certainly more massive and energetic than commonly reported. Additionally, Outflow properties are lower, on average, by almost an order of magnitude when calculated from the CO (3-2) maps compared to the CO (2-1) maps, even after accounting for different opacities, map sensitivities, and possible excitation temperature variations. It has recently been argued in the literature that the CO (3-2) line is subthermally excited in Outflows, and our results support this finding.
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radiation hydrodynamic simulations of protostellar Outflows synthetic observations and data comparisons
The Astrophysical Journal, 2011Co-Authors: Stella S R Offner, Eve J Lee, Alyssa A Goodman, Hector G ArceAbstract:We present results from three-dimensional, self-gravitating, radiation-hydrodynamic simulations of low-mass protostellar Outflows. We construct synthetic observations in 12CO in order to compare with observed Outflows and evaluate the effects of beam resolution and Outflow orientation on inferred Outflow properties. To facilitate the comparison, we develop a quantitative prescription for measuring Outflow opening angles. Using this prescription, we demonstrate that, in both simulations and synthetic observations, Outflow opening angles broaden with time similarly to observed Outflows. However, the interaction between the Outflowing gas and the turbulent core envelope produces significant asymmetry between the redshifted and blueshifted Outflow lobes. We find that applying a velocity cutoff may result in Outflow masses that are underestimated by a factor five or more, and masses derived from optically thick CO emission further underpredict the mass of the high-velocity gas by a factor of 5-10. Derived excitation temperatures indicate that Outflowing gas is hotter than the ambient gas with temperature rising over time, which is in agreement with the simulation gas temperatures. However, excitation temperatures are otherwise not well correlated with the actual gas temperature.
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radiation hydrodynamic simulations of protostellar Outflows synthetic observations and data comparisons
arXiv: Solar and Stellar Astrophysics, 2011Co-Authors: Stella S R Offner, Eve J Lee, Alyssa A Goodman, Hector G ArceAbstract:We present results from three-dimensional, self-gravitating, radiation-hydrodynamic simulations of low-mass protostellar Outflows. We construct synthetic observations in 12CO in order to compare with observed Outflows and evaluate the effects of beam resolution and Outflow orientation on inferred Outflow properties. To facilitate the comparison, we develop a quantitative prescription for measuring Outflow opening angles. Using this prescription, we demonstrate that, in both simulations and synthetic observations, Outflow opening angles broaden with time similarly to observed Outflows. However, the interaction between the Outflowing gas and the turbulent core envelope produces significant asymmetry between the red and blue shifted Outflow lobes. We find that applying a velocity cutoff may result in Outflow masses that are underestimated by a factor 5 or more, and masses derived from optically thick CO emission further underpredict the mass of the high-velocity gas by a factor of 5-10. Derived excitation temperatures indicate that Outflowing gas is hotter than the ambient gas with temperature rising over time, which is in agreement with the simulation gas temperatures. However, excitation temperatures are otherwise not well correlated with the actual gas temperature.
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the evolution of Outflow envelope interactions in low mass protostars
The Astrophysical Journal, 2006Co-Authors: Hector G Arce, Anneila I SargentAbstract:We present multiline and continuum observations of the circumstellar environment within 10to the 4th AU of a sample of protostars to investigate how the effects of Outflows on their immediate environment change over time. 12CO (1–0) emission probes the high-velocity molecular Outflows near the protostars and demonstrates that the Outflow opening angle widens as the nascent star evolves. Maps of the 13CO (1–0) and HCO+ (1–0) Outflow emission show that protostellar winds erode the circumstellar envelope through the entrainment of the outer envelope gas. The spatial and velocity distribution of the dense circumstellar envelope, as well as its mass, is traced by the C to the 18th O (1–0) emission and also displays evolutionary changes. We show that Outflows are largely responsible for these changes and propose an empirical model for the evolution of Outflow-envelope interactions. In addition, some of the Outflows in our sample appear to affect the chemical composition of the surrounding environment, enhancing the HCO+ abundance. Overall, our results confirm that Outflows play a major role in the star formation process through their strong physical and chemical impacts on the environments of the young protostars.
G Busch - One of the best experts on this subject based on the ideXlab platform.
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the close agn reference survey cars a massive multi phase Outflow impacting the edge on galaxy he 1353 1917
Astronomy and Astrophysics, 2019Co-Authors: B Husemann, J Scharwachter, Timothy A Davis, M A Pereztorres, I Smirnovapinchukova, G R Tremblay, M Krumpe, F Combes, S A Baum, G BuschAbstract:Context. Galaxy-wide Outflows driven by star formation and/or an active galactic nucleus (AGN) are thought to play a crucial rule in the evolution of galaxies and the metal enrichment of the inter-galactic medium. Direct measurements of these processes are still scarce and new observations are needed to reveal the nature of Outflows in the majority of the galaxy population. Aims. We combine extensive, spatially-resolved, multi-wavelength observations, taken as part of the Close AGN Reference Survey (CARS), for the edge-on disc galaxy HE 1353−1917 in order to characterise the impact of the AGN on its host galaxy via Outflows and radiation. Methods. Multi-color broad-band photometry was combined with spatially-resolved optical, near-infrared (NIR) and sub-mm and radio observations taken with the Multi-Unit Spectroscopy Explorer (MUSE), the Near-infrared Integral Field Spectrometer (NIFS), the Atacama Large Millimeter Array (ALMA), and the Karl G. Jansky Very Large Array (VLA) to map the physical properties and kinematics of the multi-phase interstellar medium. Results. We detect a biconical extended narrow-line region ionised by the luminous AGN orientated nearly parallel to the galaxy disc, extending out to at least 25 kpc. The extra-planar gas originates from galactic fountains initiated by star formation processes in the disc, rather than an AGN Outflow, as shown by the kinematics and the metallicity of the gas. Nevertheless, a fast, multi-phase, AGN-driven Outflow with speeds up to 1000 km s−1 is detected close to the nucleus at 1 kpc distance. A radio jet, in connection with the AGN radiation field, is likely responsible for driving the Outflow as confirmed by the energetics and the spatial alignment of the jet and multi-phase Outflow. Evidence for negative AGN feedback suppressing the star formation rate (SFR) is mild and restricted to the central kpc. But while any SFR suppression must have happened recently, the Outflow has the potential to greatly impact the future evolution of the galaxy disc due to its geometrical orientation. Conclusions.. Our observations reveal that low-power radio jets can play a major role in driving fast, multi-phase, galaxy-scale Outflows even in radio-quiet AGN. Since the Outflow energetics for HE 1353−1917 are consistent with literature, scaling relation of AGN-driven Outflows the contribution of radio jets as the driving mechanisms still needs to be systematically explored.
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the close agn reference survey cars a massive multi phase Outflow impacting the edge on galaxy he1353 1917
arXiv: Astrophysics of Galaxies, 2019Co-Authors: B Husemann, J Scharwachter, Timothy A Davis, M A Pereztorres, I Smirnovapinchukova, G R Tremblay, M Krumpe, F Combes, S A Baum, G BuschAbstract:[Abridged] We combine extensive spatially-resolved multi-wavelength observations, taken as part of the Close AGN Reference Survey (CARS), for the edge-on disc galaxy HE1353-1917 to characterize the impact of the AGN on its host galaxy via Outflows and radiation. Multi-color broad-band photometry is combined with spatially-resolved optical, NIR and sub-mm and radio observations taken with VLT/MUSE, Gemini-N/NIFS, ALMA and the VLA to map the physical properties and kinematics of the multi-phase inter-stellar medium (ISM). We detect a biconical extended narrow-line region (ENLR) ionized by the luminous AGN oriented nearly parallel to the galaxy disc, extending out to at least 25kpc. The extra-planar gas originates from galactic fountains initiated by star formation processes in the disc, rather than an AGN Outflow, as shown by the kinematics and the metallicity of the gas. Nevertheless, a fast multi-phase AGN-driven Outflow with speeds up to 1000km/s is detected close to the nucleus at 1kpc distance. A radio jet, in connection with the AGN radiation field, is likely responsible for driving the Outflow as confirmed by the energetics and the spatial alignment of the jet and multi-phase Outflow. Evidence for negative AGN feedback suppressing the star formation rate (SFR) is mild and restricted to the central kpc. But while any SFR suppression must have happened recently, the Outflow has the potential to greatly impact the future evolution of the galaxy disc due to its geometrical orientation. Our observations reveal that low-power radio jets can play a major role in driving fast multi-phase galaxy-scale Outflows even in radio-quiet AGN. Since the Outflow energetics for HE1353-1917 are consistent with literature scaling relations of AGN-driven Outflows the contribution of radio jets as the driving mechanisms still needs to be systematically explored.
Timothy A Davis - One of the best experts on this subject based on the ideXlab platform.
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centrally concentrated molecular gas driving galactic scale ionized gas Outflows in star forming galaxies
Monthly Notices of the Royal Astronomical Society, 2020Co-Authors: L M Hogarth, Timothy A Davis, Amelie Saintonge, L Cortese, S M Croom, Joss Blandhawthorn, Sarah Brough, Julia J Bryant, Barbara Catinella, Thomas J FletcherAbstract:We perform a joint-analysis of high spatial resolution molecular gas and star-formation rate (SFR) maps in main-sequence star-forming galaxies experiencing galactic-scale Outflows of ionised gas. Our aim is to understand the mechanism that determines which galaxies are able to launch these intense winds. We observed CO(1-0) at 1" resolution with ALMA in 16 edge-on galaxies, which also have 2" spatial resolution optical integral field observations from the SAMI Galaxy Survey. Half the galaxies in the sample were previously identified as harbouring intense and large-scale Outflows of ionised gas ("Outflow-types"), the rest serve as control galaxies. The dataset is complemented by integrated CO(1-0) observations from the IRAM 30-m telescope to probe the total molecular gas reservoirs. We find that the galaxies powering Outflows do not possess significantly different global gas fractions or star-formation efficiencies when compared with a control sample. However, the ALMA maps reveal that the molecular gas in the Outflow-type galaxies is distributed more centrally than in the control galaxies. For our Outflow-type objects, molecular gas and star-formation is largely confined within their inner effective radius ($\rm r_{eff}$), whereas in the control sample the distribution is more diffuse, extending far beyond $\rm r_{eff}$. We infer that Outflows in normal star-forming galaxies may be caused by dynamical mechanisms that drive molecular gas into their central regions, which can result in locally-enhanced gas surface density and star-formation.
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the close agn reference survey cars a massive multi phase Outflow impacting the edge on galaxy he 1353 1917
Astronomy and Astrophysics, 2019Co-Authors: B Husemann, J Scharwachter, Timothy A Davis, M A Pereztorres, I Smirnovapinchukova, G R Tremblay, M Krumpe, F Combes, S A Baum, G BuschAbstract:Context. Galaxy-wide Outflows driven by star formation and/or an active galactic nucleus (AGN) are thought to play a crucial rule in the evolution of galaxies and the metal enrichment of the inter-galactic medium. Direct measurements of these processes are still scarce and new observations are needed to reveal the nature of Outflows in the majority of the galaxy population. Aims. We combine extensive, spatially-resolved, multi-wavelength observations, taken as part of the Close AGN Reference Survey (CARS), for the edge-on disc galaxy HE 1353−1917 in order to characterise the impact of the AGN on its host galaxy via Outflows and radiation. Methods. Multi-color broad-band photometry was combined with spatially-resolved optical, near-infrared (NIR) and sub-mm and radio observations taken with the Multi-Unit Spectroscopy Explorer (MUSE), the Near-infrared Integral Field Spectrometer (NIFS), the Atacama Large Millimeter Array (ALMA), and the Karl G. Jansky Very Large Array (VLA) to map the physical properties and kinematics of the multi-phase interstellar medium. Results. We detect a biconical extended narrow-line region ionised by the luminous AGN orientated nearly parallel to the galaxy disc, extending out to at least 25 kpc. The extra-planar gas originates from galactic fountains initiated by star formation processes in the disc, rather than an AGN Outflow, as shown by the kinematics and the metallicity of the gas. Nevertheless, a fast, multi-phase, AGN-driven Outflow with speeds up to 1000 km s−1 is detected close to the nucleus at 1 kpc distance. A radio jet, in connection with the AGN radiation field, is likely responsible for driving the Outflow as confirmed by the energetics and the spatial alignment of the jet and multi-phase Outflow. Evidence for negative AGN feedback suppressing the star formation rate (SFR) is mild and restricted to the central kpc. But while any SFR suppression must have happened recently, the Outflow has the potential to greatly impact the future evolution of the galaxy disc due to its geometrical orientation. Conclusions.. Our observations reveal that low-power radio jets can play a major role in driving fast, multi-phase, galaxy-scale Outflows even in radio-quiet AGN. Since the Outflow energetics for HE 1353−1917 are consistent with literature, scaling relation of AGN-driven Outflows the contribution of radio jets as the driving mechanisms still needs to be systematically explored.
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the close agn reference survey cars a massive multi phase Outflow impacting the edge on galaxy he1353 1917
arXiv: Astrophysics of Galaxies, 2019Co-Authors: B Husemann, J Scharwachter, Timothy A Davis, M A Pereztorres, I Smirnovapinchukova, G R Tremblay, M Krumpe, F Combes, S A Baum, G BuschAbstract:[Abridged] We combine extensive spatially-resolved multi-wavelength observations, taken as part of the Close AGN Reference Survey (CARS), for the edge-on disc galaxy HE1353-1917 to characterize the impact of the AGN on its host galaxy via Outflows and radiation. Multi-color broad-band photometry is combined with spatially-resolved optical, NIR and sub-mm and radio observations taken with VLT/MUSE, Gemini-N/NIFS, ALMA and the VLA to map the physical properties and kinematics of the multi-phase inter-stellar medium (ISM). We detect a biconical extended narrow-line region (ENLR) ionized by the luminous AGN oriented nearly parallel to the galaxy disc, extending out to at least 25kpc. The extra-planar gas originates from galactic fountains initiated by star formation processes in the disc, rather than an AGN Outflow, as shown by the kinematics and the metallicity of the gas. Nevertheless, a fast multi-phase AGN-driven Outflow with speeds up to 1000km/s is detected close to the nucleus at 1kpc distance. A radio jet, in connection with the AGN radiation field, is likely responsible for driving the Outflow as confirmed by the energetics and the spatial alignment of the jet and multi-phase Outflow. Evidence for negative AGN feedback suppressing the star formation rate (SFR) is mild and restricted to the central kpc. But while any SFR suppression must have happened recently, the Outflow has the potential to greatly impact the future evolution of the galaxy disc due to its geometrical orientation. Our observations reveal that low-power radio jets can play a major role in driving fast multi-phase galaxy-scale Outflows even in radio-quiet AGN. Since the Outflow energetics for HE1353-1917 are consistent with literature scaling relations of AGN-driven Outflows the contribution of radio jets as the driving mechanisms still needs to be systematically explored.
