A 10 kpc SCALE SEYFERT GALAXY OUTFLOW:<i>HST</i>/COS OBSERVATIONS OF IRAS F22456–5125

Borguet, B.; Edmonds, Douglas A.; Arav, Nahum; Dunn, Jay P.; Kriss, G. A.

doi:10.1088/0004-637x/751/2/107

Cited by 79 publications

(109 citation statements)

References 36 publications

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“…Corroborating evidence for these outflows also comes from studies of absorption lines in the rest-frame UV spectrum of AGNs in the local universe (e.g., Arav et al 2012;Borguet et al 2012;Crenshaw & Kraemer 2012;Liu et al 2015) and at higher redshift (e.g., Moe et al 2009;Lucy et al 2014;Chamberlain & Arav 2015). While these studies provide convincing evidence for strong nongravitational motions affecting the ionized gas of luminous AGNs, they were unable to properly constrain either the detailed physical properties of these outflows or their impact on the host galaxies owingto the lack of spatially resolved information.…”

Section: Introductionmentioning

confidence: 99%

Unraveling the Complex Structure of Agn-Driven Outflows. I. Kinematics and Sizes

Karouzos

Woo

Bae

2016

ApJ

105

156

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Outflows driven by active galactic nuclei (AGNs) are often invoked as agents of the long-sought AGN feedback. Yet, characterizing and quantifying the impact on their host galaxies has been challenging. We present Gemini Multi-Object Spectrograph integral field unit data of six local (z 0.1 < ) and luminous (L 10In the first of a series of papers, we investigate the kinematics and constrain the size of the outflows. The ionized gas kinematics can be described as a superposition of a gravitational component that follows the stellar motion and an outflow-driven component that shows large velocity (up to 600 km s −1 ) and large velocity dispersion (up to 800 km s −1 ). Using the spatially resolved measurements of the gas, we kinematically measure the size of the outflow, which is found to be between 1.3 and 2.1 kpc. Owingto the lack of a detailed kinematic analysis, previous outflow studies likely overestimate their size by up to more than a factor of two, depending on how the size is estimated and whether the [O III] or Hα emission line is used. The relatively small size of the outflows for all six of our objects casts doubts on their potency as a mechanism for negative AGN feedback.

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Section: Introductionmentioning

confidence: 99%

Unraveling the Complex Structure of Agn-Driven Outflows. I. Kinematics and Sizes

Karouzos

Woo

Bae

2016

ApJ

105

156

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“…Fe ii, Si ii, and C ii have been detected in a handful of cases (e.g. Moe et al 2009;Dunn et al 2010;Borguet et al 2012). In the X-rays the identification of metastable lines from O v is hampered by uncertainties in the predicted line wavelength (Kaastra et al 2004).…”

Section: Introductionmentioning

confidence: 99%

SimultaneousXMM-Newtonand HST-COS observation of 1H0419-577

Gesu¹,

Costantini²,

Arav³

et al. 2013

A&A

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In this paper we analyze the X-ray, UV, and optical data of the Seyfert 1.5 galaxy 1H0419-577 with the aim of detecting and studying an ionized-gas outflow. The source was observed simultaneously in the X-rays with XMM-Newton and in the UV with HST-COS. Optical data were also acquired with the XMM-Newton Optical Monitor. We detected a thin, lowly ionized warm absorber (log ξ ≈ 0.03, log N H ≈ 19.9 cm −2 ) in the X-ray spectrum, which is consistent to be produced by the same outflow already detected in the UV. Provided the gas density estimated in the UV, the outflow is consistent to be located in the host galaxy at ∼kpc scale. Narrow emission lines were detected in the X-rays, in the UV and also in the optical spectrum. A single photoionized-gas model cannot account for all the narrow lines emission, indicating that the narrow line region is probably a stratified environment, differing in density and ionization. X-ray lines are unambiguously produced in a more highly ionized gas phase than the one emitting the UV lines. The analysis also suggests that the X-ray emitter may just be a deeper portion of the same gas layer producing the UV lines. Optical lines are probably produced in another disconnected gas system. The different ionization condition and the ∼pc scale location, suggested by the line width for the narrow lines emitters, are evidences against a connection between the warm absorber and the narrow line region in this source.

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“…A very heterogeneous data, covering a wide range in redshift z ∼ 0.1 − 2, are used in the figure. Our compilation include AGN which are known to show wind signatures in absorption (Edmonds et al 2011;Rupke et al 2005a;Krug et al 2010;Borguet et al 2012;Arav et al 2013;Borguet et al 2013;Rupke & Veilleux 2013;Chamberlain & Arav 2015), in ionized gas emission (Liu et al 2013;Rupke & Veilleux 2013;Harrison et al 2014Harrison et al , 2016McElroy et al 2015;Carniani et al 2015;Zakamska et al 2016) and in molecular gas (Combes et al 2013;Cicone et al 2014;Sun et al 2014;García-Burillo et al 2015;Tombesi et al 2015) All the absorption line and molecular gas based kinetic wind power measurements are taken directly from values published in the literature, while all the emission-line based the wind power measurements except those taken from Rupke & Veilleux (2013) are based on our calculations. Where the wind power measurements for the ionized gas are not available, we estimate them following the standard methods and assumptions (e.g., Nesvadba et al 2006;Harrison et al 2014;Zakamska et al 2016).…”

Section: Discussionmentioning

confidence: 99%

No Evidence for Feedback: Unexceptional Low-ionization Winds in Host Galaxies of Low Luminosity Active Galactic Nuclei at Redshift z ∼ 1

Yesuf

Koo

Faber

et al. 2017

ApJ

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We study winds in 12 X-ray AGN host galaxies at z ∼ 1. We find, using the low-ionization Fe II λ2586 absorption in the stacked spectra, that the probability distribution function (PDF) of the centroid velocity shift in AGN has a median, 16th and 84th percentiles of (-87, -251, +86) km s −1 respectively. The PDF of the velocity dispersion in AGN has a median, 84th and 16th percentile of (139, 253, 52) km s −1 respectively. The centroid velocity and the velocity dispersions are obtained from a two component (ISM+wind) absorption line model. The equivalent width PDF of the outflow in AGN has median, 84th and 16th percentiles of (0.4, 0.8, 0.1) Å. There is a strong ISM component in Fe II λ2586 absorption with (1.2, 1.5, 0.8) Å, implying presence of substantial amount cold gas in the host galaxies. For comparison, star-forming and X-ray undetected galaxies at a similar redshift, matched roughly in stellar mass and galaxy inclination, have a centroid velocity PDF with percentiles of (-74, -258, +90) km s −1 , and a velocity dispersion PDF percentiles of (150, 259, 57) km s −1 . Thus, winds in the AGN are similar to star-formation-driven winds, and are too weak to escape and expel substantial cool gas from galaxies. Our sample doubles the previous sample of AGN studied at z ∼ 0.5 and extends the analysis to z ∼ 1. A joint reanalysis of the z ∼ 0.5 AGN sample and our sample yields consistent results to the measurements above.

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A 10 kpc SCALE SEYFERT GALAXY OUTFLOW:HST/COS OBSERVATIONS OF IRAS F22456–5125

Cited by 79 publications

References 36 publications

Unraveling the Complex Structure of Agn-Driven Outflows. I. Kinematics and Sizes

Unraveling the Complex Structure of Agn-Driven Outflows. I. Kinematics and Sizes

SimultaneousXMM-Newtonand HST-COS observation of 1H0419-577

No Evidence for Feedback: Unexceptional Low-ionization Winds in Host Galaxies of Low Luminosity Active Galactic Nuclei at Redshift z ∼ 1

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