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Direct evidence of AGN feedback: a post-starburst galaxy stripped of its gas by AGN-driven winds

Baron, Dalya; Netzer, H; Prochaska, J. Xavier; Cai, Zheng; Cantalupo, Sebastiano; Martin, D Christopher; Matuszewski, Mateusz; Moore, Anna; Morrissey, Patrick; Neill, James D.

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Post-starburst E+A galaxies show indications of a powerful starburst that was quenched abruptly. Their disturbed, bulge-dominated morphologies suggest that they are merger remnants. The more massive E+A galaxies are suggested to be quenched by active galactic nucleus (AGN) feedback, yet little is known about AGN-driven winds in this short-lived phase. We present spatially resolved integral field unit spectroscopy by the Keck Cosmic Web Imager of SDSS J003443.68 + 251020.9, at z = 0.118. The...[Show more]

dc.contributor.authorBaron, Dalya
dc.contributor.authorNetzer, H
dc.contributor.authorProchaska, J. Xavier
dc.contributor.authorCai, Zheng
dc.contributor.authorCantalupo, Sebastiano
dc.contributor.authorMartin, D Christopher
dc.contributor.authorMatuszewski, Mateusz
dc.contributor.authorMoore, Anna
dc.contributor.authorMorrissey, Patrick
dc.contributor.authorNeill, James D.
dc.date.accessioned2020-01-09T04:53:23Z
dc.date.available2020-01-09T04:53:23Z
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/1885/196776
dc.description.abstractPost-starburst E+A galaxies show indications of a powerful starburst that was quenched abruptly. Their disturbed, bulge-dominated morphologies suggest that they are merger remnants. The more massive E+A galaxies are suggested to be quenched by active galactic nucleus (AGN) feedback, yet little is known about AGN-driven winds in this short-lived phase. We present spatially resolved integral field unit spectroscopy by the Keck Cosmic Web Imager of SDSS J003443.68 + 251020.9, at z = 0.118. The system consists of two galaxies, the larger of which is a post-starburst E+A galaxy hosting an AGN. Our modelling suggests a 400 Myr starburst, with a peak star formation rate of 120 M⊙ yr−1. The observations reveal stationary and outflowing gas, photoionized by the central AGN. We detect gas outflows to a distance of 17 kpc from the central galaxy, far beyond the region of the stars (∼3 kpc), inside a conic structure with an opening angle of 70 deg. We construct self-consistent photoionization and dynamical models for the different gas components and show that the gas outside the galaxy forms a continuous flow, with a mass outflow rate of about 24 M⊙ yr−1. The gas mass in the flow, roughly 109M⊙⁠, is larger than the total gas mass within the galaxy, some of which is outflowing too. The continuity of the flow puts a lower limit of 60 Myr on the duration of the AGN feedback. Such AGNs are capable of removing, in a single episode, most of the gas from their host galaxies and expelling enriched material into the surrounding circumgalactic medium.
dc.description.sponsorshipFunding for this work was provided by the Israel Science Foundation grant 284/13. SC gratefully acknowledges support from Swiss National Science Foundation grant PP00P2-163824. The spectroscopic analysis was made using Ipython (Perez & Granger ´ 2007). We also used the following PYTHON PACKAGE: ASTROPY.
dc.format.mimetypeapplication/pdf
dc.language.isoen_AU
dc.publisherOxford University Press
dc.rights© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
dc.sourceMonthly Notices of the Royal Astronomical Society
dc.titleDirect evidence of AGN feedback: a post-starburst galaxy stripped of its gas by AGN-driven winds
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume480
dc.date.issued2018
local.identifier.absfor020103 - Cosmology and Extragalactic Astronomy
local.identifier.absfor020106 - High Energy Astrophysics; Cosmic Rays
local.identifier.ariespublicationu3102795xPUB2507
local.publisher.urlhttp://www.oxfordjournals.org/
local.type.statusPublished Version
local.contributor.affiliationBaron, Dalya, Tel-Aviv University
local.contributor.affiliationNetzer, H, Tel Aviv University
local.contributor.affiliationProchaska, J. Xavier, University of California
local.contributor.affiliationCai, Zheng, University of California
local.contributor.affiliationCantalupo, Sebastiano, Institute for Astronomy, ETH Zurich
local.contributor.affiliationMartin, D Christopher, California Institute of Technology
local.contributor.affiliationMatuszewski, Mateusz, Cahill Center for Astrophysics, California Institute of Technology
local.contributor.affiliationMoore, Anna, College of Science, ANU
local.contributor.affiliationMorrissey, Patrick, Cahill Center for Astrophysics, California Institute of Technology
local.contributor.affiliationNeill, James D., Cahill Center for Astrophysics, California Institute of Technology
local.bibliographicCitation.issue3
local.bibliographicCitation.startpage3993
local.bibliographicCitation.lastpage4016
local.identifier.doi10.1093/mnras/sty2113
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciences
dc.date.updated2019-08-25T08:18:10Z
local.identifier.thomsonIDWOS:000449616200090
dcterms.accessRightsOpen Access
dc.provenancehttp://sherpa.ac.uk/romeo/issn/0035-8711/..."Publisher's version/PDF on Institutional repositories or Central repositories, with all rights reserved" from Sherpa/Romeo (as at 9 Jan 2020). This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
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