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dc.contributor.authorMingo, B.
dc.contributor.authorHardcastle, M. J.
dc.contributor.authorCroston, J. H.
dc.contributor.authorHota, A.
dc.contributor.authorKharb, Preeti
dc.contributor.authorKraft, Ralph P.
dc.contributor.authorEvans, Daniel A.
dc.date.accessioned2015-02-27T16:16:57Z
dc.date.available2015-02-27T16:16:57Z
dc.date.issued2011-03
dc.date.submitted2010-08
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1721.1/95729
dc.description.abstractMarkarian 6 is a nearby (D ~ 78 Mpc) Seyfert 1.5, early-type galaxy, with a double set of radio bubbles. The outer set spans ~7.5 kpc and is expanding into the halo regions of the host galaxy. We present an analysis of our new Chandra observation, together with archival XMM-Newton data, to look for evidence of emission from shocked gas around the external radio bubbles, both from spatially resolved regions in Chandra and from spectral analysis of the XMM-Newton data. We also look for evidence of a variable absorbing column along our line of sight to Mrk 6, to explain the evident differences seen in the active galactic nucleus (AGN) spectra from the various, non-contemporaneous, observations. We find that the variable absorption hypothesis explains the differences between the Chandra and XMM-Newton spectra, with the Chandra spectrum being heavily absorbed. The intrinsic N [subscript H] varies from ~8 × 10[superscript 21] atoms cm[superscript –2] to ~3 × 10[superscript 23] atoms cm[superscript –2] on short timescales (2-6 years). The past evolution of the source suggests this is probably caused by a clump of gas close to the central AGN, passing in front of us at the moment of the observation. Shells of thermal X-ray emission are detected around the radio bubbles, with a temperature of ~0.9 keV. We estimate a temperature of ~0.2 keV for the external medium using luminosity constraints from our Chandra image. We analyze these results using the Rankine-Hugoniot shock jump conditions, and obtain a Mach number of ~3.9, compatible with a scenario in which the gas in the shells is inducing a strong shock in the surrounding interstellar medium (ISM). This could be the third clear detection of strong shocks produced by a radio-powerful Seyfert galaxy. These results are compatible with previous findings on Centaurus A and NGC 3801, supporting a picture in which these AGN-driven outflows play an important role in the environment and evolution of the host galaxy.en_US
dc.language.isoen_US
dc.publisherIOP Publishingen_US
dc.relation.isversionofhttp://dx.doi.org/10.1088/0004-637x/731/1/21en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourceAmerican Astronomical Societyen_US
dc.titleMARKARIAN 6: SHOCKING THE ENVIRONMENT OF AN INTERMEDIATE SEYFERTen_US
dc.typeArticleen_US
dc.identifier.citationMingo, B., M. J. Hardcastle, J. H. Croston, D. A. Evans, A. Hota, P. Kharb, and R. P. Kraft. “MARKARIAN 6: SHOCKING THE ENVIRONMENT OF AN INTERMEDIATE SEYFERT.” The Astrophysical Journal 731, no. 1 (March 18, 2011): 21. © 2011 The American Astronomical Societyen_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.contributor.mitauthorEvans, Daniel A.en_US
dc.relation.journalThe Astrophysical Journalen_US
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsMingo, B.; Hardcastle, M. J.; Croston, J. H.; Evans, D. A.; Hota, A.; Kharb, P.; Kraft, R. P.en_US
mit.licensePUBLISHER_POLICYen_US
mit.metadata.statusComplete


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