dc.contributor.author | Mingo, B. | |
dc.contributor.author | Hardcastle, M. J. | |
dc.contributor.author | Croston, J. H. | |
dc.contributor.author | Hota, A. | |
dc.contributor.author | Kharb, Preeti | |
dc.contributor.author | Kraft, Ralph P. | |
dc.contributor.author | Evans, Daniel A. | |
dc.date.accessioned | 2015-02-27T16:16:57Z | |
dc.date.available | 2015-02-27T16:16:57Z | |
dc.date.issued | 2011-03 | |
dc.date.submitted | 2010-08 | |
dc.identifier.issn | 0004-637X | |
dc.identifier.issn | 1538-4357 | |
dc.identifier.uri | http://hdl.handle.net/1721.1/95729 | |
dc.description.abstract | Markarian 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.iso | en_US | |
dc.publisher | IOP Publishing | en_US |
dc.relation.isversionof | http://dx.doi.org/10.1088/0004-637x/731/1/21 | en_US |
dc.rights | Article 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.source | American Astronomical Society | en_US |
dc.title | MARKARIAN 6: SHOCKING THE ENVIRONMENT OF AN INTERMEDIATE SEYFERT | en_US |
dc.type | Article | en_US |
dc.identifier.citation | Mingo, 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 Society | en_US |
dc.contributor.department | MIT Kavli Institute for Astrophysics and Space Research | en_US |
dc.contributor.mitauthor | Evans, Daniel A. | en_US |
dc.relation.journal | The Astrophysical Journal | en_US |
dc.eprint.version | Final published version | en_US |
dc.type.uri | http://purl.org/eprint/type/JournalArticle | en_US |
eprint.status | http://purl.org/eprint/status/PeerReviewed | en_US |
dspace.orderedauthors | Mingo, B.; Hardcastle, M. J.; Croston, J. H.; Evans, D. A.; Hota, A.; Kharb, P.; Kraft, R. P. | en_US |
mit.license | PUBLISHER_POLICY | en_US |
mit.metadata.status | Complete | |