The magnetic field strength of the Faraday screen surrounding the radio galaxy Coma A

Show simple item record

dc.contributor.author Knuettel, Sebastian
dc.contributor.author O'Sullivan, S. P.
dc.contributor.author Curiel, S.
dc.contributor.author Emonts, B. H. C.
dc.date.accessioned 2019-05-21T14:32:28Z
dc.date.available 2019-05-21T14:32:28Z
dc.date.issued 2018-11-10
dc.identifier.citation Knuettel, S., O'Sullivan, S. P., Curiel, S. and Emonts, B. H. C. (2018) 'The magnetic field strength of the Faraday screen surrounding the radio galaxy Coma A', Monthly Notices of the Royal Astronomical Society, 482(4), pp. 4606-4616. doi: 10.1093/mnras/sty3018 en
dc.identifier.volume 482 en
dc.identifier.issued 4 en
dc.identifier.startpage 4606 en
dc.identifier.endpage 4616 en
dc.identifier.issn 0035-8711
dc.identifier.uri http://hdl.handle.net/10468/7954
dc.identifier.doi 10.1093/mnras/sty3018 en
dc.description.abstract Studying the interaction between AGN jets and lobes and their surrounding environment is important in order to understand how they transfer energy to their environment as well as determining the intrinsic physical properties of the sources themselves. This paper presents broad-band VLA polarization and Faraday rotation observations of the radio galaxy Coma A (3C 277.3) from 1 to 4 GHz, including archival VLA observations at 4.9 and 15 GHz. Through broad-band polarization model-fitting, we find that an external Faraday screen with a turbulent magnetic field provides an appropriate description to most of the data. By combining the polarization and Faraday rotation results with previous H  α observations, we identified the H α-emitting gas as the Faraday screen responsible for the observed Faraday depolarization. We were able to derive the magnetic field strength in the H α-emitting gas, finding typical field strengths of ∼1 μG, which is consistent with studies of the intragroup medium local to other radio galaxies. However, we find a highly depolarized region of the southern lobe coincident with a H α filament that has a field strength comparable to the equipartition field strength in the radio lobe (i.e. ≳36 μG). This implies that the H α filament is internal to the radio emitting plasma. Such clear examples of internal Faraday depolarization are rare, thus providing another key insight into the evolution of radio galaxies and their ability to provide significant feedback on the local gas that would otherwise cool and form stars. en
dc.description.sponsorship Irish Research Council (Government of Ireland Postgraduate Programme); Deutsche Forschungsgemeinschaft (Grant BR2026/23); Universidad Nacional Autónoma de México (PAPIIT project IA103416) en
dc.format.mimetype application/pdf en
dc.language.iso en en
dc.publisher Oxford University Press en
dc.rights © 2018, the Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. en
dc.subject Polarimetric en
dc.subject Active galaxies en
dc.subject Coma A en
dc.subject Radio continuum en
dc.subject Faraday screen en
dc.subject Radio galaxy en
dc.subject Magnetic field en
dc.title The magnetic field strength of the Faraday screen surrounding the radio galaxy Coma A en
dc.type Article (peer-reviewed) en
dc.internal.authorcontactother Sebastian Knuettel, Physics, University College Cork, Cork, Ireland. +353-21-490-3000 en
dc.internal.availability Full text available en
dc.date.updated 2019-05-21T14:20:20Z
dc.description.version Published Version en
dc.internal.rssid 486046552
dc.contributor.funder Irish Research Council en
dc.contributor.funder Deutsche Forschungsgemeinschaft en
dc.contributor.funder Universidad Nacional Autónoma de México en
dc.description.status Peer reviewed en
dc.identifier.journaltitle Monthly Notices of The Royal Astronomical Society en
dc.internal.copyrightchecked Yes
dc.internal.licenseacceptance Yes en
dc.internal.IRISemailaddress s.knuettel@mars.ucc.ie en
dc.identifier.eissn 1365-2966


Files in this item

This item appears in the following Collection(s)

Show simple item record

This website uses cookies. By using this website, you consent to the use of cookies in accordance with the UCC Privacy and Cookies Statement. For more information about cookies and how you can disable them, visit our Privacy and Cookies statement