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Jets, arcs, and shocks: NGC 5195 at radio wavelengths

Rampadarath, H. and Soria, R. and Urquhart, R. and Argo, M. K. and Brightman, M. and Lacey, C. K. and Schlegel, E. M. and Beswick, R. J. and Baldi, R. D. and Muxlow, T. W. B. and McHardy, I. M. and Williams, D. R. A. and Dumas, G. (2018) Jets, arcs, and shocks: NGC 5195 at radio wavelengths. Monthly Notices of the Royal Astronomical Society, 476 (3). pp. 2876-2889. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20180516-150943587

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Abstract

We studied the nearby, interacting galaxy NGC 5195 (M 51b) in the radio, optical and X-ray bands. We mapped the extended, low-surface-brightness features of its radio-continuum emission; determined the energy content of its complex structure of shock-ionized gas; constrained the current activity level of its supermassive nuclear black hole. In particular, we combined data from the European Very Long Baseline Interferometry Network (∼1-pc scale), from our new e-MERLIN observations (∼10-pc scale), and from the Very Large Array (∼100–1000-pc scale), to obtain a global picture of energy injection in this galaxy. We put an upper limit to the luminosity of the (undetected) flat-spectrum radio core. We find steep-spectrum, extended emission within 10 pc of the nuclear position, consistent with optically thin synchrotron emission from nuclear star formation or from an outflow powered by an active galactic nucleus (AGN). A linear spur of radio emission juts out of the nuclear source towards the kpc-scale arcs (detected in radio, Hα and X-ray bands). From the size, shock velocity, and Balmer line luminosity of the kpc-scale bubble, we estimate that it was inflated by a long-term-average mechanical power ∼3–6 × 10^(41) erg s^(−1) over the last 3–6 Myr. This is an order of magnitude more power than can be provided by the current level of star formation, and by the current accretion power of the supermassive black hole. We argue that a jet-inflated bubble scenario associated with previous episodes of AGN activity is the most likely explanation for the kpc-scale structures.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/sty390DOIArticle
https://arxiv.org/abs/1802.04417arXivDiscussion Paper
ORCID:
AuthorORCID
Brightman, M.0000-0002-8147-2602
Additional Information:© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2018 February 12. Received 2018 February 12; in original form 2017 March 6. Published: 19 February 2018. We thank the anonymous referee for their detailed comments and suggestions and their patience through various earlier versions of this work, which was much improved as a result. We also thank D. Mulcahy and M. W. Pakull for invaluable discussions. e-MERLIN is a National Facility operated by the University of Manchester at Jodrell Bank Observatory on behalf of STFC. The VLA is operated by the NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Hubble Space Telescope, is operated by NASA and the Space Telescope Science Institute. The Chandra X-ray telescope is operated for NASA by the Smithsonian Astrophysical Observatory. This work is partly based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). We used material from the NASA/IPAC Extragalactic Database (NED), operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We also used the VizieR catalogue access tool, and APLpy (Robitaille & Bressert 2012), an open-source plotting package for PYTHON. HR acknowledges support from ERC-StG 307215 (LODESTONE). RS acknowledges support from a Curtin University Senior Research Fellowship; he is also grateful for support, discussions and hospitality at the Strasbourg Observatory during part of this work. RU acknowledges that this research is supported by an Australian Government Research Training Program (RTP) Scholarship. The International Centre for Radio Astronomy Research is a joint venture between Curtin University and the University of Western Australia, funded by the state government of Western Australia and the joint venture partners.
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
European Research Council (ERC)307215
Curtin UniversityUNSPECIFIED
Australian GovernmentUNSPECIFIED
Government of Western AustraliaUNSPECIFIED
Subject Keywords:techniques: interferometric – techniques: radar astronomy – galaxies: active – galaxies: individual: NGC 5195 – radio continuum: galaxies – X-rays: galaxies
Issue or Number:3
Record Number:CaltechAUTHORS:20180516-150943587
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180516-150943587
Official Citation:H Rampadarath, R Soria, R Urquhart, M K Argo, M Brightman, C K Lacey, E M Schlegel, R J Beswick, R D Baldi, T W B Muxlow, I M McHardy, D R A Williams, G Dumas; Jets, arcs, and shocks: NGC 5195 at radio wavelengths, Monthly Notices of the Royal Astronomical Society, Volume 476, Issue 3, 21 May 2018, Pages 2876–2889, https://doi.org/10.1093/mnras/sty390
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:86430
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:18 May 2018 17:17
Last Modified:03 Oct 2019 19:43

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