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    Extended X-ray emission in PKS 1718-649

    266971.pdf (346.4Kb)
    Access Status
    Open access
    Authors
    Beuchert, T.
    Rodríguez-Ardila, A.
    Moss, V.
    Schulz, R.
    Kadler, M.
    Wilms, J.
    Angioni, R.
    Callingham, J.
    Gräfe, C.
    Krauß, F.
    Kreikenbohm, A.
    Langejahn, M.
    Leiter, K.
    Maccagni, F.
    Müller, C.
    Ojha, R.
    Ros, E.
    Tingay, Steven
    Date
    2018
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Beuchert, T. and Rodríguez-Ardila, A. and Moss, V. and Schulz, R. and Kadler, M. and Wilms, J. and Angioni, R. et al. 2018. Extended X-ray emission in PKS 1718-649. Astronomy and Astrophysics. 612: L4.
    Source Title
    Astronomy and Astrophysics
    DOI
    10.1051/0004-6361/201833064
    ISSN
    0004-6361
    School
    Curtin Institute of Radio Astronomy (Physics)
    Remarks

    Reproduced with permission from Astronomy & Astrophysics, © ESO.

    URI
    http://hdl.handle.net/20.500.11937/68686
    Collection
    • Curtin Research Publications
    Abstract

    © ESO 2018. PKS 1718-649 is one of the closest and most comprehensively studied candidates of a young active galactic nucleus (AGN) that is still embedded in its optical host galaxy. The compact radio structure, with a maximal extent of a few parsecs, makes it a member of the group of compact symmetric objects (CSO). Its environment imposes a turnover of the radio synchrotron spectrum towards lower frequencies, also classifying PKS 1718-649 as gigahertz-peaked radio spectrum (GPS) source. Its close proximity has allowed the first detection of extended X-ray emission in a GPS/CSO source with Chandra that is for the most part unrelated to nuclear feedback. However, not much is known about the nature of this emission. By co-adding all archival Chandra data and complementing these datasets with the large effective area of XMM-Newton, we are able to study the detailed physics of the environment of PKS 1718-649. Not only can we confirm that the bulk of the kiloparsec-scale environment emits in the soft X-rays, but we also identify the emitting gas to form a hot, collisionally ionized medium. While the feedback of the central AGN still seems to be constrained to the inner few parsecs, we argue that supernovae are capable of producing the observed large-scale X-ray emission at a rate inferred from its estimated star formation rate.

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