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    Why z > 1 radio-loud galaxies are commonly located in protoclusters

    Access Status
    Fulltext not available
    Authors
    Hatch, N.
    Wylezalek, D.
    Kurk, J.
    Stern, D.
    Breuck, C.D.
    Jarvis., M.
    Galametz, A.
    Gonzalez, A.
    Hartley, W.
    Mortlock, A.
    Seymour, Nick
    Stevens, J.
    Date
    2014
    Type
    Journal Article
    
    Metadata
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    Citation
    Hatch, N. and Wylezalek, D. and Kurk, J. and Stern, D. and Breuck, C.D. and Jarvis., M. and Galametz, A. et al. 2014. Why z > 1 radio-loud galaxies are commonly located in protoclusters. Monthly Notices of the Royal Astronomical Society. 445: pp. 280-289.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1093/mnras/stu1725
    ISSN
    0035-8711
    URI
    http://hdl.handle.net/20.500.11937/3116
    Collection
    • Curtin Research Publications
    Abstract

    Distant powerful radio-loud active galactic nuclei (RLAGN) tend to reside in dense environments and are commonly found in protoclusters at z > 1.3. We examine whether this occurs because RLAGN are hosted by massive galaxies, which preferentially reside in rich environments. We compare the environments of powerful RLAGN at 1.3 < z < 3.2 from the Clusters Around Radio-Loud AGN survey to a sample of radio-quiet galaxies matched in mass and redshift. We find that the environments of RLAGN are significantly denser than those of radio-quiet galaxies, implying that not more than 50 per cent of massive galaxies in this epoch can host powerful radio-loud jets. This is not an observational selection effect as we find no evidence to suggest that it is easier to observe the radio emission when the galaxy resides in a dense environment. We therefore suggest that the dense Mpc-scale environment fosters the formation of a radio jet from an AGN. We show that the number density of potential RLAGN host galaxies is consistent with every >1014 M⊙ cluster having experienced powerful radio-loud feedback of duration ~60 Myr during 1.3 < z < 3.2. This feedback could heat the intracluster medium to the extent of 0.5–1 keV per gas particle, which could limit the amount of gas available for further star formation in the protocluster galaxies.

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