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    CO(1-0) detection of molecular gas in the massive Spiderweb Galaxy (z = 2)

    236187_236187.pdf (1.431Mb)
    Access Status
    Open access
    Authors
    Emonts, B.
    Feain, I.
    Röttgering, H.
    Miley, G.
    Seymour, Nick
    Norris, R.
    Carilli, C.
    Villar-Martín, M.
    Mao, M.
    Sadler, E.
    Ekers, R.
    van Moorsel, G.
    Ivison, R.
    Pentericci, L.
    Tadhunter, C.
    Saikia, D.
    Date
    2013
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Emonts, B. and Feain, I. and Röttgering, H. and Miley, G. and Seymour, N. and Norris, R. and Carilli, C. et al. 2013. CO(1-0) detection of molecular gas in the massive Spiderweb Galaxy (z = 2). Monthly Notices of the Royal Astronomical Society. 430 (4): pp. 3465-3471.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1093/mnras/stt147
    ISSN
    0035-8711
    School
    Department of Physics and Astronomy
    Remarks

    This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/34978
    Collection
    • Curtin Research Publications
    Abstract

    The high-redshift radio galaxy MRC 1138−262 (‘Spiderweb Galaxy’; z = 2.16) is one of the most massive systems in the early Universe and surrounded by a dense ‘web’ of proto-cluster galaxies. Using the Australia Telescope Compact Array, we detected CO(1–0) emission from cold molecular gas – the raw ingredient for star formation – across the Spiderweb Galaxy. We infer a molecular gas mass of MH2 = 6 × 1010 M☉ (for MH2/L′CO = 0.8). While the bulk of the molecular gas coincides with the central radio galaxy, there are indications that a substantial fraction of this gas is associated with satellite galaxies or spread across the intergalactic medium on scales of tens of kpc. In addition, we tentatively detect CO(1–0) in the star-forming proto-cluster galaxy HAE 229, 250 kpc to the West. Our observations are consistent with the fact that the Spiderweb Galaxy is building up its stellar mass through a massive burst of widespread star formation. At maximum star formation efficiency, the molecular gas will be able to sustain the current star formation rate (SFR ≈ 1400 M☉ yr−1, as traced by Seymour et al.) for about 40 Myr. This is similar to the estimated typical lifetime of a major starburst event in infrared luminous merger systems.

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