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    The Dragonfly Galaxy: II. ALMA unveils a triple merger and gas exchange in a hyper-luminous radio galaxy at z = 2

    236186_236186.pdf (2.715Mb)
    Access Status
    Open access
    Authors
    Emonts, B.
    De Breuck, C.
    Lehnert, M.
    Vernet, J.
    Gullberg, B.
    Villar-Martin, M.
    Nesvadba, N.
    Drouart, G.
    Ivison, R.
    Seymour, Nick
    Wylezalek, D.
    Barthel, P.
    Date
    2015
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Emonts, B. and De Breuck, C. and Lehnert, M. and Vernet, J. and Gullberg, B. and Villar-Martin, M. and Nesvadba, N. et al. 2015. The Dragonfly Galaxy: II. ALMA unveils a triple merger and gas exchange in a hyper-luminous radio galaxy at z = 2. Astronomy and Astrophysics. 584.
    Source Title
    Astronomy and Astrophysics
    DOI
    10.1051/0004-6361/201526090
    ISSN
    0004-6361
    School
    Department of Physics and Astronomy
    Remarks

    Reproduced with permission from Astronomy & Astrophysics, © ESO

    URI
    http://hdl.handle.net/20.500.11937/7309
    Collection
    • Curtin Research Publications
    Abstract

    The Dragonfly Galaxy (MRC 0152-209), at redshift z ~  2, is one of the most vigorously star-forming radio galaxies in the Universe. What triggered its activity? We present ALMA Cycle 2 observations of cold molecular CO(6−5) gas and dust, which reveal that this is likely a gas-rich triple merger. It consists of a close double nucleus (separation ~4 kpc) and a weak CO-emitter at ~10  kpc distance, all of which have counterparts in HST/NICMOS imagery. The hyper-luminous starburst and powerful radio-AGN were triggered at this precoalescent stage of the merger. The CO(6−5) traces dense molecular gas in the central region, and complements existing CO(1−0) data, which reveal more widespread tidal debris of cold gas. We also find ~1010 M☉ of molecular gas with enhanced excitation at the highest velocities. At least 20−50% of this high-excitation, high-velocity gas shows kinematics that suggests it is being displaced and redistributed within the merger, although with line-of-sight velocities of |v| < 500 km s-1, this gas will probably not escape the system. The processes that drive the redistribution of cold gas are likely related to either the gravitational interaction between two kpc-scale discs, or starburst/AGN-driven outflows. We estimate that the rate at which the molecular gas is redistributed is at least [Ṁentity!#x2009!]~ 1200 ± 500 M☉ yr-1, and could perhaps even approach the star formation rate of ~3000 ± 800 M☉ yr-1. The fact that the gas depletion and gas redistribution timescales are similar implies that dynamical processes can be important in the evolution of massive high-z galaxies.

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