Farrah, D. and Geach, J. and Fox, M. and Serjeant, S. and Oliver, S. and Verma, A. and Kaviani, A. and Rowan-Robinson, M. (2004) The environments of hyperluminous infrared galaxies at 0.44 < z < 1.55. Monthly Notices of the Royal Astronomical Society, 349 (2). pp. 518-526. ISSN 0035-8711.
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We present deep wide-field K-s-band observations of six Hyperluminous Infrared Galaxies (HLIRGs) spanning a redshift range 0.44<z<1.55. The sample resides in a wide variety of environments, from the field to Abell 2 clusters, with a mean galaxy-HLIRG clustering amplitude of <B-gh>=190+/-45 Mpc(1.77). The range in environments, and the mean clustering level, are both greater than those seen in local IR-luminous galaxies, from which we infer that the range of galaxy evolution processes driving IR-luminous galaxy evolution at z>0.5 is greater than locally, and includes mergers between gas-rich spiral galaxies in the field, but also includes encounters in clusters and hierarchical build-up. The similarity in the range of environments and mean clustering amplitude between our sample and QSOs over a similar redshift range is consistent with the interpretation where evolutionary connections between IR-luminous galaxies and QSOs are stronger at z>0.5 than locally, and that, at these redshifts, the processes that drive QSO evolution are similar to those that drive IR-luminous galaxy evolution. From comparison of the HLIRG and QSO host galaxies we further postulate that a larger fraction of IR-luminous galaxies pass through an optical QSO stage at z>0.5 than locally.
|Additional information:||61 BLACKWELL PUBLISHING LTD 810HE|
|Uncontrolled keywords:||galaxies : clusters : general; galaxies : evolution; galaxies : starburst; galaxies :; active; infrared : galaxies|
|Divisions:||Faculties > Science Technology and Medical Studies > School of Physical Sciences|
|Depositing User:||Maggie Francis|
|Date Deposited:||18 Sep 2008 15:05|
|Last Modified:||14 Jan 2010 14:46|
|Resource URI:||http://kar.kent.ac.uk/id/eprint/11776 (The current URI for this page, for reference purposes)|
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