Serjeant, S. and Farrah, D. and Geach, J. and Takagi, T. and Verma, A. and Kaviani, A. and Fox, M. (2003) The K-band Hubble diagram of submillimetre galaxies and hyperluminous galaxies. Monthly Notices of the Royal Astronomical Society, 346 (4). L51-L56. ISSN 0035-8711.
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We present the K-band Hubble diagrams (K-z relations) of submillimetre-selected galaxies and hyperluminous galaxies (HLIRGs). We report the discovery of a remarkably tight K-z relation of HLIRGs, indistinguishable from that of the most luminous radio galaxies. Like radio galaxies, the HLIRG K-z relation at z less than or similar to 3 is consistent with a passively evolving similar to3L(*) instantaneous starburst starting from a redshift of z similar to 10 . In contrast, many submillimetre-selected galaxies are greater than or similar to2 mag fainter, and the population has a much larger dispersion. We argue that dust obscuration and/or a larger mass range may be responsible for this scatter. The galaxies so far proved to be hyperluminous may have been biased towards higher AGN bolometric contributions than submillimetre-selected galaxies due to the 60-mum selection of some, so the location on the K-z relation may be related to the presence of the most massive active galactic nucleus. Alternatively, a particular host galaxy mass range may be responsible for both extreme star formation and the most massive active nuclei.
|Additional information:||65 BLACKWELL PUBLISHING LTD 753XK|
|Uncontrolled keywords:||galaxies : evolution; galaxies : formation; galaxies : starburst; cosmology : observations; infrared : galaxies; submillimetre ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMATION HISTORY; IRAS 1-JY SAMPLE; RADIO GALAXIES; HIGH-REDSHIFT; DEEP-FIELD; LUMINOSITY FUNCTION; SCUBA GALAXIES; QUASARS; IDENTIFICATIONS|
|Divisions:||Faculties > Science Technology and Medical Studies > School of Physical Sciences|
|Depositing User:||Maggie Francis|
|Date Deposited:||12 Sep 2008 11:39|
|Last Modified:||14 Jan 2010 14:47|
|Resource URI:||http://kar.kent.ac.uk/id/eprint/11806 (The current URI for this page, for reference purposes)|
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