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|Title:||The discovery of a significant sample of massive galaxies at redshifts 5 < z < 6 in the UKIDSS Ultra Deep Survey early data release|
Watson, Michael G.
|Publisher:||Blackwell Publishing on behalf of the Royal Astronomical Society|
|Citation:||Monthly Notices of the Royal Astronomical Society, 2006, 372 (1), pp. 357-368 (12)|
|Abstract:||We have exploited the large area coverage of the combined UKIDSS Ultra Deep Survey (UDS) and Subaru/XMM-Newton Deep Survey (SXDS) to search for bright Lyman-break galaxies (LBGs) at z >= 5. Using the available optical + near-infrared photometry to efficiently exclude low-redshift contaminants, we identify nine z >= 5 LBG candidates brighter than z'(AB) = 25 within the 0.6-deg(2) overlap region between the UDS early data release and the optical coverage of the SXDS. Accounting for selection incompleteness, we estimate the corresponding surface density of z >= 5 LBGs z'(AB) <= 25 to be 0.005 +/- 0.002 arcmin(-2). Modelling of the optical + near-infrared photometry constrains the candidates' redshifts to lie in the range, and provides estimates for their stellar masses. Although the stellar mass estimates are individually uncertain, a stacking analysis suggests that the typical stellar mass of the LBG candidates is greater than or similar to 5 x 10(10) M circle dot which, if confirmed, places them amongst the most massive galaxies currently known at z >= 5. It is found that Lambda cold dark matter structure formation can produce sufficient numbers of dark matter haloes at z >= 5 to accommodate our estimated number density of massive LBGs for plausible values of sigma(8) and the ratio of stellar to dark matter. Moreover, it is found that recent galaxy formation models can also account for the existence of such massive galaxies at z >= 5. Finally, no evidence is found for the existence of LBGs with stellar masses in excess of similar or equal to 3 x 10(11) M circle dot at this epoch, despite the large comoving volume surveyed.|
|Rights:||Copyright © 2006 The Authors. Journal compilation © 2006 RAS. Deposited with reference to the publisher's archiving policy available from the Journal Exclusive Licence Form, which permits posting of the Blackwell Publishing PDF 6 months after publication. The definitive version is available from www.blackwell-synergy.com|
|Appears in Collections:||Published Articles, Dept. of Physics and Astronomy|
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|j.1365-2966.2006.10864.x.pdf||Published (publisher PDF)||550.02 kB||Adobe PDF||View/Open|
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