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Star Formation at z~6: i-dropouts in the ACS GTO fields | | R.J. Bouwens
; G.D. Illingworth
; P. Rosati
; C. Lidman
; T. Broadhurst
; M. Franx
; H.C. Ford
; D. Magee
; N. Benitez
; J.P. Blakeslee
; G.R. Meurer
; M. Clampin
; G.F. Hartig
; D.R. Ardila
; F. Bartko
; R.A. Brown
; C.J. Burrows
; E.S. Cheng
; N.J.G. Cross
; P.D. Feldman
; D.A. Golimowski
; C. Gronwall
; L. Infante
; R.A. Kimble
; J.E. Krist
; M.P. Lesser
; A.R. Martel
; F. Menanteau
; G.K. Miley
; M. Postman
; M. Sirianni
; W.B. Sparks
; H.D. Tran
; Z.I. Tsvetanov
; R.L. White & W. Zheng
; | | Date: |
11 Jun 2003 | | Journal: | Astrophys.J. 595 (2003) 589-602 | | Subject: | astro-ph | | Abstract: | Using an i-z dropout criterion, we determine the space density of z~6 galaxies from two deep ACS GTO fields with deep optical-IR imaging. A total of 23 objects are found over 46 arcmin^2, or ~0.5 objects/arcmin^2 down to z~27.3 (6 sigma; all AB mag) (including one probable z~6 AGN). Combining deep ISAAC data for our RDCS1252-2927 field (J~25.7 and Ks~25.0 (5 sigma)) and NICMOS data for the HDF North (JH~27.3 (5 sigma)), we verify that these dropouts have flat spectral slopes. i-dropouts in our sample range in luminosity from ~1.5 L* (z~25.6) to ~0.3 L* (z~27.3) with the exception of one very bright candidate at z~24.2. The half-light radii vary from 0.09" to 0.29", or 0.5 kpc to 1.7 kpc. We derive the z~6 rest-frame UV luminosity density using three different procedures, each utilizing simulations based on a CDF South V dropout sample. First, we compare our findings with a no-evolution projection of this V-dropout sample. We find 23+/-25% more i-dropouts than we predict. Adopting previous results to z~5, this works out to a 20+/-29% drop in the luminosity density from z~3 to z~6. Second, we use these same V-dropout simulations to derive a selection function for our i-dropout sample and compute the UV-luminosity density (7.2+/-2.5 x 10^25 ergs/s/Hz/Mpc^3 down to z~27). We find a 39+/-21% drop over the same redshift range. This is our preferred value and suggests a star formation rate of 0.0090+/-0.0031 M_sol/yr/Mpc^3 to z~27, or ~0.036+/- 0.012 M_sol/yr/Mpc^3 extrapolating the LF to the faint limit. Third, we follow a very similar procedure, but assume no incompleteness, finding a luminosity density which is ~2-3X lower. This final estimate constitutes a lower limit. All three estimates are within the canonical range of luminosity densities necessary for reionization of the universe at this epoch. (abridged) | | Source: | arXiv, astro-ph/0306215 | | Services: | Forum | Review | PDF | Favorites | |
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