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23 April 2024 |
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Faint Galaxies in deep ACS observations | | N. Benitez
; H. Ford
; R. Bouwens
; F. Menanteau
; J. Blakeslee
; C. Gronwall
; G. Illingworth
; G. Meurer
; T.J.Broadhurst
; M. Clampin
; M. Franx
; G. Hartig
; D. Magee
; M. Sirianni
; D.R. Ardila
; F. Bartko
; R.A. Brown
; C.J. Burrows
; E.S. Cheng
; N.J.G.Cross
; P.D. Feldman
; D.A. Golimowski
; L. Infante
; R.A. Kimble
; J.E. Krist
; M.P. Lesser
; Z. Levay
; A.R. Martel
; G.K. Miley
; M. Postman
; P. Rosati
; W.B. Sparks
; H.D. Tran
; Z.I. Tsvetanov
; R.L. White & W. Zheng
; | | Date: |
2 Sep 2003 | | Subject: | astro-ph | | Abstract: | We present the analysis of the faint galaxy population in the Advanced Camera for Surveys (ACS) Early Release Observation fields VV 29 (UGC 10214) and NGC 4676. Here we attempt to thoroughly consider all aspects relevant for faint galaxy counting and photometry, developing methods which are based on public software and that are easily reproducible by other astronomers. Using simulations we determine the best SExtractor parameters for the detection of faint galaxies in deep HST observations, paying special attention to the issue of deblending, which significantly affects the normalization and shape of the number count distribution. We confirm, as claimed by Bernstein, Freedman and Madore (2002), that Kron-like magnitudes, such as the ones generated by SExtractor, can miss more than half of the light of faint galaxies, what dramatically affects the slope of the number counts. We present catalogs for the VV 29 and NGC 4676 fields with photometry in the g,V and I bands. We also show that combining the bayesian software BPZ with superb ACS data and new spectral templates enables us to estimate reliable photometric redshifts for a significant fraction of galaxies with as few as three filters. After correcting for selection effects, we measure slopes of 0.32+- 0.01 for 22 < g < 28, 0.34+-0.01 for 22< V <27.5 and 0.33+-0.01 for 22 < I < 27. The counts do not flatten (except perhaps in the g-band), up to the depth of our observations. We find that the faint counts m_{AB}> 25.5 can be well approximated in all our filters by a passive luminosity evolution model based on the COMBO-17 luminosity function (alpha=-1.5), with a strong merging rate following the prescription of Glazebrook et al. (1994), phi^*propto (1+Qz), with Q=4. | | Source: | arXiv, astro-ph/0309077 | | Services: | Forum | Review | PDF | Favorites | |
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