Oesch, P.A. and Stiavelli, M. and Carollo, C.M. and Bergeron, L.E. and Koekemoer, A.M. and Lucas, R.A. and Pavlovsky, C.M. and Trenti, M. and Lilly, S.J. and Beckwith, S.V.W. and Dahlen, T. and Ferguson, H.C. and Gardner, J.P. and Lacey, C. and Mobasher, B. and Panagia, N. and Rix, H.-W. (2007) 'The UDF05 follow-up of the Hubble Ultra Deep Field. I. The faint-end slope of the Lyman Break Galaxy Population at z ~ 5.', Astrophysical journal., 671 (2). p. 1212.
We present the UDF05 HST program, which consists of three disjoint fields—NICP12, NICP34, plus the HUDF—with deep ACS (F606W, F775W, and F850LP) and NICMOS (F110W and F160W) imaging. Here we use the ACS data for the NICP12 and HUDF fields to implement a (V − i) − (i − z) selection criterion that allows us to identify a sample of 101 (133) z ~ 5 Lyman break galaxies (LBGs) down to z850 = 28.5 (29.25) mag in NICP12 (HUDF). We construct the rest-frame 1400 Å LBG luminosity function (LF) over the range M1400 = [ − 21.4, − 17.1] , i.e. down to ~0.04L* at z ~ 5, and use Subaru Deep Field results (Yoshida et al. 2006) to constrain our LF at the bright end (M1400 ≥ − 22.2). We show that (1) different assumptions regarding the LBG SED distribution, dust properties, and intergalactic absorption result in a 25% variation in the number density of LBGs at z ~ 5; (2) under consistent assumptions for dust properties and intergalactic absorption, the HUDF is ~30% underdense in z ~ 5 LBGs relative to the NICP12 field, a variation which is well explained by cosmic variance; and (3) the faint-end slope of the LF does not depend on the input parameters, and has a value of α ~ − 1.6, similar to the faint-end slope of the LF of z ~ 3 and z ~ 6 LBGs. Our study therefore supports no variation in the faint end of the LBG LF over the whole redshift range z ~ 3 to z ~ 6. Based on a comparison with semianalytical models, we speculate that the z ~ 5 LBGs might have a top-heavy IMF.
|Keywords:||Dark matter, Galaxies: evolution, Galaxies: formation, Galaxies: high-redshift, Galaxies: luminosity function, mass function.|
|Full text:||(VoR) Version of Record|
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|Publisher Web site:||http://dx.doi.org/10.1086/522423|
|Publisher statement:||© 2007. The American Astronomical Society. All rights reserved.|
|Date accepted:||No date available|
|Date deposited:||28 January 2015|
|Date of first online publication:||December 2007|
|Date first made open access:||No date available|
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