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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/29651
Title: The Evolution of the Galaxy Rest-frame Ultraviolet Luminosity Function over the First Two Billion Years
Authors: Finkelstein, Steven L.
Ryan, Russell E., Jr.
Papovich, Casey
DICKINSON, MARK
Song, Mimi
Somerville, Rachel S.
Ferguson, Henry C.
Salmon, Brett
Giavalisco, Mauro
Koekemoer, Anton M.
Ashby, Matthew L. N.
Behroozi, Peter
CASTELLANO, MARCO 
Dunlop, James S.
Faber, Sandy M.
Fazio, Giovanni G.
FONTANA, Adriano 
Grogin, Norman A.
Hathi, Nimish
Jaacks, Jason
Kocevski, Dale D.
Livermore, Rachael
McLure, Ross J.
MERLIN, Emiliano 
Mobasher, Bahram
Newman, Jeffrey A.
Rafelski, Marc
Tilvi, Vithal
Willner, S. P.
Issue Date: 2015
Journal: THE ASTROPHYSICAL JOURNAL 
Number: 810
Issue: 1
First Page: 71
Abstract: We present a robust measurement and analysis of the rest-frame ultraviolet (UV) luminosity functions at z = 4-8. We use deep Hubble Space Telescope imaging over the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey/GOODS fields, the Hubble Ultra Deep Field, and the Hubble Frontier Field deep parallel observations near the Abell 2744 and MACS J0416.1-2403 clusters. The combination of these surveys provides an effective volume of 0.6-1.2 × 10<SUP>6</SUP> Mpc<SUP>3</SUP> over this epoch, allowing us to perform a robust search for faint ({M}<SUB>{UV</SUB>}=-18) and bright (M{}<SUB>{UV</SUB>}\lt -21) high-redshift galaxies. We select candidate galaxies using a well-tested photometric redshift technique with careful screening of contaminants, finding a sample of 7446 candidate galaxies at 3.5 \lt z \lt 8.5, with >1000 galaxies at z ≈ 6-8. We measure both a stepwise luminosity function for candidate galaxies in our redshift samples, and a Schechter function, using a Markov Chain Monte Carlo analysis to measure robust uncertainties. At the faint end, our UV luminosity functions agree with previous studies, yet we find a higher abundance of UV-bright candidate galaxies at z ≥slant 6. Our best-fit value of the characteristic magnitude {M}<SUB>{UV</SUB>}<SUP>*</SUP> is consistent with -21 at z ≥slant 5, which is different than that inferred based on previous trends at lower redshift, and brighter at ̃2σ significance than previous measures at z = 6 and 7. At z = 8, a single power law provides an equally good fit to the UV luminosity function, while at z = 6 and 7 an exponential cutoff at the bright end is moderately preferred. We compare our luminosity functions to semi-analytical models, and find that the lack of evolution in {M}<SUB>{UV</SUB>}<SUP>*</SUP> is consistent with models where the impact of dust attenuation on the bright end of the luminosity function decreases at higher redshift, although a decreasing impact of feedback may also be possible. We measure the evolution of the cosmic star-formation rate (SFR) density by integrating our observed luminosity functions to {M}<SUB>{UV</SUB>}=-17, correcting for dust attenuation, and find that the SFR density declines proportionally to (1 +z){}<SUP>-4.3+/- 0.5</SUP> at z \gt 4, which is consistent with observations at z ≥slant 9. Our observed luminosity functions are consistent with a reionization history that starts at z ≳ 10, completes at z \gt 6, and reaches a midpoint (x{}<SUB>{{H</SUB>} {{II}}} = 0.5) at 6.7 \lt z \lt 9.4. Finally, using a constant cumulative number density selection and an empirically derived rising star-formation history, our observations predict that the abundance of bright z = 9 galaxies is likely higher than previous constraints, although consistent with recent estimates of bright z ̃ 10 galaxies.
Acknowledgments: We thank Kristian Finlator, Brian Siana, Rychard Bouwens, Pascal Oesch, Dan Jaffe, and Jon Trump for useful conversations. S.L.F. acknowledges support from the University of Texas at Austin College of Natural Sciences. M.S. was supported by a NASA Astrophysics and Data Analysis Program award issued by JPL/Caltech. R.J.M. acknowledges ERC funding via the award of a consolidator grant. This work is based on observations made with the NASA/ESA Hubble Space Telescope , obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #12060. This work is also based in part on observations made with the Spitzer Space Telescope , which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.
URI: http://hdl.handle.net/20.500.12386/29651
URL: https://iopscience.iop.org/article/10.1088/0004-637X/810/1/71
ISSN: 0004-637X
DOI: 10.1088/0004-637X/810/1/71
Bibcode ADS: 2015ApJ...810...71F
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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