The VIMOS Ultra-Deep Survey (VUDS): fast increase in the fraction of strong Lyman-α emitters from z = 2 to z = 6
Journal
Date Issued
2015
Author(s)
Cassata, P.
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Tasca, L. A. M.
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Le Fèvre, O.
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Lemaux, B. C.
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Le Brun, V.
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Maccagni, D.
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Thomas, R.
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Zamorani, G.
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Amorin, R.
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Capak, P.
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•
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Cimatti, A.
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Cuby, J. G.
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•
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Durkalec, A.
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Giavalisco, M.
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Hathi, N. P.
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Ilbert, O.
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Moreau, C.
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Paltani, S.
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Ribeiro, B.
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Salvato, M.
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Schaerer, D.
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Sommariva, V.
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Talia, M.
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Taniguchi, Y.
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Tresse, L.
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Wang, P. W.
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Charlot, S.
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Contini, T.
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Fotopoulou, S.
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Koekemoer, A. M.
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López-Sanjuan, C.
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Mellier, Y.
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Scoville, N.
Description
We thank ESO staff for their continuous support for the VUDS survey, particularly the Paranal staff conducting the observations and Marina Rejkuba and the ESO user support group in Garching. This work is supported by funding from the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010–2011. D.M. gratefully acknowledges LAM hospitality during the initial phases of the project. This work is based on data products made available at the CESAM data center, Laboratoire d’Astrophysique de Marseille. This work partly uses observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.
Abstract
Aims: The aim of this work is to constrain the evolution of the fraction of strong Lyα emitters among UV selected star-forming galaxies at 2 *FUV at 2 *FUV at 2 0(Lyα) < 10 Å, and correspondingly fesc(Lyα) < 1%. By comparing these results with the literature, we conclude that the bulk of the Lyα luminosity at 2 0(Lyα) and fesc(Lyα). This tail of large EW0(Lyα) and fesc(Lyα) becomes more important as the redshift increases, and causes the fraction of strong Lyα with EW0(Lyα) > 25 Å to increase from ~5% at z ~ 2 to ~30% at z ~ 6, with the increase being stronger beyond z ~ 4. We observe no difference, for the narrow range of UV luminosities explored in this work, between the fraction of strong Lyα emitters among galaxies fainter or brighter than M*FUV, although the fraction for the faint galaxies evolves faster, at 2 esc(Lyα): generally galaxies with high fesc(Lyα) also have small amounts of dust (and vice versa). However, when the dust content is low (E(B - V) < 0.05) we observe a very broad range of fesc(Lyα), ranging from 10-3 to 1. This implies that the dust alone is not the only regulator of the amount of escaping Lyα photons. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791.
Volume
573
Start page
A24
Issn Identifier
0004-6361
Ads BibCode
2015A&A...573A..24C
Rights
open.access
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