NDLI: The VIMOS Ultra-Deep Survey (VUDS): fast increase in the fraction of strong Lyman-α emitters from z = 2 to z = 6

Content Provider	EDP Sciences
Author	P. Cassata L. A. M. Tasca O. Le Fèvre B. C. Lemaux B. Garilli V. Le Brun D. Maccagni L. Pentericci R. Thomas E. Vanzella G. Zamorani E. Zucca R. Amorin S. Bardelli P. Capak L. P. Cassarà M. Castellano A. Cimatti J. G. Cuby O. Cucciati S. de la Torre A. Durkalec A. Fontana M. Giavalisco A. Grazian N. P. Hathi O. Ilbert C. Moreau S. Paltani B. Ribeiro M. Salvato D. Schaerer M. Scodeggio V. Sommariva M. Talia Y. Taniguchi L. Tresse D. Vergani P. W. Wang S. Charlot T. Contini S. Fotopoulou A. M. Koekemoer C. López-Sanjuan Y. Mellier N. Scoville
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 <z< 6, and to measure the stellar escape fraction of Lyα photons over the same redshift range.Methods. We exploit the ultradeep spectroscopic observations with VIMOS on the VLT collected by the VIMOS Ultra-Deep Survey (VUDS) to build an unique, complete, and unbiased sample of ~4000 spectroscopically confirmed star-forming galaxies at 2 <z< 6. Our galaxy sample includes UV luminosities brighter than M^{^{_{FUV_{at 2 <z< 6, and luminosities down to one magnitude fainter than M^{^{_{FUV_{at 2 <z< 3.5. Results. We find that 80% of the star-forming galaxies in our sample have EW_{0_{(Lyα) < 10 Å, and correspondingly f_{esc_{(Lyα) < 1%. By comparing these results with the literature, we conclude that the bulk of the Lyα luminosity at 2 <z< 6 comes from galaxies that are fainter in the UV than those we sample in this work. The strong Lyα emitters constitute, at each redshift, the tail of the distribution of the galaxies with extreme EW_{0_{(Lyα) and f_{esc_{(Lyα). This tail of large EW_{0_{(Lyα) and f_{esc_{(Lyα) becomes more important as the redshift increases, and causes the fraction of strong Lyα with EW_{0_{(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 <z< 3.5, than for the bright ones. We do observe an anticorrelation between E(B − V) and f_{esc_{(Lyα): generally galaxies with high f_{esc_{(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 f_{esc_{(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.}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}}
Page Count	12
File Format	HTM / HTML PDF
ISSN	00046361
Alternate Webpage(s)	https://www.aanda.org/articles/aa/abs/2015/01/aa23824-14/aa23824-14.html
e-ISSN	14320746
Journal	Astronomy & Astrophysics
Volume Number	573
DOI	10.1051/0004-6361/201423824
Language	English
Publisher	EDP Sciences
Publisher Date	2015-01-01
Access Restriction	Open
Rights Holder	© ESO, 2014
Subject Keyword	galaxies: evolution galaxies: formation galaxies: high-redshift galaxies: fundamental parameters cosmology: observations galaxies: evolution / galaxies: formation / galaxies: high-redshift / galaxies: fundamental parameters / cosmology: observations
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Space and Planetary Science

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