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http://hdl.handle.net/20.500.12386/24570
Title: | The VIMOS Ultra Deep Survey: Lyα emission and stellar populations of star-forming galaxies at 2 < z < 2.5 | Authors: | Hathi, N. P. Le Fèvre, O. Ilbert, O. Cassata, P. Tasca, L. A. M. Lemaux, B. C. GARILLI, BIANCA MARIA ROSA Le Brun, V. Maccagni, D. PENTERICCI, Laura Thomas, R. VANZELLA, Eros Zamorani, G. ZUCCA, Elena Amorín, R. BARDELLI, Sandro CASSARA, LETIZIA PASQUA CASTELLANO, MARCO Cimatti, A. CUCCIATI, Olga Durkalec, A. FONTANA, Adriano Giavalisco, M. GRAZIAN, Andrea Guaita, L. Koekemoer, A. Paltani, S. Pforr, J. Ribeiro, B. Schaerer, D. SCODEGGIO, MARCO Sommariva, V. Talia, M. Tresse, L. VERGANI, DANIELA Capak, P. Charlot, S. Contini, T. Cuby, J. G. de la Torre, S. Dunlop, J. Fotopoulou, S. López-Sanjuan, C. Mellier, Y. Salvato, M. Scoville, N. Taniguchi, Y. Wang, P. W. |
Issue Date: | 2016 | Journal: | ASTRONOMY & ASTROPHYSICS | Number: | 588 | First Page: | A26 | Abstract: | The aim of this paper is to investigate spectral and photometric properties of 854 faint (I<SUB>AB</SUB> ≲ 25 mag) star-forming galaxies (SFGs) at 2 < z < 2.5 using the VIMOS Ultra-Deep Survey (VUDS) spectroscopic data and deep multi-wavelength photometric data in three extensively studied extragalactic fields (ECDFS, VVDS, COSMOS). These SFGs were targeted for spectroscopy as a result of their photometric redshifts. The VUDS spectra are used to measure the UV spectral slopes (β) as well as Lyα equivalent widths (EW). On average, the spectroscopically measured β (-1.36 ± 0.02), is comparable to the photometrically measured β (-1.32 ± 0.02), and has smaller measurement uncertainties. The positive correlation of β with the spectral energy distribution (SED)-based measurement of dust extinction E<SUB>s</SUB>(B-V) emphasizes the importance of β as an alternative dust indicator at high redshifts. To make a proper comparison, we divide these SFGs into three subgroups based on their rest-frame Lyα EW: SFGs with no Lyα emission (SFG<SUB>N</SUB>; EW ≤ 0 Å), SFGs with Lyα emission (SFG<SUB>L</SUB>; EW > 0 Å), and Lyα emitters (LAEs; EW ≥ 20 Å). The fraction of LAEs at these redshifts is ~10%, which is consistent with previous observations. We compared best-fitSED-estimated stellar parameters of the SFG<SUB>N</SUB>, SFG<SUB>L</SUB> and LAE samples. For the luminosities probed here (~ L<SUP>∗</SUP>), we find that galaxies with and without Lyα in emission have small but significant differences in their SED-based properties. We find that LAEs have less dust, and lower star-formation rates (SFR) compared to non-LAEs. We also find that LAEs are less massive compared to non-LAEs, though the difference is smaller and less significant compared to the SFR and E<SUB>s</SUB>(B-V). When we divide the LAEs according to their Spitzer/IRAC 3.6 μm fluxes, we find that the fraction of IRAC-detected (m<SUB>3.6</SUB> ≲ 25 mag) LAEs is much higher than the fraction of IRAC-detected narrow band (NB)-selected LAEs at z ≃ 2-3. This could imply that UV-selected LAEs host a more evolved stellar population, which represents a later stage of galaxy evolution, compared to NB-selected LAEs. <P />Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791. | URI: | http://hdl.handle.net/20.500.12386/24570 | URL: | https://www.aanda.org/articles/aa/abs/2016/04/aa26012-15/aa26012-15.html | ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/201526012 | Bibcode ADS: | 2016A&A...588A..26H | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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aa26012-15.pdf | pdf editoriale | 1.9 MB | Adobe PDF | View/Open |
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