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http://hdl.handle.net/20.500.12386/32058
Title: | The VANDELS survey: global properties of CIII]λ1908 Å emitting star-forming galaxies at z ∼ 3⋆ | Authors: | M. Llerena R. Amorín F. Cullen PENTERICCI, Laura A. Calabrò R. McLure A. Carnall E. Pérez-Montero F. Marchi BONGIORNO, ANGELA CASTELLANO, MARCO FONTANA, Adriano D. J. McLeod M. Talia N. P. Hathi P. Hibon MANNUCCI, FILIPPO A. Saxena D. Schaerer G. Zamorani |
Issue Date: | 2022 | Journal: | ASTRONOMY & ASTROPHYSICS | Number: | 659 | First Page: | A16 | Abstract: | We study the mean properties of a large representative sample of 217 galaxies showing CIII] emission at $2<z<4$, selected from a parent sample of $\sim$750 main-sequence star-forming galaxies in the VANDELS survey. These CIII] emitters have a broad range of UV luminosities, thus allowing a detailed stacking analysis to characterize their stellar mass, star formation rate (SFR) and stellar metallicity, as a function of the UV emission line ratios, EWs, and the carbon-to-oxygen (C/O) abundance ratio. Reliable CIII] detections represent $\sim$30% of the parent sample. Extreme CIII] emitters (EW(CIII])$\gtrsim$8\r{A}) are exceedingly rare ($\sim$3%) in VANDELS. The UV line ratios of the sample suggest no ionization source other than massive stars. Stacks with larger EW(CIII]) show larger EW(Ly$\alpha$) and lower metallicity, but not all CIII] emitters are Ly$\alpha$ emitters. The stellar metallicities of CIII] emitters are not significantly different from that of the parent sample, increasing from $\sim$10% to $\sim$40% solar for stellar masses $\log$(M$_{\star}$/M$_{\odot})\sim$9-10.5. The stellar mass-metallicity relation of the CIII] emitters is consistent with previous works showing strong evolution from $z=0$ to $z\sim3$. The C/O abundances of the sample range 35%-150% solar, with a noticeable increase with FUV luminosity and a smooth decrease with the CIII] EW. We discuss the CIII] emitters in the C/O-Fe/H and the C/O-O/H planes and find they follow stellar and nebular abundance trends consistent with those of Milky Way halo and thick disc stars and local HII galaxies, respectively. A qualitative agreement is also found with chemical evolution models, which suggests that CIII] emitters at $z\sim$3 are experiencing an active phase of chemical enrichment. | URI: | http://hdl.handle.net/20.500.12386/32058 | URL: | http://arxiv.org/abs/2107.00660v2 https://www.aanda.org/articles/aa/abs/2022/03/aa41651-21/aa41651-21.html |
ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/202141651 | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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aa41651-21 compr.pdf | Pdf editoriale | 2 MB | Adobe PDF | View/Open |
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