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|Title:||The VANDELS survey: dust attenuation in star-forming galaxies at z = 3-4||Authors:||Cullen, F.
McLure, R. J.
Dunlop, J. S.
Dalla Vecchia, C.
Carnall, A. C.
Fynbo, J. P. U.
GARILLI, BIANCA MARIA ROSA
|Issue Date:||2018||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||476||Issue:||3||First Page:||3218||Abstract:||We present the results of a new study of dust attenuation at redshifts 3 < z < 4 based on a sample of 236 star-forming galaxies from the VANDELS spectroscopic survey. Motivated by results from the First Billion Years (FiBY) simulation project, we argue that the intrinsic spectral energy distributions (SEDs) of star-forming galaxies at these redshifts have a self-similar shape across the mass range 8.2 ≤ log (M<SUB>⋆</SUB>/M<SUB>☉</SUB>) ≤ 10.6 probed by our sample. Using FiBY data, we construct a set of intrinsic SED templates which incorporate both detailed star formation and chemical abundance histories, and a variety of stellar population synthesis (SPS) model assumptions. With this set of intrinsic SEDs, we present a novel approach for directly recovering the shape and normalization of the dust attenuation curve. We find, across all of the intrinsic templates considered, that the average attenuation curve for star-forming galaxies at z ≃ 3.5 is similar in shape to the commonly adopted Calzetti starburst law, with an average total-to-selective attenuation ratio of R<SUB>V</SUB> = 4.18 ± 0.29. In contrast, we find that an average attenuation curve as steep as the SMC extinction law is strongly disfavoured. We show that the optical attenuation (A<SUB>V</SUB>) versus stellar mass (M<SUB>⋆</SUB>) relation predicted using our method is consistent with recent ALMA observations of galaxies at 2 < z < 3 in the Hubble Ultra Deep Field (HUDF), as well as empirical A<SUB>V</SUB> - M<SUB>⋆</SUB> relations predicted by a Calzetti-like law. In fact, our results, combined with other literature data, suggest that the A<SUB>V</SUB>-M<SUB>⋆</SUB> relation does not evolve over the redshift range 0 < z < 5, at least for galaxies with log(M<SUB>⋆</SUB>/M<SUB>☉</SUB>) ≳ 9.5. Finally, we present tentative evidence which suggests that the attenuation curve may become steeper at lower masses log(M<SUB>⋆</SUB>/M<SUB>☉</SUB>) ≲ 9.0.||URI:||http://hdl.handle.net/20.500.12386/29989||URL:||https://academic.oup.com/mnras/article-abstract/476/3/3218/4898075||ISSN:||0035-8711||DOI:||10.1093/mnras/sty469||Bibcode ADS:||2018MNRAS.476.3218C||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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