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Fudamoto, Y; Oesch, P. A; Schinnerer, E; Groves, B; Karim, A; Magnelli, B; Sargent, M. T; Cassata, P; Lang, P; Liu, D; Le Fèvre, O; Leslie, S; Smolčić, V; Tasca, L
Monthly notices of the Royal Astronomical Society, 11/2017, Letnik: 472, Številka: 1Journal Article
Abstract We present results on the dust attenuation of galaxies at redshift ∼3–6 by studying the relationship between the UV spectral slope (βUV) and the infrared excess (IRX; L IR/L UV) using Atacama Large Millimeter/submillimeter Array (ALMA) far-infrared continuum observations. Our study is based on a sample of 67 massive, star-forming galaxies with a median mass of M * ∼ 1010.7 M ⊙ spanning a redshift range z = 2.6–3.7 (median z = 3.2) that were observed with ALMA at $\lambda _{\text{rest}}=300\,{\rm \mu m}$ . Both the individual ALMA detections (41 sources) and stacks including all galaxies show the IRX–βUV relationship at z ∼ 3 is mostly consistent with that of local starburst galaxies on average. However, we find evidence for a large dispersion around the mean relationship by up to ±0.5 dex. Nevertheless, the locally calibrated dust correction factors based on the IRX–βUV relation are on average applicable to main-sequence z ∼ 3 galaxies. This does not appear to be the case at even higher redshifts, however. Using public ALMA observations of z ∼ 4–6 galaxies we find evidence for a significant evolution in the IRX–βUV and the IRX–M * relations beyond z ∼ 3 towards lower IRX values. We discuss several caveats that could affect these results, including the assumed dust temperature. ALMA observations of larger z > 3 galaxy sample spanning a wide range of physical parameters (e.g. lower stellar mass) will be important to investigate this intriguing redshift evolution further.
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