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http://hdl.handle.net/20.500.12386/30795
Title: | Characterizing the UV-to-NIR shape of the dust attenuation curve of IR luminous galaxies up to z ∼ 2 | Authors: | Lo Faro, B. Buat, V. Roehlly, Y. Álvarez-Márquez, J. Burgarella, D. SILVA, Laura Efstathiou, A. |
Issue Date: | 2017 | Journal: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Number: | 472 | Issue: | 2 | First Page: | 1372 | Abstract: | In this work we investigate the far-UV to NIR shape of the dust attenuation curve of a sample of IR selected dust obscured (U)LIRGs at z$\sim$2. The spectral energy distributions (SEDs) are fitted with CIGALE, a physically-motivated spectral synthesis model based on energy balance. Its flexibility allows us to test a wide range of different analytical prescriptions for the dust attenuation curve, including the well-known Calzetti and Charlot & Fall curves, and modified versions of them. The attenuation curves computed under the assumption of our reference double power-law model are in very good agreement with those derived, in previous works, with radiative transfer (RT) SED fitting. We investigate the position of our galaxies in the IRX-$\beta$ diagram and find this to be consistent with grayer slopes, on average, in the UV. We also find evidence for a flattening of the attenuation curve in the NIR with respect to more classical Calzetti-like recipes. This larger NIR attenuation yields larger derived stellar masses from SED fitting, by a median factor of $\sim$ 1.4 and up to a factor $\sim$10 for the most extreme cases. The star formation rate appears instead to be more dependent on the total amount of attenuation in the galaxy. Our analysis highlights the need for a flexible attenuation curve when reproducing the physical properties of a large variety of objects. | URI: | http://hdl.handle.net/20.500.12386/30795 | URL: | https://academic.oup.com/mnras/article/472/2/1372/4044703 | ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stx1901 | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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stx1901.pdf | Pdf editoriale | 2.44 MB | Adobe PDF | View/Open |
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