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dc.contributor.authorMcLure, R. J.
dc.contributor.authorDunlop, J. S.
dc.contributor.authorCullen, F.
dc.contributor.authorBourne, N.
dc.contributor.authorBest, P. N.
dc.contributor.authorKhochfar, S.
dc.contributor.authorBowler, R. A. A.
dc.contributor.authorBiggs, A. D.
dc.contributor.authorGeach, J. E.
dc.contributor.authorScott, D.
dc.contributor.authorMichalowski, M. J.
dc.contributor.authorRujopakarn, W.
dc.contributor.authorKampen, E. van
dc.contributor.authorKirkpatrick, A.
dc.contributor.authorPope, A.
dc.date.accessioned2018-09-05T00:13:03Z
dc.date.available2018-09-05T00:13:03Z
dc.date.issued2018-05-21
dc.identifier.citationMcLure , R J , Dunlop , J S , Cullen , F , Bourne , N , Best , P N , Khochfar , S , Bowler , R A A , Biggs , A D , Geach , J E , Scott , D , Michalowski , M J , Rujopakarn , W , Kampen , E V , Kirkpatrick , A & Pope , A 2018 , ' Dust attenuation in 2 <z <3 star-forming galaxies from deep ALMA observations of the Hubble Ultra Deep Field ' , Monthly Notices of the Royal Astronomical Society , vol. 476 , no. 3 , pp. 3991-4006 . https://doi.org/10.1093/mnras/sty522
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 15274162
dc.identifier.otherPURE UUID: 05595fbb-cc42-43f8-b8de-7be140f27498
dc.identifier.otherArXiv: http://arxiv.org/abs/1709.06102v2
dc.identifier.otherScopus: 85047996106
dc.identifier.urihttp://hdl.handle.net/2299/20518
dc.description17 pages, 7 figures, accepted version to be published in MNRAS
dc.description.abstractWe present the results of a new study of the relationship between infrared excess (IRX ≡ L IR/L UV), ultraviolet (UV) spectral slope (β) and stellar mass at redshifts 2 < z < 3, based on a deep Atacama Large Millimeter Array (ALMA) 1.3-mm continuum mosaic of the Hubble Ultra Deep Field. Excluding the most heavily obscured sources, we use a stacking analysis to show that z ≃ 2.5 star-forming galaxies in the mass range 9.25 ≤ log(M*/M ⊙) ≤ 10.75 are fully consistent with the IRX-β relation expected for a relatively grey attenuation curve, similar to the commonly adopted Calzetti law. Based on a large, mass-complete sample of 2 ≤ z ≤ 3 star-forming galaxies drawn frommultiple surveys, we proceed to derive a new empirical relationship between β and stellar mass, making it possible to predict UV attenuation (A1600) and IRX as a function of stellar mass, for any assumed attenuation law. Once again, we find that z ≃ 2.5 star-forming galaxies follow A1600-M* and IRX-M* relations consistent with a relatively grey attenuation law, and find no compelling evidence that star-forming galaxies at this epoch follow a reddening law as steep as the Small Magellanic Cloud (SMC) extinction curve. In fact, we use a simple simulation to demonstrate that previous determinations of the IRX-β relation may have been biased towards low values of IRX at red values of β, mimicking the signature expected for an SMC-like dust law. We show that this provides a plausible mechanism for reconciling apparently contradictory results in the literature and that, based on typical measurement uncertainties, stellar mass provides a cleaner prediction of UV attenuation than β. Although the situation at lower stellar masses remains uncertain, we conclude that for 2 < z < 3 star-forming galaxies with log(M*/M ⊙) ≥ 9.75, both the IRX-β and IRX-M* relations are well described by a Calzetti-like attenuation law.en
dc.format.extent16
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectGalaxies: evolution
dc.subjectGalaxies: high-redshift
dc.subjectGalaxies: star formation
dc.subjectGalaxies: starburst
dc.subjectSubmillimetre: galaxies
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleDust attenuation in 2<z<3 star-forming galaxies from deep ALMA observations of the Hubble Ultra Deep Fielden
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85047996106&partnerID=8YFLogxK
dc.identifier.urlhttps://arxiv.org/abs/1709.06102
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/sty522
rioxxterms.typeJournal Article/Review


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