RT Journal Article
T1 Breaking the curve with candels: a Bayesian approach to reveal the non-universality of the dust-attenuation law at high redshift
A1 Pérez González, Pablo Guillermo
A1 otros, ...
AB Dust attenuation affects nearly all observational aspects of galaxy evolution, yet very little is known about the form of the dust-attenuation law in the distant universe. Here, we model the spectral energy distributions of galaxies at z ~ 1.5–3 from CANDELS with rest-frame UV to near-IR imaging under different assumptions about the dust law, and compare the amount of inferred attenuated light with the observed infrared (IR) luminosities. Some individual galaxies show strong Bayesian evidence in preference of one dust law over another, and this preference agrees with their observed location on the plane of infrared excess (IRX, L_TIR/L_UV) and UV slope (β). We generalize the shape of the dust law with an empirical model, A_ λ,σ  =E(B-V)k_ λ  (λ / λ v)^ σ where k_λ is the dust law of Calzetti et al., and show that there exists a correlation between the color excess E(B-V) and tilt δ with δ =(0.62±0.05)log(E(B-V))+(0.26±0.02). Galaxies with high color excess have a shallower, starburst-like law, and those with low color excess have a steeper, SMC-like law. Surprisingly, the galaxies in our sample show no correlation between the shape of the dust law and stellar mass, star formation rate, or β. The change in the dust law with color excess is consistent with a model where attenuation is caused by scattering, a mixed star–dust geometry, and/or trends with stellar population age, metallicity, and dust grain size. This rest-frame UV-to-near-IR method shows potential to constrain the dust law at even higher redshifts (z>3).
PB American Astronomical Society
SN 0004-637X
YR 2016
FD 2016-08-10
LK https://hdl.handle.net/20.500.14352/19011
UL https://hdl.handle.net/20.500.14352/19011
LA eng
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NO © 2016. The American Astronomical Society. Artículo firmado por 16 autores. We thank the referee for thoughtful and constructive feedback on this work. We acknowledge our colleagues in the CANDELS collaboration for very useful comments and suggestions. We also thank the great effort of all the CANDELS team members for their work to provide a robust and valuable data set. We thank Karl Gordon for insightful discussions on the physical implications of these results. We also thank Daniela Calzetti and Veronique Buat for helpful comments and comments. This work is based in part on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is supported by HST program No. GO-12060. Support for Program No. GO-12060 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. We acknowledge the Spanish MINECO grant AYA2012-31277 for funding the contribution from Pablo Pérez Gonzalez. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration (NASA). The authors acknowledge the Texas A&M University Brazos HPC cluster that contributed to the research reported here. URL: http://brazos.tamu.edu.
NO Ministerio de Economía y Competitividad (MINECO)
NO National Aeronautics and Space Administration (NASA)
NO Hubble Space Telescope program
NO Space Telescope Science Institute
DS Docta Complutense
RD 1 may 2024