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A deeper look at the dust attenuation law of star-forming galaxies at high redshift

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Tress, M. and Ferreras, I. and Pérez González, Pablo Guillermo and Bressan, A. and Barro, G. and Domínguez Sánchez, H. and Eliche Moral, María del Carmen (2019) A deeper look at the dust attenuation law of star-forming galaxies at high redshift. Monthly noticies of the royal astronomical society, 488 (2). pp. 2301-2311. ISSN 0035-8711

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Official URL: http://dx.doi.org/10.1093/mnras/stz1851




Abstract

A diverse range of dust attenuation laws is found in star-forming galaxies. In particular, Tress et al. (2018) studied the SHARDS survey to constrain the NUV bump strength (B) and the total-to-selective ratio (R_(V)) of 1,753 star-forming galaxies in the GOODS-N field at 1.5<z<3. We revisit here this sample to assess the implications and possible causes of the correlation found between R_(V) and B. The UVJ bicolour plot and main sequence of star formation are scrutinised to look for clues into the observed trend. The standard boundary between quiescent and star-forming galaxies is preserved when taking into account the wide range of attenuation parameters. However, an additional degeneracy – regarding the effective attenuation law – is added to the standard loci of star-forming galaxies in the UVJ diagram. A simple phenomenological model with an age-dependent extinction (at fixed dust composition) is compatible with the observed trend between R_(V) and B, whereby the opacity decreases with the age of the populations, resulting in a weaker NUV bump when the overall attenuation is shallower (greyer). In addition, we compare the constraints obtained by the SHARDS sample with dust models from the literature, supporting a scenario where geometry could potentially drive the correlation between R_(V) and B.


Item Type:Article
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© 2019 RAS.

Uncontrolled Keywords:Spectral energy-distributions; Interstellar dust; Formation histories; Quiescent galaxies; Milky-Way; Ultraviolet; Extinction; Stellar; Model; Resolution
Subjects:Sciences > Physics > Astrophysics
ID Code:57607
Deposited On:22 Nov 2019 11:33
Last Modified:22 Nov 2019 11:33

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