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Dusty galaxies in the Epoch of Reionization: simulations
Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy..
Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.;Museo Stor Fis, Ctr Fermi, Piazza Viminale 1, I-00184 Rome, Italy.;Ctr Studi & Ric Enrico Fermi, Piazza Viminale 1, I-00184 Rome, Italy.;Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 OHE, England.;Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England..
Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.;Univ Tokyo, Kavli IPMU, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan..
Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy..
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2018 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 477, no 1, p. 552-565Article in journal (Refereed) Published
Abstract [en]

The recent discovery of dusty galaxies well into the Epoch of Reionization (redshift z > 6) poses challenging questions about the properties of the interstellar medium in these pristine systems. By combining state-of-the-art hydrodynamic and dust radiative transfer simulations, we address these questions focusing on the recently discovered dusty galaxy A2744_YD4 (z = 8.38, Laporte et al.). We show that we can reproduce the observed spectral energy distribution (SED) only using different physical values with respect to the inferred ones by Laporte et al., i.e. a star formation rate of SFR = 78 M(circle dot)yr(-1), a factor approximate to 4 higher than deduced from simple SED fitting. In this case, we find: (i) dust attenuation (corresponding to tau(v) = 1.4) is consistent with a Milky Way (MW) extinction curve; (ii) the dust-to-metal ratio is low, f(d) similar to 0.08, implying that early dust formation is rather inefficient;(iii) the luminosity-weighted dust temperature is high, T-d = 91 23 K, as a result of the intense (approximate to 100 x MW) interstellar radiation field; and (iv) due to the high T-d, the Atacama Large Millimeter/submillimeter Array Band 7 detection can be explained by a limited dust mass, M-d = 1.6 x 10(6) M-circle dot. Finally, the high dust temperatures might solve the puzzling low infrared excess (IRX) recently deduced for high-z galaxies from the IRX-beta relation.

Place, publisher, year, edition, pages
Oxford University Press, 2018. Vol. 477, no 1, p. 552-565
Keywords [en]
methods: numerical, dust, extinction, galaxies: evolution, galaxies: high-redshift, galaxies: ISM, infrared: general
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:kth:diva-230487DOI: 10.1093/mnras/sty552ISI: 000432660300039Scopus ID: 2-s2.0-85046698516OAI: oai:DiVA.org:kth-230487DiVA, id: diva2:1218181
Note

QC 20180614

Available from: 2018-06-14 Created: 2018-06-14 Last updated: 2018-06-14Bibliographically approved

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