The infrared-dark dust content of high redshift galaxies

Ferrara, Andrea; Hirashita, Hiroyuki; Ouchi, Masami; Fujimoto, Seiji

doi:10.1093/mnras/stx1898

Cited by 59 publications

(61 citation statements)

References 40 publications

(44 reference statements)

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“…In between, we see an apparent maximum observed in IRX and sM dust for the present Hi-z LBG sample at sSFR ∼10 −8 yr −1 that needs to be confirmed by future observational data. Both IRX and sM dust decline and age increases to a locus at sSFR∼10 −10 -10 −9 yr −1 where we find the LBGs with upper limits as those discussed in Capak et al (2015), Ferrara et al (2017) and Faisst et al 2017. This seems to define an evolutionary sequence from the right of the DFRD where the first dust grains form to the left where they are removed/destroyed.…”

Section: Resultssupporting

confidence: 80%

Observational and theoretical constraints on the formation and early evolution of the first dust grains in galaxies at 5 < z < 10

Burgarella

Nanni

Hirashita

et al. 2020

A&A

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Context. The first generation of stars were born a few hundred million years after the big bang. These stars synthesized elements heavier than H and He, that are later expelled into the interstellar medium, initiating the rise of metals. Within this enriched medium, the first dust grains formed. This event is cosmological crucial for molecule formation as dust plays a major role by cooling lowmetallicity star-forming clouds which can fragment to create lower mass stars. Collecting information on these first dust grains is difficult because of the negative alliance of large distances and low dust masses. Aims. We combine the observational information from galaxies at redshifts 5 z 10 to constrain their dust emission and theoretically understand the first evolutionary phases of the dust cycle. Methods. Spectral energy distributions (SEDs) are fitted with CIGALE and the physical parameters and their evolution are modelled. From this SED fitting, we build a dust emission template for this population of galaxies in the epoch of reionization. Results. Our new models explain why some early galaxies are observed and others are not. We follow in time the formation of the first grains by supernovae later destroyed by other supernova blasts and expelled in the circumgalactic and intergalactic media. Conclusions. We have found evidence for the first dust grains formed in the universe. But, above all, this paper underlines the need to collect more data and to develop new facilities to further constrain the dust cycle in galaxies in the epoch of reionization.

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Section: Resultssupporting

confidence: 80%

Observational and theoretical constraints on the formation and early evolution of the first dust grains in galaxies at 5 < z < 10

Burgarella

Nanni

Hirashita

et al. 2020

A&A

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“…At the same time, the increased energy absorbed in the UV boosts the IR emission. Thus, on general grounds, a positive correlation between the two quantities is expected (see Ferrara et al 2017, for an in-depth discussion).…”

Section: The Irx-β Relationmentioning

confidence: 98%

Dusty galaxies in the Epoch of Reionization: simulations

Behrens

Pallottini

Ferrara

et al. 2018

Monthly Notices of the Royal Astronomical Society

138

191

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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. 2017). 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. (2017), i.e. a star formation rate of SFR = 78 M yr −1 , a factor ≈ 4 higher than deduced from simple Spectral Energy Distribution fitting. In this case we find: (a) dust attenuation (corresponding to τ V = 1.4) is consistent with a Milky Way extinction curve; (b) the dust-to-metal ratio is low, f d ∼ 0.08, implying that early dust formation is rather inefficient; (c) the luminosity-weighted dust temperature is high, T d = 91 ± 23 K, as a result of the intense (≈ 100× MW) interstellar radiation field; (d) due to the high T d , the ALMA Band 7 detection can be explained by a limited dust mass, M d = 1.6 × 10 6 M . Finally, the high dust temperatures might solve the puzzling low infrared excess recently deduced for high-z galaxies from the IRX-β relation.

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“…Multiple theoretical efforts have addressed the origin of observed variations in the IRX -β relation (e.g., Granato et al 2000;Ferrara et al 2016;Mancini et al 2016;Cullen et al 2017;Narayanan et al 2017;Safarzadeh, Hayward & Ferguson 2017). These works have highlighted stellar population age, variations in the dust attenuation curve, the temperature of the dust, and the geometry of the dust distribution as possible origins for observed deviations from the Meurer et al IRX -β relation.…”

Section: Introductionmentioning

confidence: 99%

Dissecting the IRX–β dust attenuation relation: exploring the physical origin of observed variations in galaxies

Popping

Puglisi

Norman

2017

Monthly Notices of the Royal Astronomical Society

121

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The use of ultraviolet (UV) emission as a tracer of galaxy star-formation rate (SFR) is hampered by dust obscuration. The empirical relationship between UV slope, β, and the ratio between far-infrared and UV luminosity, IRX, is commonly employed to account for obscured UV emission. We present a simple model that explores the physical origin of variations in the IRX -β dust attenuation relation. A relative increase in FUV compared to NUV attenuation and an increasing stellar population age cause variations towards red UV slopes for a fixed IRX. Dust geometry effects (turbulence, dust screen with holes, mixing of stars within the dust screen, two-component dust model) cause variations towards blue UV slopes. Poor photometric sampling of the UV spectrum causes additional observational variations. We provide an analytic approximation for the IRX -β relation invoking a subset of the explored physical processes (dust type, stellar population age, turbulence). We discuss observed variations in the IRX -β relation for local (sub-galactic scales) and high-redshift (normal and dusty star-forming galaxies, galaxies during the epoch of reionization) galaxies in the context of the physical processes explored in our model. High spatial resolution imaging of the UV and sub-mm emission of galaxies can constrain the IRX -β dust attenuation relation for different galaxy types at different epochs, where different processes causing variations may dominate. These constraints will allow the use of the IRX -β relation to estimate intrinsic SFRs of galaxies, despite the lack of a universal relation.

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The infrared-dark dust content of high redshift galaxies

Cited by 59 publications

References 40 publications

Observational and theoretical constraints on the formation and early evolution of the first dust grains in galaxies at 5 < z < 10

Observational and theoretical constraints on the formation and early evolution of the first dust grains in galaxies at 5 < z < 10

Dusty galaxies in the Epoch of Reionization: simulations

Dissecting the IRX–β dust attenuation relation: exploring the physical origin of observed variations in galaxies

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