Infrared emission of z ∼ 6 galaxies: AGN imprints

Journal
Date Issued
2021
Author(s)
Di Mascia, F.
•
Gallerani, S.
•
Behrens, C.
•
Pallottini, A.
•
Carniani, S.
•
Ferrara, A.
•
•
•
Zana, T.
DOI
Abstract
We investigate the infrared (IR) emission of high-redshift (z ∼ 6), highly star-forming ( ${{\rm SFR}\gt 100\,{\rm M}_{\odot }\, {\rm yr}^{-1}}$ ) galaxies, with/without active galactic nuclei (AGN), using a suite of cosmological simulations featuring dust radiative transfer. Synthetic spectral energy distributions (SEDs) are used to quantify the relative contribution of stars/AGN to dust heating. In dusty (Md ≳ 3 × 107 M⊙) galaxies, ≳50-90 per cent of the ultraviolet (UV) radiation is obscured by dust inhomogeneities on scales ≳100 pc. In runs with AGN, a clumpy, warm (≈250 K) dust component coexists with a colder (≈60 K) and more diffuse one, heated by stars. Warm dust provides up to ${50 {{\ \rm per\ cent}}}$ of the total infrared (IR) luminosity, but only ${\lesssim}0.1 {{\ \rm per\ cent}}$ of the total mass content. The AGN boosts the MIR flux by 10-100 times with respect to star-forming galaxies, without significantly affecting the far-IR. Our simulations successfully reproduce the observed SED of bright (MUV ∼ -26) z ∼ 6 quasars, and show that these objects are part of complex, dust-rich merging systems, containing multiple sources (accreting black holes and/or star-forming galaxies) in agreement with recent HST and ALMA observations. Our results show that the proposed ORIGINS missions will be able to investigate the mid-IR (MIR) properties of dusty star-forming galaxies and to obtain good-quality spectra of bright quasars at z ∼ 6. Finally, the MIR-to-FIR flux ratio of faint (MUV ∼ -24) AGN is >10 times higher than for normal star-forming galaxies. This implies that combined JWST/ORIGINS/ALMA observations will be crucial to identify faint and/or dust-obscured AGN in the distant Universe.
Volume
503
Issue
2
Start page
2349
Uri
Url
Issn Identifier
0035-8711
Ads BibCode
2021MNRAS.503.2349D
Rights
open.access
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