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A physical model for [C II] line emission from galaxies
Stockholm University, Nordic Institute for Theoretical Physics (Nordita). Leiden University, the Netherlands.ORCID iD: 0000-0002-3258-3672
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Number of Authors: 82019 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 489, no 1, p. 1-12Article in journal (Refereed) Published
Abstract [en]

A tight relation between the [C II] 158 mu m line luminosity and star formation rate is measured in local galaxies. At high redshift (z > 5), though, a much larger scatter is observed, with a considerable (15-20 per cent) fraction of the outliers being [C II]-deficient. Moreover, the [C II] surface brightness (Sigma([C II])) of these sources is systematically lower than expected from the local relation. To clarify the origin of such [C II]-deficiency, we have developed an analytical model that fits local [C II] data and has been validated against radiative transfer simulations performed with CLOUDY. The model predicts an overall increase of Sigma([C II]) with Sigma(SFR). However, for Sigma(SFR) greater than or similar to 1M(circle dot) yr(-1) kpc(-2), Sigma([C II]) saturates. We conclude that underluminous [C II] systems can result from a combination of three factors: (a) large upward deviations from theKennicutt-Schmidt relation (kappa(s) >> 1), parametrized by the 'burstiness' parameter kappa(s); (b) low metallicity; (c) low gas density, at least for the most extreme sources (e.g. CR7). Observations of [C II] emission alone cannot break the degeneracy among the above three parameters; this requires additional information coming from other emission lines (e.g. [OIII]88 mu m, C III]1909 degrees, CO lines). Simple formulae are given to interpret available data for low- and high- z galaxies.

Place, publisher, year, edition, pages
2019. Vol. 489, no 1, p. 1-12
Keywords [en]
photodissociation region (PDR), galaxies: high-redshift, galaxies: ISM
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Physical Sciences
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URN: urn:nbn:se:su:diva-175853DOI: 10.1093/mnras/stz2031ISI: 000489292800001OAI: oai:DiVA.org:su-175853DiVA, id: diva2:1369360
Available from: 2019-11-11 Created: 2019-11-11 Last updated: 2019-12-09Bibliographically approved

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Vallini, LiviaPallottini, A.Kohandel, M.Decataldo, D.
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