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The Origins of [C II] Emission in Local Star-forming Galaxies

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dc.contributor.authorCroxall, K V
dc.contributor.authorSmith, J. D.
dc.contributor.authorPellegrini, E.
dc.contributor.authorGroves, Brent
dc.contributor.authorBolatto, Alberto
dc.contributor.authorHerrera-Camus, Rodrigo
dc.contributor.authorSandstrom, Karin M
dc.contributor.authorDraine, Bruce T
dc.contributor.authorWolfire, M.
dc.contributor.authorArmus, Lee
dc.contributor.authorBoquien, Médéric
dc.contributor.authorBrandl, B
dc.contributor.authorDale, Daniel A
dc.contributor.authorGalametz, Maud
dc.contributor.authorHunt, Leslie
dc.contributor.authorKennicutt, Robert C
dc.contributor.authorKreckel, K.
dc.contributor.authorRigopoulou, D.
dc.contributor.authorVan der Werf, P.
dc.contributor.authorWilson, Christine D.
dc.date.accessioned2021-09-30T23:13:26Z
dc.date.issued2017
dc.date.updated2020-11-23T11:19:06Z
dc.description.abstractThe [C ii] 158 μm fine-structure line is the brightest emission line observed in local star-forming galaxies. As a major coolant of the gas-phase interstellar medium, [C ii] balances the heating, including that due to far-ultraviolet photons, which heat the gas via the photoelectric effect. However, the origin of [C ii] emission remains unclear because C+ can be found in multiple phases of the interstellar medium. Here we measure the fractions of [C ii] emission originating in the ionized and neutral gas phases of a sample of nearby galaxies. We use the [N ii] 205 μm fine-structure line to trace the ionized medium, thereby eliminating the strong density dependence that exists in the ratio of [C ii]/[N ii] 122 μm. Using the FIR [C ii] and [N ii] emission detected by the KINGFISH (Key Insights on Nearby Galaxies: a Far- Infrared Survey with Herschel) and Beyond the Peak Herschel programs, we show that 60%–80% of [C ii] emission originates from neutral gas. We find that the fraction of [C ii] originating in the neutral medium has a weak dependence on dust temperature and the surface density of star formation, and has a stronger dependence on the gas-phase metallicity. In metal-rich environments, the relatively cooler ionized gas makes substantially larger contributions to total [C ii] emission than at low abundance, contrary to prior expectations. Approximate calibrations of this metallicity trend are provideden_AU
dc.description.sponsorshipK.V.C. acknowledges support from the Deutsche Forschungsgemeinschaft Priority Program ISM-SPP 1573 and the MPIA, and thanks the KINGFISH & BTP teams for their support. J.D.S. acknowledges visiting support from the Alexander von Humboldt Foundation and the MPIA. B.G. acknowledges the support of the Australian Research Council via a Future Fellowship (FT140101202). A.D.B. acknowledges partial support from NSFAST0955836 and 1412419. B.T.D. acknowledges partial support from NSF-AST1408723. M.B. was supported by MINEDUC-UA project, code ANT 1655. Beyond the Peak research has been supported by a NASA/JPL grant (RSA 1427378).en_AU
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.issn0004-637Xen_AU
dc.identifier.urihttp://hdl.handle.net/1885/249095
dc.language.isoen_AUen_AU
dc.provenancehttps://v2.sherpa.ac.uk/id/publication/6401..."The Accepted Version can be archived in a Non-Commercial Institutional Repository" from SHERPA/RoMEO site (as at 8/10/2021).
dc.publisherIOP Publishingen_AU
dc.relationhttp://purl.org/au-research/grants/arc/FT140101202
dc.rights© 2017. The American Astronomical Society.en_AU
dc.sourceThe Astrophysical Journalen_AU
dc.subjectgalaxies: ISMen_AU
dc.subjectISM: lines and bandsen_AU
dc.titleThe Origins of [C II] Emission in Local Star-forming Galaxiesen_AU
dc.typeJournal articleen_AU
dcterms.accessRightsOpen Access
local.bibliographicCitation.issue2en_AU
local.bibliographicCitation.lastpage7en_AU
local.bibliographicCitation.startpage1en_AU
local.contributor.affiliationCroxall, K V, Ohio State Universityen_AU
local.contributor.affiliationSmith, J. D., University of Toledoen_AU
local.contributor.affiliationPellegrini, E., University of Toledoen_AU
local.contributor.affiliationGroves, Brent Allan, College of Science, ANUen_AU
local.contributor.affiliationBolatto, Alberto, University of Marylanden_AU
local.contributor.affiliationHerrera-Camus, Rodrigo, Max Planck Institut fur extraterrestrische Physiken_AU
local.contributor.affiliationSandstrom, Karin M, University of Californiaen_AU
local.contributor.affiliationDraine, Bruce T, Princeton Universityen_AU
local.contributor.affiliationWolfire, M., University of Marylanden_AU
local.contributor.affiliationArmus, Lee, California Institute of Technologyen_AU
local.contributor.affiliationBoquien, Médéric, Universidad de Antofagasta, Unidad de Astronomíaen_AU
local.contributor.affiliationBrandl, B, Leiden Observatory at Leiden Universityen_AU
local.contributor.affiliationDale, Daniel A, University of Wyomingen_AU
local.contributor.affiliationGalametz, Maud, ESOen_AU
local.contributor.affiliationHunt, Leslie, INAF-Osservatorio Astrofisico di Arcetrien_AU
local.contributor.affiliationKennicutt, Robert C , University of Cambridgeen_AU
local.contributor.affiliationKreckel, K., Max Planck Institut fur Astronomieen_AU
local.contributor.affiliationRigopoulou, D., Department of Astrophysics, University of Oxforden_AU
local.contributor.affiliationVan der Werf, P., Leiden Observatory, Leiden Universityen_AU
local.contributor.affiliationWilson, Christine D., McMaster Universityen_AU
local.contributor.authoruidGroves, Brent Allan, u9816125en_AU
local.description.notesImported from ARIESen_AU
local.identifier.absfor020103 - Cosmology and Extragalactic Astronomyen_AU
local.identifier.ariespublicationu4351680xPUB44en_AU
local.identifier.citationvolume845en_AU
local.identifier.doi10.3847/1538-4357/aa8035en_AU
local.identifier.scopusID2-s2.0-85028757333
local.identifier.thomsonID000407801100006
local.publisher.urlhttp://iopscience.iop.org/0004-637Xen_AU
local.type.statusAccepted Versionen_AU

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