Full-disc 13CO(1-0) mapping across nearby galaxies of the EMPIRE survey and the CO-to-H2 conversion factor

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dc.contributor.authorCormier, Diane
dc.contributor.authorBigiel, F
dc.contributor.authorJimenez-Donaire, Maria J.
dc.contributor.authorLeroy, Adam K
dc.contributor.authorGallagher, Molly
dc.contributor.authorUsero, Antonio
dc.contributor.authorSandstrom, Karin M
dc.contributor.authorBolatto, Alberto
dc.contributor.authorHughes, A.
dc.contributor.authorKramer, C.
dc.contributor.authorKrumholz, Mark
dc.date.accessioned2021-10-29T01:15:34Z
dc.date.available2021-10-29T01:15:34Z
dc.date.issued2018-01-09
dc.date.updated2020-11-23T11:41:58Z
dc.description.abstractCarbon monoxide (CO) provides crucial information about the molecular gas properties of galaxies. While 12CO has been targeted extensively, isotopologues such as 13CO have the advantage of being less optically thick and observations have recently become accessible across full galaxy discs. We present a comprehensive new data set of 13CO(1-0) observations with the IRAM30-m telescope of the full discs of nine nearby spiral galaxies from the EMPIRE survey at a spatial resolution of ~1.5 kpc. 13CO(1-0) is mapped out to 0.7 - 1 r25 and detected at high signal-to-noise ratio throughout our maps. We analyse the 12CO(1-0)-to-13CO(1-0) ratio (R) as a function of galactocentric radius and other parameters such as the 12CO(2-1)-to- 12CO(1-0) intensity ratio, the 70-to-160 μm flux density ratio, the star formation rate surface density, the star formation efficiency, and the CO-to-H2 conversion factor.We find that R varies by a factor of 2 at most within and amongst galaxies, with a median value of 11 and larger variations in the galaxy centres than in the discs.We argue that optical depth effects, most likely due to changes in the mixture of diffuse/dense gas, are favoured explanations for the observed R variations, while abundance changes may also be at play. We calculate a spatially resolved 13CO(1-0)-to-H2 conversion factor and find an average value of 1.0×1021 cm-2 (K km s-1)-1 over our sample with a standard deviation of a factor of 2. We find that 13CO(1-0) does not appear to be a good predictor of the bulk molecular gas mass in normal galaxy discs due to the presence of a large diffuse phase, but it may be a better tracer of the mass than 12CO(1-0) in the galaxy centres where the fraction of dense gas is larger.en_AU
dc.description.sponsorshipDC is supported by the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 702622. DC also acknowledges support from the DAAD/PROCOPE projects 57210883/35265PE. MJJD and FB acknowledge support from the German Research Foundation (DFG) grant BI 1546/1-1. FB acknowledges funding from the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 726384 – EMPIRE). The work of MG and AKL is partially supported by the National Science Foundation under grants nos 1615105, 1615109, and 1653300. ER is supported by a Discovery Grant from the Natural Sciences and Engineering Research Council of Canada (NSERC) of Canada. ES acknowledges funding from the European Research Council under the European Unions Horizon 2020 research and innovation programme (grant agreement no. 694343).en_AU
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.issn0035-8711en_AU
dc.identifier.urihttp://hdl.handle.net/1885/251295
dc.language.isoen_AUen_AU
dc.provenancehttps://v2.sherpa.ac.uk/id/publication/24618..."Published Version can be archived in an Institutional Repository" from SHERPA/RoMEO site (as at 29.10.2021).en_AU
dc.publisherOxford University Press (OUP)en_AU
dc.rights© 2018 The Author(s)en_AU
dc.sourceMonthly Notices of the Royal Astronomical Societyen_AU
dc.subjectISM: moleculesen_AU
dc.subjectgalaxies: spiralen_AU
dc.subjectgalaxies: star formationen_AU
dc.titleFull-disc 13CO(1-0) mapping across nearby galaxies of the EMPIRE survey and the CO-to-H2 conversion factoren_AU
dc.typeJournal articleen_AU
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.issue3en_AU
local.bibliographicCitation.lastpage3933en_AU
local.bibliographicCitation.startpage3909en_AU
local.contributor.affiliationCormier, Diane, Zentrum für Astronomie der Universität Heidelbergen_AU
local.contributor.affiliationBigiel, F, Universität Heidelbergen_AU
local.contributor.affiliationJimenez-Donaire, Maria J., Zentrum für Astronomie der Universität Heidelbergen_AU
local.contributor.affiliationLeroy, Adam K, The Ohio State Universityen_AU
local.contributor.affiliationGallagher, Molly, The Ohio State Universityen_AU
local.contributor.affiliationUsero, Antonio, Observatorio Astronómico Nacionaen_AU
local.contributor.affiliationSandstrom, Karin M, University of Californiaen_AU
local.contributor.affiliationBolatto, Alberto, University of Marylanden_AU
local.contributor.affiliationHughes, A., Université de Toulouseen_AU
local.contributor.affiliationKramer, C., Instituto de Radioastronomıa Milimetricaen_AU
local.contributor.affiliationKrumholz, Mark, College of Science, ANUen_AU
local.contributor.authoremailu1000557@anu.edu.auen_AU
local.contributor.authoruidKrumholz, Mark, u1000557en_AU
local.description.notesImported from ARIESen_AU
local.identifier.absfor020104 - Galactic Astronomyen_AU
local.identifier.ariespublicationa383154xPUB9797en_AU
local.identifier.citationvolume475en_AU
local.identifier.doi10.1093/mnras/sty059en_AU
local.identifier.scopusID2-s2.0-85045945904
local.identifier.uidSubmittedBya383154en_AU
local.publisher.urlhttp://mnras.oxfordjournals.org/en_AU
local.type.statusPublished Versionen_AU

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