¹³CO/C¹⁸O Gradients across the Disks of Nearby Spiral Galaxies

dc.contributor.authorJimenez-Donaire, Maria J.
dc.contributor.authorCormier, Diane
dc.contributor.authorBigiel, Frank
dc.contributor.authorLeroy, Adam K
dc.contributor.authorGallagher, Molly
dc.contributor.authorKrumholz, Mark
dc.contributor.authorUsero, Antonio
dc.contributor.authorHughes, Annie
dc.contributor.authorKramer, Carsten
dc.contributor.authorMeier, David
dc.contributor.authorMurphy, Eric
dc.contributor.authorPety, Jerome
dc.contributor.authorSchinnerer, Eva
dc.contributor.authorSchruba, Andreas
dc.contributor.authorSchuster, Karl
dc.contributor.authorSliwa, Kazimierz
dc.contributor.authorTomicic, Neven
dc.date.accessioned2021-04-23T00:57:01Z
dc.date.issued2017
dc.date.updated2020-11-23T10:04:03Z
dc.description.abstractWe use the IRAM Large Program EMPIRE and new high-resolution ALMA data to measure 13CO(1-0)/C18O(1-0) intensity ratios across nine nearby spiral galaxies. These isotopologues of 12CO are typically optically thin across most of the area in galaxy disks, and this ratio allows us to gauge their relative abundance due to chemistry or stellar nucleosynthesis effects. Resolved 13CO/C18O gradients across normal galaxies have been rare due to the faintness of these lines. We find a mean 13CO/C18O ratio of 6.0 ± 0.9 for the central regions of our galaxies. This agrees well with results in the Milky Way, but differs from results for starburst galaxies (3.4 ± 0.9) and ultraluminous infrared galaxies (1.1 ± 0.4). In our sample, the 13CO/C18O ratio consistently increases with increasing galactocentric radius and decreases with increasing star formation rate surface density. These trends could be explained if the isotopic abundances are altered by fractionation; the sense of the trends also agrees with those expected for carbon and oxygen isotopic abundance variations due to selective enrichment by massive stars.en_AU
dc.description.sponsorshipF.B., M.J., and D.C. acknowledge support from DFG grant BI 1546/1-1. A.H. acknowledges support from the Centre National d’Etudes Spatiales (CNES). A.U. acknowledges support from Spanish MINECO grants FIS2012-32096 and ESP2015-68964. The work of A.K.L. is partially supported by the National Science Foundation under grants No. 1615105 and 1615109. M.R.K. acknowledges support from ARC DP160100695. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO. ALMA #2011.0.00004.SV. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.en_AU
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.issn2041-8205en_AU
dc.identifier.urihttp://hdl.handle.net/1885/230985
dc.language.isoen_AUen_AU
dc.provenancehttps://v2.sherpa.ac.uk/id/publication/6402..."The Accepted Version can be archived in a Non-Commercial Institutional Repository. 12 months embargo" from SHERPA/RoMEO site (as at 27/04/2021).
dc.publisherInstitute of Physics Publishing Ltd.en_AU
dc.relationhttp://purl.org/au-research/grants/arc/DP160100695en_AU
dc.rights© 2017. The American Astronomical Societyen_AU
dc.sourceAstrophysical Journal Lettersen_AU
dc.subjectgalaxies: ISMen_AU
dc.subjectISM: moleculesen_AU
dc.subjectradio lines: galaxiesen_AU
dc.title¹³CO/C¹⁸O Gradients across the Disks of Nearby Spiral Galaxiesen_AU
dc.typeJournal articleen_AU
dcterms.accessRightsOpen Access
local.bibliographicCitation.issue2en_AU
local.bibliographicCitation.lastpage6en_AU
local.bibliographicCitation.startpage1en_AU
local.contributor.affiliationJimenez-Donaire, Maria J., Zentrum für Astronomie der Universität Heidelbergen_AU
local.contributor.affiliationCormier, Diane, Zentrum für Astronomie der Universität Heidelbergen_AU
local.contributor.affiliationBigiel, Frank, 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.affiliationKrumholz, Mark, College of Science, ANUen_AU
local.contributor.affiliationUsero, Antonio, Observatorio Astronómico Nacionaen_AU
local.contributor.affiliationHughes, Annie, Université de Toulouseen_AU
local.contributor.affiliationKramer, Carsten, IAA-CSIC, Glorieta de la Astronomíen_AU
local.contributor.affiliationMeier, David, New Mexico Institute of Mining and Technologyen_AU
local.contributor.affiliationMurphy, Eric, National Radio Astronomy Observatoryen_AU
local.contributor.affiliationPety, Jerome, Observatoire de Parisen_AU
local.contributor.affiliationSchinnerer, Eva, Max Planck Institut fur Astronomieen_AU
local.contributor.affiliationSchruba, Andreas, Max-Planck-Institut fuer extraterrestrische Physiken_AU
local.contributor.affiliationSchuster, Karl, Institut de Radioastronomie Millimetriqueen_AU
local.contributor.affiliationSliwa, Kazimierz, Max-Planck-Institut für Astronomieen_AU
local.contributor.affiliationTomicic, Neven, Max-Planck-Institut für Astronomieen_AU
local.contributor.authoremailu1000557@anu.edu.auen_AU
local.contributor.authoruidKrumholz, Mark, u1000557en_AU
local.description.notesImported from ARIESen_AU
local.identifier.absfor020199 - Astronomical and Space Sciences not elsewhere classifieden_AU
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciencesen_AU
local.identifier.ariespublicationa383154xPUB5311en_AU
local.identifier.citationvolume836en_AU
local.identifier.doi10.3847/2041-8213/836/2/L29en_AU
local.identifier.scopusID2-s2.0-85014348890
local.identifier.thomsonID000396007700003
local.identifier.uidSubmittedBya383154en_AU
local.publisher.urlhttp://iopscience.iop.org/2041-8205en_AU
local.type.statusAccepted Versionen_AU

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