Show simple item record

dc.contributor.authorPettitt, AR
dc.contributor.authorDobbs, CL
dc.contributor.authorBaba, J
dc.contributor.authorColombo, D
dc.contributor.authorDuarte-Cabral, A
dc.contributor.authorEgusa, F
dc.contributor.authorHabe, A
dc.date.accessioned2021-06-01T06:41:50Z
dc.date.issued2020-08-06
dc.description.abstractThe nature of galactic spiral arms in disc galaxies remains elusive. Regardless of the spiral model, arms are expected to play a role in sculpting the star-forming interstellar medium (ISM). As such, different arm models may result in differences in the structure of the ISM and molecular cloud properties. In this study, we present simulations of galactic discs subject to spiral arm perturbations of different natures. We find very little difference in how the cloud population or gas kinematics vary between the different grand design spirals, indicating that the ISM on cloud scales cares little about where spiral arms come from. We do, however, see a difference in the interarm/arm mass spectra, and minor differences in tails of the distributions of cloud properties (as well as radial variations in the stellar/gaseous velocity dispersions). These features can be attributed to differences in the radial dependence of the pattern speeds between the different spiral models, and could act as a metric of the nature of spiral structure in observational studies.en_GB
dc.description.sponsorshipJapanese Society for the Promotion of Science (JSPS)en_GB
dc.description.sponsorshipEuropean Union Horizon 2020en_GB
dc.description.sponsorshipDeutsche Forschungsgemeinschaft (DFG)en_GB
dc.description.sponsorshipRoyal Societyen_GB
dc.description.sponsorshipHeising-Simons Foundationen_GB
dc.description.sponsorshipNational Science Foundationen_GB
dc.identifier.citationVol. 498 (1), pp. 1159 - 1174en_GB
dc.identifier.doi10.1093/mnras/staa2242
dc.identifier.grantnumber20K14456en_GB
dc.identifier.grantnumber18H01248.en_GB
dc.identifier.grantnumber818940en_GB
dc.identifier.grantnumberSFB956Aen_GB
dc.identifier.grantnumberURF/R1/191609en_GB
dc.identifier.grantnumberP19K03923en_GB
dc.identifier.grantnumber17K14259en_GB
dc.identifier.grantnumberNSF PHY-1748958en_GB
dc.identifier.urihttp://hdl.handle.net/10871/125889
dc.language.isoenen_GB
dc.publisherOxford University Press (OUP) / Royal Astronomical Societyen_GB
dc.rights© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Societyen_GB
dc.subjectmethods: numericalen_GB
dc.subjectISM: cloudsen_GB
dc.subjectISM: structureen_GB
dc.subjectgalaxies: ISMen_GB
dc.subjectgalaxies: spiralen_GB
dc.subjectgalaxies: structureen_GB
dc.titleHow do different spiral arm models impact the ISM and GMC population?en_GB
dc.typeArticleen_GB
dc.date.available2021-06-01T06:41:50Z
dc.identifier.issn0035-8711
dc.descriptionThis is the final version. Available from Oxford University Press via the DOI in this recorden_GB
dc.descriptionData availability: The data underlying this article will be shared on reasonable request to the corresponding author.en_GB
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen_GB
dc.rights.urihttp://www.rioxx.net/licenses/all-rights-reserveden_GB
dcterms.dateAccepted2020-07-27
exeter.funder::European Commissionen_GB
rioxxterms.versionVoRen_GB
rioxxterms.licenseref.startdate2020-08-06
rioxxterms.typeJournal Article/Reviewen_GB
refterms.dateFCD2021-05-31T13:48:53Z
refterms.versionFCDVoR
refterms.dateFOA2021-06-01T06:42:04Z
refterms.panelBen_GB


Files in this item

This item appears in the following Collection(s)

Show simple item record