dc.contributor.author | Pettitt, AR | |
dc.contributor.author | Dobbs, CL | |
dc.contributor.author | Baba, J | |
dc.contributor.author | Colombo, D | |
dc.contributor.author | Duarte-Cabral, A | |
dc.contributor.author | Egusa, F | |
dc.contributor.author | Habe, A | |
dc.date.accessioned | 2021-06-01T06:41:50Z | |
dc.date.issued | 2020-08-06 | |
dc.description.abstract | The 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.sponsorship | Japanese Society for the Promotion of Science (JSPS) | en_GB |
dc.description.sponsorship | European Union Horizon 2020 | en_GB |
dc.description.sponsorship | Deutsche Forschungsgemeinschaft (DFG) | en_GB |
dc.description.sponsorship | Royal Society | en_GB |
dc.description.sponsorship | Heising-Simons Foundation | en_GB |
dc.description.sponsorship | National Science Foundation | en_GB |
dc.identifier.citation | Vol. 498 (1), pp. 1159 - 1174 | en_GB |
dc.identifier.doi | 10.1093/mnras/staa2242 | |
dc.identifier.grantnumber | 20K14456 | en_GB |
dc.identifier.grantnumber | 18H01248. | en_GB |
dc.identifier.grantnumber | 818940 | en_GB |
dc.identifier.grantnumber | SFB956A | en_GB |
dc.identifier.grantnumber | URF/R1/191609 | en_GB |
dc.identifier.grantnumber | P19K03923 | en_GB |
dc.identifier.grantnumber | 17K14259 | en_GB |
dc.identifier.grantnumber | NSF PHY-1748958 | en_GB |
dc.identifier.uri | http://hdl.handle.net/10871/125889 | |
dc.language.iso | en | en_GB |
dc.publisher | Oxford University Press (OUP) / Royal Astronomical Society | en_GB |
dc.rights | © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society | en_GB |
dc.subject | methods: numerical | en_GB |
dc.subject | ISM: clouds | en_GB |
dc.subject | ISM: structure | en_GB |
dc.subject | galaxies: ISM | en_GB |
dc.subject | galaxies: spiral | en_GB |
dc.subject | galaxies: structure | en_GB |
dc.title | How do different spiral arm models impact the ISM and GMC population? | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2021-06-01T06:41:50Z | |
dc.identifier.issn | 0035-8711 | |
dc.description | This is the final version. Available from Oxford University Press via the DOI in this record | en_GB |
dc.description | Data availability: The data underlying this article will be shared on reasonable request to the corresponding author. | en_GB |
dc.identifier.journal | Monthly Notices of the Royal Astronomical Society | en_GB |
dc.rights.uri | http://www.rioxx.net/licenses/all-rights-reserved | en_GB |
dcterms.dateAccepted | 2020-07-27 | |
exeter.funder | ::European Commission | en_GB |
rioxxterms.version | VoR | en_GB |
rioxxterms.licenseref.startdate | 2020-08-06 | |
rioxxterms.type | Journal Article/Review | en_GB |
refterms.dateFCD | 2021-05-31T13:48:53Z | |
refterms.versionFCD | VoR | |
refterms.dateFOA | 2021-06-01T06:42:04Z | |
refterms.panel | B | en_GB |