The neutral hydrogen properties of galaxies in gas-rich groups

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dc.contributor.authorDzudzar, Robert
dc.contributor.authorKilborn, Virginia A
dc.contributor.authorMeurer, Gerhardt
dc.contributor.authorSweet, Sarah
dc.contributor.authorDrinkwater, Michael John
dc.contributor.authorBekki, Kenji
dc.contributor.authorAudcent-Ross, Fiona
dc.contributor.authorKoribalski, Baerbel S
dc.contributor.authorKim, Ji Hoon
dc.contributor.authorPutman, Mary E
dc.contributor.authorDopita, Michael
dc.contributor.authorFreeman, Kenneth
dc.date.accessioned2022-05-03T00:23:07Z
dc.date.available2022-05-03T00:23:07Z
dc.date.issued2019
dc.date.updated2020-12-27T07:24:07Z
dc.description.abstractWe present an analysis of the integrated neutral hydrogen (H I) properties for 27 galaxies within nine low-mass, gas-rich, late-type dominated groups which we denote 'Choirs'. We find that majority of the central Choir galaxies have average H I content: they have a normal gas-mass fraction with respect to isolated galaxies of the same stellar mass. In contrast, we find more satellite galaxies with a lower gas-mass fraction than isolated galaxies of the same stellar mass. A likely reason for the lower gas content in these galaxies is tidal stripping. Both the specific star formation rate and the star formation efficiency of the central group galaxies are similar to galaxies in isolation. The Choir satellite galaxies have similar specific star formation rate as galaxies in isolation, therefore satellites that exhibit a higher star formation efficiency simply owe it to their lower gas-mass fractions. We find that the most H I massive galaxies have the largest H I discs and fall neatly on to the H I size-mass relation, while outliers are galaxies that are experiencing interactions. We find that high specific angular momentum could be a reason for galaxies to retain the large fraction of H I gas in their discs. This shows that for the Choir groups with no evidence of interactions, as well as those with traces of minor mergers, the internal galaxy properties dominate over the effects of residing in a group. The probed galaxy properties strengthen evidence that the Choir groups represent the early stages of group assembly.en_AU
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.issn0035-8711en_AU
dc.identifier.urihttp://hdl.handle.net/1885/264242
dc.language.isoen_AUen_AU
dc.provenancehttps://v2.sherpa.ac.uk/id/publication/24618..."The Published Version can be archived in an Institutional Repository" from SHERPA/RoMEO site (as at 3/05/2022). This article has been accepted for publication in [Monthly Notices of the Royal Astronomical Society] ©: 2018 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.en_AU
dc.publisherOxford University Pressen_AU
dc.rights© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Societyen_AU
dc.sourceMonthly Notices of the Royal Astronomical Societyen_AU
dc.subjectgalaxies: evolutionen_AU
dc.subjectgalaxies: generalen_AU
dc.subjectgalaxies: groups: generalen_AU
dc.subjectgalaxies: groups: individual: HIPASSJ1250-20en_AU
dc.subjectgalaxies: interactionsen_AU
dc.subjectgalaxies: ISMen_AU
dc.titleThe neutral hydrogen properties of galaxies in gas-rich groupsen_AU
dc.typeJournal articleen_AU
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.issue4en_AU
local.bibliographicCitation.lastpage5425en_AU
local.bibliographicCitation.startpage5409en_AU
local.contributor.affiliationDzudzar, Robert, Swinburne University of Technologyen_AU
local.contributor.affiliationKilborn, Virginia A, Swinburne University of Technologyen_AU
local.contributor.affiliationMeurer, Gerhardt, International Centre for Radio Astronomy Researchen_AU
local.contributor.affiliationSweet, Sarah, Swinburne University of Technologyen_AU
local.contributor.affiliationDrinkwater, Michael John, University of Queenslanden_AU
local.contributor.affiliationBekki, Kenji, International Centre for Radio Astronomy Researchen_AU
local.contributor.affiliationAudcent-Ross, Fiona, University of Western Australiaen_AU
local.contributor.affiliationKoribalski, Baerbel S, CSIRO, Australia Telescope National Facilityen_AU
local.contributor.affiliationKim, Ji Hoon, National Astronomical Observatory of Japanen_AU
local.contributor.affiliationPutman, Mary E, Columbia Universityen_AU
local.contributor.affiliationDopita, Michael, College of Science, ANUen_AU
local.contributor.affiliationFreeman, Kenneth, College of Science, ANUen_AU
local.contributor.authoremailu7501303@anu.edu.auen_AU
local.contributor.authoruidDopita, Michael, u7501303en_AU
local.contributor.authoruidFreeman, Kenneth, u7000399en_AU
local.description.notesImported from ARIESen_AU
local.identifier.absfor020103 - Cosmology and Extragalactic Astronomyen_AU
local.identifier.absfor020201 - Atomic and Molecular Physicsen_AU
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciencesen_AU
local.identifier.ariespublicationu3102795xPUB2142en_AU
local.identifier.citationvolume483en_AU
local.identifier.doi10.1093/mnras/sty3500en_AU
local.identifier.scopusID2-s2.0-85062274036
local.identifier.thomsonID4.62282E+11
local.identifier.uidSubmittedByu3102795en_AU
local.publisher.urlhttp://mnras.oxfordjournals.org/en_AU
local.type.statusPublished Versionen_AU

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