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dc.contributor.authorSharma, Anubhav
dc.contributor.authorMasters, Karen L
dc.contributor.authorStark, David V
dc.contributor.authorGarland, James
dc.contributor.authorDrory, Niv
dc.contributor.authorFraser-McKelvie, Amelia
dc.contributor.authorWeijmans, Anne-Marie
dc.date.accessioned2023-10-09T09:30:07Z
dc.date.available2023-10-09T09:30:07Z
dc.date.issued2023-11-01
dc.identifier.citationSharma , A , Masters , K L , Stark , D V , Garland , J , Drory , N , Fraser-McKelvie , A & Weijmans , A-M 2023 , ' HI-rich but low star formation galaxies in MaNGA : physical properties and comparison to control samples ' , Monthly Notices of the Royal Astronomical Society , vol. 526 , no. 1 , pp. 1573-1587 . https://doi.org/10.1093/mnras/stad2695en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 294266913
dc.identifier.otherPURE UUID: 82fdcbfc-5af5-4c69-907d-080a43c1c84c
dc.identifier.otherJisc: 1387952
dc.identifier.otherORCID: /0000-0002-5908-6852/work/144461941
dc.identifier.otherScopus: 85174510015
dc.identifier.otherJisc: 1344036
dc.identifier.urihttps://hdl.handle.net/10023/28512
dc.descriptionFunding: This publication acknowledges Haverford College Koshland Integrated Natural Sciences Center (KINSC)’s support in summer 2020 and summer 2021 research programmes through a Summer Research Grant.en
dc.description.abstractGas-rich galaxies are typically star forming. We make use of H i-MaNGA, a programme of H i follow-up for the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey of the Sloan Digital Sky Surveys, to construct a sample of unusual neutral hydrogen (H i, 21 cm)-rich galaxies that have low star formation rates (SFRs), using infrared colour from the Wide-field Infrared Survey Explorer as a proxy for specific SFR. Out of a set of 1575 MaNGA galaxies with H i-MaNGA detections, we find that 83 (5 per cent) meet our selection criteria to be H i rich with low SFR. We construct two stellar mass-matched control samples: H i-rich galaxies with typical SFR (high SF control) and H i-poor galaxies with low SFR (low H i control). We investigate the properties of each of these samples, comparing physical parameters such as ionization state maps, stellar and ionized gas velocity and dispersion, environment measures, metallicity, and morphology to search for the reasons why these unusual H i-rich galaxies are not forming stars. We find evidence for recent external accretion of gas in some galaxies (via high counter-rotating fractions), along with some evidence for active galactic nucleus (AGN) feedback (from a high central low-ionization emission-line region and/or red geyser fraction), and bar quenching (via an enhanced strong bar fraction). Some galaxies in the sample are consistent with simply having their H i in a high angular momentum, large-radius, low-density disc. We conclude that no single physical process can explain all H i-rich, low-SFR galaxies.
dc.format.extent15
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stad2695.en
dc.subjectGalaxies: evolutionen
dc.subjectCataloguesen
dc.subjectSurveysen
dc.subjectGalaxies: star formationen
dc.subject3rd-DASen
dc.subjectMCCen
dc.titleHI-rich but low star formation galaxies in MaNGA : physical properties and comparison to control samplesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. Centre for Contemporary Arten
dc.identifier.doihttps://doi.org/10.1093/mnras/stad2695
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/2309.04854en


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