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dc.contributor.authorJohnson, H.~L.
dc.contributor.authorHarrison, C.~M.
dc.contributor.authorSwinbank, A.~M.
dc.contributor.authorBower, R.~G.
dc.contributor.authorSmail, I.
dc.contributor.authorKoyama, Y.
dc.contributor.authorGeach, J.~E.
dc.date.accessioned2016-12-16T15:57:39Z
dc.date.available2016-12-16T15:57:39Z
dc.date.issued2016-07-21
dc.identifier.citationJohnson , H L , Harrison , C M , Swinbank , A M , Bower , R G , Smail , I , Koyama , Y & Geach , J E 2016 , ' The Spatially Resolved Dynamics of Dusty Starburst Galaxies in a z tilde 0.4 Cluster: Beginning the Transition from Spirals to S0s ' Monthly Notices of the Royal Astronomical Society , vol. 460 , no. 1 , pp. 1059-1076 . https://doi.org/10.1093/mnras/stw1030
dc.identifier.issn1365-2966
dc.identifier.otherPURE: 10175306
dc.identifier.otherPURE UUID: 0901103e-cdbf-4512-9e66-51178a461342
dc.identifier.otherBibtex: urn:65b655ef8175f66456d55da906147404
dc.identifier.otherScopus: 84979085005
dc.identifier.urihttp://hdl.handle.net/2299/17441
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2016 H.L. Johnson, C. M. Harrison, A. M. Swinbank, R. G. Bower, Iam Smail, Y. Koyama, J. E. Geach. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.description.abstractTo investigate what drives the reversal of the morphology–density relation at intermediate/high redshift, we present a multiwavelength analysis of 27 dusty starburst galaxies in the massive cluster Cl 0024+17 at z = 0.4. We combine Hα dynamical maps from the VLT/FLAMES multi-IFU system with far-infrared imaging using Herschel/SPIRE and millimetre spectroscopy from IRAM/NOEMA, in order to measure the dynamics, star formation rates and gas masses of this sample. Most galaxies appear to be rotationally supported, with a median ratio of rotational-support to line-of-sight velocity dispersion v/σ ∼ 5 ± 2, and specific angular momentum λR = 0.83 ± 0.06 – comparable to field spirals of a similar mass at this redshift. The star formation rates of 3–26 M⊙ yr−1 and average 12CO-derived gas mass of ∼ 1 × 1010 M⊙ suggest gas depletion time-scales of ∼1 Gyr (∼0.25 of the cluster crossing time). We derive characteristic dust temperatures (mean Td = 26 ± 1 K) consistent with local galaxies of similar far-infrared luminosity, suggesting that the low-density gas is yet to be stripped. Taken together, these results suggest that these starbursts have only recently accreted from the field, with star formation rates likely enhanced due to the effects of ram pressure. In order to make the transition to cluster S0s these galaxies must lose ∼40 per cent of their specific angular momentum. We suggest this must occur ≥1 Gyr later, after the molecular gas has been depleted and/or stripped, via multiple tidal interactions with other cluster members.en
dc.format.extent18
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectgalaxies: clusters
dc.subjectgalaxies: starburst
dc.subjectgalaxies: evolution
dc.titleThe Spatially Resolved Dynamics of Dusty Starburst Galaxies in a z tilde 0.4 Cluster: Beginning the Transition from Spirals to S0sen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2016-04-28
rioxxterms.versionAM
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stw1030
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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