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dc.contributor.authorKaviraj, S.
dc.contributor.authorDarg, D.
dc.contributor.authorLintott, C.
dc.contributor.authorSilk, J.
dc.contributor.authorSchawinski, K.
dc.date.accessioned2013-10-30T11:00:54Z
dc.date.available2013-10-30T11:00:54Z
dc.date.issued2012-01-01
dc.identifier.citationKaviraj , S , Darg , D , Lintott , C , Silk , J & Schawinski , K 2012 , ' Tidal dwarf galaxies in the nearby Universe ' Monthly Notices of the Royal Astronomical Society , vol. 419 , no. 1 , pp. 70-79 . https://doi.org/10.1111/j.1365-2966.2011.19673.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 2067122
dc.identifier.otherPURE UUID: 1c51cb24-d83d-4812-a985-326acf2b0fb4
dc.identifier.otherScopus: 83555175944
dc.identifier.urihttp://hdl.handle.net/2299/11918
dc.description.abstractWe present a statistical observational study of the tidal dwarf (TD) population in the nearby Universe by exploiting a large, homogeneous catalogue of galaxy mergers compiled from the Sloan Digital Sky Survey. 95percent of TD-producing mergers involve two spiral progenitors (typically both in the blue cloud), while most remaining systems have at least one spiral progenitor. The fraction of TD-producing mergers where both parents are early-type galaxies is less than 2percent, suggesting that TDs are unlikely to form in such mergers. The bulk of TD-producing mergers inhabit a field environment and have mass ratios greater than ~1:7 (the median value is 1:2.5). TDs forming at the tidal-tail tips are ~4 times more massive than those forming at the base of the tails. TD stellar masses are less than 10percent of the stellar masses of their parents (the median is 0.6percent) and lie within 15 optical half-light radii of their parent galaxies. The TD population is typically bluer than the parents, with a median offset of ~0.3mag in the (g-r) colour and the TD colours are not affected by the presence of active galactic nuclei (AGN) activity in their parents. An analysis of their star formation histories indicates that TDs contain both newly formed stars (with a median age of ~30Myr) and old stars drawn from the parent discs, each component probably contributing roughly equally to the stellar mass of the object. Thus TDs are not formed purely through gas condensation in tidal tails but host a significant component of old stars from the parent discs. Finally, an analysis of the TD contribution to the observed dwarf-to-massive galaxy ratio in the local Universe indicates that ~6percent of dwarfs in nearby clusters may have a tidal origin, if TD production rates in nearby mergers are representative of those in the high-redshift Universe. Even if TD production rates at high redshift were several factors higher, it seems unlikely that the entire dwarf galaxy population today is a result of merger activity over the lifetime of the Universe.en
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.titleTidal dwarf galaxies in the nearby Universeen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=83555175944&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeSubmitted Version
rioxxterms.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2011.19673.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstyperestrictedAccess


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