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dc.contributor.authorRuhland, Christine
dc.contributor.authorBell, Eric F.
dc.contributor.authorRix, Hans-Walter
dc.contributor.authorXue, Xiang-Xiang
dc.date.accessioned2011-12-21T09:01:04Z
dc.date.available2011-12-21T09:01:04Z
dc.date.issued2011-04-20
dc.identifier.citationRuhland , C , Bell , E F , Rix , H-W & Xue , X-X 2011 , ' The structure of the Sagittarius stellar stream as traced by blue horizontal branch stars ' , The Astrophysical Journal , vol. 731 , no. 2 , 119 . https://doi.org/10.1088/0004-637X/731/2/119
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 492896
dc.identifier.otherPURE UUID: 979b0456-bf08-4ed6-9aca-7877a38d5a85
dc.identifier.otherWOS: 000289779600042
dc.identifier.otherScopus: 79955034370
dc.identifier.urihttp://hdl.handle.net/2299/7436
dc.description.abstractWe use a sample of blue horizontal branch (BHB) stars from the Sloan Digital Sky Survey Data Release 7 to explore the structure of the tidal tails from the Sagittarius Dwarf Galaxy. We use a method yielding BHB star candidates with up to similar to 70% purity from photometry alone. The resulting sample has a distance precision of roughly 5% and can probe distances in excess of 100 kpc. Using this sample, we identify a possible extension to the trailing arm at distances of 60-80 kpc from the Sun with an estimated significance of at least 3.8 sigma. Current models predict that a distant "returning" segment of the debris stream should exist, but place it substantially closer to the Sun where no debris is observed in our data. Exploiting the distance precision of our tracers, we estimate the mean line-of-sight thickness of the leading arm to be similar to 3 kpc, and show that the two "bifurcated" branches of the debris stream differ by only 1-2 kpc in distance. With a spectroscopic very pure BHB star subsample, we estimate the velocity dispersion in the leading arm, 37 km s(-1), which is in reasonable agreement with models of Sgr disruption. We finally present a sample of high-probability Sgr BHB stars in the leading arm of Sgr, selected to have distances and velocities consistent with Sgr membership, to allow further study.en
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rightsOpen
dc.subjectgalaxies: dwarf
dc.subjectgalaxies: interactions
dc.subjectGalaxy: halo
dc.subjectGalaxy: stellar content
dc.subjectDIGITAL SKY SURVEY
dc.subjectDWARF SPHEROIDAL GALAXY
dc.subjectDARK-MATTER HALO
dc.subjectMILKY-WAY SATELLITE
dc.subjectGALACTIC GLOBULAR-CLUSTERS
dc.subjectRR-LYRAE STARS
dc.subjectA-TYPE STARS
dc.subjectTIDAL STREAMS
dc.subjectSURVEY VIEW
dc.subjectSPIRAL GALAXIES
dc.titleThe structure of the Sagittarius stellar stream as traced by blue horizontal branch starsen
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.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeSubmitted Version
dcterms.dateAccepted2011-04-20
rioxxterms.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/731/2/119
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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