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dc.contributor.authorLunnan, Ragnhild
dc.contributor.authorCasey, Andrew R.
dc.contributor.authorNorris, John E.
dc.contributor.authorWyse, Rosemary F. G.
dc.contributor.authorGilmore, Gerard
dc.contributor.authorFrebel, Anna L.
dc.date.accessioned2015-02-13T19:58:36Z
dc.date.available2015-02-13T19:58:36Z
dc.date.issued2013-06
dc.date.submitted2012-12
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1721.1/94536
dc.description.abstractWe present a chemical abundance analysis of 300S-1, the brightest likely member star of the 300 km s[superscript –1] stream near the faint satellite galaxy Segue 1. From a high-resolution Magellan/MIKE spectrum, we determine a metallicity of [Fe/H] = –1.46 ± 0.05 ± 0.23 (random and systematic uncertainties) for star 300S-1, and find an abundance pattern similar to typical halo stars at this metallicity. Comparing our stellar parameters to theoretical isochrones, we estimate a distance of 18 ± 7 kpc. Both the metallicity and distance estimates are in good agreement with what can be inferred from comparing the Sloan Digital Sky Survey photometric data of the stream stars to globular cluster sequences. While several other structures overlap with the stream in this part of the sky, the combination of kinematic, chemical, and distance information makes it unlikely that these stars are associated with either the Segue 1 galaxy, the Sagittarius Stream, or the Orphan Stream. Streams with halo-like abundance signatures, such as the 300 km s[superscript –1] stream, present another observational piece for understanding the accretion history of the Galactic halo.en_US
dc.description.sponsorshipSmithsonian Astrophysical Observatory (Clay Mathematics Institute)en_US
dc.language.isoen_US
dc.publisherIOP Publishingen_US
dc.relation.isversionofhttp://dx.doi.org/10.1088/0004-637X/771/1/39en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourceAmerican Astronomical Societyen_US
dc.titleTHE 300 km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STARen_US
dc.typeArticleen_US
dc.identifier.citationFrebel, Anna, Ragnhild Lunnan, Andrew R. Casey, John E. Norris, Rosemary F. G. Wyse, and Gerard Gilmore. “THE 300 Km s[superscript –1] STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR.” The Astrophysical Journal 771, no. 1 (July 1, 2013): 39. © The American Astronomical Societyen_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Physicsen_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.contributor.mitauthorFrebel, Anna L.en_US
dc.contributor.mitauthorCasey, Andrew R.en_US
dc.relation.journalThe Astrophysical Journalen_US
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsFrebel, Anna; Lunnan, Ragnhild; Casey, Andrew R.; Norris, John E.; Wyse, Rosemary F. G.; Gilmore, Gerarden_US
dc.identifier.orcidhttps://orcid.org/0000-0002-2139-7145
mit.licensePUBLISHER_POLICYen_US


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