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    Rights statement: This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.1088/0004-637X/805/2/189

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Selecting Sagittarius: identification and chemical characterization of the Sagittarius stream

Research output: Contribution to journalJournal articlepeer-review

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  • E. A. Hyde
  • S. Keller
  • D. B. Zucker
  • R. Ibata
  • A. Siebert
  • G. F. Lewis
  • J. Penarrubia
  • M. Irwin
  • G. Gilmore
  • R. R. Lane
  • A. Koch
  • A. R. Conn
  • F. I. Diakogiannis
  • S. Martell
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Article number189
<mark>Journal publication date</mark>2/06/2015
<mark>Journal</mark>The Astrophysical Journal
Issue number2
Volume805
Number of pages13
Publication StatusPublished
<mark>Original language</mark>English

Abstract

Wrapping around the Milky Way, the Sagittarius stream is the dominant substructure in the halo. Our statistical selection method has allowed us to identify 106 highly likely members of the Sagittarius stream. Spectroscopic analysis of metallicity and kinematics of all members provides us with a new mapping of the Sagittarius stream. We find correspondence between the velocity distribution of stream stars and those computed for a triaxial model of the Milky Way dark matter halo. The Sagittarius trailing arm exhibits a metallicity gradient, ranging from −0.59 to −0.97 dex over 142°. This is consistent with the scenario of tidal disruption from a progenitor dwarf galaxy that possessed an internal metallicity gradient. We note high metallicity dispersion in the leading arm, causing a lack of detectable gradient and possibly indicating orbital phase mixing. We additionally report on a potential detection of the Sextans dwarf spheroidal in our data.

Bibliographic note

This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.1088/0004-637X/805/2/189