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    A Diffuse Metal-poor Component of the Sagittarius Stream Revealed by the H3 Survey

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    Johnson_2020_ApJ_900_103.pdf
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    Author
    Johnson, Benjamin D. cc
    Conroy, Charlie
    Naidu, Rohan P.
    Bonaca, Ana
    Zaritsky, Dennis
    Ting, Yuan-Sen
    Cargile, Phillip A.
    Han, Jiwon Jesse
    Speagle, Joshua S.
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2020-09
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Johnson, B. D., Conroy, C., Naidu, R. P., Bonaca, A., Zaritsky, D., Ting, Y. S., ... & Speagle, J. S. (2020). A Diffuse Metal-Poor Component of the Sagittarius Stream Revealed by the H3 Survey. The Astrophysical Journal, 900(2), 103.
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    © 2020. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    The tidal disruption of the Sagittarius dwarf galaxy has generated a spectacular stream of stars wrapping around the entire Galaxy. We use data from Gaia and the H3 Stellar Spectroscopic Survey to identify 823 high-quality Sagittarius members based on their angular momenta. The H3 Survey is largely unbiased in metallicity, and so our sample of Sagittarius members is similarly unbiased. Stream stars span a wide range in [Fe/H] from -0.2 to -3.0, with a mean overall metallicity of <[F/H]> = -0.99. We identify a strong metallicity dependence to the kinematics of the stream members. At [Fe/H] > -0.8 nearly all members belong to the well-known cold (sigma(v) < 20 km s(-1)) leading and trailing arms. At intermediate metallicities (-1.9 < [Fe/H] < -0.8) a significant population (24%) emerges of stars that are kinematically offset from the cold arms. These stars also appear to have hotter kinematics. At the lowest metallicities ([Fe/H] less than or similar to -2), the majority of stars (69%) belong to this kinematically offset diffuse population. Comparison to simulations suggests that the diffuse component was stripped from the Sagittarius progenitor at earlier epochs, and therefore resided at larger radius on average than the colder metal-rich component. We speculate that this kinematically diffuse, low-metallicity population is the stellar halo of the Sagittarius progenitor system.
    Note
    Immediate access
    ISSN
    0004-637X
    EISSN
    1538-4357
    DOI
    10.3847/1538-4357/abab08
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/abab08
    Scopus Count
    Collections
    UA Faculty Publications

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