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dc.contributor.authorHasselquist, Sten
dc.contributor.authorCarlin, Jeffrey L.
dc.contributor.authorHoltzman, Jon A.
dc.contributor.authorShetrone, Matthew
dc.contributor.authorHayes, Christian R.
dc.contributor.authorCunha, Katia
dc.contributor.authorSmith, Verne
dc.contributor.authorBeaton, Rachael L.
dc.contributor.authorSobeck, Jennifer
dc.contributor.authorAllende Prieto, Carlos
dc.contributor.authorMajewski, Steven R.
dc.contributor.authorAnguiano, Borja
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorGarcia-Hernandez, D. A.
dc.contributor.authorLane, Richard R.
dc.contributor.authorPan, Kaike
dc.contributor.authorNidever, David L.
dc.contributor.authorFernandez-Trincado, Jose G.
dc.contributor.authorWilson, John C.
dc.contributor.authorZamora, Olga
dc.date.accessioned2019-04-23T18:32:44Z
dc.date.available2019-04-23T18:32:44Z
dc.date.issued2019-02
dc.identifier.citationHasselquist, Sten, Jeffrey L. Carlin, Jon A. Holtzman, Matthew Shetrone, Christian R. Hayes, Katia Cunha, Verne Smith, Rachael L. Beaton, Jennifer Sobeck, Carlos Allende Prieto, Steven R. Majewski, Borja Anguiano, Dmitry Bizyaev, D. A. Garcia-Hernandez, Richard R. Lane, Kaike Pan, David L. Nidever, Jose. G. Fernandez-Trincado, John C. Wilson, and Olga Zamora. "Identifying Sagittarius Stream Stars by Their APOGEE Chemical Abundance Signatures." Astrophysical Journal 872, no. 1 (February 2019): 1-14. DOI:10.3847/1538-4357/aafdac.en_US
dc.identifier.issn1538-4357
dc.identifier.urihttps://scholarworks.montana.edu/xmlui/handle/1/15466
dc.description.abstractThe SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey provides precise chemical abundances of 18 chemical elements for similar to 176,000 red giant stars distributed over much of the Milky Way Galaxy (MW), and includes observations of the core of the Sagittarius dwarf spheroidal galaxy (Sgr). The APOGEE chemical abundance patterns of Sgr have revealed that it is chemically distinct from the MW in most chemical elements. We employ a k-means clustering algorithm to six-dimensional chemical space defined by [(C+N)/Fe], [O/Fe], [Mg/Fe], [Al/Fe], [Mn/Fe], and [Ni/Fe] to identify 62 MW stars in the APOGEE sample that have Sgr-like chemical abundances. Of the 62 stars, 35 have Gaia kinematics and positions consistent with those predicted by N-body simulations of the Sgr stream, and are likely stars that have been stripped from Sgr during the last two pericenter passages (<2 Gyr ago). Another 20 of the 62 stars exhibit chemical abundances indistinguishable from the Sgr stream stars, but are on highly eccentric orbits with median r(apo) similar to 25 kpc. These stars are likely the "accreted" halo population thought to be the result of a separate merger with the MW 8-11 Gyr ago. We also find one hypervelocity star candidate. We conclude that Sgr was enriched to [Fe/H] similar to -0.2 before its most recent pericenter passage. If the "accreted halo" population is from one major accretion event, then this progenitor galaxy was enriched to at least [Fe/H] similar to -0.6, and had a similar star formation history to Sgr before merging.en_US
dc.description.sponsorshipAlfred P. Sloan Foundation; U.S. Department of Energy Office of Scienceen_US
dc.language.isoenen_US
dc.rightsThis Item is protected by copyright and/or related rights. You are free to use this Item in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you need to obtain permission from the rights-holder(s).en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en_US
dc.titleIdentifying Sagittarius Stream Stars by Their APOGEE Chemical Abundance Signaturesen_US
dc.typeArticleen_US
mus.citation.extentfirstpage1en_US
mus.citation.extentlastpage14en_US
mus.citation.issue1en_US
mus.citation.journaltitleAstrophysical Journalen_US
mus.identifier.categoryPhysics & Mathematicsen_US
mus.identifier.doi10.3847/1538-4357/aafdacen_US
mus.relation.collegeCollege of Letters & Scienceen_US
mus.relation.departmentPhysics.en_US
mus.relation.universityMontana State University - Bozemanen_US
mus.data.thumbpage7en_US


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