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dc.contributor.authorCunha, Katia
dc.contributor.authorSmith, Verne V.
dc.contributor.authorHasselquist, Sten
dc.contributor.authorSouto, Diogo
dc.contributor.authorShetrone, M.
dc.contributor.authorPrieto, Carlos Allende
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorFrinchaboy, P. M.
dc.contributor.authorGarcía-Hernández, D. Anibal
dc.contributor.authorHoltzman, J.
dc.contributor.authorJohnson, Jennifer A.
dc.contributor.authorJőnsson, Henrik
dc.contributor.authorMajewski, Steven R.
dc.contributor.authorMészáros, Szabolcs
dc.contributor.authorNidever, David L.
dc.contributor.authorPinsonneault, Marc
dc.contributor.authorSchiavon, Ricardo P.
dc.contributor.authorSobeck, Jennifer
dc.contributor.authorSkrutskie, Michael F.
dc.contributor.authorZamora, Olga
dc.contributor.authorZasowski, Gail
dc.contributor.authorFernández-Trincado, J. G.
dc.date.accessioned2017-08-22T15:55:34Z
dc.date.available2017-08-22T15:55:34Z
dc.date.issued2017-08-01
dc.identifier.citationAdding the s-Process Element Cerium to the APOGEE Survey: Identification and Characterization of Ce ii Lines in the H-band Spectral Window 2017, 844 (2):145 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aa7beb
dc.identifier.urihttp://hdl.handle.net/10150/625301
dc.description.abstractNine Ce II lines have been identified and characterized within the spectral window observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey (between lambda 1.51 and 1.69 mu m). At solar metallicities, cerium is an element that is produced predominantly as a result of the slow capture of neutrons (the s-process) during asymptotic giant branch stellar evolution. The Ce II lines were identified using a combination of a high-resolution (R = lambda/delta lambda = 100,000) Fourier Transform Spectrometer (FTS) spectrum of a Boo and an APOGEE spectrum (R. =. 22,400) of a metal-poor, but s-process enriched, red giant (2M16011638-1201525). Laboratory oscillator strengths are not available for these lines. Astrophysical gf-values were derived using alpha Boo as a standard star, with the absolute cerium abundance in alpha Boo set by using optical Ce II lines that have precise published laboratory gf-values. The near-infrared Ce II lines identified here are also analyzed, as consistency checks, in a small number of bright red giants using archival FTS spectra, as well as a small sample of APOGEE red giants, including two members of the open cluster NGC 6819, two field stars, and seven metal-poor N-and Al-rich stars. The conclusion is that this set of Ce II lines can be detected and analyzed in a large fraction of the APOGEE red giant sample and will be useful for probing chemical evolution of the s-process products in various populations of the Milky Way.
dc.description.sponsorshipNational Science Foundation [AST1109888]; Ramon y Cajal fellowship [RYC201314182]; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA201458082-P]; Premium Postdoctoral Research Program of the Hungarian Academy of Sciences; Hungarian NKFI Grants of the Hungarian National Research, Development and Innovation Office [K-119517]; National Aeronautics and Space Administration; National Science Foundation; Spanish MINECO [AYA2014-56359-P]; Birgit and Hellmuth Hertz' Foundation; Royal Physiographic Society of Lund, Sweden; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; High-Performance Computing at the University of Utahen
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/844/i=2/a=145?key=crossref.7f93d9795cec3f52b6542fe8c4746f83en
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectstars: abundancesen
dc.titleAdding the s-Process Element Cerium to the APOGEE Survey: Identification and Characterization of Ce ii Lines in the H-band Spectral Windowen
dc.typeArticleen
dc.contributor.departmentUniv Arizonaen
dc.identifier.journalThe Astrophysical Journalen
dc.description.collectioninformationThis 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.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-09-11T22:25:32Z
html.description.abstractNine Ce II lines have been identified and characterized within the spectral window observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey (between lambda 1.51 and 1.69 mu m). At solar metallicities, cerium is an element that is produced predominantly as a result of the slow capture of neutrons (the s-process) during asymptotic giant branch stellar evolution. The Ce II lines were identified using a combination of a high-resolution (R = lambda/delta lambda = 100,000) Fourier Transform Spectrometer (FTS) spectrum of a Boo and an APOGEE spectrum (R. =. 22,400) of a metal-poor, but s-process enriched, red giant (2M16011638-1201525). Laboratory oscillator strengths are not available for these lines. Astrophysical gf-values were derived using alpha Boo as a standard star, with the absolute cerium abundance in alpha Boo set by using optical Ce II lines that have precise published laboratory gf-values. The near-infrared Ce II lines identified here are also analyzed, as consistency checks, in a small number of bright red giants using archival FTS spectra, as well as a small sample of APOGEE red giants, including two members of the open cluster NGC 6819, two field stars, and seven metal-poor N-and Al-rich stars. The conclusion is that this set of Ce II lines can be detected and analyzed in a large fraction of the APOGEE red giant sample and will be useful for probing chemical evolution of the s-process products in various populations of the Milky Way.


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