Adding the s-Process Element Cerium to the APOGEE Survey: Identification and Characterization of Ce ii Lines in the H-band Spectral Window

Nine Ce ii lines have been identified and characterized within the spectral window observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey (between λ1.51 and 1.69 m). At solar metallicities, cerium is an element that is produced predominantly as a result of the slow ca...

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Bibliographic Details
Published in:	The Astrophysical journal 2017-08, Vol.844 (2), p.145
Main Authors:	Cunha, Katia, Smith, Verne V., Hasselquist, Sten, Souto, Diogo, Shetrone, Matthew D., Allende Prieto, Carlos, Bizyaev, Dmitry, Frinchaboy, Peter, García-Hernández, D. Anibal, Holtzman, Jon, Johnson, Jennifer A., J nsson, Henrik, Majewski, Steven R., Mészáros, Szabolcs, Nidever, David, Pinsonneault, Mark, Schiavon, Ricardo P., Sobeck, Jennifer, Skrutskie, Michael F., Zamora, Olga, Zasowski, Gail, Fernández-Trincado, J. G.
Format:	Article
Language:	eng
Subjects:	ABUNDANCE ASTROPHYSICS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY CERIUM FOURIER TRANSFORM SPECTROMETERS GALACTIC EVOLUTION METALLICITY MILKY WAY NEUTRONS S PROCESS SPECTRA STARS stars: abundances
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Summary:	Nine Ce ii lines have been identified and characterized within the spectral window observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey (between λ1.51 and 1.69 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 ( ) Fourier Transform Spectrometer (FTS) spectrum of 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 Boo as a standard star, with the absolute cerium abundance in 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.
ISSN:	0004-637X 1538-4357 1538-4357