APOGEE Data Releases 13 and 14: Data and Analysis

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Author
Holtzman, J. cc
Hasselquist, Sten
Shetrone, Matthew
Cunha, Katia
Prieto, Carlos Allende
Anguiano, Borja
Bizyaev, Dmitry
Bovy, Jo cc
Casey, Andrew
Edvardsson, Bengt
Affiliation
Univ Arizona
Issue Date
2018-09
Keywords
methods: data analysis
stars: abundances
techniques: spectroscopic

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Publisher
IOP PUBLISHING LTD
Citation
Jon A. Holtzman et al 2018 AJ 156 125
Journal
ASTRONOMICAL JOURNAL
Rights
© 2018. 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 data and analysis methodology used for the SDSS/APOGEE Data Releases 13 and 14 are described, highlighting differences from the DR12 analysis presented in Holtzman et al. Some improvement in the handling of telluric absorption and persistence is demonstrated. The derivation and calibration of stellar parameters, chemical abundances, and respective uncertainties are described, along with the ranges over which calibration was performed. Some known issues with the public data related to the calibration of the effective temperatures (DR13), surface gravity (DR13 and DR14), and C and N abundances for dwarfs (DR13 and DR14) are highlighted. We discuss how results from a data-driven technique, The Cannon, are included in DR14 and compare those with results from the APOGEE Stellar Parameters and Chemical Abundances Pipeline. We describe how using The Cannon in a mode that restricts the abundance analysis of each element to regions of the spectrum with known features from that element leads to Cannon abundances can lead to significantly different results for some elements than when all regions of the spectrum are used to derive abundances.
ISSN
1538-3881
DOI
10.3847/1538-3881/aad4f9
Version
Final published version
Sponsors
Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; Center for High-Performance Computing at the University of Utah; Brazilian Participation Group; Carnegie Institution for Science; Carnegie Mellon University; Chilean Participation Group; French Participation Group; Harvard-Smithsonian Center for Astrophysics; Instituto de Astrofisica de Canarias; Johns Hopkins University; Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo; Lawrence Berkeley National Laboratory; Leibniz Institut fur Astrophysik Potsdam (AIP); Max-Planck-Institut fur Astronomie (MPIA Heidelberg); Max-Planck-Institut fur Astrophysik (MPA Garching); Max-Planck-Institut fur Extra-terrestrische Physik (MPE); National Astronomical Observatories of China; New Mexico State University; New York University; University of Notre Dame; Observatorio Nacional/MCTI; Ohio State University; Pennsylvania State University; Shanghai Astronomical Observatory; United Kingdom Participation Group; Universidad Nacional Autonoma de Mexico; University of Arizona; University of Colorado Boulder; University of Oxford; University of Portsmouth; University of Utah; University of Virginia; University of Washington; University of Wisconsin; Vanderbilt University; Yale University; National Science Foundation [AST-1109178]; NSF [AST-1616636, AST-1211673]; Premium Postdoctoral Research Program of the Hungarian Academy of Sciences; Hungarian NKFI Grants of the Hungarian National Research, Development and Innovation Office [K-119517]; Birgit and Hellmuth Hertz Foundation (via the Royal Physiographic Society of Lund); Crafoord Foundation; Stiftelsen Olle Engkvist Byggmastare
Additional Links
http://stacks.iop.org/1538-3881/156/i=3/a=125?key=crossref.33c7965dc53a037653cf4d202ddba46b
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