THE SDSS-III APOGEE SPECTRAL LINE LIST FOR H-BAND SPECTROSCOPY

By M. Shetrone, D. Bizyaev, J. E. Lawler, C. Allende Prieto, Jennifer A. Johnson, V. Smith, K. Cunha, J. Holtzman, A. G. Pérez, Szabolcs Mészáros and 8 more. 2015

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We present the H-band spectral line lists adopted by the Apache Point Observatory Galactic Evolution Experiment (APOGEE). The APOGEE line lists comprise astrophysical, theoretical, and laboratory sources from the literature, as well as newly evaluated astrophysical oscillator strengths and damping parameters. We discuss the construction of the APOGEE line list, which is one of the critical inputs for the APOGEE Stellar Parameters and Chemical Abundances Pipeline, and present three different versions that have been used at various stages of the project. The methodology for the newly calculated astrophysical line lists is reviewed. The largest of these three line lists contains 134,457 molecular and atomic transitions. In addition to the format adopted to store the data, the line lists are available in MOOG, Synspec, and Turbospectrum formats. The limitations of the line lists along with guidance for its use on different spectral types are discussed. We also present a list of H-band spectral features that are either poorly represented or completely missing in our line list. This list is based on the average of a large number of spectral fit residuals for APOGEE observations spanning a wide range of stellar parameters.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/625c5432118f736d338058035bcdda13542a56b9

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Citations in the corpus

Target Selection for the SDSS-IV APOGEE-2 Survey (2017, background): “…survey (Holtzman et al. 2015) include the raw and reduced spectra, radial velocities (Nidever et al. 2015), fundamental stellar parameters (Garćıa Pérez et al. 2016; Mészáros et al. 2013; Zamora et al. 2015), and abundances for∼20-25 elements per star (Shetrone et al. 2015; Smith et al. 2013).”
THE STELLAR POPULATION STRUCTURE OF THE GALACTIC DISK (2015, methodology): “We find that [Fe/H]M67 = 0.10 dex and [α/Fe]M67 = 0.03 dex; the large offset in [Fe/H]M67 is at least partly due to an incorrect line list used in DR12 (see Shetrone et al. 2015).”
The age–metallicity structure of the Milky Way disc using APOGEE (2017, methodology): “…processed (Nidever et al. 2015), then fed into the APOGEE Stellar Parameters and Chemical Abundances Pipeline (ASPCAP, García Pérez et al. 2016), which makes use of a specifically computed spectral library (Zamora et al. 2015), calculated using a customised H-band line-list (Shetrone et al. 2015).”
ASPCAP: THE APOGEE STELLAR PARAMETER AND CHEMICAL ABUNDANCES PIPELINE (2015, methodology): “The APOGEE line list is based on a solar and Arcturus analysis (Shetrone et al. 2015).”
APOGEE Data and Spectral Analysis from SDSS Data Release 16: Seven Years of Observations Including First Results from APOGEE-South (2020, methodology): “Software:ASPCAP (García Pérez et al. 2016), AstroLines (Bizyaev & Shetrone 2015), FERRE (Allende Prieto et al. 2006), MARCS (Gustafsson et al. 2008), Synspec (Hubeny 1988; Hubeny & Lanz 2017), Turbospectrum (Alvarez & Plez 1998; Plez 2012).”
Chemical tagging with APOGEE: Discovery of a large population of N-rich stars in the inner Galaxy (2016, methodology): “The DR12 APOGEE abundances employed in this work are based on χ2-minimisation of the observed spectra against a large spectral library calculated on the basis of state of the art model photospheres (Mészáros et al. 2012) and a customised line list (Shetrone et al 2015).”