ABUNDANCES, STELLAR PARAMETERS, AND SPECTRA FROM THE SDSS-III/APOGEE SURVEY

By J. Holtzman, M. Shetrone, Jennifer A. Johnson, C. Allende Prieto, Friedrich Anders, B. Andrews, Timothy C. Beers, D. Bizyaev, M. Blanton, Jo Bovy and 33 more. 2015

344 citations recorded by the source corpus.

The SDSS-III/Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey operated from 2011–2014 using the APOGEE spectrograph, which collects high-resolution (R ∼ 22,500), near-IR (1.51–1.70 μm) spectra with a multiplexing (300 fiber-fed objects) capability. We describe the survey data products that are publicly available, which include catalogs with radial velocity, stellar parameters, and 15 elemental abundances for over 150,000 stars, as well as the more than 500,000 spectra from which these quantities are derived. Calibration relations for the stellar parameters ( T eff ?> , log g ?> , [M/H], [α/M]) and abundances (C, N, O, Na, Mg, Al, Si, S, K, Ca, Ti, V, Mn, Fe, Ni) are presented and discussed. The internal scatter of the abundances within clusters indicates that abundance precision is generally between 0.05 and 0.09 dex across a broad temperature range; it is smaller for some elemental abundances within more limited ranges and at high signal-to-noise ratio. We assess the accuracy of the abundances using comparison of mean cluster metallicities with literature values, APOGEE observations of the solar spectrum and of Arcturus, comparison of individual star abundances with other measurements, and consideration of the locus of derived parameters and abundances of the entire sample, and find that it is challenging to determine the absolute abundance scale; external accuracy may be good to 0.1–0.2 dex. Uncertainties may be larger at cooler temperatures ( T eff ?> < 4000 K ?> ). Access to the public data release and data products is described, and some guidance for using the data products is provided.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/311c0e87688c51e10302832ae61e6fedc626e066

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In Astronomy and Astrophysics

1. Hans-Walter Rix
2. D. Schneider
3. C. Conroy
4. P. Hopkins
5. Jo Bovy
6. L. Hernquist
7. Simon D. M. White
8. M. Blanton

In Instrumentation

1. C. Conroy
2. Hans-Walter Rix
3. M. Cappellari
4. D. Schneider
5. I. Minchev
6. M. Blanton
7. P. Hopkins
8. Jo Bovy

Citations in the corpus

• THE SDSS-III APOGEE SPECTRAL LINE LIST FOR H-BAND SPECTROSCOPY (2015, background): “We refer to Holtzman et al. (2015) for such a discussion.”
• Target Selection for the SDSS-IV APOGEE-2 Survey (2017, methodology): “During 2011–2014, APOGEE obtained high-resolution (R ∼ 22, 000), high SNR, H-band spectra for ∼163,000 stars in the bulge, disk, and halo of the MW (Zasowski et al. 2013; Holtzman et al. 2015), spanning up to ∼12 kpc away in the midplane.”
• The GALAH survey: observational overview and Gaia DR1 companion (2016, methodology): “APOGEE is also consistent with GALAH, showing a mean offset of 0.05±0.81 km s−1 (Figure 10, right panel).”
• THE STELLAR POPULATION STRUCTURE OF THE GALACTIC DISK (2015, methodology): “Abundance measurements and main subsamples We make use of the abundance measurements provided in the DR12 release of APOGEE data (Holtzman et al. 2015).”
• Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18 (2019, background): “As for Teff , also spectroscopic surface gravity A94, page 17 of 34 values suffer from some level of systematics (Holtzman et al. 2015; Valentini et al. 2016).”
• The age–metallicity structure of the Milky Way disc using APOGEE (2017, methodology): “Outputs from ASPCAP are analysed, calibrated and tabulated (Holtzman et al. 2015).”
• Asteroseismology and Gaia: Testing Scaling Relations Using 2200 Kepler Stars with TGAS Parallaxes (2017, methodology): “For giants, we adopted ASPCAP parameters from SDSS DR13 (Holtzman et al. 2015; SDSS Collaboration et al. 2016).”
• CHEMICAL TAGGING CAN WORK: IDENTIFICATION OF STELLAR PHASE-SPACE STRUCTURES PURELY BY CHEMICAL-ABUNDANCE SIMILARITY (2016, methodology): “DATA: APOGEE GIANTS WITH ABUNDANCES FROM The Cannon Our analysis draws on the spectra of 98,462 giant stars (log g < 3.9) from APOGEE DR12 (Holtzman et al. 2015), with no warning flags set in the APOGEE ASPCAP (Garćıa Pérez et al. 2015) pipeline reductions.”
• The ASAS-SN catalogue of variable stars I: The Serendipitous Survey (2018, methodology): “We used ∼ 35, 000 sources from the APOGEE (Holtzman et al. 2015) survey for this process.”
• Chemical tagging with APOGEE: Discovery of a large population of N-rich stars in the inner Galaxy (2016, methodology): “As discussed by Holtzman et al. (2015), the zero-point corrections are small and do not affect our conclusions in any important way.”
• Red giant masses and ages derived from carbon and nitrogen abundances (2015, neutral): “Stellar parameters for dwarfs have to be taken with extreme caution in DR12 because the spectral grids used to fit the observed spectra do not include rotation (see Holtzman et al. 2015).”
• CHEMICAL CARTOGRAPHY WITH APOGEE: METALLICITY DISTRIBUTION FUNCTIONS AND THE CHEMICAL STRUCTURE OF THE MILKY WAY DISK (2015, methodology): “…in Hayden et al. (2014), the DR10 paper (Ahn et al. 2014), the APOGEE reduction pipeline paper (Nidever et al. 2015), the DR12 calibration paper (Holtzman et al. 2015), the APOGEE linelist paper (Shetrone et al. 2015), the APOGEE spectral libraries paper (Zamora et al. 2015), and the APOGEE…”
• ASPCAP: THE APOGEE STELLAR PARAMETER AND CHEMICAL ABUNDANCES PIPELINE (2015, methodology): “Jobs Management and Data Organization The wrapper takes care of writing the ferre input files, submitting the ferre jobs to the execution queue, organizing the output, setting quality flags, and doing calibrations (see Holtzman et al. 2015, for more details on flags and calibration).”
• The Close Binary Fraction of Solar-type Stars Is Strongly Anticorrelated with Metallicity (2018, methodology): “After calibrating their observations to both synthetic spectra and empirical relations, APOGEE measured the stellar parameters to high precision, e.g., δTeff≈90 K, δlog g≈0.11 dex, and δ[Fe/H]≈0.15 dex (Holtzman et al. 2015).”
• The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure (2018, methodology): “Stellar parameters All the spectra are originally processed by the APOGEE Stellar Parameter and Chemical Abundances (ASPCAP, Garćıa Pérez et al. 2016) pipeline, provid- 4 ing various stellar properties, including the abundances (Holtzman et al. 2015).”
• The Fifteenth Data Release of the Sloan Digital Sky Surveys: First Release of MaNGA-derived Quantities, Data Visualization Tools, and Stellar Library (2018, methodology): “SDSS/APOGEE DR13 and DR14 Pipeline Processing and Data Description Holtzman et al. (2018) describes the data and analysis methodology used for the SDSS/APOGEE Data Releases 13 and 14 as well as highlights differences from the DR12 analysis presented in Holtzman et al. (2015).”