THE DATA REDUCTION PIPELINE FOR THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT

By D. Nidever, J. Holtzman, C. Allende Prieto, S. Béland, C. Bender, D. Bizyaev, A. Burton, R. Desphande, S. Fleming, A. G. García Pérez and 10 more. 2015

326 citations recorded by the source corpus.

The Apache Point Observatory Galactic Evolution Experiment (APOGEE), part of the Sloan Digital Sky Survey III, explores the stellar populations of the Milky Way using the Sloan 2.5-m telescope linked to a high resolution (R ∼ 22,500), near-infrared (1.51–1.70 μm) spectrograph with 300 optical fibers. For over 150,000 predominantly red giant branch stars that APOGEE targeted across the Galactic bulge, disks and halo, the collected high signal-to-noise ratio (>100 per half-resolution element) spectra provide accurate (∼0.1 km s−1) RVs, stellar atmospheric parameters, and precise (≲0.1 dex) chemical abundances for about 15 chemical species. Here we describe the basic APOGEE data reduction software that reduces multiple 3D raw data cubes into calibrated, well-sampled, combined 1D spectra, as implemented for the SDSS-III/APOGEE data releases (DR10, DR11 and DR12). The processing of the near-IR spectral data of APOGEE presents some challenges for reduction, including automated sky subtraction and telluric correction over a 3°-diameter field and the combination of spectrally dithered spectra. We also discuss areas for future improvement.

Subfields: Astronomy and Astrophysics, Instrumentation, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/2d2f9ac7936a6677056251c36c96b40c1643faa3

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Citations in the corpus

Target Selection for the SDSS-IV APOGEE-2 Survey (2017, background): “Data products publicly released by the 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…”
ASPCAP: THE APOGEE STELLAR PARAMETER AND CHEMICAL ABUNDANCES PIPELINE (2015, methodology): “This pipeline operates on combined visit or individualvisit spectra processed by the APOGEE data reduction pipeline (Nidever et al. 2015).”
The Close Binary Fraction of Solar-type Stars Is Strongly Anticorrelated with Metallicity (2018, background): “…spectroscopic survey (data release 13) measured the effective temperatures, surface gravities, metallicities, and RVs of ≈164,000 stars in various environments, including the galactic disk, bulge, and halo (Zasowski et al. 2013; Holtzman et al. 2015; Nidever et al. 2015; Albareti et al. 2017).”
THE SDSS-III APOGEE SPECTRAL LINE LIST FOR H-BAND SPECTROSCOPY (2015, methodology): “Stellar parameters and individual chemical abundances are derived from the combined APOGEE spectra (Nidever et al. 2015) with the APOGEE Stellar Parameters and Chemical Abundances Pipeline (ASPCAP), which is described in detail in Garćıa Pérez et al. (2015, in prep.).”
CHEMICAL CARTOGRAPHY WITH APOGEE: METALLICITY DISTRIBUTION FUNCTIONS AND THE CHEMICAL STRUCTURE OF THE MILKY WAY DISK (2015, background): “…of observing and reduction procedures is described 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…”
The age–metallicity structure of the Milky Way disc using APOGEE (2017, methodology): “The data were 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…”
The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution (2016, methodology): “Benefited from the high resolutionand high SNRs of APOGEE spectra, the random errors ofVl s delivered for APOGEE stars are at the level of∼ 0.1 km s−1 with a zeropoint uncertainty at the level of∼ 0.5 km s−1 (Nidever et al. 2015).”
Chemical tagging with APOGEE: Discovery of a large population of N-rich stars in the inner Galaxy (2016, background): “Further in-depth information on the APOGEE survey, data, and the data reduction pipeline can be found in Majewski et al. (2015), Holtzman et al. (2015), and Nidever et al. (2015), respectively.”
The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure (2018, background): “It is also a known issue that the uncertainties of various quantities (e.g. RVs) may be significantly underestimated, or that there may be a correlation in RVs for sources with Teff<3000 K (Nidever et al. 2015).”
THE STELLAR POPULATION STRUCTURE OF THE GALACTIC DISK (2015, methodology): “The data processing (Nidever et al. 2015), stellar-parameters and chemical-abundances analysis (Shetrone et al. 2015; Zamora et al. 2015; Garćıa Pérez et al. 2015, and the DR12 data analysis and calibration (Holtzman et al. 2015) are performed with automated SDSS software; we make use of standard…”
Binary Companions of Evolved Stars in APOGEE DR14: Search Method and Catalog of ∼5000 Companions (2018, methodology): “Data taken as part of the APOGEE survey are reduced with a multi-step data reduction pipeline that ultimately solves for the stellar parameters, chemical abundances, and radial velocities for each target (Nidever et al. 2015).”
Red giant masses and ages derived from carbon and nitrogen abundances (2015, unknown): “The raw spectra are ﬁrst processed by the APOGEE data reduction pipeline, as described in Nidever et al. (2015).”