ASPCAP: THE APOGEE STELLAR PARAMETER AND CHEMICAL ABUNDANCES PIPELINE

By A. G. García Pérez, C. Allende Prieto, J. Holtzman, M. Shetrone, S. M'esz'aros, D. Bizyaev, R. Carrera, K. Cunha, D. A. Garc'ia-Hern'andez, Jennifer A. Johnson and 20 more. 2015

529 citations recorded by the source corpus.

The Apache Point Observatory Galactic Evolution Experiment (APOGEE) has built the largest moderately high-resolution (R ≈ 22,500) spectroscopic map of the stars across the Milky Way, and including dust-obscured areas. The APOGEE Stellar Parameter and Chemical Abundances Pipeline (ASPCAP) is the software developed for the automated analysis of these spectra. ASPCAP determines atmospheric parameters and chemical abundances from observed spectra by comparing observed spectra to libraries of theoretical spectra, using χ2 minimization in a multidimensional parameter space. The package consists of a fortran90 code that does the actual minimization and a wrapper IDL code for book-keeping and data handling. This paper explains in detail the ASPCAP components and functionality, and presents results from a number of tests designed to check its performance. ASPCAP provides stellar effective temperatures, surface gravities, and metallicities precise to 2%, 0.1 dex, and 0.05 dex, respectively, for most APOGEE stars, which are predominantly giants. It also provides abundances for up to 15 chemical elements with various levels of precision, typically under 0.1 dex. The final data release (DR12) of the Sloan Digital Sky Survey III contains an APOGEE database of more than 150,000 stars. ASPCAP development continues in the SDSS-IV APOGEE-2 survey.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4eccb953de90d311940365650a311eb99b4be7c1

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Citations in the corpus

Binary Companions of Evolved Stars in APOGEE DR14: Search Method and Catalog of ∼5000 Companions (2018, methodology): “The stellar parameters— surface gravity, glog , and effective temperature, Teff—and the chemical abundances are determined from the coadded spectrum as a part of the APOGEE Stellar Parameters and Chemical Abundances Pipeline (ASPCAP; García Pérez et al. 2016).”
Target Selection for the SDSS-IV APOGEE-2 Survey (2017, methodology): “REFERENCES Abolfathi, B., Aguado, D. S., Aguilar, G., et al. 2017, ArXiv e-prints Adibekyan, V. Z., Sousa, S. G., Santos, N. C., et al. 2012, A&A, 545, A32 Anders, F., Chiappini, C., Rodrigues, T. S., et al. 2017, A&A, 597, A30 Baglin, A., Auvergne, M., Boisnard, L., et al. 2006, in 36th COSPAR Scie”
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).”
A RADIAL AGE GRADIENT IN THE GEOMETRICALLY THICK DISK OF THE MILKY WAY (2016, methodology): “The spectra are treated by the APOGEE Stellar Parameter and Chemical Abundances Pipeline (García Pérez et al. 2015), providing stellar parameters (Teff , glog , [M/H], [α/M], [C/M], and [N/M]), as well as 15 element abundances for over 150,000 stars.”
CHEMICAL TAGGING CAN WORK: IDENTIFICATION OF STELLAR PHASE-SPACE STRUCTURES PURELY BY CHEMICAL-ABUNDANCE SIMILARITY (2016, methodology): “…not limited to (a) improvements in the determination of pseudo-continuum, (b) the use of more spectral range than just unblended element windows (Garćıa Pérez et al. 2015), and (c) accurate spectral predictions (The Cannon delivers accurate predictions because it is fit to observed data).”
The GALAH survey: observational overview and Gaia DR1 companion (2016, background): “APOGEE spectra have a resolution of R ∼22,000; the most recent data release3 includes abundances for up to 21 elements per star (Garćıa Pérez et al. 2016).”
The biggest splash (2019, background): “In particular, spectroscopic information from the APOGEE (Majewski et al. 2017; Garcı́a Pérez et al. 2016) DR14 (Abolfathi et al. 2018), LAMOST DR3 (Large Sky Area MultiObject Fibre Spectroscopic Telescope, Cui et al. 2012; Zhao et al. 2012), RAVE (Steinmetz et al. 2006) DR5 (Kunder et al. 2017),…”