THE SEGUE STELLAR PARAMETER PIPELINE. I. DESCRIPTION AND COMPARISON OF INDIVIDUAL METHODS

By Y. S. Lee, Timothy C. Beers, T. Sivarani, C. Allende Prieto, L. Koesterke, R. Wilhelm, P. Fiorentin, Coryn A. L. Bailer-Jones, J. Norris, C. Rockosi and 5 more. 2007

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We describe the development and implementation of the Sloan Extension for Galactic Exploration and Understanding (SEGUE) Stellar Parameter Pipeline (SSPP). The SSPP is derived, using multiple techniques, radial velocities, and the fundamental stellar atmospheric parameters (effective temperature, surface gravity, and metallicity) for AFGK-type stars, based on medium-resolution spectroscopy and ugriz photometry obtained during the course of the original Sloan Digital Sky Survey (SDSS-I) and its Galactic extension (SDSS-II/SEGUE). The SSPP also provides spectral classification for a much wider range of stars, including stars with temperatures outside the window where atmospheric parameters can be estimated with the current approaches. This is Paper I in a series of papers on the SSPP; it provides an overview of the SSPP, and tests of its performance using several external data sets. Random and systematic errors are critically examined for the current version of the SSPP, which has been used for the sixth public data release of the SDSS (DR-6).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3bc623ceb0b570ae0bd296d8221bf46ef921b7d7

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Citations in the corpus

THE SEGUE STELLAR PARAMETER PIPELINE. V. ESTIMATION OF ALPHA-ELEMENT ABUNDANCE RATIOS FROM LOW-RESOLUTION SDSS/SEGUE STELLAR SPECTRA (2010, methodology): “These SDSS/SEGUE stellar spectra are processed through the SEGUE Stellar Parameter Pipeline (SSPP; Lee et al. 2008a, 2008b; Allende Prieto et al. 2008; Smolinski et al. 2010; Paper I, Paper II, Paper III, and Paper IV, respectively, hereafter), and the three primary stellar parameters (Teff , log…”
SDSS DR7 WHITE DWARF CATALOG (2012, background): “The Sloan Extension for Galactic Exploration and Understanding survey (SEGUE; Lee et al. 2008), part of the second-generation SDSS surveys, extended the survey’s mission to unraveling the nature and structure of our own Milky Way galaxy by targeting mostly new ﬁelds in and around the Galactic disk.”
THE SEGUE STELLAR PARAMETER PIPELINE. IV. VALIDATION WITH AN EXTENDED SAMPLE OF GALACTIC GLOBULAR AND OPEN CLUSTERS (2010, methodology): “The SEGUE Stellar Parameter Pipeline (SSPP; Lee et al. 2008a, 2008b; Allende Prieto et al. 2008) processes the wavelength- and flux-calibrated spectra generated by the standard SDSS spectroscopic reduction pipeline (Stoughton et al. 2002), obtains equivalent widths and/or line indices for 85 atomic…”
ASPCAP: THE APOGEE STELLAR PARAMETER AND CHEMICAL ABUNDANCES PIPELINE (2015, methodology): “The code is written in fortran90 and can take advantage of multi-core processors, performing optimizations for several spectra in parallel using OpenMP. ferre has been applied to a number of data sets before APOGEE (e.g., SDSS SEGUE and BOSS, as illustrated in Allende Prieto et al. 2006, 2014).26 fe”
PROBING THE OUTER GALACTIC HALO WITH RR LYRAE FROM THE CATALINA SURVEYS (2012, methodology): “In contrast to these methods, the SDSS team applied 12 separate methods for determining [Fe/H] in DR8 via the SEGUE pipeline (Lee et al. 2008, 2011).”
THE ELEVENTH AND TWELFTH DATA RELEASES OF THE SLOAN DIGITAL SKY SURVEY: FINAL DATA FROM SDSS-III (2015, methodology): “Instead, the SDSS pipeline was used with some custom modifications to provide stellar spectra suitable for processing with the SEGUE Spectroscopic Processing Pipeline (SSPP; Lee et al. 2008).”
THE SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY (2008, methodology): “See Table 5 in Lee et al. (2008a) for the naming convention for each technique.”
The first data release (DR1) of the LAMOST regular survey (2015, methodology): “To quickly get an initial guess of the effective temperature for CFI as a prior, the code uses the NGS1 grid (Lee et al. 2008).”