SEGUE Stellar Parameter Pipeline

The SEGUE Stellar Parameter Pipeline (SSPP) implements a "multi-method" approach, using a combination of techniques to extract reliable estimates of stellar parameters from the SEGUE spectroscopic data. Details of the SSPP can be found in two recent publications:

SEGUE Stellar Spectroscopic Pipeline. I. Description and Initial Validation Tests, Y. S. Lee et al. (2007).
SEGUE Stellar Spectroscopic Pipeline. II. Validation with Galactic Globular and Open Clusters, Y. S. Lee et al. (2007).

Stellar Parameter Estimation

The SEGUE Stellar Parameter Pipeline (SSPP) makes use of multiple techniques in order to estimate the fundamental stellar atmospheric parameters:

effective temperature →T_eff
surface gravity → log g
metallicity → parameterized by [Fe/H]

for stars with spectra and ugriz photometry obtained during the course of the original Sloan Digital Sky Survey (SDSS-I) and its first extension (SDSS-II/SEGUE).

The use of multiple approaches allows for an empirical determination of the internal errors for each derived parameter, based on the range of the reported values from each method. Based on about 120,000 spectra for stars obtained during SDSS-I and SEGUE that satisfy S/N ≥ 10/1 (average value over the spectra range 3,850-6,000Å, and have derived temperatures in the range 4500K ≤ T_eff ≤ 7,500K, typical internal errors obtained by the SSPP are:

σ(T_eff) ≤ 75K
σ(log g) ≤ 0.20 dex
σ([Fe/H]) ≤ 0.10 dex

A comparison with an analysis of high-resolution spectra for over 150 SDSS-I/SEGUE stars suggests that the SSPP is able to estimate T_eff, log g, and [Fe/H] to an external uncertainty (random plus systematic errors ) of 117K, 0.26 dex, and 0.22 dex, respectively, in the temperature range 4500K ≤ T_eff ≤ 7,500K. These errors apply for the very highest S/N spectra obtained from SDSS (S/N > 50/1), as only quite bright stars were targeted for high-resolution observations. Outside of the quoted temperature range, we presently to do not have sufficient high-resolution spectra to fully test the parameters obtained by the SSPP.

An analysis of likely member stars in a handful of Galactic open and globular clusters indicates that the SSPP slightly over-estimates [Fe/H] (by on the order of 0.15 dex) for stars with [Fe/H] < -2.0, and underestimates [Fe/H] for stars with near solar metallicities by ~ 0.3 dex. Determinations of T_eff and log g exhibit no obvious offsets relative to expectations.

Despite these small remaining uncertainties, the SSPP determines stellar atmospheric parameters with sufficient accuracy and precision, in the temperature range 4500K ≤ T_eff ≤ 7,500K, to carry out detailed explorations of the chemical compositions and kinematics of the thick-disk and halo populations of the Milky Way.

See 'sppParams' Table for SSPP parameter definitions.

Line Indices

The initial step in calculation of line indices for SDSS spectra is to transform the wavelength scale of the original SDSS spectrum over to an air-based (rather than vacuum-based) wavelength scale, and to linearly rebin the spectrum to 1 Å bins in the blue (3,800-6,000 Å), and 1.5 bins in the red (6,000-9,000 Å). Then, based on the adopted radial velocity described above, the wavelength scale is shifted to zero rest wavelength.

The SSPP measures 77 atomic and molecular lines. Line index calculations are performed in two modes; one is to use a global continuum fit over the entire wavelength range (3,850-9,000 Å), the other is to obtain a local continuum around the line bands of interest. The choice between which mode is used depends on the line depth and width of the feature under consideration. Local continua are employed for the determinations of stellar atmospheric parameters based on techniques that depend on individual line indices. Other techniques, such as the neural network, spectral matching, and autocorrelation methods, require wider ranges to be considered; for these the global continuum is used. We make use of the errors in the fluxes reported by the SDSS spectroscopic reduction pipeline in order to obtain estimates in the uncertainties in the line indices.

DR6 'sppLines' Table