THE SEGUE STELLAR PARAMETER PIPELINE. IV. VALIDATION WITH AN EXTENDED SAMPLE OF GALACTIC GLOBULAR AND OPEN CLUSTERS

By J. Smolinski, Y. S. Lee, Timothy C. Beers, D. An, S. Bickerton, Jennifer A. Johnson, C. Loomis, C. Rockosi, T. Sivarani, Brian Yanny. 2010

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Spectroscopic and photometric data for likely member stars of five Galactic globular clusters (M3, M53, M71, M92, and NGC 5053) and three open clusters (M35, NGC 2158, and NGC 6791) are processed by the current version of the SEGUE Stellar Parameter Pipeline (SSPP), in order to determine estimates of metallicities and radial velocities (RVs) for the clusters. These results are then compared to values from the literature. We find that the mean metallicity (〈[Fe/H]〉) and mean radial velocity (〈RV〉) estimates for each cluster are almost all within 2σ of the adopted literature values; most are within 1σ. We also demonstrate that the new version of the SSPP achieves small, but noteworthy, improvements in 〈[Fe/H]〉 estimates at the extrema of the cluster metallicity range, as compared to a previous version of the pipeline software. These results provide additional confidence in the application of the SSPP for studies of the abundances and kinematics of stellar populations in the Galaxy.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8ed21c9474627af614f8b5428ca06a08cf1022db

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THE NINTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA FROM THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY (2012, methodology): “…126 high-resolution spectra of SDSS/SEGUE stars, taken with Keck, Subaru, the Hobby-Eberly Telescope and the Very Large Telescope, have been analyzed in a homogeneous fashion, and a new set of stellar parameters were obtained from this analysis (Allende Prieto et al. 2008; Smolinski et al. 2011).”
MEASURING REDDENING WITH SLOAN DIGITAL SKY SURVEY STELLAR SPECTRA AND RECALIBRATING SFD (2010, methodology): “The data release 8 version of the SSPP introduced substantial changes to metallicity estimates for stars around solar metallicity, by about 0.4 dex (Smolinski et al. 2011).”
CARBON-ENHANCED METAL-POOR STARS IN SDSS/SEGUE. I. CARBON ABUNDANCE ESTIMATION AND FREQUENCY OF CEMP STARS (2013, methodology): “Accordingly, it appears that, within±200 K, which is equivalent to the typical error of the SSPP-determinedTeff (Smolinski et al. 2011), the [C/Fe] estimate is perturbed by less than±0.25 dex, which is smaller than the rms scatter of 0.30 dex, the typical total error of our measured [C/Fe] from Tabl”
The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution (2016, methodology): “The typical external errors of the stellar atmospheric parameters yielded by SSPP are∼ 5 km s−1 in Vlos, 180 K inTeff , 0.24 dex inlog g and 0.23 dex in [Fe/H] (Smolinski et al. 2011).”
THE SPATIAL STRUCTURE OF MONO-ABUNDANCE SUB-POPULATIONS OF THE MILKY WAY DISK (2011, methodology): “All of the selected objects have valid values for their stellar atmospheric parameters as determined by the SEGUE Stellar Parameter Pipeline (Lee et al. 2008a,b; Allende Prieto et al. 2008; Lee et al. 2011a; Smolinski et al. 2011).”
THE SEGUE STELLAR PARAMETER PIPELINE. V. ESTIMATION OF ALPHA-ELEMENT ABUNDANCE RATIOS FROM LOW-RESOLUTION SDSS/SEGUE STELLAR SPECTRA (2010, methodology): “…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 g,…”
Empirical extinction coefficients for the GALEX, SDSS, 2MASS and WISE passbands (2013, background): “Typical uncertainties given by the SSPP for Teff, log g and [Fe/H] are 180 K, 0.25 dex and 0.23 dex, respectively, dominated by the systematic errors (Schlesinger et al. 2010; Smolinski et al. 2011).”
HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS FROM SDSS/SEGUE. I. ATMOSPHERIC PARAMETERS AND CHEMICAL COMPOSITIONS (2012, background): “See Lee et al. (2008a,b), Allende Prieto et al. (2008), Smolinski et al. (2011), and Lee et al. (2011) for additional discussion of the SSPP.”
THE METALLICITY DISTRIBUTION FUNCTIONS OF SEGUE G AND K DWARFS: CONSTRAINTS FOR DISK CHEMICAL EVOLUTION AND FORMATION (2011, methodology): “All literature values are from Smolinski et al. (2011) unless otherwise noted.”
THE CASE FOR THE DUAL HALO OF THE MILKY WAY (2011, background): “…SG/G: subgiant and giant, FHB: Field Horizontal-Branch, and AGB: Asymptotic Giant Branch.1 Details of the development, calibration, and validation of the SSPP can be found in Lee et al. (2008a,b), Allende Prieto et al. (2008), and Smolinski et al. (2011), to which we refer the interested reader.”
N-body modelling of globular clusters: masses, mass-to-light ratios and intermediate-mass black holes (2016, unknown): “…(2015) LOS Watkins et al. (2015a) PM NGC 6809 Carretta et al. (2009b) LOS Lane et al. (2011) LOS NGC 6838 Peterson & Latham (1986) LOS Carretta et al. (2009b) LOS Smolinski et al. (2011) LOS Kimmig et al. (2015) LOS Cordero et al. (2015) LOS Drukier, Fahlman & Richer (1992) SD NGC 7078 Peterson,…”
The GALAH survey: observational overview and Gaia DR1 companion (2016, background): “Globular and open star clusters provide important anchor points for large stellar surveys like GALAH (e.g., Smolinski et al. 2011; Anguiano et al. 2015).”
LAMOST Experiment for Galactic Understanding and Exploration (LEGUE) — The survey's science plan (2012, background): “Delicately selected “standard open clusters” (e.g., M67, see Smolinski et al. 2011) can play a role as “models” for calibrating LAMOST observations and the data-processing pipeline.”
A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters (2018, unknown): “…Marino et al. (2018) LOS NGC 7006 Saviane et al. (2012) LOS NGC 7078 de Marchi & Paresce (1995a) MF Abolfathi et al. (2017) LOS Kamann et al. (2018) LOS NGC 7089 Smolinski et al. (2011) LOS Yong et al. (2014) LOS Abolfathi et al. (2017) LOS Kamann et al. (2018) LOS NGC 7099 Piotto, Cool & King…”
FORMATION AND EVOLUTION OF THE DISK SYSTEM OF THE MILKY WAY: [α/Fe] RATIOS AND KINEMATICS OF THE SEGUE G-DWARF SAMPLE (2011, methodology): “…were determined by the most recent version of the SEGUE Stellar Parameter Pipeline (SSPP; Lee et al. 2008a, 2008b; Allende Prieto et al. 2008; Smolinski et al. 2011); typical external errors in these estimates are 180 K inTeff, 0.24 dex in logg, and 0.23 dex in [Fe/H] (Smolinski et al. 2011).”
A DIRECT DYNAMICAL MEASUREMENT OF THE MILKY WAY'S DISK SURFACE DENSITY PROFILE, DISK SCALE LENGTH, AND DARK MATTER PROFILE AT 4 kpc ≲ R ≲ 9 kpc (2013, background): “…affords velocity determinations good to ∼ 5 to 10 km s−1(Yanny et al. 2009), as well as good abundance ([α/Fe], [Fe/H]) determinations (δ[α/Fe] ∼ 0.1 dex, δ[Fe/H] ∼ 0.2 dex 5, Lee et al. 2008a,b; Allende Prieto et al. 2008; Schlesinger et al. 2010; Lee et al. 2011a; Smolinski et al. 2011;BO12c).”