STELIB: A library of stellar spectra at R 2000 ?;??

By J. L. Borgne, G. Bruzual, R. Pelló, A. Lançon, B. Rocca-Volmerange, B. Sanahuja, D. Schaerer, C. Soubiran, R. Vílchez-Gómez. 2003

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We present STELIB ? , a new spectroscopic stellar library, available at http://webast.ast.obs-mip.fr/stelib. STELIB consists of an homogeneous library of 249 stellar spectra in the visible range (3200 to 9500 A), with an intermediate spectral resolution (<3 A) and sampling (1 A). This library includes stars of various spectral types and luminosity classes, spanning a relatively wide range in metallicity. The spectral resolution, wavelength and spectral type coverage of this library represents a substantial improvement over previous libraries used in population synthesis models. The overall absolute photo- metric uncertainty is 3%.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/318b46a2df0001a67ab2452b777edf1efd068705

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Citations in the corpus

Stellar population models at high spectral resolution (2011, methodology): “…stellar population models in a relatively broad wavelength range to be calculated (the Pickles library, Pickles 1998; the Jones’s library, Jones 1999; the STELIB library, Le Borgne et al. 2003; the ELODIE library Prugniel & Soubiran 2001, and the MILES library, Sanchez-Blazques et al. 2006).”
THE SEGUE STELLAR PARAMETER PIPELINE. I. DESCRIPTION AND COMPARISON OF INDIVIDUAL METHODS (2007, methodology): “Tests of the accuracy of the Hammer code with degraded (S/N ∼ 5/1) STELIB (Le Borgne et al. 2003), MILES (Sánchez-Blázquez et al. 2006), and SDSS (Hawley et al. 2002) dwarf template spectra reveal that the Hammer code assigns spectral types accurate to within ± 2 subtypes for K and M stars.”
Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers (2012, methodology): “The two models are also based on independent libraries of stellar spectra, with MaStro using the latest MILES models [77] and BC03 using STELIB [78].”
Semi‐empirical analysis of Sloan Digital Sky Survey galaxies – I. Spectral synthesis method (2005, methodology): “1, were computed with the STELIB library (Le Borgne et al. 2003), Padova-2004 models, and Chabrier (2003) IMF (see BC03 for details).”
First Results from the CHARA Array. I. An Interferometric and Spectroscopic Study of the Fast Rotator α Leonis (Regulus) (2005, methodology): “The optical spectrophotometry is an average of the observations from Alekseeva et al. (1996) and Le Borgne et al. (2003).”
On Determining Extinction from Reddening (2004, methodology): “Suitable for these tasks is STELIB, a homogeneous library of spectra constructed by Le Borgne et al. (2003) from which HILIB is completely independent.”
Stellar Populations in the Nuclei of Late-Type Spiral Galaxies (2006, methodology): “In the following only metallicities from 0.004 to 0.05 are used, as lower metallicities are not well sampled by the empirical stellar library used for predicting SEDs (STELIB, Le Borgne et al., 2003).”
Alternative diagnostic diagrams and the 'forgotten' population of weak line galaxies in the SDSS (2009, methodology): “As in previous papers in this series, the spectral fits are based on the Bruzual & Charlot (2003) models with the STELIB library (Le Borgne et al. 2003), ‘Padova 1994’ tracks (Bertelli et al. 1994) and Chabrier (2003) initial mass function.”
Fitting the integrated spectral energy distributions of galaxies (2010, background): “…Kurucz 1992; Westera et al. 2002; Smith et al. 2002; Coelho et al. 2005; Martins et al. 2005; Lançon et al. 2007) and empirical, e.g. STELIB (Le Borgne et al. 2003), MILES (SánchezBlázquez et al. 2006; Cenarro et al. 2007), Indo-US (Valdes et al. 2004), ELODIE (Prugniel and Soubiran 2001;…”
A multiwavelength view on the dusty Wolf-Rayet star WR 48a ★ (2014, methodology): “The ‘LB’ denotes that the data are from the STELIB library of stellar spectra (Le Borgne et al. 2003).”
The Origin of the Mass-Metallicity Relation: Insights from 53,000 Star-forming Galaxies in the Sloan Digital Sky Survey (2004, background): “The BC03 models incorporate an empirical spectral library (Le Borgne et al. 2003) with a wavelength coverage (3200 - 9300 Å) and spectral resolution (∼ 3 Å) which is well matched to that of the SDSS data.”
Bursty stellar populations and obscured active galactic nuclei in galaxy bulges (2007, background): “This mismatch results from spectrophotometric calibration differences between the SDSS data set and stars in the Stelib stellar spectral library (Le Borgne et al. 2003), which underpins the BC03 models.”
The star formation history of CALIFA galaxies: Radial structures (2013, methodology): “(b) Base CB is an updated version of the Bruzual & Charlot (2003) models that replaces STELIB (Le Borgne et al. 2003) with a combination of the MILES (Sánchez-Blázquez et al. 2006; Falcón-Barroso et al. 2011) and granada (Martins et al. 2005) spectral libraries.”
Age-dating luminous red galaxies observed with the Southern African Large Telescope (2016, methodology): “The SSP models that we used are based on galaxev models (Bruzual & Charlot 2003, hereafter BC03), which were generated using the stelib library (Le Borgne et al. 2003) with a resolution about 3 Å (full width at half–maximum) across the whole spectral range of 3200 – 9500 Å, the Chabrier initial…”
On the massive stellar population of the super star cluster Westerlund 1 (2005, methodology): “Data are from 1Munari & Tomasella (1999), 2Le Borgne et al. (2003), and 3Cenarro et al. (2001).”
Stellar SEDs from 0.3 to 2.5 μm: Tracing the Stellar Locus and Searching for Color Outliers in the SDSS and 2MASS (2007, methodology): “…type, we have measured these indices in 594 dwarf standards taken from the spectral libraries of Pickles (1998), Hawley et al. (2002), Valdes et al. (2004), Le Borgne et al. (2003), Sanchez-Blazquez et al. (2006), and Bochanski et al. (2007), spanning a range in spectral type from O5 to L8.”
Evolutionary stellar population synthesis at high spectral resolution: optical wavelengths (2005, methodology): “This library also presents some improvements with respect to STELIB5 (Le Borgne et al. 2003), the stellar library used by galaxev; in particular, it includes models with Teff > 25000 K, and Teff 6 4000 K and log g 6 1.0, which allow the prediction of the spectral evolution of the stellar…”
The sizes, masses and specific star formation rates of massive galaxies at 1.3 < z < 1.5: strong evidence in favour of evolution via minor mergers (2012, methodology): “The velocity dispersions were measured via χ2 minimization in pixel space, using a template library of 215 high SNR stellar spectra taken from STELIB stellar library (Le Borgne et al. 2003), as illustrated in Fig.”