Coudé-feed stellar spectral library – atmospheric parameters

By Yue Wu, Harinder P. Singh, P. Prugniel, Ranjan Gupta, M. Koleva. 2010

183 citations recorded by the source corpus.

Context. Empirical libraries of stellar spectra play an important role in different fields. For example, they are used as reference for the automatic determination of atmospheric parameters, or for building synthetic stellar populations to study galaxies. The CFLIB (Coude-feed library, Indo-US) database is at present one of the most complete libraries, in terms of its coverage of the atmospheric parameters space (Teff ,l ogg and [Fe/H]) and wavelength coverage 3460–9464 A at a resolution of ∼ 1A FWHM. Although the atmospheric parameters of most of the stars were determined from detailed analyses of high-resolution spectra, for nearly 300 of the 1273 stars of the library at least one of the three parameters is missing. For the others, the measurements, compiled from the literature, are inhomogeneous. Aims. In this paper, we re-determine the atmospheric parameters, directly using the CFLIB spectra, and compare them to the previous studies. Methods. We use the ULySS program to derive the atmospheric parameters, using the ELODIE library as a reference. Results. Based on comparisons with several previous studies we conclude that our determinations are unbiased. For the 958 F, G, and K type stars the precision on Teff ,l ogg ,a nd [Fe/ H] is respectively 43 K, 0.13 dex and 0.05 dex. For the 53 Ms tars they are 82 K, 0.22 dex and 0.28 dex. And for the 260 OBA type stars the relative precision on Teff is 5.1%, and on log g ,a nd [Fe/H] the precision is respectively 0.19 dex and 0.16 dex. These parameters will be used to re-calibrate the CFLIB fluxes and to produce synthetic spectra of stellar populations.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/41311b9694a95e1e1479886cbb997e7f9de2deae

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. C. Conroy
2. P. V. van Dokkum
3. M. Koleva
4. P. Prugniel
5. Simon D. M. White
6. C. Soubiran
7. Yue Wu
8. P. Hopkins

In Instrumentation

1. C. Conroy
2. P. V. van Dokkum
3. M. Koleva
4. P. Prugniel
5. Yue Wu
6. I. Vauglin
7. C. Soubiran
8. Licai Deng

Citations in the corpus

• The first data release (DR1) of the LAMOST regular survey (2015, methodology): “The LASP consecutively adopts two methods — Correlation Functio Initial (CFI) value and UlySS (Wu et al. 2011a) — to determine stellar parameters.”
• Four new observational H(z) data from luminous red galaxies in the Sloan Digital Sky Survey data release seven (2012, methodology): “This method has already been successfully tested in Wu et al. (2011).”
• Fundamental parameters and infrared excesses of Hipparcos stars (2012, background): “Wu et al. (2011) place the star at a metallicity of [Fe/H] = –1, making it reminiscent of the featureless excesses we have previously found in metal-poor globular cluster giant stars (McDonald et al. 2010a, 2011a,d).”
• Gaia FGK benchmark stars: Metallicity (2013, background): “A discussion of the impact of parameters when the exact resolution of spectra is not given can also be found in Wu et al. (2011).”
• COUNTING LOW-MASS STARS IN INTEGRATED LIGHT (2011, methodology): “We have found parameters for 35 of the stars (38% of the sample) in one or more of the MILES, ELODIE (Prugniel & Soubiran 2001), SPOCS (Valenti & Fischer 2005), and Indo-US (Valdes et al. 2004; Wu et al. 2011) libraries.”
• The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) (2012, methodology): “…the ‘redshift desert’ and eight new quasars discovered by Wu et al. (2010b), as well as eight new candidates of metal-poor stars discovered by Li et al. (2010) and another eight new candidates discovered inthe pipeline for automatic determination of stellar atmospheric parameters (Wu et al. 2011a).”
• The atmospheric parameters and spectral interpolator for the MILES stars (2011, methodology): “The last version, ELODIE 3.2 is preliminary described in Wu et al. (2011).”
• A BCool magnetic snapshot survey of solar-type stars (2013, unknown): “…0.323+0.021 −0.017 2.2+0.5 −0.5 +0.324+0.016 −0.017 1,2 - 0 - Moon G2V 5770+18 −18 4.44+X −X +0.00+0.01 −0.01 0.000+0.000 −0.000 4.32+1.68 −1.72 1.01+0.02 −0.02 1.000+0.000 −0.000 X 1.7+0.2 −0.2 +0.307+0.017 −0.013 1 References: 1: Valenti & Fischer (2005), 2: Takeda et al. (2007a), 3: Boyajian…”
• Automatic determination of stellar atmospheric parameters and construction of stellar spectral templates of the Guoshoujing Telescope (LAMOST) (2011, methodology): “Methods in Singh et al. (1998), BailerJones (2002), Hawley et al. (2002), Covey et al. (2007), and Bazarghan & Gupta (2008) may be adopted if they could provide reliable results for GSJT observations (Wu et al. 2011b in preparation).”