Abundances for metal-poor stars with accurate parallaxes , I. Basic data

By R. Gratton, E. Carretta, R. Claudi, S. Lucatello, M. T. I. A. Padova, Italy., Dip. Astr., U. Padova, Cisas. 2003

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We present element-to-element abundance ratios measured from high dispersion spectra for 150 field subdwarfs and early subgiants with accurate Hipparcos parallaxes (errors <20%). For 50 stars new spectra were obtained with the UVES on Kueyen (VLT UT2), the McDonald 2.7 m telescope, and SARG at TNG. Additionally, literature equivalent widths were taken from the works by Nissen & Schuster, Fulbright, and Prochaska et al. to complement our data. The whole sample includes both thick disk and halo stars (and a few thin disk stars); most stars have metallicities in the range $-2<\rm [Fe/H]<-0.6$. We found our data, that of Nissen & Schuster, and that of Prochaska to be of comparable quality; results from Fulbright scatter a bit more, but they are still of very good quality and are extremely useful due to the large size of his sample. The results of the present analysis will be used in forthcoming papers to discuss the chemical properties of the dissipational collapse and accretion components of our Galaxy.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f6d0746237a743f0ffc46dbeeda8ec520adfcf90

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Citations in the corpus

Abundance Variations within Globular Clusters (2004, unknown): “…(1995) (+0.3 ≥ [Fe/H] ≥ –0.9); Feltzing & Gustafsson (1998) (+0.5 ≥ [Fe/H] ≥ –0.1); Fulbright (2000) (0.0 ≥ [Fe/H] ≥ –3.0); Reddy et al. (2003) (+0.1 ≥ [Fe/H] ≥ –0.7); Gratton et al. (2003) (+0.1 ≥ [Fe/H] ≥ –2.6); and Simmerer et al. (2003) and J.A. Simmerer, T.C. Beers, C. Sneden & B.W. Carney…”
Detailed abundances of a large sample of giant stars in M 54 and in the Sagittarius nucleus (2010, methodology): “…are typically obtained from two to three high excitation lines, while abundances of Si (partly produced in proton-capture reactions if the temperature is high enough) are estimated from several transitions (see Carretta et al. 2009b for details; and Gratton et al. 2003 for the atomic parameters).”
Population Synthesis in the Blue. IV. Accurate Model Predictions for Lick Indices and UBV Colors in Single Stellar Populations (2007, methodology): “Titanium abundances were taken from Thévenin (1998) and Gratton et al. (2003).”
Na-O anticorrelation and HB - VIII. Proton-capture elements and metallicities in 17 globular clusters from UVES spectra (2009, background): “The adopted line lists, atomic parameters, and reference solar abundances (from Gratton et al. 2003) are strictly homogeneous for all stars analysed in all clusters of the present programme.”
Galactic Chemical Evolution: Carbon through Zinc (2006, background): “A plateau of [O/Fe] ∼ 0.3− 0.45 is seen at −2 < ∼ [Fe/H] < ∼ − 1: [O/Fe] ∼ 0.45 (Carretta et al. 2000), 0.35 (Melendez & Barbuy 2002), and 0.3 with 3D correction (Nissen et al. 2002).”
On the correlation of elemental abundances with kinematics among galactic disk stars (2004, methodology): “For [Mg/H], we have carried out the comparison with Idiart & Thévenin (2000) and Gratton et al (2003) who have also used the NLTE approach.”
“Sculptor-ing” the Galaxy? The Chemical Compositions of Red Giants in the Sculptor Dwarf Spheroidal Galaxy (2004, methodology): “A large sample of Galactic field stars with detailed abundance analyses is now available (e.g., McWilliam 1997; Burris et al. 2000; Ryan et al. 1996; Carretta et al. 2002; Nissen & Schuster 1997; Fulbright 2002; Johnson 2002; Gratton et al. 2003; Stephens & Boesgaard 2002).”
CHEMODYNAMICAL SIMULATIONS OF THE MILKY WAY GALAXY (2008, unknown): “(b) In the solar neighborhood, we can reproduce the observational trend (Edvardsson et al. 1993, open circles; Bensby et al. 2004, small filled circles; Gratton et al. 2003, triangles; Cayrel et al. 2004, large filled circles).”
Na-O Anticorrelation and HB. VII. The chemical composition of first and second-generation stars in 15 globular clusters from GIRAFFE spectra (2009, background): “Adopted line lists, atomic parameters, and reference solar abundances (from Gratton et al. 2003) are strictly homogeneous for all stars analysed in the present programme.”
Distances and ages of NGC 6397, NGC 6752 and 47 Tuc (2003, methodology): “These analyses are described in Gratton et al. (2001), Carretta et al. (2003), and Gratton et al. (2003).”
Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “4.2) results in a gravity of 4.51±0.04, which is closer to the values by Gratton et al. (2003), Allende Prieto et al. (2004), Reddy et al. (2006), and Ramírez et al. (2007) from the parallax method.”
STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG (2014, background): “These differences may be the result of weak, blended Cr II lines (Neves et al. 2009), different surface gravities for the two ionization states (Reddy et al. 2003; Gratton et al. 2003), or overionization from Cr II (Feltzing & Gustafsson 1998).”
Properties of stellar generations in globular clusters and relations with global parameters (2010, methodology): “To this purpose, we collected data for field stars from three different sources: Gratton et al. (2003a); Venn et al. (2004), and Fulbright et al. (2007).”
The PASTEL catalogue of stellar parameters (2010, background): “A large dispersion is also seen in the comparison of Gratton’s and Mishenina’s datasets, which have a significant fractionof metal-poor stars in common.”