Stellar Abundances for the Galactic Archeology (SAGA) Database — Compilation of the Characteristics of Known Extremely Metal-Poor Stars

By T. Suda, Y. Katsuta, S. Yamada, T. Suwa, C. Ishizuka, Y. Komiya, K. Sorai, M. Aikawa, Masayuki Y. Fujimoto Hokkaido Univ., T. Univ and 1 more. 2008

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We describe the construction of a database of extremely metal-poor (EMP) stars in the Galaxy. Our database contains detailed elemental abundances, reported equivalent widths, atmospheric parameters, photometry, and binarity status, compiled from papers in the literature that report on studies of EMP halo stars with [Fe=H] �� 2.5. The compilation procedures for this database were designed to assemble data effectively from electronic tables available from online journals. We have also developed ad ata retrieval system that enables data searches by various criteria and illustrations to explore relationships between stored variables. Currently, our sample includes 1212 unique stars (many of which are studied by more than one group) with more than 15000 individual reported elemental abundances, covering relevant papers published by 2007 December. We discuss the global characteristics of the present database, as revealed by the EMP stars observed to date. For stars with [Fe=H] �� 2.5, the number of giants with reported abundances is larger than that of dwarfs by a factor of two. The fraction of carbon-rich stars (among the sample for which the carbon abundance is reported) amounts to � 30% for [Fe=H] �� 2.5. We find that known binaries exhibit different distributions of the orbital period, according to whether they are giants or dwarfs, and also as a function of the metallicity, although the total sample of such stars is still quite small.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8570b3a15d4b844e4360a431912404d781da7cab

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Citations in the corpus

CARBON-ENHANCED METAL-POOR STAR FREQUENCIES IN THE GALAXY: CORRECTIONS FOR THE EFFECT OF EVOLUTIONARY STATUS ON CARBON ABUNDANCES (2014, methodology): “Our sample is based on the most recent version of the SAGA database (Suda et al. 2008) and the compilation of literature data by Frebel et al. (2010).”
Wind Roche-lobe overflow: Application to carbon-enhanced metal-poor stars (2013, methodology): “To compare our models with observations we use a database of VMP stars based on the SAGA observational database compiled by Suda et al. (2008, 2011), combined with data of metal-poor stars from Frebel et al. (2006) and from Lucatello et al. (2006).”
THE s-PROCESS IN ASYMPTOTIC GIANT BRANCH STARS OF LOW METALLICITY AND THE COMPOSITION OF CARBON-ENHANCED METAL-POOR STARS (2011, methodology): “3For data on the ls elements we searched the SAGA database (Suda et al. 2008).”
The s process: Nuclear physics, stellar models, and observations (2010, result): “…has been found by many authors despite the different physics adopted in the various works (Campbell and Lattanzio, 2008; Cristallo et al., 2007; Fujimoto et al., 2000; Hollowell et al., 1990; Iwamoto et al., 2004; Lau et al., 2009; Straniero et al., 2004; Suda et al., 2008; Woodward et al., 2008).”
The most metal-poor damped Lyα systems: insights into chemical evolution in the very metal-poor regime★ (2011, background): “The recent interest in the most metal-poor DLAs (Pettini et al. 2008; Penprase et al. 2010) complements the ongoing local studies of metal-poor stars in the halo of the Milky Way (Cayrel et al. 2004; Beers & Christlieb 2005; Suda et al. 2008; Frebel 2010).”
THE MOST METAL-POOR STARS. II. CHEMICAL ABUNDANCES OF 190 METAL-POOR STARS INCLUDING 10 NEW STARS WITH [Fe/H] ⩽ −3.5,, (2012, methodology): “As the numbers of metal-poor stars with detailed chemical abundance measurements have grown, databases have been compiled (Suda et al. 2008, 2011; Frebel 2010) which facilitate studies of the global characteristics of metal-poor sta s (see also Roederer 2009, who assembled and studied a compilation…”
The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014, background): “…data and include barium and CH-type stars, carbon enhanced metal-poor (CEMP) stars, dwarf C stars, and some planetary nebulae (Luck & Bond 1991; Allen & Barbuy 2006a,b; Allen & Porto de Mello 2007; Suda et al. 2008, 2011; Masseron et al. 2010; Pereira et al. 2012; Miszalski et al. 2013).”
Evolution and nucleosynthesis of extremely metal-poor and metal-free low- and intermediate-mass stars - I. Stellar yield tables and the CEMPs (2008, background): “…C- and N-rich – although they generally have lower N abundances than C, they are also strongly enriched in N. Thenewly constructed ‘Stellar Abundances for Galactic Archeology’ (SAGA) Internet database of Suda et al. (2008), which contains more observational data, also shows these features.”
The PASTEL catalogue: 2016 version (2016, background): “…stars (Adibekyan et al. 2012); – homogeneous abundances from the literature for 743 stars (Soubiran & Girard 2005); – detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood (Bensby et al. 2014); – the SAGA database of extremely metal-poor stars (Suda et al. 2008).”
Galactic r-process enrichment by neutron star mergers in cosmological simulations of a Milky Way-mass galaxy (2014, background): “1 also shows observational data points for [Eu/Fe], where plusses show detections and downward arrows show upper limits (Suda et al. 2008).2 Eu is an ideal tracer of r-process enrichment, because it is almost solely produced in r-process events (Burris et al. 2000).”
HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS FROM SDSS/SEGUE. I. ATMOSPHERIC PARAMETERS AND CHEMICAL COMPOSITIONS (2012, methodology): “The results are compared with those obtained by previous studies, also taken from the SAGA database (Suda et al. 2008), which are shown by open circles (carbon-normal stars) and asterisks (carbon-enhanced stars).”