Abundances and Kinematics of Field Halo and Disk Stars. I. Observational Data and Abundance Analysis

By Jon P. Fulbright. 2000

385 citations recorded by the source corpus.

We describe observations and abundance analysis of a high-resolution, high signal-to-noise ratio survey of 168 stars, most of which are metal-poor dwarfs. We follow a self-consistent LTE analysis technique to determine the stellar parameters and abundances, and we estimate the effects of random and systematic uncertainties on the resulting abundances. Element-to-iron ratios are derived for key α-, odd-Z, Fe-peak, and r- and s-process elements. Effects of non-LTE on the analysis of Fe I lines are shown to be very small on average. Spectroscopically determined surface gravities are derived that are quite close to those obtained from Hipparcos parallaxes.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4e495178adc91f000dfca76252e13d4021fdbe6b

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In Astronomy and Astrophysics

1. C. Sneden
2. Timothy C. Beers
3. Martin Asplund
4. A. Helmi
5. C. Conroy
6. James S. Bullock
7. J. Cohen
8. P. Hopkins

In Instrumentation

1. A. Helmi
2. C. Sneden
3. James S. Bullock
4. E. Carretta
5. R. Gratton
6. Timothy C. Beers
7. A. Bragaglia
8. J. Cohen

Citations in the corpus

• Coudé-feed stellar spectral library – atmospheric parameters (2010, background): “For HD 224930 our temperature (5427 K) agrees with that of Soubiran et al. (2008) (5413 K) and ELODIE (5446 K), while Takeda et al. (2007) give 5681 K and Fulbright (2000) 5275 K.”
• MULTI-ELEMENT ABUNDANCE MEASUREMENTS FROM MEDIUM-RESOLUTION SPECTRA. II. CATALOG OF STARS IN MILKY WAY DWARF SATELLITE GALAXIES (2010, background): “Each of these authors selected targets from low-resolution surveys for metal-poor stars in the Galactic halo (Bond 1980; Beers et al. 1985, 1992; Norris et al. 1999, and additional references from Fulbright 2000).”
• On the correlation of elemental abundances with kinematics among galactic disk stars (2004, methodology): “To check the adopted model atmosphere parameters, we compared our values with those derived by Edvardsson et al (1993), Gratton et al (1996) Fuhrmann (1998), Chen et al (2000) and Fulbright (2000).”
• Elemental abundance trends in the Galactic thin and thick disks as traced by nearby F and G dwarf stars (2003, neutral): “For example Edvardsson et al. (1993) used ξ t = 1.15 km s−1, Feltzing & Gustafsson (1998) 1.00 km s−1, Chen et al. (2000) 1.44 km s−1, Prochaska et al. (2000) 1.00 km s−1, and Fulbright (2000) 0.80 km s−1.”
• Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, background): “…2000; Mishenina & Kovtyukh 2001; Korn et al. 2003; Gehren et al. 2006), and five others performed an equivalent width analysis of Fe I lines, with excitation equilibrium as a constraint for Teff (Fulbright 2000; Stephens & Boesgaard 2002; Heiter & Luck 2003; Luck & Heiter 2005; Takeda et al. 2005).”
• First stars VIII. Enrichment of the neutron-capture elements in the early Galaxy (2007, neutral): “…al. 1987; Gilroy et al. 1988; Gratton et al. 1988; Gratton & Sneden 1991; Edvardsson et al. 1993; Gratton & Sneden 1994; McWilliam et al. 1995; Carney et al. 1997; Nissen & Schuster 1997; McWilliam 1998; Stephens 1999; Burris et al. 2000; Fulbright 2000; Carretta et al. 2002; Johnson & Bolte 2002).”
• Abundances in Stars from the Red Giant Branch Tip to Near the Main-Sequence Turnoff in M71. III. Abundance Ratios (2001, methodology): “…the detections is 1.10 0.16 (on the scale H = 12.0 dex), which is 0.8 dex less than the mean log (Li) (1.90 0.42) for a sample of 11 halo dwarf stars of similar [Fe/H] from the sample of Fulbright (2000) and is evidence of the strong depletion among the cooler stars in which Li was detected here.”
• The chemical compositions of Galactic disc F and G dwarfs (2002, methodology): “…of [X/Fe] versus [Fe/H] (Figures 9, 10 & 11), we begin by making brief comparisons with published results, principally those from the recent extensive surveys of disc F and G dwarfs by EAGLNT, Feltzing & Gustafsson (1998), Fulbright (2000), and Chen et al. over the common interval in [Fe/H].”
• A Globular Cluster Metallicity Scale Based on the Abundance of Feii (2002, background): “…the Lick-Texas group (hereafter“LTG”; Sneden et al. 1994, Kraft et al. 1995, Shetrone 1996, Kraft et al. 1997, Sneden et al. 1997, Ivans et al. 1999, Fulbright 2000, Shetrone & Keane 2000, Ivans et al. 2001, but see Kraft 1994 for references to earlier papers in the series); Minniti et al. 1993,…”
• Stellar Abundances for the Galactic Archeology (SAGA) Database — Compilation of the Characteristics of Known Extremely Metal-Poor Stars (2008, background): “…many high-resolution spectroscopic studies that have been conducted (Gilroy et al. 1988; Ryan et al. 1991; McWilliam et al. 1995; Ryan et al. 1996; Fulbright 2000; Preston & Sneden 2000; Burris et al. 2000; Mishenina & Kovtyukh 2001; Aoki et al. 2002; Cohen et al. 2002; Carretta et al. 2002;…”
• Abundances for metal-poor stars with accurate parallaxes , I. Basic data (2003, methodology): “Eight of these stars have parallax error ∆π/π 0.2, and are considered in this paper – Fulbright (2000) recently published a very extensive analysis of the abundances of 168 field halo and disk stars.”
• Stellar Chemical Signatures and Hierarchical Galaxy Formation (2004, methodology): “…star in our sample that clearly stands out in Figure 2 is BD +80 245 (first noticed by Carney et al. 1997 from proper-motion surveys); it is the Galactic halo star with very low [ /Fe] (¼ 0:1) at ½Fe=H ¼ 2:1 (abundances from Fulbright 2000; also recently analyzed in detail by Ivans et al. 2003).”
• Near-Ultraviolet Observations of HD 221170: New Insights into the Nature of r-Process-rich Stars (2006, methodology): “In panel (c), our Keck HIRES EWs are compared with independentlymeasured McDonald 2d-coudé (Simmerer et al. 2004) and Lick Hamilton (Fulbright 2000) EWs.”
• Abundances of Baade’s Window Giants from Keck HIRES Spectra. II. The Alpha and Light Odd Elements (2006, background): “In Figure 12 we compare the [<SiCaTiI>/Fe] results from Fulbright (2000), for red giant stars identified as thick disk members by Venn et al. (2004), with results for thick disk dwarfs from Prochaska et al. (2000), Bensby et al. (2005), and Brewer & Carney (2006).”
• Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “…observational data (dots) are taken from the following sources: Cayrel et al. (2004) (large open circles); Honda et al. (2004) ( filled pentagons); Fulbright (2000) (crosses); and Reddy et al. (2003), Reddy, Lambert & Prieto (2006), and Reddy & Lambert (2008) for thin (small filled circles) and…”