Nearby stars of the Galactic disc and halo – IV

By K. Fuhrmann. 2008

187 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2e34d8bca2715b7994881a9e63f1a26d63e929d2

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Accurate fundamental parameters for 23 bright solar-type stars (2010, background): “Each column is identified by the first author, i.e. Fuhrmann (1998, 2004, 2008), Sousa et al. (2008), Soubiran et al. (1998), Santos et al. (2004, 2005), and Valenti & Fischer (2005).”
The Gaia-ESO Survey : radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk (2014, background): “…al. 2012b,c; Schlesinger et al. 2012; Cheng et al. 2012), RAVE (e.g. Boeche et al. 2013), and APOGEE (e.g. Anders et al. 2013; Hayden et al. 2013), as well as smaller samples of stars with high-resolution observations (e.g. Bensby et al. 2003; Fuhrmann 2008; Ruchti et al. 2011; Bensby et al. 2014).”
Through thick and thin: kinematic and chemical components in the solar neighbourhood (2010, background): “…older and more highly enriched in α elements than their thin disk counterparts supports the twocomponent nature of the Galactic disk (Gratton et al. 1996; Fuhrmann 1998; Prochaska et al. 2000; Bensby et al. 2003; Gilmore & Wyse 1985; Reddy et al. 2006; Bensby et al. 2007; Fuhrmann 2008).”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, background): “Recent claims of a more massive thick disk may arise from the survey selection extending into the low [α/Fe] population (e.g., Snaith et al. 2014) or from the use of a tiny survey volume (e.g., Fuhrmann 2008).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, result): “While some studies (e.g., Edvardsson et al. 1993; Favata et al. 1997; Fuhrmann 2008) rely on kinematically unbi- ased samples, many investigations (e.g., Feltzing & Gustafsson 1998; Bensby et al. 2003; Reddy et al. 2006; Bensby et al. 2007; Ramı́rez et al. 2007; Soubiran et al. 2008) make use of…”
The Milky Way’s stellar disk (2013, background): “In many existing Galactic survey analyses emphasis has been given—in the initial survey design, the targeting choices and the subsequent sample culling—to getting as simple a selection function as possible, e.g.Kuijken & Gilmore (1989a); Nordström et al. (2004); Fuhrmann (2011); Moni Bidin et al. (”
OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, background): “In fact, the work by Fuhrmann (2008), who uses the magnesium abundance as indicator of α-element enhancement, has already hinted at the importance of “transition” objects in the Galactic disk (see also Fuhrmann 1998, 2004).”
Thin disc, thick disc and halo in a simulated galaxy (2012, methodology): “…together (separated by ∼0.01– 0.05 dex in [O/Fe]) than the Milky Way tracks (separated by ∼0.2 dex in [O/Fe]; Bensby et al. 2005; Reddy et al. 2006; Fuhrmann 2008), which has been interpreted by chemical evolution models as indicating that the Milky Way experienced a hiatus in star formation…”
Chemodynamics of the Milky Way - I. The first year of APOGEE data (2013, background): “…surveys of the Galactic disc have been limited to very small Galactic volumes – 25 pc in the case of Fuhrmann’s Solar neighbourhood survey (Fuhrmann 1998, 2002, 2004, 2008, 2011), ∼ 100 pc in the case of Bensby et al. (2003) and Adibekyan et al. (2011), a small number of pen- 12 The…”
Spectroscopic stellar parameters for 582 FGK stars in the HARPS volume-limited sample. Revising the metallicity-planet correlation (2011, result): “This distribution is very similar to the ones presented in studies dealing specifically with the metallicity distribution in the solar neighborhood which are based on unbiased, volume-limited samples (e.g. Haywood, 2001; Fuhrmann, 2004, 2008; Casagrande et al., 2011).”
THICK DISKS OF EDGE-ON GALAXIES SEEN THROUGH THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G): LAIR OF MISSING BARYONS? (2011, background): “On the other hand, one other Milky Way study, by Fuhrmann (2008), considers the mass of the Milky Way’s thick disk to be comparable with that of the thin disk, which would make it a “typical” galaxy in our sample.”
THE METALLICITY DISTRIBUTION FUNCTIONS OF SEGUE G AND K DWARFS: CONSTRAINTS FOR DISK CHEMICAL EVOLUTION AND FORMATION (2011, background): “…spectroscopic analyses of these low-luminosity targets were limited to hundreds of stars along individual lines of sight (Wyse & Gilmore 1995; Favata et al. 1997; Fuhrmann 1998, 2004, 2008, 2011; Allende Prieto et al. 2004; Luck & Heiter 2005, 2006, 2007; Arnadottir et al. 2009; Katz et al. 2011).”
Exploring the Milky Way stellar disk - A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood (2013, background): “Fuhrmann (1998, 2000, 2004, 2008, 2011) showed that stars very close to the Sun trace two distinct abundance trends.”
The metallicity distribution of bulge clump giants in Baade’s window (2011, methodology): “14, we plotted the thin and thick A80, page 14 of 20 disc stars abundances from the studies of Bensby et al. (2005); Reddy et al. (2006) and Fuhrmann (2008).”
FORMATION AND EVOLUTION OF THE DISK SYSTEM OF THE MILKY WAY: [α/Fe] RATIOS AND KINEMATICS OF THE SEGUE G-DWARF SAMPLE (2011, methodology): “…Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, 20921-400 Rio de Janeiro, Brazil et al. 2006), possess higher [α/Fe] ratios12, and are older and more metal-poor than typical thin-disk stars (Bensby et al. 2003, 2005; Reddy et al. 2006, 2010; Fuhrmann 2008; Haywood 2008).”
The chemical composition of the Sun (2009, background): “…be borne in mind that most large-scale abundance analyses of Galactic thin disk stars to date (e.g. Bensby et al. 2005, Edvardsson et al. 1993, Fuhrmann 2008, Ramı́rez, Allende Prieto & Lambert 2007, Reddy et al. 2003) have been performed differentially relative to the Sun to remove the…”
A FIRST CONSTRAINT ON THE THICK DISK SCALE LENGTH: DIFFERENTIAL RADIAL ABUNDANCES IN K GIANTS AT GALACTOCENTRIC RADII 4, 8, AND 12 kpc (2011, background): “…(e.g., Gilmore et al. 1995; Wyse & Gilmore 1995); the thick disk is older than the thin disk (e.g., Fuhrmann 2008; Bensby et al. 2007); and the thick disk is α-enhanced, at a given metallicity, with respect to the thin disk (e.g., Fuhrmann 2008; Bensby et al. 2003, 2004, 2005; Reddy et al. 2006).”