The solar neighborhood age-metallicity relation - Does it exist?

By S. Feltzing, J. Holmberg, J. Hurley. 2001

136 citations recorded by the source corpus.

We test the hypothesis that the spread in the age-metallicity plot of the solar neighborhood is due to a mixture of stars belonging to kinematically different sub-populations of the Galactic disk, i.e., the thin and the thick disk. We use a kinematic subsample of similar to 600 stars from a sample of similar to 6000 dwarf and subgiant stars from the Hipparcos catalog. All of these stars have a full set of stellar parameters determined, including good ages. We find that a significant spread in [Me/H] is present in both kinematic populations, especially at large stellar ages. This implies that a simple one-to-one relation between ages and metallicities is not possible. In fact, there are stars that are-truly old and at the same time have [Me/H] > 0.2 dex. (Less)

Subfields: Astronomy and Astrophysics, Education, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c553444725083f19784fb4de77f458b03640ab67

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Citations in the corpus

Determination of stellar ages from isochrones: Bayesian estimation versus isochrone fitting (2005, unknown): “…include Edvardsson et al. (1993), Gómez et al. (1997), Ng & Bertelli (1998), Lachaume et al. (1999), Chen et al. (2000), Liu & Chaboyer (2000), Feltzing et al. (2001), Ibukiyama & Arimoto (2002), Lastennet & Valls-Gabaud (2002), Laws et al. (2003), Reddy et al. (2003), Pont & Eyer (2004), and…”
The Gaia-ESO Survey : radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk (2014, background): “Also, Feltzing et al. (2001), and later the Geneva-Copenhagen Survey (Nordström et al. 2004; Holmberg et al. 2007, 2009; Casagrande et al. 2011), found a large scatter in metallicity at all ages, and confirmed the tentative existence of an old metal-rich population.”
STECMAP: STEllar Content from high-resolution galactic spectra via Maximum A Posteriori (2005, unknown): “The example of the Milky Way tells us that any given stellar population of a galaxy may consist of stars with non-trivial distributions in age, metallicity, or even relative abundances (Feltzing et al. 2001; Prochaska et al. 2000; Gratton et al. 2000).”
Exploring the Milky Way stellar disk - A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood (2013, methodology): “For the first observing runs, between 2000 and 2002 with FEROS and SOFIN, the stars were selected from the catalogue by Feltzing et al. (2001).”
Isochrone ages for field dwarfs: method and application to the age–metallicity relation (2004, background): “For large samples, uncertainties of approximately 0.10 dex or larger in [Fe/H] are more typical (see, for instance, Feltzing et al. 2001; Ibukiyama & Arimoto 2002), implying even wider age PDFs.”
alpha-, r-, and s-process element trends in the Galactic thin and thick disks (2004, methodology): “Note that known binaries have been excluded from the data (see Feltzing et al. 2001).”
Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, background): “Since the benchmark work by Edvardsson et al. (1993a), there have been a number of large observational surveys to obtain a true age – metallicity relationship in the solar neighborhood (Feltzing et al. 2001; Ibukiyama & Arimoto 2002; Nordström et al. 2004).”
Basic physical parameters of a selected sample of evolved stars (2006, methodology): “We refer to Carraro et al. (1998), Feltzing et al. (2001) and Nordström et al. (2004) for recent determinations of the AMR and a general discussion of its properties.”
STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG (2014, background): “Notable results obtained over the past few decades include correlations of metallicity with age and Galactocentric distance, and whether the Sun is suitably “average” (Eggen et al. 1962; Twarog 1980; Feltzing et al. 2001; Robles et al. 2008a,b).”
Stellar Abundance and Galactic Chemical Evolution through LAMOST Spectroscopic Survey (2006, background): “Earlier and recent extensive work has been concentrated on the ubvyβ photometric or/and photoelectric surveys of the nearby F and G stars (Olsen 1983, 1993, 1994; Feltzing et al. 2001; Nordstrom et al. 2004).”
Elemental abundance trends in the Galactic thin and thick disks as traced by nearby F and G dwarf stars (2003, methodology): “For all stars, in Feltzing et al. (2001), with radial velocities from Barbier-Brossat et al. (1994) and positions and proper motions from the Hipparcos catalogue we calculated Galactic velocity components, ULSR, VLSR and WLSR, relative to the local standard of rest (LSR) (see Appendix A).”
Vertical distribution of Galactic disk stars , IV. AMR and AVR from clump giants (2007, background): “There is no young star with a metallicity lower than -0.32, and no old star with a metallicity higher than -0.13, contrary to common findings in samples of dwarfs, as for instance in Feltzing et al. (2001) and Nordström et al. (2004).”
Measuring the vertical age structure of the Galactic disc using asteroseismology and SAGA (2015, background): “…been largely debated in the literature because of the intrinsic difficulty of deriving reliable ages for field stars, as well as issues with sample selection biases (e.g. McClure & Tinsley 1976; Twarog 1980; Edvardsson et al. 1993; Ng & Bertelli 1998; Rocha-Pinto et al. 2000; Feltzing et al. 2001).”
The New Galaxy: Signatures of Its Formation (2002, background): “More recently it has become clear that an AMR is apparent only in the solar neighbourhood and is strictly true only for stars younger than 2 Ga and hotter than log Teff = 3.8 (Feltzing et al. 2001).”