Models for Old, Metal-Poor Stars with Enhanced α-Element Abundances. II. Their Implications for the Ages of the Galaxy’s Globular Clusters and Field Halo Stars

By D. VandenBerg. 2000

142 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f03cc0956cae87b3ca260f290cd3eaee611c530e

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In Astronomy and Astrophysics

1. C. Conroy
2. Aaron Dotter
3. Jay Anderson
4. A. Renzini
5. G. Piotto
6. H. Baumgardt
7. L. Bedin
8. A. Milone

In Instrumentation

1. C. Conroy
2. Jay Anderson
3. Aaron Dotter
4. R. Gratton
5. G. Piotto
6. A. Renzini
7. E. Carretta
8. L. Bedin

Citations in the corpus

• THE AGES OF 55 GLOBULAR CLUSTERS AS DETERMINED USING AN IMPROVED METHOD ALONG WITH COLOR–MAGNITUDE DIAGRAM CONSTRAINTS, AND THEIR IMPLICATIONS FOR BROADER ISSUES (2013, background): “…are obtained for M 92 when its distance is similarly derived either from fits to local subdwarfs (An et al. 2009, see their Table 2) or from the luminosity of its HB stars (VandenBerg 2000, also see Benedict et al. 2011), appear to rule out a common age for 47 Tuc and the most metal-deficient GCs.”
• The Detailed Star Formation History in the Spheroid, Outer Disk, and Tidal Stream of the Andromeda Galaxy (2006, background): “…not surprising that our own Galaxy drives the textbook picture of a giant spiral galaxy, with an ancient, metal-poor halo (e.g., Ryan & Norris 1991; VandenBerg 2000), an ancient, metal-rich bulge (e.g., Zoccali 1 Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the…”
• THE ACS SURVEY OF GALACTIC GLOBULAR CLUSTERS. IX. HORIZONTAL BRANCH MORPHOLOGY AND THE SECOND PARAMETER PHENOMENON (2009, background): “Given that VandenBerg (2000) carried out his analysis using a heterogeneous collection of data in B−V and V − I, and used distances set by the level of the HB, it is encouraging that all three AMRs reveal the same basic trends.”
• Properties of stellar generations in globular clusters and relations with global parameters (2010, methodology): “When neither of these estimates was available, we adopted the ones calculated by Vandenberg (2000), normalised to the Marin-Franch scale by assuming that 13.5 Gyr = 1.00.”
• The bifurcated age–metallicity relation of Milky Way globular clusters and its implications for the accretion history of the galaxy (2013, background): “This is complicated, however, by the long-standing difficulty of determining accurate relative (let alone absolute) ages for GCs (e.g., compare the sometimes discordant results reported by Rosenberg et al. 1999, VandenBerg 2000, De Angeli et al. 2005, Maŕın-Franch et al. 2009).”
• Stellar population models of Lick indices with variable element abundance ratios (2002, background): “Ages between 9 and 14 Gyr which are derived from colormagnitude diagrams (VandenBerg 2000).”
• Flash Mixing on the White Dwarf Cooling Curve: Understanding Hot Horizontal Branch Anomalies in NGC 2808 (2001, methodology): “VandenBerg (2000) has derived a somewhat younger age of 11 Gyr for NGC 2808 from isochrone Ðtting to the optical CMD after using the theoretical ZAHB luminosity to set the distance modulus.”
• THE ACS SURVEY OF GALACTIC GLOBULAR CLUSTERS. VII. RELATIVE AGES (2008, background): “…made in GGC relative ages, improving our understanding with each technological or theoretical advance (e. g. Chaboyer, Demarque, & Sarajedini 1996; Richer et al. 1996; Stetson et al. 1996; Salaris & Weiss 1998; Buonanno et al. 1998; Rosenberg et al. 1999; VandenBerg 2000; De Angeli et al. 2005).”
• From star clusters to dwarf galaxies: the properties of dynamically hot stellar systems (2008, background): “• MWGCs contain old stellar populations (older than ≈ 10Gyr, VandenBerg 2000; Salaris & Weiss 2002).”
• Theoretical isochrones in several photometric systems I. Johnson-Cousins-Glass, HST/WFPC2, HST/NICMOS, Washington, and ESO Imaging Survey filter sets (2002, background): “Anyway, it has been demonstrated by Salaris et al. (1993; see also Salaris & Weiss 1998; and VandenBerg 2000), that for low metallicities one may safely use scaled-solar stellar models instead of α-enhanced ones of same Z.”
• Models of Metal-poor Stars with Gravitational Settling and Radiative Accelerations. II. The Age of the Oldest Stars (2001, methodology): “Those calculations are able to reproduce observed CMDs exceedingly well (see VandenBerg 2000), including that of M92 (Grundahl et al. 2000).”
• A Large Stellar Evolution Database for Population Synthesis Studies. II. Stellar Models and Isochrones for an α-enhanced Metal Distribution (2006, background): “In the last years Salaris & Weiss (1998), VandenBerg et al. (2000), VandenBerg (2000), Salasnich et al. (2000), Kim et al. (2002) have published sets of α-enhanced isochrones that cover to different degrees the age and metallicity parameter range.”
• Evolution of Stars and Stellar Populations (2005, background): “Recent results about absolute and relative age determinations of large samples of Galactic globular clusters ([170], [183], [226]) based on the methods described below provide a broadly consistent picture in which the metal-poorer clusters ([Fe/H] below ∼−1 6) are coeval (have the same age) within ∼”
• A Globular Cluster Metallicity Scale Based on the Abundance of Feii (2002, background): “Thus for an age of 13 Gyr and a hydrogen content of 0.75, M⋆ = 0.80 M⊙ (VandenBerg 2000).”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, background): “…(Gilliland et al. 2010), the color–magnitude diagrams of resolved stellar and sub-stellar populations in the Milky Way and nearby galaxies (e.g., VandenBerg 2000; Dotter et al. 2010), the integrated light of distant galaxies and star clusters via population synthesis techniques (e.g., Worthey…”
• A Comparison of Elemental Abundance Ratios in Globular Clusters, Field Stars, and Dwarf Spheroidal Galaxies (2005, methodology): “In Figure 7 we show age as a function of [Fe/H], where the ages have been determined by Vandenberg (2000) and Salaris &Weiss (2002).”