Statistical cataloging of archival data for luminosity class IV–V stars

Taylor, Benjamin J.

doi:10.1051/0004-6361:20021675

Cited by 46 publications

(27 citation statements)

References 52 publications

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“…The agreement is excellent, with mean differences of only 0.02 and 0.00 dex and dispersions around the mean of 0.08 and 0.11, respectively. A further comparison with the compilation by Taylor (2003) shows a mean difference of only 0.01 dex, but a larger dispersion of 0.12 dex, as expected for a compilation from many sources of varying quality.…”

Section: Metal Abundancessupporting

confidence: 60%

“…For stars outside the limits of both calibrations, we have derived a new relation, using the same terms as Schuster & Nissen (1989) for F stars. In addition to the above new spectroscopic sources, we used Burkhart & Coupry (1991), Glaspey et al (1994) and Taylor (2003) 2 . The fit of these photometric metallicities to the spectroscopic values is shown in Fig.…”

Section: Metal Abundancesmentioning

confidence: 99%

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The Geneva-Copenhagen survey of the Solar neighbourhood

Nordström

Mayor

Andersen

et al. 2004

A&A

1,583

184

2,121

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Abstract. We present and discuss new determinations of metallicity, rotation, age, kinematics, and Galactic orbits for a complete, magnitude-limited, and kinematically unbiased sample of 16 682 nearby F and G dwarf stars. Our ∼63 000 new, accurate radial-velocity observations for nearly 13 500 stars allow identification of most of the binary stars in the sample and, together with published uvbyβ photometry, Hipparcos parallaxes, Tycho-2 proper motions, and a few earlier radial velocities, complete the kinematic information for 14 139 stars. These high-quality velocity data are supplemented by effective temperatures and metallicities newly derived from recent and/or revised calibrations. The remaining stars either lack Hipparcos data or have fast rotation. A major effort has been devoted to the determination of new isochrone ages for all stars for which this is possible. Particular attention has been given to a realistic treatment of statistical biases and error estimates, as standard techniques tend to underestimate these effects and introduce spurious features in the age distributions. Our ages agree well with those by Edvardsson et al. (1993), despite several astrophysical and computational improvements since then. We demonstrate, however, how strong observational and theoretical biases cause the distribution of the observed ages to be very different from that of the true age distribution of the sample. Among the many basic relations of the Galactic disk that can be reinvestigated from the data presented here, we revisit the metallicity distribution of the G dwarfs and the age-metallicity, age-velocity, and metallicity-velocity relations of the Solar neighbourhood. Our first results confirm the lack of metal-poor G dwarfs relative to closed-box model predictions (the "G dwarf problem"), the existence of radial metallicity gradients in the disk, the small change in mean metallicity of the thin disk since its formation and the substantial scatter in metallicity at all ages, and the continuing kinematic heating of the thin disk with an efficiency consistent with that expected for a combination of spiral arms and giant molecular clouds. Distinct features in the distribution of the V component of the space motion are extended in age and metallicity, corresponding to the effects of stochastic spiral waves rather than classical moving groups, and may complicate the identification of thick-disk stars from kinematic criteria. More advanced analyses of this rich material will require careful simulations of the selection criteria for the sample and the distribution of observational errors.Key words. Galaxy: disk -Galaxy: solar neighbourhood -Galaxy: stellar content -Galaxy: kinematics and dynamicsGalaxy: evolution -stars: fundamental parameters Send offprint requests to: B. Nordström, e-mail: birgitta@astro.ku.dkBased on observations made with the Danish 1.5-m telescope at ESO, La Silla, Chile, and with the Swiss 1-m telescope at Observatoire de Haute-Provence, France.Complete Tables 1 and 2 are only available in electro...

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Section: Metal Abundancessupporting

confidence: 60%

Section: Metal Abundancesmentioning

confidence: 99%

The Geneva-Copenhagen survey of the Solar neighbourhood

Nordström

Mayor

Andersen

et al. 2004

A&A

1,583

184

2,121

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“…Initial values for 6 Li and 7 Li in low metallicity disk stars which, as discussed before, are not observationally known, are taken from the chemical galactic model calculations by Valle et al (2002). Table 3 summarizes recent observational physical parameters for the two selected stars (Nissen et al 1999;Bensby et al 2003;Taylor 2003;Nordstrom et al 2004). The T e evaluation by different authors can vary by ±≈100 K and that absolute visual magnitudes are calculated from the observed visual ones.…”

Section: Astrophysical Implicationsmentioning

confidence: 99%

Trojan Horse estimate of bare nucleus astrophysical S(E)-factor for the $\mathsf{^{6}}$Li(p,α)$^{\mathsf{3}}$He reaction and its astrophysical implications

Pizzone

Туміно

Degl’Innocenti

et al. 2005

A&A

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Abstract.The 6 Li(p, α) 3 He bare nucleus cross-section at astrophysical energies has been indirectly measured in the framework of the Trojan-Horse Method, finding an agreement within the experimental errors with the results of data extrapolations from direct methods. This result is thus an independent check of the extrapolation method used until now. The method of measure is recalled and the results are shown with particular attention to the bare cross section value at the Gamow energy. The quoted agreement between direct and indirect methods is discussed in the context of the surface lithium abundances in stars. It is shown that the problem of stellar lithium abundances is not at the nuclear physics level but it is an astrophysics problem that requires improvements in our knowledge of the mixing mechanisms, the reduction of the uncertainties on the other (nonnuclear) physical inputs, and more precise observational data.

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“…For a sample of 42 Pop. I dwarfs with spectroscopically determined [Fe/H], log g and T eff values and BV I photometry (e.g., Clementini et al 1995;Taylor 2003), we got σ = 0.14 dex between the spectroscopic and our photometric [Fe/H]. A much more limited sample of 10 Galactic Cepheids yielded σ = 0.19 dex.…”

Section: Metallicities From Bvi Colorsmentioning

confidence: 56%

On the Cepheid Metallicity Dichotomy

Kovács

2009

EAS Publications Series

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Abstract. With the aid of stellar atmosphere models, we derive iron abundances [Fe/H] from the OGLE B, V , I photometry on the Magellanic Cloud Cepheids. We show that in both clouds the average metallicities of the first overtone variables are lower than those of the fundamental ones (by ∼ 0.2 and ∼ 0.3 dex in the LMC and SMC, respectively). Consequently, there is a correlation between the overall [Fe/H] and luminosity; the lower luminosity stars tend to be also of lower metallicity. These metallicity dependencies are concordant with the ones derived for the two types of double-mode Cepheids from pulsation theory. Yet another support of this dichotomy comes from the evolution theories that require lower metallicities for blue-looping lowluminosity stars than for high-luminosity ones. We also comment on the possibility of using period-luminosity-color relations to derive more accurate metallicities.

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Statistical cataloging of archival data for luminosity class IV–V stars

Cited by 46 publications

References 52 publications

The Geneva-Copenhagen survey of the Solar neighbourhood

The Geneva-Copenhagen survey of the Solar neighbourhood

Trojan Horse estimate of bare nucleus astrophysical S(E)-factor for the $\mathsf{^{6}}$Li(p,α)$^{\mathsf{3}}$He reaction and its astrophysical implications

On the Cepheid Metallicity Dichotomy

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