Stellar Abundances in the Solar Neighborhood: The Hypatia Catalog

Hinkel, Natalie R.; Timmes, F. X.; Young, Patrick; Pagano, Michael; Turnbull, Margaret

doi:10.1088/0004-6256/148/3/54

Cited by 211 publications

(325 citation statements)

References 199 publications

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“…The last column indicates the number of lines used to derive the final abundance. (Hinkel et al 2014). A general comparison of our results (see Appendix A) and the literature is shown in Figs.…”

Section: Appendix A: Final Abundancesmentioning

confidence: 53%

GaiaFGK benchmark stars: abundances ofαand iron-peak elements

Jofré

Heiter

Soubiran

et al. 2015

A&A

134

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Context. In the current era of large spectroscopic surveys of the Milky Way, reference stars for calibrating astrophysical parameters and chemical abundances are of paramount importance. Aims. We determine elemental abundances of Mg, Si, Ca, Sc, Ti, V, Cr, Mn, Co, and Ni for our predefined set of Gaia FGK benchmark stars. Methods. By analysing high-resolution spectra with a high signal-to-noise ratio taken from several archive datasets, we combined results of eight different methods to determine abundances on a line-by-line basis. We performed a detailed homogeneous analysis of the systematic uncertainties, such as differential versus absolute abundance analysis. We also assessed errors that are due to non-local thermal equilibrium and the stellar parameters in our final abundances. Results. Our results are provided by listing final abundances and the different sources of uncertainties, as well as line-by-line and method-by-method abundances. Conclusions. The atmospheric parameters of the Gaia FGK benchmark stars are already being widely used for calibration of several pipelines that are applied to different surveys. With the added reference abundances of ten elements, this set is very suitable for calibrating the chemical abundances obtained by these pipelines.

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Section: Appendix A: Final Abundancesmentioning

confidence: 53%

GaiaFGK benchmark stars: abundances ofαand iron-peak elements

Jofré

Heiter

Soubiran

et al. 2015

A&A

134

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“…Given the sample size for metallicity determination, i.e., 694 for the Doppler sample and 12,400 for the Kepler sample, the standard error in the metallicity measurement is small. However, the systematic error in the metallicity measurement is estimated at ∼0.05 dex (Hinkel et al 2014), which is much higher than the standard error. Taking the systematic error into account, stellar metallicity may lead to a factor of 1.35 difference, but still is not adequate to explain the factor of two to three difference in the HJ occurrence rate.…”

Section: Metallicity Differencementioning

confidence: 77%

On the Occurrence Rate of Hot Jupiters in Different Stellar Environments

Fischer

Horch

et al. 2015

ApJ

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Many hot Jupiters (HJs) are detected by the Doppler and transit techniques. From surveys using these two techniques, however, the measured HJ occurrence rates differ by a factor of two or more. Using the California Planet Survey sample and the Kepler sample, we investigate the causes for this difference in the HJ occurrence rate. First, we find that 12.8% ± 0.24% of HJs are misidentified in the Kepler mission because of photometric dilution and subgiant contamination. Second, we explore the differences between the Doppler sample and the Kepler sample that can account for the different HJ occurrence rate. Third, we discuss how to measure the fundamental HJ occurrence rates by synthesizing the results from the Doppler and Kepler surveys. The fundamental HJ occurrence rates are measures of the HJ occurrence rate as a function of stellar multiplicity and evolutionary stage, e.g., the HJ occurrence rate for single and multiple stars or for main-sequence and subgiant stars. While we find qualitative evidence that HJs occur less frequently in subgiants and multiple stellar systems, we conclude that our current knowledge of stellar properties and the stellar multiplicity rate is too limited for us to reach any quantitative result for the fundamental HJ occurrence rates. This concern extends to η Earth , the occurrence rate of Earth-like planets.

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“…Taylor & Croxall 2005;Reid et al 2007;Bensby et al 2014;Hinkel et al 2014). The large majority of stars fall in the range -0. significant tails make substantial contributions to -0.9 < ∼ [Fe/H] < ∼ +0.6 dex.…”

Section: Metallicitymentioning

confidence: 99%

Fundamental parameters and infrared excesses of Tycho–Gaia stars

McDonald

Zijlstra

Watson

2017

Monthly Notices of the Royal Astronomical Society

106

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Effective temperatures and luminosities are calculated for 1 475 921 Tycho-2 and 107 145 Hipparcos stars, based on distances from Gaia Data Release 1. Parameters are derived by comparing multi-wavelength archival photometry to bt-settl model atmospheres. The 1σ uncertainties for the Tycho-2 and Hipparcos stars are ±137 K and ±125 K in temperature and ±35 per cent and ±19 per cent in luminosity. The luminosity uncertainty is dominated by that of the Gaia parallax. Evidence for infrared excess between 4.6 and 25 µm is found for 4256 stars, of which 1883 are strong candidates. These include asymptotic giant branch (AGB) stars, Cepheids, Herbig Ae/Be stars, young stellar objects, and other sources. We briefly demonstrate the capabilities of this dataset by exploring local interstellar extinction, the onset of dust production in AGB stars, the age and metallicity gradients of the solar neighbourhood and structure within the Gould Belt. We close by discussing the potential impact of future Gaia data releases.

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Stellar Abundances in the Solar Neighborhood: The Hypatia Catalog

Cited by 211 publications

References 199 publications

GaiaFGK benchmark stars: abundances ofαand iron-peak elements

GaiaFGK benchmark stars: abundances ofαand iron-peak elements

On the Occurrence Rate of Hot Jupiters in Different Stellar Environments

Fundamental parameters and infrared excesses of Tycho–Gaia stars

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