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Title:
Spectral Properties of Cool Stars: Extended Abundance Analysis of 1,617 Planet-search Stars [ Erratum: 2017ApJS..230...12B ]
Authors:
Brewer, John M.; Fischer, Debra A.; Valenti, Jeff A.; Piskunov, Nikolai
Affiliation:
AA(Department of Astronomy, Yale University and 260 Whitney Avenue, New Haven, CT 06511, USA 0000-0002-9873-1471), AB(Department of Astronomy, Yale University and 260 Whitney Avenue, New Haven, CT 06511, USA 0000-0003-2221-0861), AC(Space Telescope Science Institute and 3700 San Martin Drive, Baltimore, MD 21218, USA ), AD(Uppsala University and Department of Physics and Astronomy, Box 516, SE-75120 Uppsala, Sweden )
Publication:
The Astrophysical Journal Supplement Series, Volume 225, Issue 2, article id. 32, 36 pp. (2016). (ApJS Homepage)
Publication Date:
08/2016
Origin:
IOP
Astronomy Keywords:
catalogs, methods: data analysis, stars: abundances, stars: fundamental parameters, stars: solar type, techniques: spectroscopic
DOI:
10.3847/0067-0049/225/2/32
Bibliographic Code:
2016ApJS..225...32B

Abstract

We present a catalog of uniformly determined stellar properties and abundances for 1,617 F, G, and K stars using an automated spectral synthesis modeling procedure. All stars were observed using the HIRES spectrograph at Keck Observatory. Our procedure used a single line list to fit model spectra to observations of all stars to determine effective temperature, surface gravity, metallicity, projected rotational velocity, and the abundances of 15 elements (C, N, O, Na, Mg, Al, Si, Ca, Ti, V, Cr, Mn, Fe, Ni, and Y). Sixty percent of the sample had Hipparcos parallaxes and V-band photometry, which we combined with the spectroscopic results to obtain mass, radius, and luminosity. Additionally, we used the luminosity, effective temperature, metallicity and alpha-element enhancement to interpolate in the Yonsei-Yale isochrones to derive mass, radius, gravity, and age ranges for those stars. Finally, we determined new relations between effective temperature and macroturbulence for dwarfs and subgiants. Our analysis achieved precisions of 25 K in {T}{eff}, 0.01 dex in [M/H], 0.028 dex for {log}g, and 0.5 km s-1 in v\sin I based on multiple observations of the same stars. The abundance results were similarly precise, between ˜0.01 and ˜0.04 dex, though trends with respect to {T}{eff} remained for which we derived empirical corrections. The trends, though small, were much larger than our uncertainties and are shared with published abundances. We show that changing our model atmosphere grid accounts for most of the trend in [M/H] between 5000 and 5500 K, indicating a possible problem with the atmosphere models or opacities.

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