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Spectral Properties Of Cool Stars: Extended Abundance Analysis Of 1,617 Planet-Search Stars
Yale Univ, Dept Astron, New Haven, CT 06511 USA.;260 Whitney Ave, New Haven, CT 06511 USA..
Yale Univ, Dept Astron, New Haven, CT 06511 USA.;260 Whitney Ave, New Haven, CT 06511 USA..
Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.;3700 San Martin Dr, Baltimore, MD 21218 USA..
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
2016 (English)In: Astrophysical Journal Supplement Series, ISSN 0067-0049, E-ISSN 1538-4365, Vol. 225, no 2, 32Article in journal (Refereed) Published
Abstract [en]

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 similar to 0.01 and similar to 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.

Place, publisher, year, edition, pages
2016. Vol. 225, no 2, 32
Keyword [en]
catalogs, methods: data analysis, stars: abundances, stars: fundamental parameters, stars: solar type, techniques: spectroscopic
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:uu:diva-304411DOI: 10.3847/0067-0049/225/2/32ISI: 000382309500015OAI: oai:DiVA.org:uu-304411DiVA: diva2:1033147
Available from: 2016-10-05 Created: 2016-10-05 Last updated: 2016-10-05Bibliographically approved

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