Cool Star Oxygen Abundances from Spectral Synthesis of TiO Bands

We have used spectral synthesis of the γ R 2 R 2 0–0 TiO band at 7054 Å to determine oxygen abundances in dwarfs previously analyzed for iron and titanium abundances from their atomic lines. With the abundances of Fe and Ti held fixed, the band profiles are sensitive to the oxygen abundances. For th...

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Bibliographic Details
Published in:Publications of the Astronomical Society of the Pacific 2009-10, Vol.121 (884), p.1083-1089
Main Authors: Schmidt, Sarah J., Wallerstein, George, Woolf, Vincent M., Bean, Jacob L.
Format: Article
Language:English
Subjects:
Astronomy
Cool stars
Data lines
Earth, ocean, space
Exact sciences and technology
M dwarfs
Metal abundance
Molecular spectra
Oxygen
Spectral bands
Stars
Stellar properties
Stellar spectra
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Summary:We have used spectral synthesis of the γ R 2 R 2 0–0 TiO band at 7054 Å to determine oxygen abundances in dwarfs previously analyzed for iron and titanium abundances from their atomic lines. With the abundances of Fe and Ti held fixed, the band profiles are sensitive to the oxygen abundances. For the late K and M dwarfs analyzed, the [O/Fe] trend agrees with previous work for higher mass stars from[Fe/H] = +0.1 [ Fe / H ] = + 0.1 to[Fe/H] = -1.5 [ Fe / H ] = - 1.5 . Beyond[Fe/H] = -1.5 [ Fe / H ] = - 1.5 , the TiO band becomes too weak to analyze except in cooler stars for which Ti abundances are difficult to determine because their TiIlines are frequently blended. We find that the abundance trend derived for our stars matches those derived for solar neighborhood stars by other methods.
ISSN:0004-6280
1538-3873
DOI:10.1086/644605