Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasp..106.1248g&link_type=abstract
Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 106, no. 706, p. 1248-1257
Astronomy and Astrophysics
Astronomy
79
Calibrating, Cool Stars, Dwarf Stars, Line Spectra, Stellar Temperature, Abundance, Astronomical Photometry, Astronomical Spectroscopy, Error Analysis, Metallicity, Signal To Noise Ratios, Stellar Color
Scientific paper
The use of spectral line-depth ratios as a stellar thermometer in G and K dwarfs is developed and refined beyond an earlier study (Gray and Johanson 1991). Ratios incorporating a line with any degree of saturation, as with the wavelength 6252 V I to wavelength 6253 Fe I ratio used in the 1991 work, produce metallicity dependent results. This dependence is investigated here, and a correction derived. Ten line-depth ratios using only weak lines are shown to have negligible metallicity dependence and resolve temperature differences as small as 6 K for early K dwarfs from a single exposure having a signal-to-noise ratio of 500. Precision deteriorates badly toward G0 for these particular spectral lines. Smaller temperature differences can be resolved by combining exposures. Relative temperatures of 65 dwarfs are given, a few having errors near 1 K. Inconsistencies of approximately = 50 K between temperatures derived from color indices and from spectral lines are most likely a result of interstellar reddening affecting the photometry.
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