KOVTYUKH, V. V.; MISHENINA, T. V.; GORBANEVA, T. I.; BIENAYMÉ, O.; SOUBIRAN, C.; KANTSEN, E. L.

doi:10.1134/S1063772906020065

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KOVTYUKH, V. V.
Odessa Astronomical Observatory

MISHENINA, T. V.
Odessa Astronomical Observatory

GORBANEVA, T. I.
Odessa Astronomical Observatory

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Astronomy reports (Astronomicheskii Zhurnal). 2006, vol. 50-2, p. 134-142

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Spectral lines with high and low excitation potentials respond differently to changes of the effective temperature (T eff), making the ratio of their depths (or equivalent widths) a very sensitive temperature indicator. We derive a set of 100 equations relating T eff to the line-depth ratios, calibrated against accurate (to within 1%) published temperature determinations for giants. These relations are used to determine very accurate temperatures for a sample of 110 giants with nearly solar metallicities based on high-resolution (R = 42 000) échelle spectra with high signal-to-noise ratios (SNRs). The calibration relations are valid for temperatures of 4000–7000 K (F2III–K4III). The internal errors of each of the calibration relations are below 95 K, and applying all these relations together to spectra with SNR = 100 reduces the errors to 5–25 K (1 ?). A major advantage of this technique is that it is independent from interstellar reddening, spectroscopic resolution, and line broadening due to rotation and microturbulence.< Réduire

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Determinations of high-precision effective temperatures for giants based on spectroscopic criteria

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