Method to Estimate the Effective Temperatures of Late-Type Giants using Line-Depth Ratios in the Wavelength Range 0.97-1.32$\mu$m

Abstract

The effective temperature, one of the most fundamental atmospheric parameters of a star, can be estimated using various methods, and here we focus on the method using line-depth ratios (LDRs). This method combines low- and high-excitation lines and makes use of relations between LDRs of these line pairs and the effective temperature. It has an advantage, for example, of being minimally affected by interstellar reddening, which changes stellar colours. We report 81 relations between LDRs and the effective temperature established with high-resolution, $\lambda /\Delta \lambda \sim 28,000$, spectra of nine G- to M-type giants in Y and J bands. Our analysis gives the first comprehensive set of LDR relations for this wavelength range. The combination of all these relations can be used to determine the effective temperatures of stars that have 3700<Teff<5400K and -0.5<[Fe/H]<+0.3dex to the precision of $\pm$10K in the best cases.

9 pages, 5 figures, 6 tables, accepted for publication in MNRAS

References in corpus (1)

• The Gaia FGK Benchmark Stars - High resolution spectral library

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• Effective Temperature Estimations from Line Depth Ratios in the \H\ and \K-band Spectra of IGRINS
• Line-depth ratios as indicators of effective temperature and surface gravity
• The effect of surface gravity on line-depth ratios in the wavelength range 0.97-1.32 μm
• Red supergiant stars in IC 1613 and metallicity-dependent mixing length in the evolutionary model