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Determining the effective temperatures (T eff) of red supergiants (RSGs) observationally is important in many fields of stellar physics and galactic astronomy, yet some significant difficulties remain as a result of the model uncertainty, which originates mainly in the extended atmospheres of RSGs. Here we propose a line-depth ratio (LDR) method in which we use only Fe  i lines. As opposed to the conventional LDR method, in which lines of multiple species are involved, this LDR method is insensitive to surface gravity effects and is expected to circumvent the uncertainty originating in the upper atmosphere of RSGs. Therefore, the LDR– T eff relationships that we calibrated empirically with red giants can be directly applied to RSGs, although various differences between the two groups of objects, for example caused by 3D non-local thermodynamic equilibrium (non-LTE) effects, need to be kept in mind. Using the near-infrared YJ -band spectra of nine well-known solar-metallicity red giants observed with the WINERED high-resolution spectrograph, we selected 12 pairs of Fe  i lines that were the least contaminated with other lines. After applying their LDR– T eff relation to 10 nearby RSGs, the resulting T eff with an internal precision of |$30\!-\!70\, \mathrm{K}$| shows good agreement with previous observational results assuming 1D LTE and with the Geneva stellar evolution model. We found no evidence of significant systematic bias caused by various differences, including those in the size of the non-LTE effects, between red giants and RSGs, except for one line pair that we rejected because the non-LTE effects may be as large as |$\sim \! 250\, \mathrm{K}$|⁠. Nevertheless, it is difficult to evaluate the systematic bias, and further study is required, for example including the 3D non-LTE calculations of all the lines involved. [ABSTRACT FROM AUTHOR]

A line-depth ratio (LDR) of two spectral lines with different excitation potentials is expected to be correlated with the effective temperature (T eff). It is possible to determine T eff of a star with a precision of tens of Kelvin if dozens or hundreds of tight LDR– T eff relations can be used. Most of the previous studies on the LDR method were limited to optical wavelengths, but Taniguchi and collaborators reported 81 LDR relations in the YJ band, 0.97–1.32 µm, in 2018. However, with their sample of only 10 giants, it was impossible to account for the effects of surface gravity and metallicity on the LDRs well. Here, we investigate the gravity effect based on YJ -band spectra of 63 stars including dwarfs, giants, and supergiants observed with the WINERED spectrograph. We found that some LDR– T eff relations show clear offsets between the sequence of dwarfs and those of giants/supergiants. The difference between the ionization potentials of the elements considered in each line pair and the corresponding difference in the depths can, at least partly, explain the dependency of the LDR on the surface gravity. In order to expand the stellar parameter ranges that the LDR method can cover with high precision, we obtained new sets of LDR– T eff relations for solar-metal G0–K4 dwarfs and F7–K5 supergiants, respectively. The typical precision that can be achieved with our relations is 10–30 K for both dwarfs and supergiants. [ABSTRACT FROM AUTHOR]

Ratios of carefully selected line depths are sensitive to the stellar effective temperature (T eff). Relations established between the line-depth ratio (LDR) and T eff allow T eff to be determined precisely. LDRs can also, however, depend on metallicity and abundance ratios, which can limit the accuracy of the LDR method unless such effects are properly taken into account. We investigate the metallicity effect using H -band spectra and stellar parameters published by the APO Galactic Evolution Experiment (APOGEE) project. We clearly detect the effects of metallicity and abundance ratios: T eff derived from a given LDR depends on the metallicity, 100–800 K dex−1, and a dependence on the abundance ratios, 150–1000 K dex−1, also exists when the LDR involves absorption lines of different elements. For the 11 line pairs in the H - band that we investigated, the LDR– T eff relations with metallicity- and abundance-dependent terms added have scatters as small as 30–90 K within the range of 3700 < T eff < 5000 K and −0.7 < [Fe/H] < +0.4 dex. By comparing the observed spectra with synthetic ones, we find that saturation of the absorption lines at least partly explains the metallicity effect. [ABSTRACT FROM AUTHOR]

We are carrying out near-infrared spectroscopy of Cepheids in the Galactic nuclear disk. The H-band spectra taken with SUBARU/IRCS indicate that their kinematics are consistent with the rotation of the nuclear disk. [ABSTRACT FROM PUBLISHER]