Calibration of metallicity of LAMOST M dwarf stars Using FGK+M wide binaries

Abstract

Estimating precise metallicity of M dwarfs is a well-known difficult problem due to their complex spectra. In this work, we empirically calibrate the metallicity using wide binaries with a F, G, or K dwarf and a M dwarf companion. With 1308 FGK+M wide binaries well observed by LAMOST, we calibrated M dwarf’s [Fe/H] by using the Stellar LAbel Machine (SLAM) model, a data-driven method based on support vector regression (SVR). The [Fe/H] labels of the training data are from FGK companions in range of [-1,0.5] dex. The Teffs are based on APOGEE, spanning [3100,4400] K. The uncertainties in SLAM estimates of [Fe/H] and Teff are ∼0.15 dex and ∼40 K, respectively, at snri >100, where snri is the signal-to-noise ratio (SNR) at i-band of M dwarf spectra. We applied the trained SLAM model to determine the [Fe/H] and Teff for ∼630,000 M dwarfs with low-resolution spectra in LAMOST DR9. Compared to other literature also using FGK+M wide binaries for calibration, our [Fe/H] estimates show no bias but a scatter of ∼ 0.14-0.18 dex. However, the [Fe/H] compared to APOGEE shows a systematic difference of ∼ 0.10-0.15 dex with a scatter of ∼ 0.15-0.20 dex. While the Teff compared to APOGEE has a bias of 3 K with a scatter of 62 K, it is systematically higher by 180 K compared to other calibrations based on the bolometric temperature. Finally, we calculated the ζ index for 1308 M dwarf secondaries and presents a moderate correlation between ζ and [Fe/H].