Stellar Parameters of BOSS M dwarfs in SDSS-V DR19

TL;DR

This paper presents a data-driven method using Support Vector Regression to derive stellar parameters for M dwarfs in SDSS-V DR19, calibrated with multiple datasets, and compares the results with other methods to assess accuracy and biases.

Contribution

The study introduces SLAM, a novel data-driven model for estimating stellar parameters of M dwarfs from low-resolution spectra, calibrated with diverse datasets and validated against independent measurements.

Findings

SLAM predicts [Fe/H] with 0.11 dex scatter in M+M binaries.

Effective temperatures from SLAM agree within ~100 K with interferometric and LAMOST measurements.

A correction equation for ASPCAP [Fe/H] biases is provided.

Abstract

We utilized the Stellar LAbel Machine (SLAM), a data-driven model based on Support Vector Regression, to derive stellar parameters ([Fe/H], $T_{\rm eff}$, and $\log{g}$) for SDSS-V M dwarfs using low-resolution optical spectra (R$\sim$2000) obtained with the BOSS spectrographs. These parameters are calibrated using LAMOST F, G or K dwarf companions ([Fe/H]), and APOGEE Net ($T_{\rm eff}$ and $\log{g}$), respectively. Comparisons of SLAM predicted [Fe/H] values between two components of M+M dwarfs wide binaries show no bias but with a scatter of 0.11 dex. Further comparisons with two other works, which also calibrated the [Fe/H] of M dwarfs by using the F/G/K companions, reveal biases of -0.06$\pm$0.16 dex and 0.02$\pm$0.14 dex, respectively. The SLAM-derived effective temperatures agree well with the temperature which is calibrated by using interferometric angular diameters (bias: -27$\pm$92 K) and those of the LAMOST (bias: -34$\pm$65 K), but are systematically lower than those from an empirical relationship between the color index and $T_{\rm eff}$ by 146$\pm$45 K. The SLAM surface gravity aligns well with those of LAMOST (bias: -0.01$\pm$0.07 dex) and those derived from the stellar mass and radius (bias: -0.04$\pm$0.09 dex). Finally, we investigated a bias in [Fe/H] between SLAM and APOGEE ASPCAP. It depends on ASPCAP's [Fe/H] and $T_{\rm eff}$, we provide an equation to correct the ASPCAP metallicities.