ODUSSEAS: Upgraded version with new reference scale and parameter determinations for 82 planet-host M dwarf stars in SWEET-Cat

TL;DR

The upgraded ODUSSEAS tool accurately derives stellar parameters for M dwarf stars using a new reference scale, improving precision and confirming the link between stellar metallicity and planetary mass.

Contribution

This paper introduces an improved version of ODUSSEAS with a new reference scale and parameter determinations for 82 M dwarf stars, enhancing accuracy over previous methods.

Findings

Enhanced accuracy in stellar parameter determination.

Consistent results across multiple instruments.

Confirmed correlation between planetary mass and stellar metallicity.

Abstract

Aims: Obtaining accurate derivations of stellar atmospheric parameters is crucial in the fields of stellar and exoplanet characterization. We present the upgraded version of our computational tool ODUSSEAS with a new reference scale applied to derive $T_{\mathrm{eff}}$ and [Fe/H] values for M dwarfs. Methods: The new reference dataset of ODUSSEAS consists of $T_{\mathrm{eff}}$ values based on interferometry, and [Fe/H] values derived by applying updated values for the parallaxes. These reference parameters are related to the pseudo-equivalent widths (EWs) of more than 4000 stellar absorption lines. The machine learning Python "scikit learn" package creates models to determine the stellar parameters for subsequent analysis. Results: We determined $T_{\mathrm{eff}}$ and [Fe/H] values for 82 planet-host stars in SWEET-Cat. We demonstrate that our new version of ODUSSEAS is capable of determining the parameters with a greater accuracy than the original by comparing our results to other methods in literature. We also compared our parameters for the same stars by measuring their spectra obtained from several instruments, showing the consistency of our determinations with standard deviation of 30 K and 0.03 dex. Finally, we examined the correlation among planetary mass and stellar metallicity, confirming prior evidence indicating that massive planets mainly form around metal-rich stars in the case of M dwarfs as well.