A. Antoniadis-Karnavas, S. G. Sousa, E. Delgado Mena, N. C. Santos, G. D. C. Teixeira, V. Neves
Abstract
Aims. The derivation of spectroscopic parameters for M dwarf stars is very important in the fields of stellar and exoplanet characterization. The goal of this work is the creation of an automatic computational tool able to quickly and reliably derive the Teff and [Fe/H] of M dwarfs using optical spectra obtained by different spectrographs with different resolutions.
Methods. ODUSSEAS (Observing Dwarfs Using Stellar Spectroscopic Energy-Absorption Shapes) is based on the measurement of the pseudo equivalent widths for more than 4000 stellar absorption lines and on the use of the machine learning Python package “scikit-learn” for predicting the stellar parameters.
Results. We show that our tool is able to derive parameters accurately and with high precision, having precision errors of ~30 K for Teff and ~0.04 dex for [Fe/H]. The results are consistent for spectra with resolutions of between 48 000 and 115 000 and a signal-to-noise ratio above 20.
Keywords
stars: fundamental parameters; stars: atmospheres; stars: late-type; methods: data analysis; techniques: spectroscopic; Astrophysics - Solar and Stellar Astrophysics
Notes
ODUSSEAS can be tested by downloading the files from https://github.com/AlexandrosAntoniadis/ODUSSEAS, after reading the README instructions for clarifying the technical details.
Astronomy & Astrophysics
Volume 636, Article Number A9, Number of pages 15
2020 April
