![Top panel: Comparison of our determined [Fe/H] values (blue line) against the reported metallicity from Mann et al. (2015), Passegger et al. (2019), Maldonado et al. (2020), Marfil et al. (2021) and Cristofari et al. (2022). The red shaded area represents the typical distribution of M dwarfs metallicity from SDSS DR18 (Almeida et al. 2023). Bottom panel: Residuals are plotted to compare the median metallicity values from all referenced studies against each individual work. All measurements are consistent. -- astro-ph.SR](https://i0.wp.com/astrobiology.com/wp-content/uploads/2024/11/Chemical-Fingerprints-of-M-Dwarfs.png?resize=1200%2C717&ssl=1)
We extend the methodology introduced by Jahandar et al. (2024) to determine the effective temperature and chemical abundances of 31 slowly-rotating solar neighborhood M dwarfs (M1-M5) using high-resolution spectra from […]
PHOENIX-ACES
![Analysis of the stellar parameters derived with our methodology. The dots are colour-coded according to the estimated metallicity. The size of the dots is proportional to the estimated projected rotational velocity. The top left panel shows a Kiel diagram, with the red, black, and blue dashed lines corresponding to 5 Gyr PARSEC isochrones with [M/H] = −0.4, 0.0 and 0.1 dex, respectively. Empty squares represent the stars reported to have a behaviour akin to subdwarfs both in Mar21 and Schw19 (same for bottom left panel). Top right: black and grey dashed lines correspond to solar metallicity PARSEC isochrones for 5 and 0.1 Gyr, respectively. Black and grey dotted lines correspond to solar metallicity Baraffe et al. (2015) isochrones for 5 and 0.1 Gyr, respectively. Bottom left: triangles represent stars identified as Hα active in Schöfer et al. (2019). Empty stars depict members of the thick disc Galactic population (Cortés-Contreras et al., in prep.). Bottom right: plus symbols correspond to stars identified as members of the young disc Galactic population by Cortés-Contreras et al. (in prep.). Empty circles represent stars with a possible membership in a young stellar associaton, as explained in Section 4.1. -- astro-ph.SR](https://i0.wp.com/astrobiology.com/wp-content/uploads/2024/05/Using-Autoencoders-And-Deep.png?resize=1200%2C717&ssl=1)
Posted inAI - Data - Apps - Cybernetics, Astronomy & Telescopes, Imaging & Spectroscopy, Status Report, Stellar Cartography
Using Autoencoders And Deep Transfer Learning To Determine The Stellar Parameters Of 286 CARMENES M Dwarfs
Deep learning (DL) techniques are a promising approach among the set of methods used in the ever-challenging determination of stellar parameters in M dwarfs.
Posted inAstronomy & Telescopes, Barnard's Star, Habitable Zones, Imaging & Spectroscopy, Status Report
Comprehensive High-resolution Chemical Spectroscopy of Barnard’s Star with SPIRou
Determination of fundamental parameters of stars impacts all fields of astrophysics, from galaxy evolution to constraining the internal structure of exoplanets.