Chemical composition of the Taurus-Auriga association

TL;DR

This study provides a high-resolution spectroscopic analysis of seven low-mass stars in the Taurus-Auriga association, revealing a solar metallicity and low dispersion among members, which supports theories about star formation and planetary system development.

Contribution

The paper presents the first detailed metallicity measurements of Taurus-Auriga members using high-resolution spectroscopy, confirming a solar metallicity with minimal dispersion.

Findings

Mean [Fe/H] = -0.01 ± 0.05, indicating solar metallicity.

No significant metallicity dispersion among members.

Supports the idea that planet-host stars originate in the inner Galactic disc.

Abstract

The Taurus-Auriga association is perhaps the most famous prototype of a low-mass star forming region, surveyed at almost all wavelengths. Unfortunately, like several other young clusters/associations, this T association lacks an extensive abundance analysis determination. We present a high-resolution spectroscopic study of seven low-mass members of Taurus-Auriga, including both weak-lined and classical T Tauri stars designed to help robustly determine their metallicity. After correcting for spectral veiling, we performed equivalent width and spectral synthesis analyses using the GAIA set of model atmospheres and the 2002 version of the code MOOG. We find a solar metallicity, obtaining a mean value of [Fe/H]=$-0.01\pm$0.05. The $\alpha$-element Si and the Fe-peak one Ni confirm a solar composition. Our work shows that the dispersion among members is well within the observational errors at variance with previous claims. As in other star forming regions, no metal-rich members are found, reinforcing the idea that old planet-host stars form in the inner part of the Galactic disc and subsequently migrate.