The chemical composition of the Orion star forming region: I. Homogeneity of O and Si abundances in B-type stars

TL;DR

This study uses improved spectroscopic analysis to show that B-type stars in the Orion OB1 association have homogeneous oxygen and silicon abundances, aligning with recent findings in the solar neighborhood.

Contribution

It demonstrates that previous perceived abundance inhomogeneities were due to errors, and provides a refined, self-consistent abundance analysis of Orion B-type stars.

Findings

Homogeneity in O and Si abundances in Orion OB1 stars

Previous abundance inhomogeneities were due to systematic errors

Results align with recent solar neighborhood abundance measurements

Abstract

Recent accurate abundance analyses of B-type main sequence stars in the solar vicinity has shown that abundances derived from these stellar objects are more homogeneous and metal-rich than previously thought. We investigate whether the inhomogeneity of abundances previously found in B-type stars in the Ori OB1 association is real (hence a signature of enrichment of the newly formed stars in an induced star formation scenario) or a consequence of intrinsic errors induced by the use of photometric indices to establish the stellar parameters prior to the abundance analysis. We obtained a new (improved) spectroscopic data set comprising 13 B-type stars in the various Ori OB1 associations, and performed a detailed, self-consistent spectroscopic abundance analysis by means of the modern stellar atmosphere code FASTWIND. We detect systematic errors in the stellar parameters determined previously which affect the derived abundances. Once these errors are accounted for, we find a high degree of homogeneity in the O and Si abundances for stars in the four Ori OB1 subgroups. The derived abundances are in very good agreement with recent determinations in other B-type stars in the solar vicinity. We also compare our results with those obtained for the Sun during the epoch of the "solar crisis", and the Orion nebula.