Radial gradients and metallicities in the galactic disk

TL;DR

This paper combines various observational data to derive an independent [O/Fe] versus [Fe/H] relation for the galactic disk, providing insights into chemical abundance gradients and their implications.

Contribution

It introduces a new method of deriving the [O/Fe] versus [Fe/H] relation by combining different types of abundance gradients in the galactic disk.

Findings

The [O/Fe] ratio does not exceed approximately 0.4 within the studied metallicity range.

The derived relation aligns with recent observational data and theoretical models.

The study offers an independent approach to understanding chemical evolution in the galactic disk.

Abstract

Radial O/H abundance gradients derived from HII regions, hot stars and planetary nebulae are combined with [Fe/H] gradients from open cluster stars in order to derive an independent [O/Fe] x [Fe/H] relation for the galactic disk. A comparison of the obtained relation with recent observational data and theoretical models suggests that the [O/Fe] ratio is not higher than [O/Fe] ~ 0.4, at least within the metallicity range of the considered samples.