Using photo-ionisation models to derive carbon and oxygen gas-phase abundances in the rest UV
Abstract
We present a new method to derive oxygen and carbon abundances using the ultraviolet (UV) lines emitted by the gas-phase ionised by massive stars. The method is based on the comparison of the nebular emission-line ratios with those predicted by a large grid of photo-ionisation models. Given the large dispersion in the O/H - C/O plane, our method firstly fixes C/O using ratios of appropriate emission lines and, in a second step, calculates O/H and the ionisation parameter from carbon lines in the UV. We find abundances totally consistent with those provided by the direct method when we apply this method to a sample of objects with an empirical determination of the electron temperature using optical emission lines. The proposed methodology appears as a powerful tool for systematic studies of nebular abundances in star-forming galaxies at high redshift.
Keywords
Cite
@article{arxiv.1701.04411,
title = {Using photo-ionisation models to derive carbon and oxygen gas-phase abundances in the rest UV},
author = {Enrique Pérez-Montero and Ricardo Amorín},
journal= {arXiv preprint arXiv:1701.04411},
year = {2017}
}
Comments
7 pages, 4 figures. MNRAS in press (DOI: 10.1093/mnras/stx186). Modified to match the published version