Optical and mid-infrared neon abundance determinations in star-forming regions
Abstract
We employed observational spectroscopic data of star-forming regions compiled from the literature and photoionization models to analyse the neon ionic abundances obtained using both optical and mid-infrared emission-lines. Comparing Ne++/H+ ionic abundances from distinct methods, we found that, in average, the abundances obtained via IR emission-lines are higher than those obtained via optical lines by a factor of 4. Photoionization models with abundance variations along the radius of the hypothetical nebula provide a possible explanation for a large part of the difference between ionic abundances via optical and infrared emission-lines. Ionization Correction Factor (ICF) for the neon is obtained from direct determinations of ionic fractions using infrared emission-lines. A constant Ne/O ratio (logNe/O \approx -0.70) for a large range of metallicity, independently of the ICF used to compute the neon total abundance is derived.
Keywords
Cite
@article{arxiv.1304.3185,
title = {Optical and mid-infrared neon abundance determinations in star-forming regions},
author = {Oli L. Dors and Guillermo F. Hagele and Monica V. Cardaci and Enrique Perez-Montero and Angela C. Krabbe and Jose M. Vilchez and Dinalva A. Sales and Rogerio Riffel and Rogemar A. Riffel},
journal= {arXiv preprint arXiv:1304.3185},
year = {2015}
}
Comments
17 pages, 14 figures, accepted by MNRAS