Discrepancies between the [OIII] and [SIII] Temperatures in HII Regions

Luc Binette (1,2), Roy Matadamas (2), Guillermo F. Hägele (3,4,5), David C. Nicholls (6), Gladis Magris C. (7), María de los Ángeles Peña-Guerrero (8,2), Christophe Morisset (2), and Ary Rodríguez-González (9) ((1) Département de Physique, de Génie Physique et d’Optique, Université Laval, Québec, QC, Canada; (2) Instituto de Astronomía, Universidad Nacional Autónoma de México, D.F., Mexico; (3) Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Argentina; (4) Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, La Plata, Argentina; (5) Departamento de Física Teórica, C-XI, Universidad Autónoma de Madrid, Madrid, Spain; (6) Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd., Weston ACT 2611, Australia; (7) Centro de Investigaciones de Astronomía, Av. Alberto Carnevalli, Mérida, Venezuela; (8) Space Telescope Science Institute, Baltimore, Maryland 21218, USA; (9) Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Ap. 70-543, 04510 D.F., Mexico)

An analysis of the OIII and SIII temperatures measurements compiled by Perez-Montero et al. of emission line objects consisting of HII galaxies, giant extragalactic HII regions, Galactic HII regions and HII regions from the Magellanic Clouds, reveals that the OIII temperatures are higher than the corresponding values from SIII in most objects with gas metallicities in excess of 0.2 solar. We explore the possibility of temperature inhomogeneities. We also explored metallicity inhomogeneities by combining two models of widely different metallicity. We calculate models that consider a non Mawell-Boltzmann distributions for the electron energies (kappa parametrization). We also consider shock heating within the photoionized nebula.

See complete preprint –> http://arxiv.org/abs/1209.0808

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