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The Near-IR [SIII] Lines in a Sample of Star-Forming Galaxies: Chemical Abundances

Published online by Cambridge University Press:  01 August 2006

C. Kehrig ,
J. M. Vílchez ,
E. Telles ,
F. Cuisinier  and
E. Pérez-Montero
C. Kehrig
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC)Camino Bajo de Huetor 50, Apartado 3004, 18080 Granada, Spain email: kehrig@iaa.es Observatório Nacional, Rua General José Cristino 77, Rio de Janeiro, Brazil
J. M. Vílchez
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC)Camino Bajo de Huetor 50, Apartado 3004, 18080 Granada, Spain email: kehrig@iaa.es
E. Telles
Affiliation:
Observatório Nacional, Rua General José Cristino 77, Rio de Janeiro, Brazil
F. Cuisinier
Affiliation:
GEMAC, Observatório do Valongo/UFRJ, Ladeira do Pedro António 43, Rio de Janeiro, Brazil
E. Pérez-Montero
Affiliation:
Departamento de Física Teórica, C-XI, Universidad Autónoma de Madrid, 28049 Madrid, Spain
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Abstract

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We present a detailed spectroscopic study of a sample of 34 star-forming dwarf galaxies, ranging from the blue to near-infrared (λ3700Å-1μm) (Kehrig et al. 2006). The metal enrichment in this kind of objects has been operating typically at low metallicity enviroments. The spectra were observed with the 1.52m telescope at La Silla/ESO. We derive fundamental parameters for HII regions and ionizing sources in our star-forming galaxies, as well as gaseous metal abundances. All the spectra include the nebular[SIII]λλ9069,9532Å lines, that are of crucial importance in the derivation of the S/H abundances, and relevant ionization diagnostics. We study the relative hardness of their ionizing sources using the η' parameter (Vílchez & Pagel 1988), and exploring the roles played by metallicity and age. The ionic and total O/H was also derived using direct determinations of the te[OIII]. The mean S/O ratio derived in this work is constant and slightly below the solar (S/O)⊙ value (see fig 1). The data presented here are consistent with the conclusion that S/O remains constant as O/H varies among the sample of HII galaxies. Variations in S/O along the whole O/H abundance range may be present, but the scatter in S/O (due mainly to observational errors) is still large to constrain them. The assumption that the S/O ratio remains constant for all abundances is still an open question and should be explored further (Pérez-Montero et al. 2006).

Keywords

ISM: abundancesISM: HII regionsGalaxies: abundancesGalaxies: dwarf
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S235: Galaxy Evolution Across the Hubble Time , August 2006 , pp. 315
Copyright
Copyright © International Astronomical Union 2007

References

Kehrig, C., Vílchez, J.M., Telles, E., Cuisinier, F. & Pérez-Montero, E. 2006, A&A, 457, 477.Google Scholar
Pérez-Montero, E., Díaz, A.I., Vílchez, J.M. & Kehrig, C. 2006, A&A, 449, 193.Google Scholar
Vílchez, J.M., & Pagel, B.E.J. 1988, MNRAS, 231, 257.CrossRefGoogle Scholar