Astronomy and Astrophysics, volume 437, 849-859 (2005/7-3)
Spectroscopic study of blue compact galaxies. V. Oxygen abundance and the metallicity-luminosity relation.
SHI F., KONG X., LI C. and CHENG F.Z.
Abstract (from CDS):
This is the fifth paper in a series studying the stellar components, star formation histories, star formation rates and metallicities of a blue compact galaxy (BCG) sample. Based on our high-quality ground-based spectroscopic observations, we have determined the electron temperatures, electron densities, nitrogen abundances and oxygen abundances for 72 star-forming BCGs in our sample, using different oxygen abundance indicators. The oxygen abundance covers the range 7.15<12+log(O/H)<9.0, and nitrogen is found to be mostly a product of secondary nucleosynthesis for 12+log(O/H)>8.2 and apparently a product of primary nucleosynthesis for 12+log(O/H)<8.2. To assess the possible systematic differences among different oxygen abundance indicators, we have compared oxygen abundances of BCGs obtained with the Te method, R23 method, P method, N2 method and O3N2 method. The oxygen abundances derived from the Te method are systematically lower by 0.1-0.25dex than those derived from the strong line empirical abundance indicators, consistent with previous studies based on HII region samples. We confirm the existence of the metallicity-luminosity relation in BCGs over a large range of abundances and luminosities. Our sample of galaxies shows that the slope of the metallicity-luminosity relation for the luminous galaxies (~-0.05) is slightly shallower than that for the dwarf galaxies (~-0.17). An offset was found in the metallicity-luminosity relation of the local galaxies and that of the intermediate redshift galaxies. It shows that the metallicity-luminosity relation for the emission line galaxies at high redshift is displaced to lower abundances, higher luminosities, or both.
galaxies: abundances - galaxies: starburst - stars: formation
Status at CDS:
Table 1: zw 0855 and Zw 2220 not identified (incomplete format), Zw 2335 = Z 2335.2+2952 (found with the cited reference).
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