Elemental Abundances from Very Low Abundance HII Regions

Astronomy and Astrophysics – Astronomy

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Scientific paper

In 1987 we initiated a program to mitigate the deficiency of known low metallicity galaxies. Following our discoveries of very low abundance H II regions in nearby dwarf galaxies (Skillman et al. 1988, 1989a,b), we used the IDS on the INT to to collect spectra of dwarf galaxies in the Second Byurakan Survey (SBS) of UV excess galaxies. Our survey of over 40 SBS galaxies was completed in January 1990 and we have identified roughly one dozen very low metallicity H II galaxies. Now, with a significant sample of these galaxies, several observational programs are possible; foremost of these is the measurement of the primordial helium abundance (eg., Pagel et al. 1992). We report here on observations from March 1991 and 1992 using the ISIS spectrograph on the WHT to obtain very high quality spectra of 8 of these newly discovered metal-poor galaxies. The ISIS double spectrograph allows simultaneous observations of the blue (3600 - 5100 Angstroms) and red (6300 - 6800 Angstroms). Thus, He, N, O, Ne and S abundances can be derived with relatively small observational uncertainties. We compare our new observations with those in the literature. Our preliminary analysis indicates a slightly larger scatter in He/H at low O/H than had been seen previously. The small scatter may have been due simply to the paucity of observations at low metallicity. References: Pagel, B.E.J., Simonson, E.A., Terlevich, R.J., & Edmunds, M.G. 1992, MNRAS, 255, 325 Skillman, E.D., Kennicutt, R.C., & Hodge, P.W. 1989a, ApJ, 347, 875 Skillman, E.D., Melnick, J., Terlevich, R., & Moles, M. 1988, A&A, 196, 31 Skillman, E.D., Terlevich, R., & Melnick, J. 1989b, MNRAS, 240, 563

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