HEAVY ELEMENT ABUNDANCES IN A NEW SAMPLE OF LOW-METALLICITY BLUE COMPACT GALAXIES

We present high-quality spectrophotometric observations of 15 supergia nt H II regions in 14 new low-metallicity blue compact galaxies (BCGs) selected mainly from the First and Second Byurakan Surveys and with o xygen abundance 12 + log O/H between 7.37 and 8.04 (Z./35 less than or equal to Z less than or equal to Z./7). We use the data to determine abundances for the elements N, O, Ne, S, Ar, and, for the first time i n BCGs, Fe; discuss their origin; and constrain current nucleosynthesi s stellar models. The main result of the present study is that none of the heavy element-to-oxygen abundance ratios studied here (N/O, Ne/O, S/O, Ar/O, Fe/O) depend on oxygen abundance. We conclude that all the se heavy elements have a primary origin and are produced by the same m assive (M greater than or equal to 10 M.) stars. The dispersion of the N/O ratio is found to be remarkably small, being only +/- 0.08 in the log. This can only be understood if primary N is produced in massive stars, not in intermediate-mass (4 M.less than or equal to M less than or equal to 9 M.) stars as commonly thought. BCGs show the same O/Fe overabundance with respect to the Sun (similar to 0.34 in the log) as galactic halo stars, suggesting the same chemical enrichment history, and supporting the scenario of an early enrichment of the galactic hal o by massive Population III stars. We have compared the observed heavy element abundance ratios with theoretical yields from current massive star nucleosynthesis models from Weaver and Woosley (1993). The small dispersion in the heavy element abundance ratios suggests that there is not a large IMF variation between BCGs with different metallicities .