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We present the analysis of the interstellar spectrum of Pox 36 with the FarUltraviolet Spectroscopic Explorer (FUSE). Pox 36 was selected because of therelatively low foreground gas content that makes it possible to detectabsorption-lines weak enough that unseen components should not be saturated.Interstellar lines of HI, NI, OI, SiII, PII, ArI, and FeII are detected. Columndensities are derived directly from the observed line profiles except for HI,whose lines are contaminated by stellar absorption. We used the TLUSTY modelsto remove the stellar continuum and isolate the interstellar component. Thebest fit indicates that the dominant stellar population is B0. The fit of theinterstellar HI line gives a column density of 10^{20.3\pm0.4} cm-2. Chemicalabundances were then computed from the column densities using the dominantionization stage in the neutral gas. Our abundances are compared to thosemeasured from emission-line spectra in the optical. Our results suggest thatthe neutral gas of Pox 36 is metal-deficient by a factor ~7 as compared to theionized gas, and they agree with a metallicity of ~1/35 Z$_\odot$. Conclusions:The abundance discontinuity between the neutral and ionized phases implies thatmost of the metals released by consecutive star-formation episodes mixes withthe HI gas. The volume extent of the enrichment is so large that themetallicity of the neutral gas increases only slightly. The star-formingregions could be enriched only by a small fraction (~1%), but it would greatlyenhance its metallicity. Our results are compared to those of other BCDs. Weconfirm the overall underabundance of metals in their neutral gas, with perhapsonly the lowest metallicity BCDs showing no discontinuity.

Metal enrichment of the neutral gas of blue compact dwarf galaxies: the compelling case of Pox 36