WINDS OF LOW-METALLICITY OB-TYPE STARS: HST-COS SPECTROSCOPY IN IC 1613

We present the first quantitative ultraviolet spectroscopic analysis of resolved OB stars in IC 1613. Because of its alleged very low metallicity (less than or similar to 1/10Z(circle dot), from H II regions), studies in this Local Group dwarf galaxy could become a significant step forward from the Small Magellanic Cloud (SMC) toward the extremely metal-poor massive stars of the early universe. We present HST- COS data covering the similar to 1150-1800 angstrom wavelength range with resolution R similar to 2500. We find that the targets do exhibit wind features, and these are similar in strength to SMC stars. Wind terminal velocities were derived from the observed P Cygni profiles with the Sobolev plus Exact Integration method. The v(infinity)-Z relationship has been revisited. The terminal velocity of IC 1613 O stars is clearly lower than Milky Way counterparts, but there is no clear difference between IC 1613 and SMC or LMC analog stars. We find no clear segregation with host galaxy in the terminal velocities of B-supergiants, nor in the v(infinity)/v(esc) ratio of the whole OB star sample in any of the studied galaxies. Finally, we present the first evidence that the Fe-abundance of IC 1613 OB stars is similar to the SMC, which is in agreement with previous results on red supergiants. With the confirmed similar to 1/10 solar oxygen abundances of B-supergiants, our results indicate that IC 1613's alpha/Fe ratio is sub-solar.