2002ApJ...565..941T

New Far Ultraviolet Spectroscopic Explorer (FUSE) far-UV spectroscopy of the nearby metal-deficient (Z_☉/8) cometary blue compact dwarf (BCD) galaxy Markarian (Mrk) 59 is discussed. The data are used to investigate element abundances in its interstellar medium. The H I absorption lines are characterized by narrow cores that are interstellar in origin and by broad wings that are stellar in origin. The mean interstellar H I column density is ∼7x10²⁰ cm^–2 in Mrk 59. No H₂ lines are seen and N(H₂) is ≲10¹⁵ cm^–2 at the 10 σ level. The lack of diffuse H₂ is due to the combined effect of a strong UV radiation field that destroys the H₂ molecules and a low metallicity that leads to a scarcity of dust grains necessary for H₂ formation. P Cygni profiles of the S VI λλ933.4, 944.5 and O VI λλ1031.9, 1037.6 lines are seen, indicating the presence of very hot O stars and a stellar wind terminal velocity of ∼1000 km.s^–1. By fitting the line profiles with multiple components having each a velocity dispersion b=7 km.s^–1 and spanning a radial velocity range of 100 km.s^–1, some of which can be saturated, we derive heavy element abundances in the neutral gas. We find logN(O I)/N(H I)=-5.0±0.3 or [O I/H I]=-1.5 for the neutral gas, about a factor of 10 below the oxygen abundance of the supergiant H II region, implying self-enrichment of the latter.