We present HST GHRS and STIS observations of five QSOs that probe the prominent high-velocity cloud (HVC) Complex C, covering 10% of the northern sky. Based upon a single sightline measurement (Mrk 290), a metallicity [S/H]=-1.05+/-0.12 has been associated with Complex C by Wakker et al. (1999a,b). When coupled with its inferred distance (5<d<30 kpc) and line-of-sight velocity (v=-100 to -200 km/s), Complex C appeared to represent the first direct evidence for infalling low-metallicity gas onto the Milky Way, which could provide the bulk of the fuel for star formation in the Galaxy. We have extended the abundance analysis of Complex C to encompass five sightlines. We detect SII absorption in three targets (Mrk 290, Mrk 817, and Mrk 279); the resulting [SII/HI] values range from -0.36 (Mrk 279) to -0.48 (Mrk 817) to -1.10 (Mrk 290). Our preliminary OI FUSE analysis of the Mrk 817 sightline also supports the conclusion that metallicities as high as 0.3 times solar are encountered within Complex C. These results complicate an interpretation of Complex C as infalling low-metallicity Galactic fuel. Ionization corrections for HII and SIII cannot easily reconcile the higher apparent metallicities along the Mrk 817 and Mrk 279 sightlines with that seen toward Mrk 290, since H-alpha emission measures preclude the existence of sufficient HII. If gas along the other lines of sight has a similar pressure and temperature to that sampled toward Mrk 290, the predicted H-alpha emission measures would be 900 mR. It may be necessary to reclassify Complex C as mildly enriched Galactic waste from the Milky Way or processed gas torn from a disrupted neighboring dwarf, as opposed to low-metallicity Galactic fuel.
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