Metallicity and Ionization in High Velocity Cloud Complex C

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dc.creatorCollins, J. A.
dc.creatorShull, J. M.
dc.creatorGiroux, M. L.
dc.date2006-10-24
dc.date.accessioned2026-07-07T10:23:59Z
dc.date.available2026-07-07T10:23:59Z
dc.descriptionWe analyze HST and FUSE ultraviolet spectroscopic data for eleven sight lines passing through the infalling high velocity cloud (HVC) Complex C. These sight lines pass through regions with HI column densities ranging from N(HI) = 10^(18.1) to 10^(20.1). From [OI/HI] abundances, we find that Complex C metallicities range from 0.09 to 0.29 Z_solar, with a column density weighted mean of 0.13 Z_solar. Nitrogen (NI) is underabundant by factors of (0.01-0.07) (N/H)_solar, significantly less than oxygen relative to solar abundances. This pattern suggests nucleosynthetic enrichment by Type II SNe, consistent with an origin in the Galactic fountain or infalling gas produced in winds from Local Group galaxies. The range of metallicity and its possible (2 sigma) dependence on N(HI) could indicate some mixing of primordial material with enriched gas from the Milky Way, but the mixing mechanism is unclear. We also investigate the significant highly ionized component of Complex C, detected in CIV, SiIV, and OVI, but not in NV. High-ion column density ratios show little variance and are consistent with shock ionization or ionization at interfaces between Complex C and a hotter surrounding medium. Evidence for the former mechanism is seen in the Mrk 876 line profiles, where the offset in line centroids between low and high ions suggests a decelerating bowshock.
dc.descriptionSubmitted to ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0610729
dc.identifierhttp://arxiv.org/abs/astro-ph/0610729
dc.identifierAstrophys.J.657:271-285,2007
dc.identifierdoi:10.1086/510770
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/176034
dc.subjectAstrophysics
dc.titleMetallicity and Ionization in High Velocity Cloud Complex C
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