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T. Fang (MIT ), Greg L. Bryan Collaboration
Recent STIS and FUSE observations have detected OVI absorption lines at low redshift that are not clearly associated with any galactic system. In this paper, we argue that these lines are due to metal enriched hot gas in the intergalactic medium. Using numerical simulations of a cosmological-constant dominated cosmology, combined with reasonable assumptions about the metallicity distribution, we show that the number density and internal characteristics of these lines are correctly predicted. We find that the OVI is primarily produced by collisional ionization from gas at a few times 105 K for lines with equivalent widths larger than 40 mA, while weaker lines can also be produced by photo-ionization. The absorption occurs in diffuse gas in filaments at moderate overdensity (\delta ~5-100).
The author(s) of this abstract have provided an email address for comments about the abstract: fangt@mit.edu