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• W1970237306 abstract "We present the results of a large survey of H I, O VI, and C III absorption lines in the low-redshift (z < 0.3) intergalactic medium (IGM). We begin with 171 strong Lyα absorption lines (Wλ ≥ 80 mÅ) in 31 AGN sight lines studied with the Hubble Space Telescope and measure corresponding absorption from higher order Lyman lines with FUSE. Higher order Lyman lines are used to determine N and b accurately through a curve-of-growth (COG) analysis. We find that the number of H I absorbers per column density bin is a power-law distribution, d/dN ∝ N, with β = 1.68 ± 0.11. We made 40 detections of O VI λλ1032, 1038 and 30 detections of C III λ977 out of 129 and 148 potential absorbers, respectively. The column density distribution of C III absorbers has β = 1.68 ± 0.04, similar to β but not as steep as β = 2.2 ± 0.1. From the absorption-line frequency, d/dz = 12 for Wλ(C ) > 30 mÅ, we calculate a typical IGM absorber size r0 ~ 400 kpc, similar to scales derived by other means. The COG-derived b-values show that H I samples material with T < 105 K, incompatible with a hot IGM phase. By calculating a grid of CLOUDY models of IGM absorbers with a range of collisional and photoionization parameters, we find it difficult to simultaneously account for the O VI and C III observations with a single phase. Instead, the observations require a multiphase IGM in which H I and C III arise in photoionized regions, while O VI is produced primarily through shocks. From the multiphase ratio N/N, we infer the IGM metallicity to be ZC = 0.12 Z☉, similar to our previous estimate of ZO = 0.09 Z☉ from O VI." @default.
• W1970237306 created "2016-06-24" @default.
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• W1970237306 date "2006-04-01" @default.
• W1970237306 modified "2023-09-25" @default.
• W1970237306 title "The Low‐<i>z</i>Intergalactic Medium. II. Lyβ, O<scp>vi</scp>, and C<scp>iii</scp>Forest" @default.
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• W1970237306 doi "https://doi.org/10.1086/500191" @default.
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