Clues to the nature of high-redshift OVI absorption systems from their (lack of) small-scale structure

Abstract

We present results of the first survey of high-redshift (<z> ~ 2.3) OVI absorption systems along parallel lines of sight toward two lensed QSOs. After a careful and well-defined search, we find ten intervening OVI systems. Within the errors, all OVI systems appear at the same redshift and have similar line strengths in front of both QSO images, whereas in most cases CIV or SiIV show more differences across the lines of sight, either in radial velocity or line strength. We conclude that (1) the coherence length of OVI must be much larger than ~ 1 kpc, and (2) an important fraction of the CIV absorbers may not reside in the same volume as OVI. Since Doppler parameters are consistent with photoionization, we propose a model in which CIV occurs in two different photoionized phases, one large, with characteristic sizes of a few hundred kpc and bearing OVI, and another one a factor of ten smaller and containing CIII. This model is able to explain the various transverse differences observed in column density and kinematics. We apply the model successfully to 2 kinds of absorbers, with low and high metallicity. In the low-metallicity regime, [C/H] \~ -2, we find that [C/O] ~ -0.7 is required to explain the observations, which hints at late (z < 6) rather than early metal enrichment. In the high-metallicity regime, the observed dissociation between OVI and CIV gas might be produced by galactic outflows. Altogether, the relative abundances, inhomogeneous CIV and featureless OVI are consistent with gas that has been processed recently before the absorption occurred (thus close to star-forming regions). Finally, we discuss briefly three associated systems (z_abs ~ z_em) that also show OVI. (abridged)

Accepted by A&A, 22 pages

References in corpus (2)

• A Survey of O VI, C III, and H I in Highly Ionized High-Velocity Clouds
• High-Resolution Absorption Spectroscopy of Multi-phase, High-Metallicity Gas Associated with the Luminous Quasar HE 0226-4110

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