Journal Article

The nature and origin of low-redshift O <span class="smallCaps">vi</span> absorbers

Benjamin D. Oppenheimer and Romeel Davé

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 395, issue 4, pages 1875-1904
Published in print June 2009 | ISSN: 0035-8711
Published online May 2009 | e-ISSN: 1365-2966 | DOI:
The nature and origin of low-redshift O vi absorbers

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The O vi ion observed in quasar absorption-line spectra is the most accessible tracer of the cosmic metal distribution in the low-redshift (z < 0.5) intergalactic medium (IGM). We explore the nature and origin of O vi absorbers using cosmological hydrodynamic simulations including galactic outflows with a range of strengths. We consider the effects of ionization background variations, non-equilibrium ionization and cooling, uniform metallicity and small-scale (sub-resolution) turbulence. Our main results are as follows. (1) IGM O vi is predominantly photo-ionized with T≈ 104.2±0.2 K. A key reason for this is that O vi absorbers preferentially trace overenriched (by ∼×5) regions of the IGM at a given density, which enhances metal-line cooling such that absorbers can cool to photo-ionized temperatures within a Hubble time. As such, O vi is not a good tracer of the warm-hot intergalactic medium. (2) The predicted O vi properties fit observables if and only if sub-resolution turbulence is added, regardless of any other model variations. The required turbulence increases with O vi absorber strength. Stronger absorbers arise from more recent outflows, so qualitatively this can be understood if IGM turbulence dissipates on the order of a Hubble time. The amount of turbulence is consistent with other examples of turbulence observed in the IGM and galactic haloes. (3) Metals traced by O vi and H i do not trace exactly the same baryons, but reside in the same large-scale structure. Our simulations reproduce observed alignment statistics between O vi and H i, yet aligned absorbers typically have O vi arising from cooler gas, and for stronger absorbers lower densities, than H i. Owing to peculiar velocities dominating the line structure, coincident absorption often arises from spatially distinct gas. (4) Photo-ionized O vi traces gas in a variety of environments, and is not directly associated with the nearest galaxy, though is typically nearest to ∼0.1L* galaxies. Weaker O vi components trace some of the oldest cosmic metals. (5) Very strong absorbers (EW ≳ 100 mÅ) are more likely to be collisionally ionized, tracing more recent enrichment (≲2 Gyr) within or near galactic haloes.

Keywords: methods: numerical; galaxies: evolution; intergalactic medium; cosmology: theory

Journal Article.  25063 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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