2008/06/30 by Benjamin D. Oppenheimer, Romeel Davé, Romeel A. Davé · 3 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #Galaxy #Intergalactic travel #Ion #Ionization #Metallicity #Physics #Quasar #Redshift #Reionization #Spectral line #Stellar, planetary, and galactic studies #Structure formation #Thermodynamics #Turbulence #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2009.14676.x
33 pages, 18 figures, accepted to MNRAS. Two new figures added
arxiv created 2009/02/27 · openalex publication_date 2009/04/30 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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.