Astronomy and Astrophysics – Astrophysics
Scientific paper
2003-09-26
Astrophys.J.606:221-236,2004
Astronomy and Astrophysics
Astrophysics
replaced by version to appear in ApJ (conclusions unchanged, one new figure), 16 pages (emulateapj), 11 figures, version with
Scientific paper
10.1086/382727
We use a high-resolution cosmological simulation that includes hydrodynamics, multiphase star formation, and galactic winds to predict the distribution of metal line emission at z~0 from the intergalactic medium (IGM). We focus on two ultraviolet doublet transitions, OVI 1032,1038 and CIV 1548,1551. Emission from filaments with moderate overdensities is orders of magnitude smaller than the background, but isolated emission from enriched, dense regions with T~10^5-10^5.5 K and characteristic sizes of 50-100 kpc can be detected above the background. We show that the emission from these regions is substantially greater when we use the metallicities predicted by the simulation (which includes enrichment through galactic winds) than when we assume a uniform IGM metallicity. Luminous regions correspond to volumes that have recently been influenced by galactic winds. We also show that the line emission is clustered on scales ~1 h^-1 Mpc. We argue that although these transitions are not effective tracers of the warm-hot intergalactic medium, they do provide a route to study the chemical enrichment of the IGM and the physics of galactic winds.
Furlanetto Steven
Hernquist Lars
Schaye Joop
Springel Volker
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