paper

Observable Signatures of the low-z Circum-Galactic and Inter-Galactic Medium : UV Line Emission in Simulations

arXiv:1111.3028 · doi:10.1111/j.1365-2966.2011.20172.x

Abstract

We present for the first time predictions for UV line emission of intergalactic and circumgalactic gas from Adaptive Mesh Resolution (AMR) Large Scale Structure (LSS) simulations at redshifts 0.3<z<1.2, with specific emphasis on observability with current and near-future UV instrumentation. In three transitions of interest (Lya, OVI and CIV) there is a clear bimodality in the type of objects : the overwhelming majority of flux stems from discrete, compact sources, while a much larger volume fraction is filled by more tenuous gas. We characterise both object types with regard to number density, physical size and shape, brightness, luminosity, velocity structure, mass, temperature, ionisation state, and metal content. Degrading AMR grids to characteristic resolutions of available (such as FIREBall) or foreseeable instrumentation, allows to assess which inferences can be drawn from currently possible observations, and set foundations to prepare observing strategies for future missions. In general, the faint emission of the IGM and filamentary structure remains beyond capabilities of instruments with only short duration exposure potential (stratospheric balloons), even for optimistic assumptions for Lya, while the yet fainter metal line transitions for these structures will remain challenging for long duration exposures (space-based telescopes), mostly due to low metallicity pushing them more than three orders of magnitudes in brightness below Lya radiation. For the circum-galactic medium (CGM) the situation is more promising, and it is foreseeable that in the near future we will not only just dectect such sources, but the combination of all three lines in addition to velocity information will yield valuable insight into the physical processes at hand, illuminating important mechanisms during the formation of galaxies and their backreaction onto the IGM from whence they formed. (abrigded)

Accepted for publication in MNRAS (2011 November 08, received in original form 2011 September 14). 27 pages, 19 figures, 3 tables. Some of the figures have degraded resolution due to file size limitations. For high-resolution version, please contact the first author

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