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19 April 2024 |
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Bringing Simulation and Observation Together to Better Understand the Intergalactic Medium | | Hilary Egan
; Britton D. Smith
; Brian W. O'Shea
; J. Michael Shull
; | | Date: |
8 Jul 2013 | | Abstract: | The methods by which one characterizes the distribution of matter in
cosmological simulations is intrinsically different from how one performs the
same task observationally. In this paper, we make critical steps towards
comparing simulations and observations of the intergalactic medium (IGM) in a
more sensible way. We present a pipeline that generates and fits synthetic QSO
absorption spectra using sight lines cast through a cosmological simulation,
and simultaneously identifies structure by directly analyzing the variations in
H I and O VI number density. We compare synthetic absorption spectra with a
less observationally motivated, but more straightforward method for finding
absorbers. Our efforts focus on H I and O VI to better characterize the
warm/hot intergalactic medium, a subset of the IGM that is challenging to
conclusively identify observationally. We find that the two methods trace
roughly the same amount of material above observable column density limits, but
the synthetic spectra typically identify more substructure in absorbers. We use
both methods to characterize H I and O VI absorber properties. We find that
column density distributions from both methods generally agree with
observations. The distribution of Doppler parameters are similar for Ly{alpha}
and compare favorably with observational results, but are systematically
different for O VI. Comparisons of distance between absorbers and the nearest
galaxy show that O VI absorbers are tightly correlated with galaxies in our
simulation, in agreement with observations. We find a strong correlation
between O VI baryon fraction and O VI column density. We also discuss a
possible bimodality in the temperature distribution of the gas traced by O VI. | | Source: | arXiv, 1307.2244 | | Services: | Forum | Review | PDF | Favorites | |
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