X-ray Emission From The Warm-hot Intergalactic Medium (whim)

Details X-ray Emission From The Warm-hot Intergalactic Medium (whim) X-ray Emission From The Warm-hot Intergalactic Medium (whim)

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011head...12.3913u&link_type=abstract

American Astronomical Society, HEAD meeting #12, #39.13

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It is believed that a large fraction of the low redshift baryons is in the form of a warm-hot filamentary gas in the intergalactic medium (WHIM). We already have successfully used XMM-Newton data to identify and characterize the WHIM angular signature using the autocorrelation function (AcF). We have recently also reproduced the same signal using data from Chandra, extending the analysis to lower angular scales.
With the output of large scale hydrodynamic simulations we also analyzed the correlation between low energy X-ray emission and SZ effect from WHIM filaments. Most of the total luminosity in the SZ effect is associated with virialized structures, anyway our work indicates that a significant contribution comes from unbound objects, in particular from mildly overdense regions, like the WHIM. Due to the unique emission mechanism, the analysis of the correlation between X-ray and SZ gives additional constraints on the structure of the intergalactic gas.
In this presentation we will show the results of our work on the expected correlation between X-ray emission and SZ signals and its applications for current X-ray and SZ observatories. We will also present our preliminary results using actual data from Chandra and XMM-Newton, and the Atacama Cosmology Telescope (ACT).
This work is supported, in part, by NASA grant NNX11AF80G and Chandra Award No. GO1-12177.

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