Detecting The Missing Baryons With Autocorrelation Function Measurements

Details Detecting The Missing Baryons With Autocorrelation Function Measurements Detecting The Missing Baryons With Autocorrelation Function Measurements

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.0606g&link_type=abstract

American Astronomical Society, HEAD meeting #11, #6.06; Bulletin of the American Astronomical Society, Vol. 41, p.658

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The amount of detected baryons in the local universe is at least a factor of 2 smaller than measured at high redshift. It is believed that a significant fraction of the baryons in the current universe is "hiding” in a hot filamentary structure filling the intergalactic space, the warm-hot intergalactic medium (WHIM). The temperature and density of the WHIM make it invisible to all but soft X-ray and UV observations. The "hot” core of the filaments can only be studied in the soft X-ray band, mostly through excitation lines of highly ionized heavy elements, such as O VII, O VIII, Fe XVII, C VI, and N VII with energy between 0.2 and 0.7 keV.
Detecting and studying the X-ray emission from individual filaments is made difficult by the contribution from other sources of the diffuse X-ray background. The plasma filaments, however, have a characteristic angular structure that can be identified and studied using the angular autocorrelation function (AcF). We found evidence of the missing baryons in the WHIM by detecting their signature on the AcF of diffuse X-ray emission with the XMM-Newton satellite. Our result indicates that 12%±5% of the total diffuse X-ray emission in the energy range 0.4-0.6 keV is due to intergalactic filaments.
We are now expanding our investigation by looking at the cross correlations between X-ray data and Microwave background data due to the Sunyaev-Zel'dovich (SZ) effect to determine the WHIM properties. In particular, the different dependence on electron density between X-ray emission and SZ effect is invaluable to understand the density distribution of the WHIM filaments.

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