Power Spectrum of the Sunyaev-Zel'dovich Effect

Alexandre Refregier1, Eiichiro Komatsu2, David N. Spergel2 and Ue-Li Pen3

1. Institute of Astronomy, Madingley Road, University of Cambridge, Cambridge CB3 OHA, England
2. Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
3. Canadian Institute of Theoretical Astrophysics, University of Toronto, 60 St. George St., Toronto, Canada


The hot gas in the IGM produces anisotropies in the Cosmic Microwave Background (CMB) through the thermal Sunyaev-Zel'dovich (SZ) effect. The SZ effect is a powerful probe of large-scale structure in the universe, and must be carefully subtracted from measurements of the primary CMB anisotropies. We use moving-mesh hydrodynamical simulations to study the 3-dimensional statistics of the gas, and compute the mean comptonization parameter y and the angular power spectrum of the SZ fluctuations, for different cosmologies. We compare these results with predictions using the Press-Schechter formalism. We find that the two methods agree approximately, but differ in details. We discuss this discrepancy, and show that resolution limits the reliability of our results to the 200 < l < 2000 range. For cluster normalized CDM models, we find a mean y-parameter of the order of 10-6, one order of magnitude below the current observational limits from the COBE/FIRAS instrument. For these models, the SZ power spectrum is comparable to the primordial power spectrum around l=2000. It is well below the projected noise for the upcoming MAP satellite, and should thus not be a limitation for this mission. It should be easily detectable with the future Planck Surveyor mission. We show that groups and filaments (kT < 5 keV contribute about 50% of the SZ power spectrum at l=500. About half of the SZ power spectrum on these scales are produced at redshifts z < 0.1, and can thus be detected and removed using existing catalogs of galaxies and X-ray clusters.


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