AMPLITUDES OF THERMAL AND KINETIC SUNYAEV-ZEL'DOVICH SIGNALS FROM SMALL-SCALE

While the arcminute-scale Cosmic Microwave Background (CMB) anisotropies are due to secondary effects, point sources dominate the total anisotropy power spectrum. At high frequencies the point sources are primarily in the form of dusty, star-forming galaxies. Both Herschel and Planck have recently measured the anisotropy power spectrum of cosmic infrared background (CIB) generated by dusty, star-forming galaxies from a degree to sub-arcminute angular scales, including the nonlinear clustering of these galaxies at multipoles of 3000 to 6000 relevant to CMB secondary anisotropy studies. We scale the CIB angular power spectra to CMB frequencies and interpret the combined WMAP-7 year and arcminute-scale Atacama Cosmology Telescope (ACT) and South Pole Telescope (SPT) CMB power spectra measurements to constrain the Sunyaev-Zel’dovich (SZ) effects. Allowing the CIB clustering amplitude to vary, we find the amplitudes of thermal and kinetic SZ power spectra at 150 GHz and at ` = 3000 to be D `=3000 tSZ + 0:5D `=3000 kSZ = 5:7 ± 2:0 �K 2 . The 95% confidence level upper limits on the amplitudes of the thermal and kinetic SZ effects at 150 GHz and at `= 3000 are 5.4 and 6.9 �K 2 , respectively.