Final Results from the BIMA CMB Anisotropy Survey and Search for Signature of the SZ effect

Details Final Results from the BIMA CMB Anisotropy Survey and Search for Signature of the SZ effect Final Results from the BIMA CMB Anisotropy Survey and Search for Signature of the SZ effect

2006-02-18

arxiv.org/abs/astro-ph/0602413v2

Astrophys.J.647:13-24,2006

Astronomy and Astrophysics

Astrophysics

Accepted by ApJ, 17 pages

Scientific paper

10.1086/505172

We report the final results of our study of the cosmic microwave background (CMB) with the BIMA array. Over 1000 hours of observation were dedicated to this project exploring CMB anisotropy on scales between 1' and 2' in eighteen 6.6' FWHM fields. In the analysis of the CMB power spectrum, the visibility data is divided into two bins corresponding to different angular scales. Modeling the observed excess power as a flat band of average multipole ell= 5237, we find Delta T_1^2=220_{-120}^{+140} muK^2 at 68% confidence and Delta T_1^2 >0 muK^2 with 94.7% confidence. In a second band with average multipole of ell = 8748, we find Delta T_2^2 consistent with zero, and an upper limit 880 muK^2 at 95% confidence. An extensive series of tests and supplemental observations with the VLA provide strong evidence against systematic errors or radio point sources being the source of the observed excess power. The dominant source of anisotropy on these scales is expected to arise from the Sunyaev-Zel'dovich (SZ) effect in a population of distant galaxy clusters. If the excess power is due to the SZ effect, we can place constraints on the normalization of the matter power spectrum sigma_8 = 1.03^{+0.20}_{-0.29} at 68% confidence. The distribution of pixel fluxes in the BIMA images are found to be consistent with simulated observations of the expected SZ background and rule out instrumental noise or radio sources as the source of the observed excess power with similar confidence to the detection of excess power. Follow-up optical observations to search for galaxy over-densities anti-correlated with flux in the BIMA images, as might be expected from the SZ effect, proved to be inconclusive.

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