Statistics
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004phdt.......230d&link_type=abstract
Ph.D dissertation, 2004. 121 pages; United States -- California: University of California, Berkeley; 2004. Publication Number:
Statistics
1
Cosmic Microwave Background, Sunyaev-Zeldovich Effect, Low- Infrared Dust Emission, Optical Galaxies, Bima Survey, Arcminute Scale
Scientific paper
We report the results of our study of arcminute scale anisotropy in the Cosmic Microwave Background (CMB) with the Berkeley-Illinois-Maryland Association (BIMA) array. The survey consists of eighteen independent fields selected for low infrared dust emission. Over 1000 hours of integration were dedicated to the project in order to explore the contribution of the Sunyzev-Zel'dovich (SZ) effect to CMB anisotropy on scales between 1 ' and 2 ' . Using observations with the Very Large Array (VLA) at 4.8 GHz, we have identified point sources which could act as contaminants in estimates of the CMB power spectrum and removed them in the analysis. Modeling the observed power spectrum with a single flat band power of average multipole of ℓ eff = 6864, we find D T 2 = 170 +/- 110 mK 2 at 68% confidence. We have also divided the data into two bins corresponding to different spatial resolutions in the power spectrum. We find D[Special characters omitted.] = 220 +/- 130 mK 2 at 68% confidence for CMB flat band power described by an average multipole of ℓ eff = 5237 and D[Special characters omitted.] < 840 mK 2 at 95% confidence for ℓ eff = 8748. Monte Carlo simulations were used to compare the BIMA images to images generated from a model of instrumental noise and to images generated from a model of instrumental noise added to SZ clusters. Analysis of the im age statistics indicated that although the BIMA images were consistent with the Monte Carlo realizations of an SZ sky, they were not significantly different from observations including only instrumental noise. Follow-up optical observations using the Keck and Kitt Peak observatories were used to search for decrements in the BIMA data that are correlated with overdense regions of optical galaxies, but produced no significant evidence for galaxy clusters in the BIMA data.
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