Measurements of Arcminute Scale Anisotropy with the BIMA Array

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Project Overview

The Berkeley-Illinois-Maryland-Association (BIMA) Array has been used with cm-wave receivers to conduct a survey of ten independent fields in order to place limits on secondary Cosmic Microwave Background (CMB) anisotropy. Current measurements indicate a level of excess power that excludes the effects of instrumental noise by better than 95% confidence. The most likely source of these fluctuations in the CMB is believed to be the Sunyaev-Zel'dovich (SZ) effect (see Observations of clusters with the SZ effect ). Follow-up observations are planned in order to determine whether the sources of excess power in the BIMA fields are indeed clusters of galaxies.

The BIMA instrument is based out of the Radio Astronomy Laboratory at U.C. Berkeley, the Laboratory for Astronomical Imaging at U. Illinois at Urbana, and Laboratory for Millimeter-Wave Astronomy at U. Maryland.

Copyright Holzapfel Group, 2002 Page last modified December 16, 2002