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We have used the Berkeley-Illinois-Maryland-Association (BIMA) arrayoutfitted with sensitive cm-wave receivers to expand our search for arcminutescale anisotropy of the Cosmic Microwave Background (CMB). The interferometerwas placed in a compact configuration toobtain high brightness sensitivity onarcminute scales over its 6.6' FWHM field of view. The sensitivity of thisexperiment to flat band power peaks at a multipole of l=5530 which correspondsto an angular scale of ~2'. We present the analysis of a total of 470 hours ofon-source integration time on eleven independent fields which were selectedbased on their low IR contrast and lack of bright radio sources. Applying aBayesian analysis to the visibility data, we find CMB anisotropy flat bandpower Q_flat = 6.1(+2.8/-4.8) microKelvin at 68% confidence. The confidence ofa non- zero signal is 76% and we find an upper limit of Q_flat < 12.4microKelvin at 95% confidence. We have supplemented our BIMA observations withconcurrent observations at 4.8 GHz with the VLA to search for and remove pointsources. We find the point sources make an insignificant contribution to theobserved anisotropy.Comment: 8 pages, 2 figures, submitted to Astrophysical Journa

A Preliminary Detection of Arcminute-Scale Cosmic Microwave Background Anisotropy with the BIMA Array