Limits on Arcminute Scale Cosmic Microwave Background Anisotropy with the BIMA Array

Abstract

We have used the Berkeley-Illinois-Maryland-Association (BIMA) millimeter array outfitted with sensitive cm-wave receivers to search for Cosmic Microwave Background (CMB) anisotropies on arcminute scales. The interferometer was placed in a compact configuration which produces high brightness sensitivity, while providing discrimination against point sources. Operating at a frequency of 28.5 GHz, the FWHM primary beam of the instrument is 6.6 arcminutes. We have made sensitive images of seven fields, five of which where chosen specifically to have low IR dust contrast and be free of bright radio sources. Additional observations with the Owens Valley Radio Observatory (OVRO) millimeter array were used to assist in the location and removal of radio point sources. Applying a Bayesian analysis to the raw visibility data, we place limits on CMB anisotropy flat-band power Q_flat = 5.6 (+3.0 -5.6) uK and Q_flat < 14.1 uK at 68% and 95% confidence. The sensitivity of this experiment to flat band power peaks at a multipole of l = 5470, which corresponds to an angular scale of approximately 2 arcminutes. The most likely value of Q_flat is similar to the level of the expected secondary anisotropies.

15 pages, 5 figures, LaTex, aas2pp4.sty, ApJ submitted

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Cited by in corpus (17)

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• The Sunyaev-Zel'dovich Effect: Results and Future Prospects
• Cosmological Implications of the BIMA 30 Ghz Sunyaev-Zel'dovich Effect Galaxy Cluster Survey
• A Deep Chandra Observation of the Distant Galaxy Cluster MS1137.5+6625
• A Search for CMB Decrements Towards Distant Cluster Candidates PC1643+4631 and VLA1312+4237 at 28.5 GHz
• Sunyaev-Zel'dovich contribution in CMB analysis