A Search for CMB Anisotropies on Arcminute Scales with Bolocam

Details A Search for CMB Anisotropies on Arcminute Scales with Bolocam A Search for CMB Anisotropies on Arcminute Scales with Bolocam

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21111002s&link_type=abstract

American Astronomical Society, AAS Meeting #211, #110.02; Bulletin of the American Astronomical Society, Vol. 39, p.938

Astronomy and Astrophysics

Astronomy

Scientific paper

This talk describes the results of two sets of observations made in 2003 and 2004 with Bolocam from the Caltech Sub-millimeter Observatory (CSO). Bolocam is a large format camera consisting of 144 bolometers with an eight arcminute field of view at the CSO, and can be operated non-simultaneously at 1.1, 1.4, or 2.1 mm. All of the data described in this talk was collected at 2.1 mm, where the individual beams are approximately one arcminute in size. The observations were made over a total of seventy-nine nights, and consisted of surveys of two science fields, Lynx and the Subaru/XMM Deep Field (SDS1), covering a total area of approximately 1 square degree. The noise properties of the maps are extremely uniform, with RMS variations in coverage of approximately 1.5% for twenty arcsecond map pixels. The point source sensitivity of the maps is approximately 100 μKCMB per beam. Fluctuations in emission from the atmosphere limited the sensitivity of our measurements, and several algorithms designed to remove these fluctuations are described. These algorithms also removed astronomical flux, and simulations were used to determine the effect of this attenuation on a CMB power spectrum. Assuming a flat CMB band power, our data corresponds to an effective angular multipole of l = 5700, with a FWHMl = 2800. At these scales the CMB power spectrum is expected to be dominated by anisotropies induced by the Sunyaev-Zel'dovich effect (SZE), and have a reasonably flat spectrum. Our data is consistent with a CMB band power of 0 μK2CMB, and we set an upper limit for the CMB anisotropies.

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