Anisotropy in the Cosmic Microwave Background: Results from Python IV

Details Anisotropy in the Cosmic Microwave Background: Results from Python IV Anisotropy in the Cosmic Microwave Background: Results from Python IV

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...19111204k&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #112.04; Bulletin of the American Astronomical Society, Vol. 29, p.1394

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Scientific paper

We report the observations made by the Python microwave background experiment in its fourth season of operation at the Amundsen-Scott South Pole Station in Antarctica. For this season the Python telescope was fitted with a new HEMT amplifier-based radiometer, yielding sensitivity to the microwave sky from 37-45 GHz in two frequency bands for each pixel in a 1 x 2 array, each pixel with a one degree beam on the sky. The modified instrument re-observed fields which had been measured to high signal-to-noise in previous seasons with the Python 90 GHz bolometric receiver. For a portion of the new observations, the previous sampling pattern was closely replicated, allowing a simple chi (2) comparison of these parts of the two datasets. On these fields both the 40 GHz data and the 90 GHz data detect signal at high significance. They are consistent with each other assuming a common, single-component source with spectral index in temperature of beta = -0.38(+0.95}_{-0.75) . Constraints on multicomponent (CMB + foreground) models are discussed. Results from more general (although model-dependant) comparisons based on joint-likelihood ratios, and using both entire datasets, are also presented.

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