2001 (IPP)

Permanent URI for this collectionhttp://localhost:4000/handle/11007/628

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Subject: search.filters.subject.Cosmic microwave background

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    Window function for non-circular beam CMB anisotropy experiment
    (2001-07-05) Souradeep, Tarun; Ratra, Bharat
    We develop computationally rapid methods to compute the window function for a cosmic microwave background anisotropy experiment with a non-circular beam which scans over large angles on the sky. To concretely illustrate these methods we compute the window function for the Python V experiment which scans over large angles on the sky with an elliptical Gaussian beam.
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    Cosmic Microwave Background Anisotropy Measurement from Python V
    (2001-03-01) Coble, Kim; Dodelson, S.; Dragovan, Mark; et al.
    We analyze observations of the microwave sky made with the Python exper- iment in its fifth year of operation at the Amundsen-Scott South Pole Station in Antarctica. After modeling the noise and constructing a map, we extract the cosmic signal from the data. We simultaneously estimate the angular power spectrum in eight bands ranging from large (ℓ ∼ 40) to small (ℓ ∼ 260) angular scales, with power detected in the first six bands. There is a significant rise in the power spectrum from large to smaller (ℓ ∼ 200) scales, consistent with that ex- pected from acoustic oscillations in the early Universe. We compare this Python V map to a map made from data taken in the third year of Python. Python III observations were made at a frequency of 90 GHz and covered a subset of the region of the sky covered by Python V observations, which were made at 40 GHz. Good agreement is obtained both visually (with a filtered version of the map) and via a likelihood ratio test.