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Observations of the CMB on Scales of 2° to 15°

  • R.D. Davies (a1), R.J. Davis (a1), A. Wilkinson (a1), R.A. Watson (a1), S.J. Melhuish (a1), S. Dicker (a1), S. Veeraraghavan (a1), R. Rebolo (a2), C.M. Gutierrez (a2), R.J. Hoyland (a2), A.N. Lasenby (a3), S. Hancock (a3), A.W. Jones (a3) and G. Rocha (a3)...

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Beamswitching has been used at 10, 15 and 33 GHz to map the microwave background over the Declination range 30° to 45°, covering more than one steradian of the sky. The beamwidth is 5° and the beam-throw is ±8° at each frequency. The three data sets are used to separate Galactic emission from intrinsic CMB emission. For the scan at Dec = 40° the intrinsic fluctuation level is ΔT rms = 48+21 −15 μK on a coherence scale of 4°; the equivalent analysis for a Harrison-Zeldovich model gives a power spectrum normalisation of Q rms = 22+10 −6 μK. The value of the fluctuation amplitude calculated from the likelihood analysis of the two-dimensional data set is ΔT rms = 54 ± 13 μK at 10 GHz and 39+8 −7 μK at 15 GHz.

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Observations of the CMB on Scales of 2° to 15°

  • R.D. Davies (a1), R.J. Davis (a1), A. Wilkinson (a1), R.A. Watson (a1), S.J. Melhuish (a1), S. Dicker (a1), S. Veeraraghavan (a1), R. Rebolo (a2), C.M. Gutierrez (a2), R.J. Hoyland (a2), A.N. Lasenby (a3), S. Hancock (a3), A.W. Jones (a3) and G. Rocha (a3)...

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