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

Published online by Cambridge University Press:  25 May 2016

R.D. Davies ,
R.J. Davis ,
A. Wilkinson ,
R.A. Watson ,
S.J. Melhuish ,
S. Dicker ,
S. Veeraraghavan ,
R. Rebolo ,
C.M. Gutierrez  and
R.J. Hoyland
...Show all authors
R.D. Davies
Affiliation:
NRAL Jodrell Bank, University of Manchester, UK
R.J. Davis
Affiliation:
NRAL Jodrell Bank, University of Manchester, UK
A. Wilkinson
Affiliation:
NRAL Jodrell Bank, University of Manchester, UK
R.A. Watson
Affiliation:
NRAL Jodrell Bank, University of Manchester, UK
S.J. Melhuish
Affiliation:
NRAL Jodrell Bank, University of Manchester, UK
S. Dicker
Affiliation:
NRAL Jodrell Bank, University of Manchester, UK
S. Veeraraghavan
Affiliation:
NRAL Jodrell Bank, University of Manchester, UK
R. Rebolo
Affiliation:
IAC, La Laguna, Tenerife, Spain
C.M. Gutierrez
Affiliation:
IAC, La Laguna, Tenerife, Spain
R.J. Hoyland
Affiliation:
IAC, La Laguna, Tenerife, Spain
A.N. Lasenby
Affiliation:
MRAO, Cambridge University, UK
S. Hancock
Affiliation:
MRAO, Cambridge University, UK
A.W. Jones
Affiliation:
MRAO, Cambridge University, UK
G. Rocha
Affiliation:
MRAO, Cambridge University, UK

Extract

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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 ΔTrms = 48+21−15 μK on a coherence scale of 4°; the equivalent analysis for a Harrison-Zeldovich model gives a power spectrum normalisation of Qrms = 22+10−6 μK. The value of the fluctuation amplitude calculated from the likelihood analysis of the two-dimensional data set is ΔTrms = 54 ± 13 μK at 10 GHz and 39+8−7 μK at 15 GHz.

Type
II. Cosmic Microwave Background Radiation
Information
Symposium - International Astronomical Union , Volume 183: Cosmological Parameters and the Evolution of the Universe , 1999 , pp. 103
Copyright
Copyright © Kluwer 1999