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Title:
The Cosmic Background Imager
Authors:
Padin, S.; Shepherd, M. C.; Cartwright, J. K.; Keeney, R. G.; Mason, B. S.; Pearson, T. J.; Readhead, A. C. S.; Schaal, W. A.; Sievers, J.; Udomprasert, P. S.; Yamasaki, J. K.; Holzapfel, W. L.; Carlstrom, J. E.; Joy, M.; Myers, S. T.; Otarola, A.
Affiliation:
AA(), AB(), AC(), AD(), AE(), AF(), AG(), AH(California Institute of Technology, MS 105-24, Pasadena, CA 91125; , , , , , , , , , , ), AI(California Institute of Technology, MS 105-24, Pasadena, CA 91125; , , , , , , , , , , ), AJ(California Institute of Technology, MS 105-24, Pasadena, CA 91125; , , , , , , , , , , ), AK(California Institute of Technology, MS 105-24, Pasadena, CA 91125; , , , , , , , , , , ), AL(University of California, Department of Physics, 426 LeConte Hall, Berkeley, CA 94720; ), AM(University of Chicago, Department of Astronomy and Astrophysics, 5640 South Ellis Avenue, Chicago, IL 60637; ), AN(NASA Marshall Space Flight Center, Department Space Science, SD 50, Huntsville, AL 35812; ), AO(National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801; ), AP(European Southern Observatory, Balmaceda 2536, Antofagasta, Chile; )
Publication:
The Publications of the Astronomical Society of the Pacific, Volume 114, Issue 791, pp. 83-97. (PASP Homepage)
Publication Date:
01/2002
Origin:
UCP
PASP Keywords:
Cosmology: Cosmic Microwave Background, Instrumentation: Interferometers
DOI:
10.1086/324786
Bibliographic Code:
2002PASP..114...83P

Abstract

Design and performance details are given for the Cosmic Background Imager (CBI), an interferometer array that is measuring the power spectrum of fluctuations in the cosmic microwave background radiation (CMBR) for multipoles in the range 400<l<3500. The CBI is located at an altitude of 5000 m in the Atacama Desert in northern Chile. It is a planar synthesis array with 13 0.9 m diameter antennas on a 6 m diameter tracking platform. Each antenna has a cooled, low-noise receiver operating in the 26-36 GHz band. Signals are cross-correlated in an analog filterbank correlator with 10 1 GHz bands. This allows spectral index measurements that can be used to distinguish CMBR signals from diffuse galactic foregrounds. A 1.2 kHz 180° phase-switching scheme is used to reject cross talk and low-frequency pick-up in the signal processing system. The CBI has a three-axis mount that allows the tracking platform to be rotated about the optical axis, providing improved (u, v) coverage and a powerful discriminant against false signals generated in the receiving electronics. Rotating the tracking platform also permits polarization measurements when some of the antennas are configured for the orthogonal polarization.
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