First season QUaD CMB temperature and polarization power spectra

Creators: Ade, P.; Bock, J.; Bowden, M.; Brown, M. L.; Cahill, V.; Carlstrom, J. E.; Castro, P. G.; Church, S.; Culverhouse, T.; Friedman, R.; Ganga, K.; Gear, W. K.; Hinderks, J.; Kovac, J.; Lange, A. E.; Leitch, E. M.; Melhuish, S. J.; Murphy, J. A.; Orlando, A.; Schwarz, R.; O'Sullivan, C.; Piccirillo, L.; Pryke, C.; Rajguru, N.; Rusholme, B.; Taylor, A. N.; Thompson, K. L.; Wu, E. Y. S.; Zemcov, M.

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Abstract

QUaD is a bolometric CMB polarimeter sited at the South Pole, operating at frequencies of 100 and 150 GHz. In this paper we report preliminary results from the first season of operation (austral winter 2005). All six CMB power spectra are presented derived as cross spectra between the 100 and 150 GHz maps using 67 days of observation in a low foreground region of approximately 60 deg^2. These data are a small fraction of the data acquired to date. The measured spectra are consistent with the ΛCDM cosmological model. We perform jackknife tests that indicate that the observed signal has negligible contamination from instrumental systematics. In addition, by using a frequency jackknife we find no evidence for foreground contamination.

Additional Information

© 2008 American Astronomical Society. Received 2007 May 16; accepted 2007 October 24. QUaD is funded by the National Science Foundation in the USA, through grants AST-0096778, ANT-0338138, ANT-0338335, and ANT-0338238, by the Particle Physics and Astronomy Research Council in the UK, and by the Science Foundation Ireland. We would like to thank the staff of the Amundsen-Scott South Pole Station and all involved in the United States Antarctic Program for the superb support operation that makes the science presented here possible. Special thanks go to our intrepid winter-over scientist Robert Schwarz, who has spent three consecutive winter seasons tending the QUaD experiment. The BOOMERANG collaboration kindly allowed the use of their CMB maps for our calibration purposes. M.L.B. acknowledges the award of a PPARC fellowship. S.E.C. acknowledges support from a Stanford Terman Fellowship. J.R.H. acknowledges the support of an NSF Graduate Research Fellowship and a Stanford Graduate Fellowship. C.P. and J.E.C. acknowledge partial support from the Kavli Institute for Cosmological Physics through the grant NSF PHY-0114422. E.Y.W. acknowledges receipt of an NDSEG fellowship.

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