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Published August 20, 2006 | Published
Journal Article Open

A Measurement of the CMB <EE> Spectrum from the 2003 Flight of BOOMERANG


We report measurements of the CMB polarization power spectra from the 2003 January Antarctic flight of BOOMERANG. The primary results come from 6 days of observation of a patch covering 0.22% of the sky centered near R.A. = 82°.5, decl. = -45°. The observations were made using four pairs of polarization-sensitive bolometers operating in bands centered at 145 GHz. Using two independent analysis pipelines, we measure a nonzero signal in the range 201 < l < 1000 with a significance of 4.8 σ, a 2 σ upper limit of 8.6 μK^2 for any contribution, and a 2 σ upper limit of 7.0 μK^2 for the spectrum. Estimates of foreground intensity fluctuations and the nondetection of and signals rule out any significant contribution from Galactic foregrounds. The results are consistent with a ΛCDM cosmology seeded by adiabatic perturbations. We note that this is the first detection of CMB polarization with bolometric detectors.

Additional Information

© 2006 American Astronomical Society. Received 2005 July 21; accepted 2006 May 2. We gratefully acknowledge support from CIAR, CSA, and NSERC in Canada, ASI, University La Sapienza, and PNRA in Italy, PPARC and the Leverhulme Trust in the UK, and NASA (awards NAG5-9251 and NAG5-12723) and NSF (awards OPP 99-80654 and OPP 04-07592) in the US. Additional support for detector development was provided by CIT and the Jet Propulsion Laboratory (JPL). C. B. N. acknowledges support from a Sloan Foundation Fellowship; W. C. J. and T. E. M. were partially supported by NASA GSRP Fellowships. Field, logistical, and flight support was outstandingly supplied by USAP and NSBF; data recovery was especially appreciated. This research used resources at NERSC, supported by the DOE under contract DE-AC03-76SF00098, and the MacKenzie cluster at CITA, funded by the Canada Foundation for Innovation. We also thank the CASPUR Rome, Italy) computational facilities and the Applied Cluster Computing Technologies Group at JPL for computing time and technical support. Some of the results in this paper have been derived using the HEALPix (Górski et al. 2005) package, and nearly all have benefitted from the FFTW implementation of the discrete Fourier transform (Frigo & Johnson 2005).

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