Piacentini, F. and Ade, P. A. R. and Bock, J. J. and Bond, J. R. and Borrill, J. and Boscaleri, A. and Cabella, P. and Contaldi, C. R. and Crill, B. P. and de Bernardis, P. and De Gasperis, G. and de Oliveira-Costa, A. and De Troia, G. and di Stefano, G. and Hivon, E. and Jaffe, A. H. and Kisner, T. S. and Jones, W. C. and Lange, A. E. and Masi, S. and Mauskopf, P. D. and MacTavish, C. J. and Melchiorri, A. and Montroy, T. E. and Natoli, P. and Netterfield, C. B. and Pascale, E. and Pogosyan, D. and Polenta, G. and Prunet, S. and Ricciardi, S. and Romeo, G. and Ruhl, J. E. and Santini, P. and Tegmark, M. and Veneziani, M. and Vittorio, N. (2006) A Measurement of the Polarization-Temperature Angular Cross-Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG. Astrophysical Journal, 647 (2). pp. 833-839. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:20100629-095444366
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We present a measurement of the polarization-temperature angular cross power spectra, <TE> and <TB>, of the cosmic microwave background. The result is based on ~200 hr of data from eight polarization-sensitive bolometers operating at 145 GHz during the 2003 flight of BOOMERANG. We detect a significant TE correlation in the l-range between 50 and 950 with a statistical significance of >3.5 σ. Contamination by polarized foreground emission and systematic effects are negligible in comparison with statistical uncertainties. The spectrum is consistent with previous detections and with the "concordance model" that assumes adiabatic initial conditions. This is the first measurement of polarization-temperature angular cross-power spectra using bolometric detectors.
|Additional Information:||© 2006 American Astronomical Society. Received 2005 July 21; accepted 2006 February 10. 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 CITand 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 DEAC03- 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 the JPL for computing time and technical support. Some of the results in this paper have been derived using the HEALPix (Go´rski et al. 2005) package, and nearly all have benefited from the FFTW3 implementation of fast Fourier transform (Frigo & Johnson 2005). We acknowledge the referee for useful comments. The BOOMERANG field team is also grateful to the Coffee House at McMurdo Station, Antarctica, for existing.|
|Subject Keywords:||cosmic microwave background|
|Official Citation:||F. Piacentini et al 2006 ApJ 647 833 doi: 10.1086/505557|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||29 Jun 2010 18:40|
|Last Modified:||26 Dec 2012 12:11|
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