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

• Main Authors: Montroy, T. E., Ade, P. A. R., Bock, J. J., Bond, J. R., Borrill, J., Boscaleri, A., Cabella, P., Contaldi, C. R., Crill, B. P., de Bernardis, P., De Gasperis, G., De Oliveira-Costa, A., De Troia, G., Di Stefano, G., Hivon, E., Jaffe, A. H., Kisner, T. S., Jones, W. C., Lange, A. E., Masi, S., Mauskopf, P. D., MacTavish, C. J., Melchiorri, A., Natoli, P., Netterfield, C. B., Pascale, E., Piacentini, F., Pogosyan, D., Polenta, G., Prunet, S., Ricciardi, S., Romeo, G., Ruhl, J. E., Santini, P., Tegmark, M., Veneziani, M., Vittorio, N.
• Other Authors: Montroy, T. E.; Physics Department, Case Western Reserve University, Cleveland, OH, USA, Ade, P. A. R.; Dept. of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK, Bock, J. J.; Jet Propulsion Laboratory, Pasadena, CA, USA; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA, Bond, J. R.; Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, Canada, Borrill, J.; Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA; Space Sciences Laboratory, University of California, Berkeley, CA, USA, Boscaleri, A.; IFAC-CNR, Firenze, Italy, Cabella, P.; Dipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy, Contaldi, C. R.; Astrophysics Group, Imperial College, London, UK, Crill, B. P.; IPAC, California Institute of Technology, Pasadena, CA, USA, de Bernardis, P.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy, De Gasperis, G.; Dipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy, De Oliveira-Costa, A.; Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA, De Troia, G.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy, Di Stefano, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia, Hivon, E.; IPAC, California Institute of Technology, Pasadena, CA, USA, Jaffe, A. H.; Astrophysics Group, Imperial College, London, UK, Kisner, T. S.; Physics Department, Case Western Reserve University, Cleveland, OH, USA; Dept. of Physics, University of California, Santa Barbara, CA, USA, Jones, W. C.; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA, Lange, A. E.; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA, Masi, S.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy, Mauskopf, P. D.; Dept. of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK, MacTavish, C. J.; Physics Department, University of Toronto, Toronto, Ontario, Canada, Melchiorri, A.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy, Natoli, P.; Dipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy, Netterfield, C. B.; Physics Department, University of Toronto, Toronto, Ontario, Canada; Department of Astronomy and Astrophysics, University of Toronto, Toronto, Ontario, Canada, Pascale, E.; Physics Department, University of Toronto, Toronto, Ontario, Canada, Piacentini, F.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy, Pogosyan, D.; Physics Dept., University of Alberta, Edmonton, Alberta, Canada, Polenta, G.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy, Prunet, S.; Institut d’Astrophysique, Paris, France, Ricciardi, S.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy, Romeo, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia, Ruhl, J. E.; Physics Department, Case Western Reserve University, Cleveland, OH, USA, Santini, P.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy, Tegmark, M.; Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA, Veneziani, M.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy, Vittorio, N.; Dipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy, Physics Department, Case Western Reserve University, Cleveland, OH, USA, Dept. of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK, Jet Propulsion Laboratory, Pasadena, CA, USA; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA, Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, Canada, Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA; Space Sciences Laboratory, University of California, Berkeley, CA, USA, IFAC-CNR, Firenze, Italy, Dipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy, Astrophysics Group, Imperial College, London, UK, IPAC, California Institute of Technology, Pasadena, CA, USA, Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy, Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA, Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia, Physics Department, Case Western Reserve University, Cleveland, OH, USA; Dept. of Physics, University of California, Santa Barbara, CA, USA
• Format: Article in Journal/Newspaper
• Language: English
• Published: The American Astronomical Society. 2006
• Subjects: cosmic microwave background; CMB temperature anisotropy; 05. General::05.07. Space and Planetary sciences::05.07.99. General or miscellaneous; Antarctic; Antarc*
• Online Access: http://hdl.handle.net/2122/4555; http://arxiv.org/abs/astro-ph/0507514

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: ¼ 82N5, decl: ¼ 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 hEEi signal in the range 201 < l < 1000 with a significance of 4.8 , a 2 upper limit of 8.6 K2 for any hBBi contribution, and a 2 upper limit of 7.0 K2 for the hEBi spectrum. Estimates of foreground intensity fluctuations and the nondetection of hBBi and hEBi signals rule out any significant contribution from Galactic foregrounds. The results are consistent with a CDM cosmology seeded by adiabatic perturbations.We note that this is the first detection of CMB polarization with bolometric detectors. Published 813–822 2.6. TTC - Laboratorio di gravimetria, magnetismo ed elettromagnetismo in aree attive JCR Journal open