Jones, W. C. 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 Lange, A. E. and MacTavish, C. J. and Masi, S. and Mauskopf, P. D. and Melchiorri, A. and Montroy, T. E. and Natoli, P. and Netterfield, C. B. and Pascale, E. and Piacentini, F. 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 Angular Power Spectrum of the CMB Temperature Anisotropy from the 2003 Flight of BOOMERANG. Astrophysical Journal, 647 (2). pp. 823-832. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:JONapj06
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We report on observations of the cosmic microwave background (CMB) obtained during the 2003 January flight of BOOMERANG. These results are derived from 195 hr of observation with four 145 GHz polarization-sensitive bolometer (PSB) pairs, identical in design to the four 143 GHz Planck High Frequency Instrument (HFI) polarized pixels. The data include 75 hr of observations distributed over 1.84% of the sky with an additional 120 hr concentrated on the central portion of the field, which represents 0.22% of the full sky. From these data we derive an estimate of the angular power spectrum of temperature fluctuations of the CMB in 24 bands over the multipole range 50 ≤ l ≤ 1500. A series of features, consistent with those expected from acoustic oscillations in the primordial photon-baryon fluid, are clearly evident in the power spectrum, as is the exponential damping of power on scales smaller than the photon mean free path at the epoch of last scattering (l ≳ 900). As a consistency check, the collaboration has performed two fully independent analyses of the time-ordered data, which are found to be in excellent agreement.
|Additional Information:||Copyright is not claimed for this article. Printed in U.S.A. Received 2005 July 21; accepted 2006 April 28. Print publication: Issue 2 (2006 August 20). We gratefully acknowledge support from the 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 were supplied by USAP and NSBF; data recovery was particularly 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, 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 package (Górski et al. 2005), and nearly all have benefitted from the FFTW implementation of discrete Fourier transforms (Frigo & Johnson 2005). Finally, we would like to thank the referee for making significant contributions to the quality of this paper.|
|Subject Keywords:||cosmic microwave background; cosmology: observations; instrumentation: detectors|
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|Deposited On:||24 Dec 2008 21:21|
|Last Modified:||26 Dec 2012 10:40|
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