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Detection of B-mode polarization at degree angular scales by BICEP2.
Ade, P A R; Aikin, R W; Barkats, D; Benton, S J; Bischoff, C A; Bock, J J; Brevik, J A; Buder, I; Bullock, E; Dowell, C D; Duband, L; Filippini, J P; Fliescher, S; Golwala, S R; Halpern, M; Hasselfield, M; Hildebrandt, S R; Hilton, G C; Hristov, V V; Irwin, K D; Karkare, K S; Kaufman, J P; Keating, B G; Kernasovskiy, S A; Kovac, J M; Kuo, C L; Leitch, E M; Lueker, M; Mason, P; Netterfield, C B; Nguyen, H T; O'Brient, R; Ogburn, R W; Orlando, A; Pryke, C; Reintsema, C D; Richter, S; Schwarz, R; Sheehy, C D; Staniszewski, Z K; Sudiwala, R V; Teply, G P; Tolan, J E; Turner, A D; Vieregg, A G; Wong, C L; Yoon, K W.
Afiliación
  • Ade PA; School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United Kingdom.
  • Aikin RW; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
  • Barkats D; Joint ALMA Observatory, Vitacura, Santiago, Chile.
  • Benton SJ; Department of Physics, University of Toronto, Toronto, Ontario, M5S 1A7, Canada.
  • Bischoff CA; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA.
  • Bock JJ; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA and Jet Propulsion Laboratory, Pasadena, California 91109, USA.
  • Brevik JA; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
  • Buder I; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA.
  • Bullock E; Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USA.
  • Dowell CD; Jet Propulsion Laboratory, Pasadena, California 91109, USA.
  • Duband L; Service des Basses Températures, Commissariat à l'Energie Atomique, 38054 Grenoble, France.
  • Filippini JP; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
  • Fliescher S; Department of Physics, University of Minnesota, Minneapolis, Minnesota 55455, USA.
  • Golwala SR; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
  • Halpern M; Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, V6T 1Z1, Canada.
  • Hasselfield M; Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, V6T 1Z1, Canada.
  • Hildebrandt SR; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA and Jet Propulsion Laboratory, Pasadena, California 91109, USA.
  • Hilton GC; National Institute of Standards and Technology, Boulder, Colorado 80305, USA.
  • Hristov VV; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
  • Irwin KD; National Institute of Standards and Technology, Boulder, Colorado 80305, USA and Department of Physics, Stanford University, Stanford, California 94305, USA and Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California
  • Karkare KS; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA.
  • Kaufman JP; Department of Physics, University of California at San Diego, La Jolla, California 92093, USA.
  • Keating BG; Department of Physics, University of California at San Diego, La Jolla, California 92093, USA.
  • Kernasovskiy SA; Department of Physics, Stanford University, Stanford, California 94305, USA.
  • Kovac JM; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA.
  • Kuo CL; Department of Physics, Stanford University, Stanford, California 94305, USA and Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA.
  • Leitch EM; University of Chicago, Chicago, Illinois 60637, USA.
  • Lueker M; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
  • Mason P; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
  • Netterfield CB; Department of Physics, University of Toronto, Toronto, Ontario, M5S 1A7, Canada and Canadian Institute for Advanced Research, Toronto, Ontario, M5G 1Z8, Canada.
  • Nguyen HT; Jet Propulsion Laboratory, Pasadena, California 91109, USA.
  • O'Brient R; Jet Propulsion Laboratory, Pasadena, California 91109, USA.
  • Ogburn RW; Department of Physics, Stanford University, Stanford, California 94305, USA and Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA.
  • Orlando A; Department of Physics, University of California at San Diego, La Jolla, California 92093, USA.
  • Pryke C; Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USA and Department of Physics, University of Minnesota, Minneapolis, Minnesota 55455, USA.
  • Reintsema CD; National Institute of Standards and Technology, Boulder, Colorado 80305, USA.
  • Richter S; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA.
  • Schwarz R; Department of Physics, University of Minnesota, Minneapolis, Minnesota 55455, USA.
  • Sheehy CD; Department of Physics, University of Minnesota, Minneapolis, Minnesota 55455, USA and University of Chicago, Chicago, Illinois 60637, USA.
  • Staniszewski ZK; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA and Jet Propulsion Laboratory, Pasadena, California 91109, USA.
  • Sudiwala RV; School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United Kingdom.
  • Teply GP; Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
  • Tolan JE; Department of Physics, Stanford University, Stanford, California 94305, USA.
  • Turner AD; Jet Propulsion Laboratory, Pasadena, California 91109, USA.
  • Vieregg AG; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA and University of Chicago, Chicago, Illinois 60637, USA.
  • Wong CL; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA.
  • Yoon KW; Department of Physics, Stanford University, Stanford, California 94305, USA and Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA.
Phys Rev Lett ; 112(24): 241101, 2014 Jun 20.
Article en En | MEDLINE | ID: mdl-24996078
ABSTRACT
We report results from the BICEP2 experiment, a cosmic microwave background (CMB) polarimeter specifically designed to search for the signal of inflationary gravitational waves in the B-mode power spectrum around ℓ∼80. The telescope comprised a 26 cm aperture all-cold refracting optical system equipped with a focal plane of 512 antenna coupled transition edge sensor 150 GHz bolometers each with temperature sensitivity of ≈300 µK(CMB)√s. BICEP2 observed from the South Pole for three seasons from 2010 to 2012. A low-foreground region of sky with an effective area of 380 square deg was observed to a depth of 87 nK deg in Stokes Q and U. In this paper we describe the observations, data reduction, maps, simulations, and results. We find an excess of B-mode power over the base lensed-ΛCDM expectation in the range 30 < ℓ < 150, inconsistent with the null hypothesis at a significance of >5σ. Through jackknife tests and simulations based on detailed calibration measurements we show that systematic contamination is much smaller than the observed excess. Cross correlating against WMAP 23 GHz maps we find that Galactic synchrotron makes a negligible contribution to the observed signal. We also examine a number of available models of polarized dust emission and find that at their default parameter values they predict power ∼(5-10)× smaller than the observed excess signal (with no significant cross-correlation with our maps). However, these models are not sufficiently constrained by external public data to exclude the possibility of dust emission bright enough to explain the entire excess signal. Cross correlating BICEP2 against 100 GHz maps from the BICEP1 experiment, the excess signal is confirmed with 3σ significance and its spectral index is found to be consistent with that of the CMB, disfavoring dust at 1.7σ. The observed B-mode power spectrum is well fit by a lensed-ΛCDM+tensor theoretical model with tensor-to-scalar ratio r = 0.20_(-0.05)(+0.07), with r = 0 disfavored at 7.0σ. Accounting for the contribution of foreground, dust will shift this value downward by an amount which will be better constrained with upcoming data sets.
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Colección: 01-internacional Banco de datos: MEDLINE Tipo de estudio: Diagnostic_studies / Prognostic_studies Idioma: En Revista: Phys Rev Lett Año: 2014 Tipo del documento: Article País de afiliación: Reino Unido
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Colección: 01-internacional Banco de datos: MEDLINE Tipo de estudio: Diagnostic_studies / Prognostic_studies Idioma: En Revista: Phys Rev Lett Año: 2014 Tipo del documento: Article País de afiliación: Reino Unido