Статья

Improved Constraints on Cosmology and Foregrounds from BICEP2 and Keck Array Cosmic Microwave Background Data with Inclusion of 95 GHz Band

P. A. R. AdeSchool of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United KingdomZeeshan AhmedDepartment of Physics, Stanford University, Stanford, California 94305, USAR. W. AikinDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAK. D. AlexanderHarvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USAD. BarkatsHarvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USAS. J. BentonDepartment of Physics, University of Toronto, Toronto, Ontario, M5S 1A7, CanadaC. A. BischoffHarvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USAJ. J. BockDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USARachel Bowens-RubinHarvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USAJ. A. BrevikDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAI. BuderHarvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USAE. BullockMinnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USAV. BuzaDepartment of Physics, Harvard University, Cambridge, Massachusetts 02138, USAJ. ConnorsHarvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USAB. P. CrillJet Propulsion Laboratory, Pasadena, California 91109, USAL. DubandService des Basses Températures, Commissariat à l'Energie Atomique, 38054 Grenoble, FranceCora DvorkinDepartment of Physics, Harvard University, Cambridge, Massachusetts 02138, USAJ. P. FilippiniDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAS. FliescherSchool of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USAJ. GraysonDepartment of Physics, Stanford University, Stanford, California 94305, USAM. HalpernDepartment of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, V6T 1Z1, CanadaS. HarrisonHarvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USAG. C. HiltonNational Institute of Standards and Technology, Boulder, Colorado 80305, USAH. HuiDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAK. D. IrwinDepartment of Physics, Stanford University, Stanford, California 94305, USAK. S. KarkareHarvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USAE. KarpelDepartment of Physics, Stanford University, Stanford, California 94305, USAJ. P. KaufmanDepartment of Physics, University of California at San Diego, La Jolla, California 92093, USABrian KeatingDepartment of Physics, University of California at San Diego, La Jolla, California 92093, USAS. KefeliDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAS. A. KernasovskiyDepartment of Physics, Stanford University, Stanford, California 94305, USAJ. M. KovacDepartment of Physics, Harvard University, Cambridge, Massachusetts 02138, USAC. L. KuoDepartment of Physics, Stanford University, Stanford, California 94305, USAE. M. LeitchKavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USAM. LuekerDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAK. G. MegerianJet Propulsion Laboratory, Pasadena, California 91109, USAC. B. NetterfieldCanadian Institute for Advanced Research, Toronto, Ontario M5G 1Z8, CanadaH. T. NguyenJet Propulsion Laboratory, Pasadena, California 91109, USAR. O’BrientDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAR. W. OgburnDepartment of Physics, Stanford University, Stanford, California 94305, USAA. OrlandoDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAC. PrykeMinnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USAS. RichterHarvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USAR. SchwarzSchool of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USAC. D. SheehyKavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USAZ. StaniszewskiDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAB. SteinbachDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAR. V. SudiwalaSchool of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United KingdomG. P. TeplyDepartment of Physics, California Institute of Technology, Pasadena, California 91125, USAK. L. ThompsonDepartment of Physics, Stanford University, Stanford, California 94305, USAJ. E. TolanDepartment of Physics, Stanford University, Stanford, California 94305, USAC. TuckerSchool of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United KingdomA. D. TurnerJet Propulsion Laboratory, Pasadena, California 91109, USAA. G. ViereggDepartment of Physics, Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USAA. C. WeberJet Propulsion Laboratory, Pasadena, California 91109, USAD. V. WiebeDepartment of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, V6T 1Z1, CanadaJ. WillmertSchool of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USAC. L. WongDepartment of Physics, Harvard University, Cambridge, Massachusetts 02138, USAW. L. K. WuDepartment of Physics, Stanford University, Stanford, California 94305, USAK. W. YoonDepartment of Physics, Stanford University, Stanford, California 94305, USA

2016en

ABI

Аннотация

We present results from an analysis of all data taken by the BICEP2 and Keck Array cosmic microwave background (CMB) polarization experiments up to and including the 2014 observing season. This includes the first Keck Array observations at 95 GHz. The maps reach a depth of 50 nK deg in Stokes Q and U in the 150 GHz band and 127 nK deg in the 95 GHz band. We take auto- and cross-spectra between these maps and publicly available maps from WMAP and Planck at frequencies from 23 to 353 GHz. An excess over lensed ΛCDM is detected at modest significance in the 95×150 BB spectrum, and is consistent with the dust contribution expected from our previous work. No significant evidence for synchrotron emission is found in spectra such as 23×95, or for correlation between the dust and synchrotron sky patterns in spectra such as 23×353. We take the likelihood of all the spectra for a multicomponent model including lensed ΛCDM, dust, synchrotron, and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r) using priors on the frequency spectral behaviors of dust and synchrotron emission from previous analyses of WMAP and Planck data in other regions of the sky. This analysis yields an upper limit r_{0.05}<0.09 at 95% confidence, which is robust to variations explored in analysis and priors. Combining these B-mode results with the (more model-dependent) constraints from Planck analysis of CMB temperature plus baryon acoustic oscillations and other data yields a combined limit r_{0.05}<0.07 at 95% confidence. These are the strongest constraints to date on inflationary gravitational waves.

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Идентификаторы

DOI: 10.1103/physrevlett.116.031302

Цитирования и источники

Цитирований: 3Использованных источников: 0

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