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Title:
Improved Measurements of the Temperature and Polarization of the Cosmic Microwave Background from QUaD
Authors:
Brown, M. L.; Ade, P.; Bock, J.; Bowden, M.; Cahill, G.; Castro, P. G.; Church, S.; Culverhouse, T.; Friedman, R. B.; Ganga, K.; Gear, W. K.; Gupta, S.; Hinderks, J.; Kovac, J.; Lange, A. E.; Leitch, E.; Melhuish, S. J.; Memari, Y.; Murphy, J. A.; Orlando, A.; O'Sullivan, C.; Piccirillo, L.; Pryke, C.; Rajguru, N.; Rusholme, B.; Schwarz, R.; Taylor, A. N.; Thompson, K. L.; Turner, A. H.; Wu, E. Y. S.; Zemcov, M.; The QUa D collaboration
Affiliation:
AA(Cavendish Astrophysics, University of Cambridge, J. J. Thomson Avenue, Cambridge CB3 OHE, UK ; Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge CB3 OHA, UK ), AB(School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK ), AC(Jet Propulsion Laboratory, 4800 Oak Grove Dr., Pasadena, CA 91109, USA ; California Institute of Technology, Pasadena, CA 91125, USA ), AD(School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK ; Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA ), AE(Department of Experimental Physics, National University of Ireland Maynooth, Maynooth, Co. Kildare, Republic of Ireland ), AF(Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK ; Current address: CENTRA, Departamento de Física, Edifício Ciência, Piso 4, Instituto Superior Técnico - IST, Universidade Técnica de Lisboa, Av. Rovisco Pais 1, 1049-001 Lisboa, Portugal ), AG(Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA ), AH(Kavli Institute for Cosmological Physics, Department of Astronomy & Astrophysics, Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ), AI(Kavli Institute for Cosmological Physics, Department of Astronomy & Astrophysics, Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ), AJ(APC/Université Paris 7-Denis Diderot/CNRS, Bâtiment Condorcet, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France ), AK(School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK ), AL(School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK ), AM(Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA ; Current address: NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA ), AN(California Institute of Technology, Pasadena, CA 91125, USA ), AO(California Institute of Technology, Pasadena, CA 91125, USA ), AP(Jet Propulsion Laboratory, 4800 Oak Grove Dr., Pasadena, CA 91109, USA ; California Institute of Technology, Pasadena, CA 91125, USA ), AQ(School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK ), AR(Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK ), AS(Department of Experimental Physics, National University of Ireland Maynooth, Maynooth, Co. Kildare, Republic of Ireland ), AT(School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK ; California Institute of Technology, Pasadena, CA 91125, USA ), AU(Department of Experimental Physics, National University of Ireland Maynooth, Maynooth, Co. Kildare, Republic of Ireland ), AV(School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK ), AW(Kavli Institute for Cosmological Physics, Department of Astronomy & Astrophysics, Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ), AX(School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK ; Current address: Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK ), AY(Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA ; Current address: Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA), AZ(Kavli Institute for Cosmological Physics, Department of Astronomy & Astrophysics, Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ), BA(Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK ), BB(Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA ), BC(School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK ), BD(Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA ), BE(School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK ; Jet Propulsion Laboratory, 4800 Oak Grove Dr., Pasadena, CA 91109, USA ; California Institute of Technology, Pasadena, CA 91125, USA ), BF()
Publication:
The Astrophysical Journal, Volume 705, Issue 1, pp. 978-999 (2009). (ApJ Homepage)
Publication Date:
11/2009
Origin:
IOP
ApJ Keywords:
cosmic microwave background, cosmological parameters, cosmology: observations, polarization
DOI:
10.1088/0004-637X/705/1/978
Bibliographic Code:
2009ApJ...705..978B

Abstract

We present an improved analysis of the final data set from the QUaD experiment. Using an improved technique to remove ground contamination, we double the effective sky area and hence increase the precision of our cosmic microwave background (CMB) power spectrum measurements by ~30% versus that previously reported. In addition, we have improved our modeling of the instrument beams and have reduced our absolute calibration uncertainty from 5% to 3.5% in temperature. The robustness of our results is confirmed through extensive jackknife tests, and by way of the agreement that we find between our two fully independent analysis pipelines. For the standard six-parameter ΛCDM model, the addition of QUaD data marginally improves the constraints on a number of cosmological parameters over those obtained from the WMAP experiment alone. The impact of QUaD data is significantly greater for a model extended to include either a running in the scalar spectral index, or a possible tensor component, or both. Adding both the QUaD data and the results from the Arcminute Cosmology Bolometer Array Receiver experiment, the uncertainty in the spectral index running is reduced by ~25% compared to WMAP alone, while the upper limit on the tensor-to-scalar ratio is reduced from r < 0.48 to r < 0.33 (95% c.l.). This is the strongest limit on tensors to date from the CMB alone. We also use our polarization measurements to place constraints on parity-violating interactions to the surface of last scattering, constraining the energy scale of Lorentz violating interactions to <1.5 × 10-43 GeV (68% c.l.). Finally, we place a robust upper limit on the strength of the lensing B-mode signal. Assuming a single flat band power between ell = 200 and ell = 2000, we constrain the amplitude of B-modes to be <0.57 μK2 (95% c.l.).
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