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Title:
Small Angular Scale Measurements of the Cosmic Microwave Background Temperature Power Spectrum From QUaD
Authors:
Friedman, R. B.; Ade, P.; Bock, J.; Bowden, M.; Brown, M. L.; Cahill, G.; Castro, P. G.; Church, S.; Culverhouse, T.; 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.; QUa D collaboration
Affiliation:
AA(Kavli Institute for Cosmological Physics, Department of Astronomy & Astrophysics, Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ), 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, Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA ), AE(Cavendish Laboratory, University of Cambridge, J. J. Thomson Avenue, Cambridge CB3 OHE, UK ), AF(Department of Experimental Physics, National University of Ireland Maynooth, Maynooth, Co. Kildare, Republic of Ireland ), AG(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. ), AH(Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, 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, 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(Current address: 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(Current address: 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, 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, 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, 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 Letters, Volume 700, Issue 2, pp. L187-L191 (2009). (ApJL Homepage)
Publication Date:
08/2009
Origin:
IOP
ApJ Keywords:
cosmic microwave background, cosmology: observations
DOI:
10.1088/0004-637X/700/2/L187
Bibliographic Code:
2009ApJ...700L.187F

Abstract

We present measurements of the cosmic microwave background (CMB) radiation temperature anisotropy in the multipole range 2000 < ell < 3000 from the QUaD telescope's second and third observing seasons. After masking the brightest point sources our results are consistent with the primary ΛCDM expectation alone. We estimate the contribution of residual (un-masked) radio point sources using a model calibrated to our own bright source observations, and a full simulation of the source finding and masking procedure. Including this contribution slightly improves the χ2. We also fit a standard Sunyaev-Zel'dovich (SZ) template to the bandpowers and see no strong evidence of an SZ contribution, which is as expected for σ8 ≈ 0.8.
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