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Title:
CFHTLenS tomographic weak lensing cosmological parameter constraints: Mitigating the impact of intrinsic galaxy alignments
Authors:
Heymans, Catherine; Grocutt, Emma; Heavens, Alan; Kilbinger, Martin; Kitching, Thomas D.; Simpson, Fergus; Benjamin, Jonathan; Erben, Thomas; Hildebrandt, Hendrik; Hoekstra, Henk; Mellier, Yannick; Miller, Lance; Van Waerbeke, Ludovic; Brown, Michael L.; Coupon, Jean; Fu, Liping; Harnois-Déraps, Joachim; Hudson, Michael J.; Kuijken, Konrad; Rowe, Barnaby; Schrabback, Tim; Semboloni, Elisabetta; Vafaei, Sanaz; Velander, Malin
Affiliation:
AA(Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK; ), AB(Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK), AC(Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK; Imperial Centre for Inference and Cosmology, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK), AD(CEA Saclay, Service d'Astrophysique (SAp), Orme des Merisiers, Bât 709, F-91191 Gif-sur-Yvette, France; Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Germany; Universitäts-Sternwarte, Ludwig-Maximillians-Universität München, Scheinerstr. 1, D-81679 München, Germany; Institut d'Astrophysique de Paris, Université Pierre et Marie Curie - Paris 6, 98 bis Boulevard Arago, F-75014 Paris, France), AE(Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK; Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK), AF(Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK), AG(Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada), AH(Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany), AI(Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada; Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany), AJ(Leiden Observatory, Leiden University, Niels Bohrweg 2, NL-2333 CA Leiden, the Netherlands; Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2, Canada), AK(CEA Saclay, Service d'Astrophysique (SAp), Orme des Merisiers, Bât 709, F-91191 Gif-sur-Yvette, France; Institut d'Astrophysique de Paris, Université Pierre et Marie Curie - Paris 6, 98 bis Boulevard Arago, F-75014 Paris, France), AL(Department of Physics, Oxford University, Keble Road, Oxford OX1 3RH, UK), AM(Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada), AN(Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester M13 9PL, UK), AO(Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, Taipei 10617, Taiwan), AP(Key Lab for Astrophysics, Shanghai Normal University, 100 Guilin Road, 200234 Shanghai, China), AQ(Canadian Institute for Theoretical Astrophysics, University of Toronto, Ontario M5S 3H8, Canada; Department of Physics, University of Toronto, Ontario M5S 1A7, Canada), AR(Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, Canada; Perimeter Institute for Theoretical Physics, 31 Caroline Street N, Waterloo, ON N2L 1Y5, Canada), AS(Leiden Observatory, Leiden University, Niels Bohrweg 2, NL-2333 CA Leiden, the Netherlands), AT(Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK; California Institute of Technology, 1200 E California Boulevard, Pasadena, CA 91125, USA), AU(Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany; Leiden Observatory, Leiden University, Niels Bohrweg 2, NL-2333 CA Leiden, the Netherlands; Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305-4060, USA), AV(Leiden Observatory, Leiden University, Niels Bohrweg 2, NL-2333 CA Leiden, the Netherlands), AW(Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada), AX(Leiden Observatory, Leiden University, Niels Bohrweg 2, NL-2333 CA Leiden, the Netherlands; Department of Physics, Oxford University, Keble Road, Oxford OX1 3RH, UK)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 432, Issue 3, p.2433-2453 (MNRAS Homepage)
Publication Date:
07/2013
Origin:
OUP
Astronomy Keywords:
cosmology: observations
Abstract Copyright:
2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stt601
Bibliographic Code:
2013MNRAS.432.2433H

Abstract

We present a finely binned tomographic weak lensing analysis of the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS) mitigating contamination to the signal from the presence of intrinsic galaxy alignments via the simultaneous fit of a cosmological model and an intrinsic alignment model. CFHTLenS spans 154 square degrees in five optical bands, with accurate shear and photometric redshifts for a galaxy sample with a median redshift of zm = 0.70. We estimate the 21 sets of cosmic shear correlation functions associated with six redshift bins, each spanning the angular range of 1.5 < theta < 35 arcmin. We combine this CFHTLenS data with auxiliary cosmological probes: the cosmic microwave background with data from WMAP7, baryon acoustic oscillations with data from Baryon Oscillation Spectroscopic Survey and a prior on the Hubble constant from the Hubble Space Telescope distance ladder. This leads to constraints on the normalization of the matter power spectrum sigma8 = 0.799 ± 0.015 and the matter density parameter Omegam = 0.271 ± 0.010 for a flat Lambda cold dark matter (LambdaCDM) cosmology. For a flat wCDM cosmology, we constrain the dark energy equation-of-state parameter w = -1.02 ± 0.09. We also provide constraints for curved LambdaCDM and wCDM cosmologies. We find the intrinsic alignment contamination to be galaxy-type dependent with a significant intrinsic alignment signal found for early-type galaxies, in contrast to the late-type galaxy sample for which the intrinsic alignment signal is found to be consistent with zero.
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