TY - JOUR

T1 - CFHTLenS: combined probe cosmological model comparison using 2D weak gravitational lensing

AU - Kilbinger, Martin

AU - Fu, Liping

AU - Heymans, Catherine

AU - Simpson, Fergus

AU - Benjamin, Jonathan

AU - Erben, Thomas

AU - Harnois-Deraps, Joachim

AU - Hoekstra, Henk

AU - Hildebrandt, Hendrik

AU - Kitching, Thomas D.

AU - Mellier, Yannick

AU - Miller, Lance

AU - Van Waerbeke, Ludovic

AU - Benabed, Karim

AU - Bonnett, Christopher

AU - Coupon, Jean

AU - Hudson, Michael J.

AU - Kuijken, Konrad

AU - Rowe, Barnaby

AU - Schrabback, Tim

AU - Semboloni, Elisabetta

AU - Vafaei, Sanaz

AU - Velander, Malin

PY - 2013/4

Y1 - 2013/4

N2 - We present cosmological constraints from 2D weak gravitational lensing by the large-scale structure in the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS) which spans 154 deg(2) in five optical bands. Using accurate photometric redshifts and measured shapes for 4.2 million galaxies between redshifts of 0.2 and 1.3, we compute the 2D cosmic shear correlation function over angular scales ranging between 0.8 and 350 arcmin. Using non-linear models of the dark-matter power spectrum, we constrain cosmological parameters by exploring the parameter space with Population Monte Carlo sampling. The best constraints from lensing alone are obtained for the small-scale density-fluctuations amplitude sigma(8) scaled with the total matter density Omega(m). For a flat Lambda cold dark matter (Lambda CDM) model we obtain sigma(8)(Omega(m)/0.27)(0.6) = 0.79 +/- 0.03.We combine the CFHTLenS data with 7-year Wilkinson Microwave Anisotropy Probe (WMAP7), baryonic acoustic oscillations (BAO): SDSS-III (BOSS) and a Hubble Space Telescope distance-ladder prior on the Hubble constant to get joint constraints. For a flat Lambda CDM model, we find Omega(m) = 0.283 +/- 0.010 and sigma(8) = 0.813 +/- 0.014. In the case of a curved wCDM universe, we obtain Omega(m) = 0.27 +/- 0.03, sigma(8) = 0.83 +/- 0.04, w(0) = -1.10 +/- 0.15 and Omega(K) = 0.006(-0.004)(+0.006).We calculate the Bayesian evidence to compare flat and curved Lambda CDM and dark-energy CDM models. From the combination of all four probes, we find models with curvature to be at moderately disfavoured with respect to the flat case. A simple dark-energy model is indistinguishable from Lambda CDM. Our results therefore do not necessitate any deviations from the standard cosmological model.

AB - We present cosmological constraints from 2D weak gravitational lensing by the large-scale structure in the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS) which spans 154 deg(2) in five optical bands. Using accurate photometric redshifts and measured shapes for 4.2 million galaxies between redshifts of 0.2 and 1.3, we compute the 2D cosmic shear correlation function over angular scales ranging between 0.8 and 350 arcmin. Using non-linear models of the dark-matter power spectrum, we constrain cosmological parameters by exploring the parameter space with Population Monte Carlo sampling. The best constraints from lensing alone are obtained for the small-scale density-fluctuations amplitude sigma(8) scaled with the total matter density Omega(m). For a flat Lambda cold dark matter (Lambda CDM) model we obtain sigma(8)(Omega(m)/0.27)(0.6) = 0.79 +/- 0.03.We combine the CFHTLenS data with 7-year Wilkinson Microwave Anisotropy Probe (WMAP7), baryonic acoustic oscillations (BAO): SDSS-III (BOSS) and a Hubble Space Telescope distance-ladder prior on the Hubble constant to get joint constraints. For a flat Lambda CDM model, we find Omega(m) = 0.283 +/- 0.010 and sigma(8) = 0.813 +/- 0.014. In the case of a curved wCDM universe, we obtain Omega(m) = 0.27 +/- 0.03, sigma(8) = 0.83 +/- 0.04, w(0) = -1.10 +/- 0.15 and Omega(K) = 0.006(-0.004)(+0.006).We calculate the Bayesian evidence to compare flat and curved Lambda CDM and dark-energy CDM models. From the combination of all four probes, we find models with curvature to be at moderately disfavoured with respect to the flat case. A simple dark-energy model is indistinguishable from Lambda CDM. Our results therefore do not necessitate any deviations from the standard cosmological model.

KW - methods: statistical

KW - cosmological parameters

KW - MATTER POWER SPECTRUM

KW - SHEAR CORRELATION-FUNCTIONS

KW - DARK-ENERGY CONSTRAINTS

KW - POPULATION MONTE-CARLO

KW - HUBBLE-SPACE-TELESCOPE

KW - COSMIC SHEAR

KW - PHOTOMETRIC REDSHIFTS

KW - COVARIANCE-MATRIX

KW - LEGACY SURVEY

KW - INTRINSIC ALIGNMENTS

U2 - 10.1093/mnras/stt041

DO - 10.1093/mnras/stt041

M3 - Article

VL - 430

SP - 2200

EP - 2220

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -