Dark-energy constraints and correlations with systematics from CFHTLS weak lensing, SNLS supernovae Ia and WMAP5

Kilbinger, M.; Benabed, K.; Guy, J.; Astier, P.; Tereno, I.; Fu, Liping; Wraith, Darren; Coupon, J.; Mellier, Y.; Balland, C.; Bouchet, F. R.; Hamana, Takashi; Hardin, D.; McCracken, H. J.; Pain, R.; Regnault, Nicolas; Schultheis, M.; Yahagi, Hideki

doi:10.1051/0004-6361/200811247

Cited by 125 publications

(124 citation statements)

References 68 publications

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“…In particular, the combination σ 8 Ω 0. 6 M , where σ 8 is the amplitude of mass fluctuations, is measured to about 5-10% from the ground [82,78] and ∼15% from space [83], and is in concordance with values of Ω M ≃ 0.25 and σ 8 ≃ 0.8. An example adopted from Ref.…”

Section: ωM σ8supporting

confidence: 69%

Weak lensing, dark matter and dark energy

Huterer

2010

Gen Relativ Gravit

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Weak gravitational lensing is rapidly becoming one of the principal probes of dark matter and dark energy in the universe. In this brief review we outline how weak lensing helps determine the structure of dark matter halos, measure the expansion rate of the universe, and distinguish between modified gravity and dark energy explanations for the acceleration of the universe. We also discuss requirements on the control of systematic errors so that the systematics do not appreciably degrade the power of weak lensing as a cosmological probe.

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Section: ωM σ8supporting

confidence: 69%

Weak lensing, dark matter and dark energy

Huterer

2010

Gen Relativ Gravit

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“…Having eliminated this last source of systematic uncertainty, we now estimate joint constraints with WMAP-5 CMB-only data ), conducted similarly to the analysis by Kilbinger et al (2009a). Here we assume a flat ΛCDM cosmology, completely relax our priors to (68.3%/95.4% conf., MS-calib.…”

Section: Flat W Cdm Cosmologymentioning

confidence: 99%

Evidence of the accelerated expansion of the Universe from weak lensing tomography with COSMOS

Schrabback

Hartlap

Joachimi

et al. 2010

A&A

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We present a comprehensive analysis of weak gravitational lensing by large-scale structure in the Hubble Space Telescope Cosmic Evolution Survey (COSMOS), in which we combine space-based galaxy shape measurements with ground-based photometric redshifts to study the redshift dependence of the lensing signal and constrain cosmological parameters. After applying our weak lensingoptimized data reduction, principal-component interpolation for the spatially, and temporally varying ACS point-spread function, and improved modelling of charge-transfer inefficiency, we measured a lensing signal that is consistent with pure gravitational modes and no significant shape systematics. We carefully estimated the statistical uncertainty from simulated COSMOS-like fields obtained from ray-tracing through the Millennium Simulation, including the full non-Gaussian sampling variance. We tested our lensing pipeline on simulated space-based data, recalibrated non-linear power spectrum corrections using the ray-tracing analysis, employed photometric redshift information to reduce potential contamination by intrinsic galaxy alignments, and marginalized over systematic uncertainties. We find that the weak lensing signal scales with redshift as expected from general relativity for a concordance ΛCDM cosmology, including the full cross-correlations between different redshift bins. Assuming a flat ΛCDM cosmology, we measure σ 8 (Ω m /0.3) 0.51 = 0.75 ± 0.08 from lensing, in perfect agreement with WMAP-5, yielding joint constraints Ω m = 0.266 +0.025 −0.023 , σ 8 = 0.802 +0.028 −0.029 (all 68.3% conf.). Dropping the assumption of flatness and using priors from the HST Key Project and Big-Bang nucleosynthesis only, we find a negative deceleration parameter q 0 at 94.3% confidence from the tomographic lensing analysis, providing independent evidence of the accelerated expansion of the Universe. For a flat wCDM cosmology and prior w ∈ [−2, 0], we obtain w < −0.41 (90% conf.). Our dark energy constraints are still relatively weak solely due to the limited area of COSMOS. However, they provide an important demonstration of the usefulness of tomographic weak lensing measurements from space.

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“…Modelling of some of the CFHTLS-T0003 systematics is included in the analysis of Kilbinger et al (2009).…”

Section: Robustness Of the Constraintsmentioning

confidence: 99%

CFHTLS weak-lensing constraints on the neutrino masses

Tereno

Schimd

Uzan

et al. 2009

A&A

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Context. Oscillation experiments yield strong evidence that at least some neutrinos are massive. As a hot dark-matter component, massive neutrinos should modify the expansion history of the Universe as well as the evolution of cosmological perturbations, in a different way from cold dark matter or dark energy. Aims. We use the latest release of CFHTLS cosmic-shear data to constrain the sum of the masses m ν of neutrinos, assuming three degenerate mass states. We also consider a joint analysis including other cosmological observables, notably CMB anisotropies, baryonic acoustic oscillations, and distance modulus from type Ia supernovae. Methods. Combining CAMB with a lensing code, we compute the aperture mass variance using a suitable recipe to deal with matter perturbations in the non-linear regime. The statistical analysis is performed by sampling an 8-dimensional likelihood on a regular grid as well as using the importance sampling technique. Results. We obtain the first constraint on neutrino masses based on cosmic-shear data, and combine CFHTLS with WMAP, SDSS, 2dFGRS, Gold-set, and SNLS data. The joint analysis yields 0.03 eV < m ν < 0.54 eV at the 95% confidence level. The preference for massive neutrinos vanishes when systematics are included.

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Dark-energy constraints and correlations with systematics from CFHTLS weak lensing, SNLS supernovae Ia and WMAP5

Cited by 125 publications

References 68 publications

Weak lensing, dark matter and dark energy

Weak lensing, dark matter and dark energy

Evidence of the accelerated expansion of the Universe from weak lensing tomography with COSMOS

CFHTLS weak-lensing constraints on the neutrino masses

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