Cosmology constraints from the weak lensing peak counts and the power spectrum in CFHTLenS data

Liu, Jia; Petri, Andrea; Haiman, Zoltán; Hui, Lam; Kratochvíl, Jan; May, M.

doi:10.1103/physrevd.91.063507

Cited by 137 publications

(110 citation statements)

References 101 publications

Supporting

Mentioning

104

Contrasting

Order By: Relevance

“…In the literature, similar comparisons have been reported by Dietrich & Hartlap (2010) using N-body simulations and by Liu et al (2015a) using CFHTLenS data. In both studies, the authors found that peak-only constraints are tighter than 2PCF-only constraints.…”

Section: Comparison With ξ ±supporting

confidence: 65%

“…Since then, many other papers have explored the efficacy of peaks for constraining both standard and nonstandard cosmological models (Marian et al 2009(Marian et al , 2011(Marian et al , 2012(Marian et al , 2013Dietrich & Hartlap 2010;Maturi et al 2010Maturi et al , 2011Pires et al 2012;Cardone et al 2013;Lin & Kilbinger 2015a,b;Lin et al 2016). Regarding recent surveys, peak analyses have also been used to derive constraints on (σ 8 , Ω m ) with CFHTLenS data (Liu et al 2015a), CFHT Stripe-82 data (Liu et al 2015b), and DES Science Verification data (Kacprzak et al 2016). Euclid will observe approximately 15 000 deg 2 of the extragalactic sky, an area about two orders of magnitude larger than CFHTLenS and the currently available DES SV data.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Cosmological constraints with weak-lensing peak counts and second-order statistics in a large-field survey

Peel

Lin

Lanusse

et al. 2017

A&A

View full text Add to dashboard Cite

Peak statistics in weak-lensing maps access the non-Gaussian information contained in the large-scale distribution of matter in the Universe. They are therefore a promising complementary probe to two-point and higher-order statistics to constrain our cosmological models. Next-generation galaxy surveys, with their advanced optics and large areas, will measure the cosmic weak-lensing signal with unprecedented precision. To prepare for these anticipated data sets, we assess the constraining power of peak counts in a simulated Euclid-like survey on the cosmological parameters Ω m , σ 8 , and w de 0 . In particular, we study how Camelus, a fast stochastic model for predicting peaks, can be applied to such large surveys. The algorithm avoids the need for time-costly N-body simulations, and its stochastic approach provides full PDF information of observables. Considering peaks with a signal-to-noise ratio ≥1, we measure the abundance histogram in a mock shear catalogue of approximately 5000 deg 2 using a multiscale mass-map filtering technique. We constrain the parameters of the mock survey using Camelus combined with approximate Bayesian computation, a robust likelihoodfree inference algorithm. Peak statistics yield a tight but significantly biased constraint in the σ 8 -Ω m plane, as measured by the width ∆Σ 8 of the 1σ contour. We find Σ 8 = σ 8 (Ω m /0.27) α = 0.77−0.05 with α = 0.75 for a flat ΛCDM model. The strong bias indicates the need to better understand and control the model systematics before applying it to a real survey of this size or larger. We perform a calibration of the model and compare results to those from the two-point correlation functions ξ ± measured on the same field. We calibrate the ξ ± result as well, since its contours are also biased, although not as severely as for peaks. In this case, we find for peaks Σ 8 = 0.76 −0.01 and α = 0.70. We conclude that the constraining power can therefore be comparable between the two weak-lensing observables in large-field surveys. Furthermore, the tilt in the σ 8 -Ω m degeneracy direction for peaks with respect to that of ξ ± suggests that a combined analysis would yield tighter constraints than either measure alone. As expected, w de 0 cannot be well constrained without a tomographic analysis, but its degeneracy directions with the other two varied parameters are still clear for both peaks and ξ ± .

show abstract

Section: Comparison With ξ ±supporting

confidence: 65%

Section: Introductionmentioning

confidence: 99%

Cosmological constraints with weak-lensing peak counts and second-order statistics in a large-field survey

Peel

Lin

Lanusse

et al. 2017

A&A

View full text Add to dashboard Cite

show abstract

“…WL peaks, on the other hand, are high signal regions, that are closely associated with massive structures along the line-of-sight (LOS). Their statistics is a simple and effective way to capture the non-Gaussian information in the WL field, and thus highly complementary to the cosmic shear 2PCF (e.g., Kruse & Schneider 1999;Dietrich & Hartlap 2010;Shan et al 2012Shan et al , 2014Marian et al 2012Marian et al , 2013Lin & Kilbinger 2015;Martinet et al 2015;Hamana et al 2015;Liu et al, 2015aLiu et al, , b, 2016Kacprzak et al 2016).…”

mentioning

confidence: 99%

KiDS-450: cosmological constraints from weak lensing peak statistics – I. Inference from analytical prediction of high signal-to-noise ratio convergence peaks

Shan

Liu

Hildebrandt

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

This paper is the first of a series of papers constraining cosmological parameters with weak lensing peak statistics using ∼ 450 deg 2 of imaging data from the Kilo Degree Survey (KiDS-450). We measure high signal-to-noise ratio (SNR: ν) weak lensing convergence peaks in the range of 3 < ν < 5, and employ theoretical models to derive expected values. These models are validated using a suite of simulations. We take into account two major systematic effects, the boost factor and the effect of baryons on the mass-concentration relation of dark matter haloes. In addition, we investigate the impacts of other potential astrophysical systematics including the projection effects of large scale structures, intrinsic galaxy alignments, as well as residual measurement uncertainties in the shear and redshift calibration. Assuming a flat ΛCDM model, we find constraints for S 8 = σ 8 (Ω m /0.3) 0.5 = 0.746−0.107 according to the degeneracy direction of the cosmic shear analysis and−0.050 based on the derived degeneracy direction of our high-SNR peak statistics. The difference between the power index of S 8 and in Σ 8 indicates that combining cosmic shear with peak statistics has the potential to break the degeneracy in σ 8 and Ω m . Our results are consistent with the cosmic shear tomographic correlation analysis of the same dataset and ∼ 2σ lower than the Planck 2016 results.

show abstract

“…By comparing the observational measurements with the templates, we can derive cosmological constraints (e.g. Dietrich & Hartlap 2010;Liu, Petri, Haiman et al 2015. Considering the large number of cosmological parameters and different physical and observational effects, such an approach can be numerically expensive.…”

Section: Introductionmentioning

confidence: 99%

Cosmological constraints from weak lensing peak statistics with Canada-France-Hawaii Telescope Stripe 82 Survey

Liu¹,

Pan²,

Li³

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We derived constraints on cosmological parameters using weak lensing peak statistics measured on the ∼ 130 deg 2 of the Canada-France-Hawaii Telescope Stripe 82 Survey (CS82). This analysis demonstrates the feasibility of using peak statistics in cosmological studies. For our measurements, we considered peaks with signal-to-noise ratio in the range of ν = [3, 6]. For a flat ΛCDM model with only (Ω m , σ 8 ) as free parameters, we constrained the parameters of the following relation Σ 8 = σ 8 (Ω m /0.27) α to be: Σ 8 = 0.82 ± 0.03 and α = 0.43 ± 0.02. The α value found is considerably smaller than the one measured in two-point and three-point cosmic shear correlation analyses, showing a significant complement of peak statistics to standard weak lensing cosmological studies. The derived constraints on (Ω m , σ 8 ) are fully consistent with the ones from either WMAP9 or Planck. From the weak lensing peak abundances alone, we obtained marginalised mean values of Ω m = 0.38 +0.27 −0.24 and σ 8 = 0.81 ± 0.26. Finally, we also explored the potential of using weak lensing peak statistics to constrain the mass-concentration relation of dark matter halos simultaneously with cosmological parameters.

show abstract

Cosmology constraints from the weak lensing peak counts and the power spectrum in CFHTLenS data

Cited by 137 publications

References 101 publications

Cosmological constraints with weak-lensing peak counts and second-order statistics in a large-field survey

Cosmological constraints with weak-lensing peak counts and second-order statistics in a large-field survey

KiDS-450: cosmological constraints from weak lensing peak statistics – I. Inference from analytical prediction of high signal-to-noise ratio convergence peaks

Cosmological constraints from weak lensing peak statistics with Canada-France-Hawaii Telescope Stripe 82 Survey

Contact Info

Product

Resources

About