Power Spectrum Covariance of Weak Gravitational Lensing

By A. Cooray, Wayne Hu. 2000

166 citations recorded by the source corpus.

Weak gravitational lensing observations probe the spectrum and evolution of density fluctuations and the cosmological parameters that govern them. At low redshifts, the nonlinear gravitational evolution of large-scale structure produces a non-Gaussian covariance in the shear power spectrum measurements that affects their translation into cosmological parameters. Using the dark matter halo approach, we study the covariance of binned band power spectrum estimates and the four-point function of the dark matter density field that underlies it. We compare this semianalytic estimate to results from N-body numerical simulations and find good agreement. We find that for a survey out to z ~ 1, the power spectrum covariance increases the errors on cosmological parameters determined under the Gaussian assumption by about 15%.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0e4cfc50d6d37cd49bdaf13f8b59c6dc757cf2e9

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Citations in the corpus

REJUVENATING THE MATTER POWER SPECTRUM: RESTORING INFORMATION WITH A LOGARITHMIC DENSITY MAPPING (2009, background): “Näıvely then, one expects the nonlinearities there to be weak, but the power spectrum variance and covariance are surprisingly large (Meiksin & White 1999; Scoccimarro et al. 1999; Cooray & Hu 2001).”
Weak Gravitational Lensing by Large-Scale Structure (2003, methodology): “These techniques have also been used to compute the full probability distribution function of the convergence field (Bernardeau & Valageas 2000, Munshi & Jain 2000, Valageas 2000) and the errors in two-point statistics (Cooray & Hu 2001b; Munshi & Coles 2002; Schneider et al. 2002).”
The three‐point correlation function in cosmology (2002, unknown): “…the halo approach have relied on the method built in the Fourier space (Seljak 2000; Ma & Fry 2000c; Peacock & Smith 2000; Scoccimarro et al. 2001; Cooray & Hu 2001a,b; TJ02), since the Fourier-transformed counterparts of the n-point correlation function (power spectrum, bispectrum, etc.) can be…”
Cosmological parameters from lensing power spectrum and bispectrum tomography (2003, methodology): “…studied analytic models of nonlinear clustering that we have implemented: hyper-extended perturbation theory (Scoccimarro & Frieman 1999; Scoccimarro & Couchman 2001) and the dark matter halo approach (e.g., Cooray & Hu 2001a, TJ03b,c, Takada & Hamana 2003 and Cooray & Sheth 2002 for a review).”
The impact of non‐Gaussian errors on weak lensing surveys (2008, methodology): “Once an estimator of the lensing power spectrum is defined, itis straightforward to compute the covariance (Scoccimarroet al 1999; Cooray & Hu 2001; Takada & Bridle 2007).”
The shear power spectrum from the COMBO-17 survey (2002, background): “That the shape is broadly the same for the A901 field is to be expected since this part of the nonlinear power spectrum is dominated by massive clusters (Cooray & Hu 2001).”
Systematic errors in future weak-lensing surveys: requirements and prospects for self-calibration (2005, methodology): “Finally, we do not use weak lensing information beyond ℓ = 3000 in order to avoid the effects of baryonic cooling (White 2004, Zhan & Knox 2004, Huterer & Takada 2004) and non-Gaussianity (White & Hu 2000, Cooray & Hu 2001), both of which contribute more significantly at smaller scales.”
Cosmological constraints from cosmic shear two-point correlation functions with HSC survey first-year data (2019, methodology): “In the case of the TPCF, the halo-modelbased analytic covariance matrix was formulated (Cooray & Hu 2001; Takada & Jain 2009; Takada & Hu 2013).”
Putting the precision in precision cosmology: How accurate should your data covariance matrix be? (2012, methodology): “In addition, the halo model has been used to estimate the covariance matrix for the matter and weak lensing power spectra (e.g., Cooray & Hu, 2001; Takada & Bridle, 2007; Takada & Jain 2009; Kayo et al., 2012), while estimation of the data covariance matrix for a lognormal field (e.g., Hilbert, et…”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, unknown): “This term was formulated in previous work (Cooray & Hu 2001; Takada & Jain 2003; Takada & Bridle 2007), and can be expressed as Cov(NG)(C (ij) b ,C (i′j′) b′ ) = 1 Ωsky × ∫ |`∈`b| d` A(`i) ∫ |`′∈`′ b | d`′ A(`′i) T (iji ′j′)(`,−`,`′,−`′) ' 1 Ωsky T (iji ′j′)(`b, `b, `b′ , `b′), (A22) where Ωsky is…”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: mock galaxy catalogues for the BOSS Final Data Release (2015, background): “It is also not clear that their four-point statistics will be accurate (Cooray & Hu 2001; Takada & Hu 2013).”
SIMULATIONS OF WIDE-FIELD WEAK LENSING SURVEYS. I. BASIC STATISTICS AND NON-GAUSSIAN EFFECTS (2009, methodology): “…power spectrum between Pκ(l) and Pκ(l ′) is formally expressed as a sum of the Gaussian and non-Gaussian contributions (e.g. Scoccimarro et al. 1999; Cooray & Hu 2001): Cov[Pκ(l), Pκ(l ′)] ≡ 〈( P̂κ(l) − Pκ(l) )( P̂κ(l ′) − Pκ(l ′) )〉 = 2 Nl Pκ(l) 2δKl,l′ + 1 Ωs ∫ l d2l As ∫ l′ d2l′ As′ T (l,−l,…”
COSMOLIKE - cosmological likelihood analyses for photometric galaxy surveys (2016, background): “1 generalizes the nonGaussian covariance terms previously described for cosmic shear (e.g. Cooray & Hu 2001; Sato et al. 2009; Takada & Hu 2013), and the joint analysis of cosmic shear and cluster counts (Takada & Spergel 2014; Schaan, Takada & Spergel 2014) to the set of LSS tracers considered in…”
Gravitational lensing (2010, background): “The authors of [90, 172, 442] investigated how non-Gaussianity can affect cosmological parameter estimates from the”
Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, background): “Taking the scatter in halo concentration into account boosts ũh(k) on small scales (k >∼ 10h Mpc−1) by an amount that increases with σlnc (see also Cooray & Hu 2001 and Giocoli et al. 2010b).”
An accurate halo model for fitting non-linear cosmological power spectra and baryonic feedback models (2015, background): “For example,Cooray & Hu(2001) investigate a halo model with a scatter in c(M), which typically boosts the power, whileGiocoli et al.(2010) also include the power due to halo substructure via a substructure mass function.”