Cosmological parameters from lensing power spectrum and bispectrum tomography

By M. Takada, B. Jain. 2003

288 citations recorded by the source corpus.

We examine how lensing tomography with the bispectrum and power spectrum can constrain cosmological parameters and the equation of state of dark energy. Our analysis uses the full information at the two- and three-point level from angular scales of a few degrees to 5 arcmin (50 ≤ l ≤ 3000), which will be probed by lensing surveys. We use all triangle configurations, cross-power spectra and bispectra constructed from up to three redshift bins with photometric redshifts, and all relevant covariances in our analysis. We find that the parameter constraints from bispectrum tomography are comparable to those from power spectrum tomography. Combining the two improves parameter accuracies by a factor of 3 due to their complementarity. For the dark energy parametrization w(a) = ω 0 + ω a (1 - a), the marginalized errors from lensing alone are σ(ω 0 ) ∼ 0.03f -1/2 sky and σ(ω a ) ∼ 0.1 f -1/2 sky. We show that these constraints can be further improved when combined with measurements of the cosmic microwave background or Type Ia supernovae. The amplitude and shape of the mass power spectrum are also shown to be precisely constrained. We use hyperextended perturbation theory to compute the non-linear lensing bispectrum for dark energy models. Accurate model predictions of the bispectrum in the moderately non-linear regime, calibrated with numerical simulations, will be needed to realize the parameter accuracy we have estimated. Finally, we estimate how well the lensing bispectrum can constrain a model with primordial non-Gaussianity.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9ddc437931314cab9c71648c2b3161a1ab312606

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Citations in the corpus

The impact of non‐Gaussian errors on weak lensing surveys (2008, methodology): “Photometric redshift information on source galaxies allows us to subdivide galaxies into redshift bins, enabling more cosmological information to be extracted, which is referr d to as lensing tomography (e.g., Hu 1999; Huterer 2002; Takada & Jain 2004).”
Galaxy Alignments: Observations and Impact on Cosmology (2015, methodology): “The Fisher matrix approach can be extended to make an estimate of the bias on cosmological parameters, ∆pα, when an incorrect cosmological 8http://www.euclid-ec.org/ model is assumed (Huterer et al. 2006; see also Amara & Réfrégier 2008 and Appendix A of Joachimi et al. 2011): ∆pα = ∑ β F−1αβ ∑ ` ”
Evidence of the accelerated expansion of the Universe from weak lensing tomography with COSMOS (2009, methodology): “…measured as a function of source redshift, an analysis often called weak lensing tomography or 3D weak lensing (e.g. Hu 1999, 2002; Huterer 2002; Jain & Taylor 2003; Heavens 2003; Hu & Jain 2004; Bernstein & Jain 2004; Simon et al. 2004; Takada & Jain 2004; Heavens et al. 2006; Taylor et al. 2007).”
Systematic errors in future weak-lensing surveys: requirements and prospects for self-calibration (2005, methodology): “We adopt the model described in Takada & Jain (2004) to compute the lensing bispectrum.”
SIMULATIONS OF WIDE-FIELD WEAK LENSING SURVEYS. I. BASIC STATISTICS AND NON-GAUSSIAN EFFECTS (2009, background): “The cumulative signal-to-noise ratio can be defined (e.g. Takada & Jain 2004, 2009) as ( S N )2 = ∑ l,l′≤lmax Pκ(l)Cov −1[Pκ(l), Pκ(l ′)]Pκ(l ′), (21) where Cov−1 is the inverse of the covariance matrix and the power spectrum information over 72 ∼ l ≤ lmax is included (l = 72 is the fundamental…”
The Influence of Baryons on the Clustering of Matter and Weak-Lensing Surveys (2005, background): “…the projected mass distribution and is emerging as one of the most powerful and robust probes of the large-scale structure of the universe and the nature of dark matter, dark energy, and gravity (Huterer 2002; Hu 2002; Jain & Taylor 2003; Takada & Jain 2004; Ishak et al. 2005; Knox et al. 2005).”
Nuisance hardened data compression for fast likelihood-free inference (2019, unknown): “…set of cosmological parameters θ, the predicted angular power spectra between tomographic bins α and β are given by6 (Kaiser 1992, 1998; Hu 1999, 2002; Takada & Jain 2004; Kitching et al. 2017), Cγγ `,αβ = ∫ dχ χ2 wα(χ)wβ(χ) [1 + z(χ)]2 Pδ ( ` χ ; z(χ) ) , (20) 6 In the Limber approximation,…”
Fast likelihood-free cosmology with neural density estimators and active learning (2019, unknown): “…model and parameters, the predicted angular power spectra between tomographic redshift bins α and β are given by9 (Kaiser 1992, 1998; Hu 1999, 2002; Takada & Jain 2004; Kitching et al. 2017), Cγγ `,αβ = ∫ dχ χ2 wα(χ)wβ(χ) [1 + z(χ)]2 Pδ ( ` χ ; z(χ) ) , (19) with comoving distance-redshift…”
Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, background): “The observational consequences on the weak lensing bispectrum, of a primordial non-Gaussian component (of the local type) such as the one in (IV.168), have been explored in Takada & Jain (2004).”
Primordial non-Gaussianity from the large-scale structure (2010, background): “Measurements of the lensing bispectrum could also constrain a number of non-Gaussian models [204].”
Calibrating the nonlinear matter power spectrum: Requirements for future weak lensing surveys (2004, methodology): “[Cosmological parameter extraction from WL tomography has been extensively discussed in the past, e.g. Hu 1999, Huterer 2002, Hu 2003, Refregier et al. 2003, Takada & Jain 2004, Takada & White 2004, Song & Knox 2004, Ishak et al. 2004.]”
REVISING THE HALOFIT MODEL FOR THE NONLINEAR MATTER POWER SPECTRUM (2012, methodology): “…projected along the line of sight, one can extract the redshift evolution of the fluctuations, and hence accurate information on dark energy, using a technique called lensing tomography (e.g., Hu 1999; Takada & Jain 2004) or a cross-correlation with intervening objects (e.g., Oguri & Takada 2011).”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, background): “In particular adding redshift information of source galaxies into the cosmic shear measurements, the so-called cosmic shear tomography (Hu 1999; Takada & Jain 2004), enables us to improve the cosmological constraints by lifting degeneracies among parameters.”