Weak lensing and dark energy

By D. Huterer. 2001

191 citations recorded by the source corpus.

We study the power of upcoming weak lensing surveys to probe dark energy. Dark energy modifies the distance-redshift relation as well as the matter power spectrum, both of which affect the weak lensing convergence power spectrum. Some dark-energy models predict additional clustering on very large scales, but this probably cannot be detected by weak lensing alone due to cosmic variance. With reasonable prior information on other cosmological parameters, we find that a survey covering 1000 sq deg down to a limiting magnitude of $R=27$ can impose constraints comparable to those expected from upcoming type Ia supernova and number-count surveys. This result, however, is contingent on the control of both observational and theoretical systematics. Concentrating on the latter, we find that the nonlinear power spectrum of matter perturbations and the redshift distribution of source galaxies both need to be determined accurately in order for weak lensing to achieve its full potential. Finally, we discuss the sensitivity of the three-point statistics to dark energy.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ee810acf2e2e53fd0d55b53aab79628bae6e5404

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In Astronomy and Astrophysics

1. Rachel Mandelbaum
2. H. Hoekstra
3. Simon D. M. White
4. Daniel J. Eisenstein
5. Catherine Heymans
6. C. Hirata
7. Volker Springel
8. Andrey V. Kravtsov

Citations in the corpus

• Weak Lensing Measurement of the Mass--Richness Relation of SDSS redMaPPer Clusters (2016, background): “These effects can be used to measure the relationship between dark matter and visible matter, or more generally to probe cosmological models (Bartelmann & Schneider 2001; Huterer 2002; Hu 2002; Abazajian & Dodelson 2003; Refregier 2003; Schneider 2006; Hoekstra & Jain 2008; Massey et al. 2010).”
• 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).”
• Cosmological parameters from lensing power spectrum and bispectrum tomography (2003, methodology): “Following Huterer (2002), we employ the source distribution given by ps(z) = n̄g z2 2z30 e−z/z0 , (7) with z0 = 0.5.”
• SIMULATIONS OF WIDE-FIELD WEAK LENSING SURVEYS. I. BASIC STATISTICS AND NON-GAUSSIAN EFFECTS (2009, background): “The growth rate of mass fluctuations can be measured by “lensing tomography” (e.g. Hu 1999; Huterer 2002; Takada & Jain 2004) which in turn provides tight constraints on the dark energy equation of state.”
• Dark Energy and the Accelerating Universe (2008, unknown): “Weak lensing has the potential to be the most powerful probe of dark energy in the future (Hu 2002, Huterer 2002); we discuss this in detail in Sections 7 and 8.”
• Holographic dark energy (2016, methodology): “WL can provide a direct measure of the distribution of matter (independent of any assumptions about galaxy biasing), and thus provide a useful tool to probe DE through its influence on the growth of structure [119, 120, 121, 122, 123].”
• The WiggleZ Dark Energy Survey: Direct constraints on blue galaxy intrinsic alignments at intermediate redshifts (2009, background): “…utility of these applications of lensing, plus its potential to constrain models of dark energy by splitting the sample of source galaxies into redshift slices (tomography: Hu 2002; Huterer 2002), future surveys are being planned to measure the lensing signal with sub-per cent statistical errors.”
• Systematic errors in future weak-lensing surveys: requirements and prospects for self-calibration (2005, background): “This makes weak lensing a powerful probe of cosmological parameters, including those describing dark energy (Hu & Tegmark 1999, Huterer 2002, Hu 2003a, Heavens 2003, Refregier et al. 2003, Benabed & Van Waerbeke 2004, Takada & Jain 2004, Takada & White 2004, Song & Knox 2004, Ishak et al. 2004,…”
• Cosmic structure and dark energy (2003, background): “We examine the simplified, though central, quantity of the shear linear lensing power spectrum (cf. Jain & Seljak 1997; Huterer 2002): Cℓ ∼ ∫ zs 0 dzl [ Ωm(1 + zl) ( rls rs ) G(zl) ]2 1 H(zl) rl .”
• The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, methodology): “pectra or bispectra between tomographic bins. This not only adds more constraining information, and has been recognized as the optimal method for extracting cosmological information (e.g., Hu (1999); Huterer (2002); Simon et al. (2004); Takada and Jain (2004)), but can also be used in methods to dea”
• Cosmology from the Chinese Space Station Optical Survey (CSS-OS) (2019, background): “Note that the fitting results of the cosmological parameters also depends on the number of photo-z bins (e.g. Huterer 2002).”
• Detection of large-scale intrinsic ellipticity—density correlation from the Sloan Digital Sky Survey and implications for weak lensing surveys (2005, methodology): “Also, weak lensing has been shown to be a very promising tool for precision cosmology (Hu 2002; Huterer 2002; Abazajian & Dodelson 2003; Benabed & Van Waerbeke 2004; Bernstein & Jain 2004; Ishak et al. 2004; Ishak 2005; Song & Knox 2005; Tereno et al. 2005; Upadhye et al. 2005), and has the clear…”
• The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey (2017, background): “…as a function of time - can place powerful constraints on the initial amplitude of matter fluctuations, the matter density, and the nature of dark energy (e.g., Hu 2002; Huterer 2002; Takada & Jain 2004; Benabed & van Waerbeke 2004; Bernstein & Jain 2004; Ishak et al. 2004; Takada & White 2004).”
• The impact of non‐Gaussian errors on weak lensing surveys (2008, background): “Lensing tomography refers to the use of depth information inthe source galaxies to get three-dimensional information about the lensing mass (Hu 1999; Huterer 2002; Heavens 2003; Takada & Jain 2004; Song & Knox 2004; Takada & White 2004; also see Hoekstra & Jain 2008 for a recent review).”
• Optimal Surveys for Weak Lensing Tomography (2006, background): “The impact of dark energy on gravitational lensing has been widely studied (Hu and Tegmark 1999; Huterer 2002; Jain and Taylor 2003; Song and Knox 2004; Ishak 2005; Ma et al. 2006; Taylor et al. 2006), with the effect depending on the exact nature of the dark energy considered.”
• 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.]”
• CFHTLenS tomographic weak lensing cosmological parameter constraints: Mitigating the impact of intrinsic galaxy alignments (2013, background): “This idea was explored theoretically to determine the optimal number of redshift bins (see for example Huterer 2002; Simon et al. 2004) and also significantly extended to consider a fully three-dimensional analysis (Heavens 2003).”