3D weak lensing

By Alan Heavens. 2003

144 citations recorded by the source corpus.

I propose an analysis method, based on spin-spherical harmonics and spherical Bessel functions, for large-scale weak lensing surveys which have source-distance information through photometric redshifts. I show that the distance information can significantly reduce statistical errors on cosmological parameters; in particular, 3D lensing analysis offers excellent prospects for constraining the equation of state of the vacuum energy which dominates the energy density of the Universe. I show that the ratio of pressure to energy density could be determined to an accuracy of ∼1 per cent or better. Having distance information also offers significant advantages in the control of systematic effects such as the intrinsic alignment of galaxies. The case for obtaining photometric redshifts is therefore compelling. A signal-to-noise eigenmode analysis of the modes shows that the modes with highest signal-to-noise ratio correspond quite closely to ignoring the redshift information, but there is significant extra information from a few radial modes. These modes are generally long-wavelength, suggesting that useful information can be gleaned even if the photometric redshifts are relatively inaccurate.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/59d7a35b1e9171715addacb77c0d5a37bc453d5f

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Citations in the corpus

Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “The change in shape and oscillatory features introduced in the power spectrum allow the sound speed parameter to be constrained very well by Euclid, using 3D weak lensing [577, 672] with errors ∼ 10−5 [see also 265, 266].”
Results of the GREAT08 Challenge?: an image analysis competition for cosmological lensing: Results o (2009, background): “For example, three-dimensional lensing (Heavens 2003; Kitching et al. 2008a) is specifically designed to take into account the probability distributions in redshift and shear for each galaxy separately.”
Weak Gravitational Lensing (2012, background): “The 3D gravitational potential Φ can be reconstructed using the weak lensing measurements together with the redshifts for all galaxies of the field [90, 89, 3, 27, 91].”
Accurate halo-model matter power spectra with dark energy, massive neutrinos and modified gravitational forces (2016, background): “This angular scale mixing means that the clean, linear signal is difficult to isolate (although isolation can be partially achieved using tomographic or full 3D lensing Heavens 2003; Heymans et al. 2013; Kitching et al. 2014).”
Gravitational lensing (2010, unknown): “[175] developed an elegant formalism for extracting three-dimensional information from weak-lensing data (see also [385]), and [472] recovered the three-dimensional matter distribution in the field of the Combo-17 survey, using photometric redshifts as distance indicators for the source galaxies.”
Cosmic dynamics in the era of Extremely Large Telescopes (2008, background): “…history include distances and the linear growth of density perturbations (Linder & Jenkins 2003; Linder 2005), and so SNIa surveys, weak lensing (Heavens 2003; Jain & Taylor 2003) and baryon acoustic oscillations (BAOs) in the galaxy power spectrum (Seo & Eisenstein 2003; Wang 2006) are…”
The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, methodology): “Croft and Metzler (2000); Heavens et al. (2000)). They compared results from these two models for galaxy ellipticity to observations by Mandelbaum et al. (2006a), and provided parameterized fitting formulae for the correlation results. Following Heymans et al. (2004), Heymans et al. (2006) parameter”
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).”
The Shear Testing Programme – I. Weak lensing analysis of simulated ground-based observations (2005, background): “Contamination to cosmic shear analyses from the intrinsic galaxy alignment of nearby galaxies is currently thought to be a weak effect that is measured and mitigated in Heymans et al. (2004) (also see King & Schneider 2002, 2003; Heymans & Heavens 2003, and references therein).”
On model selection forecasting, Dark Energy and modified gravity (2007, methodology): “For all surveys we assume flatness and a redshift dependence of source density n(z) ∝ z2 exp [ −(z/z∗)1.5 ] , with z∗ = 1.4zm and use the 3D weak shear power spectrum analysis method of Heavens (2003) and Heavens, Kitching & Taylor (2006).”
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).”
CFHTLenS tomographic weak lensing cosmological parameter constraints: Mitigating the impact of intrinsic galaxy alignments (2013, methodology): “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).”
Cosmological parameters from lensing power spectrum and bispectrum tomography (2003, background): “Another useful application of photometric redshift information is that it allows us to remove intrinsic alignment contaminations by excluding close pairs of galaxies in the same redshift bin (Heymans & Heavens 2003; King & Schneider 2003).”
Systematic errors in future weak-lensing surveys: requirements and prospects for self-calibration (2005, background): “…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, Ishak…”
Galaxy Alignments: Observations and Impact on Cosmology (2015, methodology): “comparable samples in Hirata et al. (2007) and Joachimi et al.”