Joint galaxy - lensing observables and the dark energy

By Wayne Hu, B. Jain. 2003

196 citations recorded by the source corpus.

Deep multicolor galaxy surveys with photometric redshifts will provide a large number of two-point correlation observables: galaxy-galaxy angular correlations, galaxy-shear cross correlations, and shear-shear correlations between all redshifts. These observables can potentially enable a joint determination of the dark-energy-dependent evolution of the dark matter and distances as well as the relationship between galaxies and dark matter halos. With recent cosmic microwave background determinations of the initial power spectrum, a measurement of the mass clustering at even a single redshift will constrain a well-specified combination of dark energy (DE) parameters in a flat universe; we provide convenient fitting formulas for such studies. The combination of galaxy-shear and galaxy-galaxy correlations can determine this amplitude at multiple redshifts. We illustrate this ability in a description of the galaxy clustering with 5 free functions of redshift which can be fitted from the data. The galaxy modeling is based on a mapping onto halos of the same abundance that models a flux-limited selection. In this context and under a flat geometry, a 4000 deg${}^{2}$ galaxy-lensing survey can achieve a statistical precision of $\ensuremath{\sigma}({\ensuremath{\Omega}}_{\mathrm{DE}})=0.005$ for the dark energy density, $\ensuremath{\sigma}{(w}_{\mathrm{DE}})=0.02$ and $\ensuremath{\sigma}{(w}_{a})=0.17$ for its equation of state and evolution, evaluated at dark energy matter equality $z\ensuremath{\approx}0.4,$ as well as constraints on the 5 halo functions out to $z=1.$ More importantly, a joint analysis can make dark energy constraints robust against systematic errors in the shear-shear correlation and halo modeling.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/625a4bcac64693f3098c0ab709c471078521d272

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Citations in the corpus

Dark energy constraints from cosmic shear power spectra: impact of intrinsic alignments on photometric redshift requirements (2007, methodology): “This could come from better numerical simulations or from observations of the galaxy-shear and galaxy-galaxy cross correlation functions such as those by Mandelbaum et al. (2006); Hirata et al. (2007) or as suggested by Hu and Jain (2004).”
Constraints on intrinsic alignment contamination of weak lensing surveys using the MegaZ-LRG sample (2010, unknown): “…densityshape cross-correlations, we proceed in exact analogy and compute the three-dimensional correlation functionξphotgg (r̄p, Π̄, z̄m) from (e.g. Hu & Jain 2004) ξ ang gg (θ; z̄1, z̄2) = ∫ ∞ 0 dℓ ℓ 2π J0 (ℓθ) Cgg (ℓ; z̄1, z̄2) , (10) again by means of (A.11), where the angular power…”
Constraining primordial non-Gaussianity with future galaxy surveys (2011, methodology): “(20) yields (Hu & Jain 2004; Amara & Refregier 2007) F αβ = fsky lmax∑ l=lmin (2l + 1) 2 Tr [ D lα ( C̃ l )−1 D lβ ( C̃ l )−1] , (30) where fsky is the sky coverage of the survey.”
LSST: From Science Drivers to Reference Design and Anticipated Data Products (2008, background): “The joint analysis of LSST weak lensing and BAO is particularly powerful in constraining the dynamical behavior of dark energy, i.e., how it evolves with cosmic time or redshift (Hu & Jain 2004; Zhan 2006).”
Observational probes of cosmic acceleration (2012, methodology): “This formula, similar to that in Hu and Jain (2004), is found by varying the parameters in CAMB calculations around the WMAP7 mean values one at a time to evaluate logarithmic derivatives; spot checks indicate that it is accurate to 0.2% over the 2σ range of the WMAP7 errors, and for the range of w…”
COSMOLIKE - cosmological likelihood analyses for photometric galaxy surveys (2016, methodology): “In this section, we summarize the computation of angular (cross) power spectra for the different probes; a more detailed derivation can be found in Hu & Jain (2004).”
Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, background): “The pivot scale factor ap is defined as the point where equation (24) is minimized (Huterer & Turner 2001; Hu & Jain 2004; Albretch et al. 2006), that is ap = 1 + 〈δw0δwa〉〈 δw2a 〉 .”
Optimal Surveys for Weak Lensing Tomography (2006, methodology): “The Fisher matrix for the shear power spectrum tomography is given by (Hu and Jain 2004) Fαβ = fsky ∑ l (2l + 1)∆l 2 Tr[DlαC̃ −1 l DlβC̃ −1 l ], (2) where the sum is over bands of multipole l of width ∆l, Tr stands for the trace, and fsky is the fraction of sky covered by the survey.”
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).”
CHANDRA CLUSTER COSMOLOGY PROJECT III: COSMOLOGICAL PARAMETER CONSTRAINTS (2008, methodology): “A useful accurate tting formula can also 10 VIKHLININ ET AL. be found in Hu & Jain (2004): ∆̃R ≈ σ8 1.79 × 104 ( Ωbh2 0.024 ) 1/3 (ΩMh 2 0.14 ) −0.563 × (7.808 h)(1−n)/2 ( h 0.72 ) −0.693 0.76 G0 (3) (we adjusted numerical coe cients to take into account that the Hu & Jain approximation uses the…”
DESI and other Dark Energy experiments in the era of neutrino mass measurements (2013, background): “For weak lensing, the weight function is [122]:”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “Explicit expressions for the Fisher matrix for cosmological observables can be found in [1155] for cosmic microwave background data, in [1151] for the matter power spectrum from galaxy redshift surveys (applied to baryonic acoustic oscillations in [1075] and in [610] for weak lensing.”