Weak lensing, dark matter and dark energy

Huterer, Dragan

doi:10.1007/s10714-010-1051-z

Cited by 85 publications

(82 citation statements)

References 136 publications

(154 reference statements)

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“…This distortion allows the distribution of dark matter and its evolution with time to be measured, thereby probing the influence of dark energy on the growth of structure (for a detailed review, see e.g. Bartelmann and Schneider (2001); for brief reviews, see Hoekstra and Jain (2008) and Huterer (2010)). …”

Section: Baryon Acoustic Oscillations (Bao)mentioning

confidence: 99%

The Accelerating Universe

Huterer

2011

Adventures in Cosmology

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In this article we review the discovery of the accelerating universe using type Ia supernovae. We then outline ways in which dark energy -component that causes the acceleration -is phenomenologically described. We finally describe principal cosmological techniques to measure large-scale properties of dark energy. This chapter therefore complements articles by Caldwell and Linder (2010) in this book who describe theoretical understanding (or lack thereof) of the cause for the accelerating universe.Evidence for the missing component. Inflationary theory [Guth (1981)] explains how tiny quantum-mechanical fluctuations in the early universe could grow to become structures we see on the sky today. One of the factors that motivated inflation is that it predicts that the total energy density relative to the critical value is unity, Ω ≡ ρ/ρ crit = 1. This inflationary prediction convinced many theorists that the universe is precisely flat.Around the same time that inflation was proposed, a variety of dynamical probes of the large-scale structure in the universe were starting to indicate that the matter energy density is much lower than the value needed to make the flat. Perhaps the most specific case was made by the measurements of the clustering of galaxies, which are sensitive to the parameter combination Γ ≡ Ω M h, where Ω M is the energy density in matter relative to critical, and h is the Hubble constant in units of 100 km/s/Mpc. The measured value at the time was Γ 0.25 (with rather large errors). One way to preserve a flat universe was to postulate that the Hubble constant itself was much lower than the measurements indicated (h ∼ 0.7), so that Ω M = 1 but h ∼ 0.3 [Bartlett et al. (1995)]. Another possibility was the presence of Einstein's cosmological constant (see the Caldwell article in this book), which was World Scientific Book -9.75in x 6.5in bookchapter 2 Book Title suggested as far back as 1984 as the possible missing ingredient that could alleviate tension between data and matter-only theoretical predictions [Peebles (1984); Turner et al. (1984)] by making the universe older, and allowing flatness with a low value of the matter density. Type Ia supernovae and cosmologyThe revolutionary discovery of the accelerating universe took place in the late 1990s, but to understand it and its implications, we have to step back a few decades.Type Ia supernovae. Type Ia supernovae (SN Ia) are explosions seen to distant corners of the universe, and are thought to be cases where a rotating carbonoxygen white dwarf accretes matter from a companion star, approaches the Chandrasekhar limit, starts thermonuclear burning, and then explodes. The Ia nomenclature refers to spectra of SN Ia, which have no hydrogen, but show a prominent Silicon (Si II) line at 6150Å. SN Ia had been studied extensively by Fritz Zwicky who also gave them their name [Baade and Zwicky (1934)], and by Walter Baade, who noted that SN Ia have very uniform luminosities [Baade (1938)]. Light from type Ia supernovae brightens and fades over a period of ab...

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Section: Baryon Acoustic Oscillations (Bao)mentioning

confidence: 99%

The Accelerating Universe

Huterer

2011

Adventures in Cosmology

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“…The sensitivity of weak gravitational lensing to both luminous and dark matter (Benabed & van Waerbeke 2004;Bernstein & Jain 2004;Hu 2002;Huterer 2010;Ishak et al 2004;Takada & White 2004) makes it a powerful way to probe the nature of dark matter, dark energy and modified theories of gravity (Albrecht et al 2006;Weinberg et al 2013). However, the potential to constrain cosmological parameters to sub-percent levels can only be realized if the systematic errors in lensing surveys are even smaller than that.…”

Section: Introductionmentioning

confidence: 99%

Intrinsic alignments of galaxies in the MassiveBlack-II simulation: analysis of two-point statistics

Tenneti

Singh

Mandelbaum

et al. 2015

Monthly Notices of the Royal Astronomical Society

131

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The intrinsic alignment of galaxies with the large-scale density field is an important astrophysical contaminant in upcoming weak lensing surveys. We present detailed measurements of the galaxy intrinsic alignments and associated ellipticity-direction (ED) and projected shape (w g+ ) correlation functions for galaxies in the cosmological hydrodynamic MassiveBlack-II (MB-II) simulation. We carefully assess the effects on galaxy shapes, misalignment of the stellar component with the dark matter shape and two-point statistics of iterative weighted (by mass and luminosity) definitions of the (reduced and unreduced) inertia tensor. We find that iterative procedures must be adopted for a reliable measurement of the reduced tensor but that luminosity versus mass weighting has only negligible effects. Both ED and w g+ correlations increase in amplitude with subhalo mass (in the range of 10 10 − 6.0 × 10 14 h −1 M ), with a weak redshift dependence (from z = 1 to z = 0.06) at fixed mass. At z ∼ 0.3, we predict a w g+ that is in reasonable agreement with SDSS LRG measurements and that decreases in amplitude by a factor of ∼ 5-18 for galaxies in the LSST survey. We also compared the intrinsic alignments of centrals and satellites, with clear detection of satellite radial alignments within their host halos. Finally, we show that w g+ (using subhalos as tracers of density) and w δ+ (using dark matter density) predictions from the simulations agree with that of non-linear alignment models (NLA) at scales where the 2-halo term dominates in the correlations (and tabulate associated NLA fitting parameters). The 1-halo term induces a scale dependent bias at small scales which is not modeled in the NLA model.

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“…As shown in Ref. [30] the shear and the convergence terms can be written as a function of the projected Newtonian potentials ψ ,ij :…”

Section: Galaxy Weak Lensingmentioning

confidence: 99%

Future weak lensing constraints in a dark coupled universe

et al. 2011

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Coupled cosmologies can predict values for the cosmological parameters at low redshifts which may differ substantially from the parameters values within non-interacting cosmologies. Therefore, low redshift probes, as the growth of structure and the dark matter distribution via galaxy and weak lensing surveys constitute a unique tool to constrain interacting dark sector models. We focus here on weak lensing forecasts from future Euclid and LSST-like surveys combined with the ongoing Planck cosmic microwave background experiment. We find that these future data could constrain the dimensionless coupling to be smaller than a few ×10 −2 . The coupling parameter ξ is strongly degenerate with the cold dark matter energy density Ωch 2 and the Hubble constant H0. These degeneracies may cause important biases in the cosmological parameter values if in the universe there exists an interaction among the dark matter and dark energy sectors.

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Weak lensing, dark matter and dark energy

Cited by 85 publications

References 136 publications

The Accelerating Universe

The Accelerating Universe

Intrinsic alignments of galaxies in the MassiveBlack-II simulation: analysis of two-point statistics

Future weak lensing constraints in a dark coupled universe

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