Testing dark energy using pairs of galaxies in redshift space

Jennings, Elise; Baugh, C. M.; Pascoli, Silvia

doi:10.1111/j.1365-2966.2011.20064.x

Cited by 17 publications

(17 citation statements)

References 58 publications

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“…The Alcock-Paczynski (AP) effect refers to the geometric distortion when an incorrect cosmological model (with an incorrect value of the product H(z)D A (z)) is assumed for transforming redshift to comoving distance, induced by the fact that measured distances along and perpendicular to the line of sight are fundamentally different [142]. The AP effect can be measured through the statistical study of galaxies clustering [143,144,145], the symmetry properties of galaxy pairs [146,147,148], and the cosmic voids [149,150,151]. In addition, it is argued that measuring the redshift dependence of AP effect may also derive useful cosmological constraints on DE [152,153,154].…”

Section: • Alcock-paczynski Effectmentioning

confidence: 99%

Holographic dark energy

2017

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We review the paradigm of holographic dark energy (HDE), which arises from a theoretical attempt of applying the holographic principle (HP) to the dark energy (DE) problem. Making use of the HP and the dimensional analysis, we derive the general formula of the energy density of HDE. Then, we describe the properties of HDE model, in which the future event horizon is chosen as the characteristic length scale. We also introduce the theoretical explorations and the observational constraints for this model. Next, in the framework of HDE, we discuss various topics, such as spatial curvature, neutrino, instability of perturbation, time-varying gravitational constant, inflation, black hole and big rip singularity. In addition, from both the theoretical and the observational aspects, we introduce the interacting holographic dark energy scenario, where the interaction between dark matter and HDE is taken into account. Furthermore, we discuss the HDE scenario in various modified gravity (MG) theories, such as Brans-Dicke theory, braneworld theory, scalar-tensor theory, Horava-Lifshitz theory, and so on. Besides, we introduce the attempts of reconstructing various scalar-field DE and MG models from HDE. Moreover, we introduce other DE models inspired by the HP, in which different characteristic length scales are chosen. Finally, we make comparisons among various HP-inspired DE models, by using cosmological observations and diagnostic tools.

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Section: • Alcock-paczynski Effectmentioning

confidence: 99%

Holographic dark energy

2017

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“…Another approach is to measure the symmetry properties of close galaxy pairs (Marinoni & Buzzi 2010). Unfortunately, this method is seriously affected by dynamics at small scales (Jennings et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Cosmic Voids in the SDSS DR12 BOSS Galaxy Sample: the Alcock–Paczyński test

Mao

Berlind

Scherrer

et al. 2017

ApJ

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We apply the Alcock-Paczyński (AP) test to the stacked voids identified using the large-scale structure galaxy catalog from the Baryon Oscillation Spectroscopic Survey (BOSS). This galaxy catalog is part of the Sloan Digital Sky Survey Data Release 12 and is the final catalog of SDSS-III. We also use 1000 mock galaxy catalogs that match the geometry, density, and clustering properties of the BOSS sample in order to characterize the statistical uncertainties of our measurements and take into account systematic errors such as redshift space distortions. For both BOSS data and mock catalogs, we use the ZOBOV algorithm to identify voids, we stack together all voids with effective radii of 30 − 100h −1 Mpc in the redshift range 0.43 − 0.7, and we accurately measure the shape of the stacked voids. Our tests with the mock catalogs show that we measure the stacked void ellipticity with a statistical precision of 2.6%. The stacked voids in redshift space are slightly squashed along the line of sight, which is consistent with previous studies. We repeat this measurement of stacked void shape in the BOSS data assuming several values of Ω m within the flat ΛCDM model, and we compare to the mock catalogs in redshift space in order to perform the AP test. We obtain a constraint of Ω m = 0.38 +0.18 −0.15 at the 68% confidence level from the AP test. We discuss the various sources of statistical and systematic noise that affect the constraining power of this method. In particular, we find that the measured ellipticity of stacked voids scales more weakly with cosmology than the standard AP prediction, leading to significantly weaker constraints. We discuss how AP constraints will improve in future surveys with larger volumes and densities.

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“…One option is to use the angular distribution of small scale pairs of quasars or galaxies (Phillipps, 1994;Marinoni and Buzzi, 2010), though peculiar velocities still affect this measure, in a redshift-and cosmology-dependent way (Jennings et al, 2012b). A promising recent suggestion is to use the average shape of voids in the galaxy distribution; individual voids are ellipsoidal, but in the absence of peculiar velocities the mean shape should be spherical (Ryden, 1995;Lavaux and Wandelt, 2010).…”

Section: The Alcock-paczynski Testmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Testing dark energy using pairs of galaxies in redshift space

Cited by 17 publications

References 58 publications

Holographic dark energy

Holographic dark energy

Cosmic Voids in the SDSS DR12 BOSS Galaxy Sample: the Alcock–Paczyński test

Observational probes of cosmic acceleration

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