Rendering dark energy void

February, Sean; Larena, Julien; Smith, M.; Clarkson, Chris

doi:10.1111/j.1365-2966.2010.16627.x

Cited by 77 publications

(95 citation statements)

References 60 publications

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“…In this work we consider a test case to demonstrate the method, and so focus on an open (Ω κ > 0), dust-only background model (Λ = 0) that is asymptotically Einsteinde Sitter, and which is known to comfortably accommodate distances to SN1a (see e.g. [7]). Here we model the total (dimensionless) matter density profile today according to:…”

Section: Background Evolutionmentioning

confidence: 99%

“…If we were to live in a large, underdense void of a few giga-parsecs in diameter, distant supernovae would appear fainter than expected in a FLRW model, and the dark energy phenomenon could be explained on purely relativistic terms without invoking any new physics (see, e.g., [5,6,7,8] and [9] for a comprehensive review). Clearly, structure formation places a key constraint on such models by probing their difference from the concordance model, and so serves as a test of the Copernican principle [10].…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Evolution of linear perturbations in spherically symmetric dust spacetimes

February¹,

Larena²,

Clarkson³

et al. 2014

Class. Quantum Grav.

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Abstract. We present results from a numerical code implementing a new method to solve the master equations describing the evolution of linear perturbations in a spherically symmetric but inhomogeneous background. This method can be used to simulate several configurations of physical interest, such as relativistic corrections to structure formation, the lensing of gravitational waves and the evolution of perturbations in a cosmological void model. This paper focuses on the latter problem, i.e. structure formation in a Hubble scale void in the linear regime. This is considerably more complicated than linear perturbations of a homogeneous and isotropic background because the inhomogeneous background leads to coupling between density perturbations and rotational modes of the spacetime geometry, as well as gravitational waves. Previous analyses of this problem ignored this coupling in the hope that the approximation does not affect the overall dynamics of structure formation in such models. We show that for a giga-parsec void, the evolution of the density contrast is well approximated by the previously studied decoupled evolution only for very large-scale modes. However, the evolution of the gravitational potentials within the void is inaccurate at more than the 10% level, and is even worse on small scales.

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Section: Background Evolutionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Evolution of linear perturbations in spherically symmetric dust spacetimes

February¹,

Larena²,

Clarkson³

et al. 2014

Class. Quantum Grav.

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“…Considering the present results, such differences in the expected number densities should be greater than the CGBH-to-FLRW ones studied here, if we were to detect a significant effect on the observed number densities caused by differences in their expected values alone. February et al (2010) argue that CMB and BAO constraints may be significantly distorted by differences in the evolution of primordial perturbations caused by the curvature inside the voids. They go on to fit a number of different shapes for the inner matter profile, considering only local Universe data, namely, SNe Ia and the reconstruction of H(z) through passively evolving galaxies.…”

Section: Comparison With Other Ltb Modelsmentioning

confidence: 99%

“…Sollerman et al 2009), some of them cannot be ruled out entirely yet. Among these models, motivated mainly as alternative to dark energy, various non-homogeneous cosmologies have been proposed, with an increasing interest in the past few years (Hellaby & Alfedeel 2009;Alfedeel & Hellaby 2010;February et al 2010;Biswas et al 2010;Sussman 2010;Bolejko et al 2011b;Nadathur & Sarkar 2011;Clarkson & Regis 2011;Clarkson et al 2012;Regis & Clarkson 2012;Meures & Bruni 2012;Humphreys et al 2012;Nishikawa et al 2012;Valkenburg et al 2014;Wang & Zhang 2012;Hellaby 2012;Hoyle et al 2013;de Putter et al 2012;Keenan et al 2012;Fleury et al 2013). Some recent reviews include Célérier (2007), Bolejko et al (2011a), Ellis (2011), and Krasiński (2014).…”

Section: Introductionmentioning

confidence: 99%

Relativistic cosmology number densities in void-Lemaître-Tolman-Bondi models

Iribarrem

Andreani

February

et al. 2014

A&A

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Aims. The goal of this work is to compute the number density of far-IR selected galaxies in the comoving frame and along the past lightcone of observationally constrained Lemaître-Tolman-Bondi "giant void" models and to compare those results with their standard model counterparts. Methods. We derived integral number densities and differential number densities using different cosmological distance definitions in the Lemaître-Tolman-Bondi dust models. Then, we computed selection functions and consistency functions for the luminosity functions in the combined fields of the Herschel/PACS evolutionary probe (PEP) survey in both standard and void cosmologies, from which we derived the observed values of the above-mentioned densities. We used the Kolmogorov-Smirnov statistics to study both the evolution of the consistency functions and its connection to the evolution of the comoving density of sources. Finally, we fitted the power-law behaviour of the densities along the observer's past lightcone.Results. The analysis of the comoving number density shows that the increased flexibility of the Lemaître-Tolman-Bondi models is not enough to fit the observed redshift evolution of the number counts, if it is specialised to a recent best-fit giant void parametrisation. The results for the power-law fits of the densities along the observer's past lightcone show general agreement across both cosmological models studied here around a slope of −2.5 ± 0.1 for the integral number density on the luminosity-distance volumes. The differential number densities show much bigger slope discrepancies. Conclusions. We conclude that the differential number densities on the observer's past lightcone were still rendered dependent on the cosmological model by the flux limits of the PEP survey. In addition, we show that an intrinsic evolution of the sources must be assumed to fit the comoving number-density redshift evolution in the giant void parametrisation for the Lemaître-Tolman-Bondi models used in this work.

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“…Actually, it was claimed that such a feature have to be considered a signal of the existence of a void (underdensity) in our neighborhood [17]. Then the fact that both, the tension between low and high redshift data and the inhomogeneous connection for this feature of the reconstructed q(z), make sense only if we assume a local underdensity, means that something in the local distribution of matter is affecting the data, something that we would like to characterize.…”

Section: Introductionmentioning

confidence: 99%

Asymmetry and dark energy evolution

Cárdenas

2018

J. Phys.: Conf. Ser.

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Abstract. The well known asymmetry of type Ia supernova data is used to infer general features of an alternative model for dark energy. Using a model that allows DE to vary with redshift as a probe, the results indicate the low redshift transition of the deceleration parameter q(z) is evident only taken data points from one hemisphere of the sky. A related effect is a reconstructed DE density X(z) that shows evolution (it decreases as redshift increases) only towards the hemisphere where q(z) manifest the transition. We discuss on possible theoretical frameworks where these effects can be explained.

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Rendering dark energy void

Cited by 77 publications

References 60 publications

Evolution of linear perturbations in spherically symmetric dust spacetimes

Evolution of linear perturbations in spherically symmetric dust spacetimes

Relativistic cosmology number densities in void-Lemaître-Tolman-Bondi models

Asymmetry and dark energy evolution

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