Formation of voids in the Universe within the Lemaitre-Tolman model

Abstract

We develop models of void formation starting from a small initial fluctuation at recombination and growing to a realistic present day density profile in agreement with observations of voids. The model construction is an extension of previously developed algorithms for finding a Lemaitre-Tolman metric that evolves between two profiles of either density or velocity specified at two times. Of the 4 profiles of concern -- those of density and velocity at recombination and at the present day -- two can be specified and the other two follow from the derived model. We find that, in order to reproduce the present-day void density profiles, the initial velocity profile is more important than the initial density profile. Extrapolation of current CMB observations to the scales relevant to proto-voids is very uncertain. Even so, we find that it is very difficult to make both the initial density and velocity fluctuation amplitudes small enough, and still obtain a realistic void by today.

arXiv commentMN2e LaTeX style file, 17 pages, 16 figures, 22 figure files; replecement has minor changes in references

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Cited by in corpus (41)

• The Aspen--Amsterdam Void Finder Comparison Project
• Inhomogeneous cosmological models: exact solutions and their applications
• Observational constraints on inhomogeneous cosmological models without dark energy
• What is dust? - Physical foundations of the averaging problem in cosmology
• Clues on void evolution II: Measuring density and velocity profiles on SDSS galaxy redshift space distortions
• A (giant) void is not mandatory to explain away dark energy with a Lemaitre - Tolman model
• The Effect of Large-Scale Inhomogeneities on the Luminosity Distance
• Structure formation in the quasispherical Szekeres model
• Evolution of cosmic structures in different environments in the quasispherical Szekeres model
• Pressure gradients, shell crossing singularities and acoustic oscillations - application to inhomogeneous cosmological models
• On the Magnitude of Dark Energy Voids and Overdensities
• Galaxy properties from Voids to Clusters in the SDSS-DR4
• Alternative Methods of Describing Structure Formation in the Lemaitre-Tolman Model
• Supernovae Ia observations in the Lemaitre--Tolman model
• Complete solutions to the metric of spherically collapsing dust in an expanding spacetime with a cosmological constant
• Exact spherically-symmetric inhomogeneous model with n perfect fluids
• Gravitational entropies in LTB dust models
• Evolution of radial profiles in regular Lemaitre-Tolman-Bondi dust models
• Radial asymptotics of Lemaitre-Tolman-Bondi dust models
• A dynamical system approach to inhomogeneous dust solutions
• Inhomogeneous Universe in f(T) Theory
• Structure Formation, Backreaction and Weak Gravitational Fields
• Invariant characterization of the growing and decaying density modes in LTB dust models
• On the importance of high redshift intergalactic voids
• The Great Attractor and the Shapley Concentration
• Accelerating expansion or inhomogeneity? A comparison of the $\Lambda$CDM and Lema\^ıtre - Tolman models
• Weighed scalar averaging in LTB dust models, part I: statistical fluctuations and gravitational entropy
• Radiation in the process of the formation of voids
• The effect of pressure gradients on luminosity distance - redshift relations
• Modelling Inhomogeneity in Szekeres Spacetime
• Average luminosity distance in inhomogeneous universes
• The role of shell crossing on the existence and stability of trapped matter shells in spherical inhomogeneous Λ-CDM models
• Imprints of decaying dark matter on cosmic voids
• Weighed scalar averaging in LTB dust models, part II: a formalism of exact perturbations
• The Instantaneous Redshift Difference of Gravitationally Lensed Images: Theory and Observational Prospects
• Physical geometry of the quasispherical Szekeres models
• Non-comoving baryons and cold dark matter in cosmic voids
• Blueshifts in the Lema\^ıtre -- Tolman models
• Voids and overdensities of coupled Dark Energy
• Redshift drift in a universe with structure III: Numerical relativity
• Ricci Time in the Lemaitre-Tolman Model and the Block Universe