Redshift spherical shell energy in isotropic universes

Romano, Antonio Enea

doi:10.1103/physrevd.76.103525

Cited by 22 publications

(14 citation statements)

References 8 publications

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“…This intriguing possibility has motivated recent attempts of rooting the CP on a more solid basis. Interestingly, there are some encouraging proposals in this direction which are based on the analysis of the large-scale maps of CMB anisotropies [21,22,23,24], of galaxies [25,26,27,28] and of supernovae [29].…”

Section: Introductionmentioning

confidence: 99%

The scale of cosmic isotropy

Marinoni

Bel

Buzzi

2012

J. Cosmol. Astropart. Phys.

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Abstract. The most fundamental premise to the standard model of the universe states that the large-scale properties of the universe are the same in all directions and at all comoving positions. Demonstrating this hypothesis has proven to be a formidable challenge. The cross-over scale R iso above which the galaxy distribution becomes statistically isotropic is vaguely defined and poorly (if not at all) quantified. Here we report on a formalism that allows us to provide an unambiguous operational definition and an estimate of R iso . We apply the method to galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 7, finding that R iso ∼ 150h −1 Mpc. Besides providing a consistency test of the Copernican principle, this result is in agreement with predictions based on numerical simulations of the spatial distribution of galaxies in cold dark matter dominated cosmological models.

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Section: Introductionmentioning

confidence: 99%

The scale of cosmic isotropy

Marinoni

Bel

Buzzi

2012

J. Cosmol. Astropart. Phys.

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“…Anther possible application of our results would be to give an analytical approximation for E RSS (z) [41] , the redshift spherical energy, a quantity constructed by integrating mn(z) over varying redshift intervals ∆Z(z) corresponding to a constant time interval ∆t, which should be the characteristic time scale over which the astrophysical evolution of the astrophysical object counted can be neglected.…”

Section: Discussionmentioning

confidence: 99%

“…This should not be confused with the redshift spherical shell energy E RSS introduced in [41], which is a quantity obtained by integrating mn(z) over varying redshift intervals ∆Z(z)…”

Section: Einstein's Equations Givementioning

confidence: 99%

Testing homogeneity with galaxy number counts: light-cone metric and general low-redshift expansion for a central observer in a matter dominated isotropic universe without cosmological constant

Romano

2010

J. Cosmol. Astropart. Phys.

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As an alternative to dark energy it has been suggested that we may be at the center of an inhomogeneous isotropic universe described by a Lemaitre-Tolman-Bondi (LTB) solution of Einstein's field equations. In order to test this hypothesis we calculate the general analytical formula to fifth order for the redshift spherical shell mass. Using the same analytical method we write the metric in the light-cone by introducing a gauge invariant quantity G(z) which together with the luminosity distance D L (z) completely determine the light-cone geometry of a LTB model.

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“…Another observable which could be used to constraint LTB models is the redshift spherical shell mass mn(z) [27], which has been recently calculated [28] for a central observer up to the fifth order in the redshift, and can be generalized [29] to the more observationally related E RSS (z), the redshift spherical shell energy.…”

Section: Introductionmentioning

confidence: 99%

Mimicking the cosmological constant for more than one observable with large scale inhomogeneities

Romano

2010

Phys. Rev. D

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Assuming the definition of the inversion problem (IP) as the exact matching of the terms in the low redshift expansion of cosmological observables calculated for different cosmological models, we solve the IP for D L (z) and the redshift spherical shell mass density mn(z) for a central observer in a LTB space without cosmological constant and a generic ΛCDM model. We show that the solution of the IP is unique, corresponds to a matter density profile which is not smooth at the center and that the same conclusions can be reached expanding self-consistently to any order all the relevant quantities.On contrary to the case of a single observable inversion problem, it is impossible to solve the IP (LTB vs. ΛCDM) for both mn(z) and D L (z) while setting one the two functions k(r) or t b (r) to zero, even allowing not smooth matter profiles. Our conclusions are general, since they are exclusively based on comparing directly physical observables in redshift space, and don't depend on any special ansatz or restriction for the functions defining a LTB model.

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Redshift spherical shell energy in isotropic universes

Abstract: We introduce the redshift spherical shell energy (RSSE), which can be used to test in the redshift space the radial inhomogeneity of an isotropic universe, providing additional constraints for LTB models, and a more general test of cosmic homogeneity.

Cited by 22 publications

References 8 publications

The scale of cosmic isotropy

The scale of cosmic isotropy

Testing homogeneity with galaxy number counts: light-cone metric and general low-redshift expansion for a central observer in a matter dominated isotropic universe without cosmological constant

Mimicking the cosmological constant for more than one observable with large scale inhomogeneities

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