The luminosity distance in perturbed FLRW space-times

Pyne, Ted; Birkinshaw, Mark

doi:10.1111/j.1365-2966.2004.07362.x

Cited by 63 publications

(82 citation statements)

References 13 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Therefore, many theories which describe the inhomogeneity have been proposed to correct the distance-redshift relation [37]. Such as, LTB model [38], swisscheese model [4], weak-lensing approximation [39], and Dyer-Roeder relation [40]. Among them, the Dyer-Roeder equation is the simplest distance estimator, because it is obtained by adding small perturbation on FLRW model.…”

Section: Discussionmentioning

confidence: 99%

Constraining smoothness parameter and the DD relation of Dyer-Roeder equation with supernovae

Yang¹,

Yu²,

Zhang

2013

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Abstract. Our real universe is locally inhomogeneous. Dyer and Roeder introduced the smoothness parameter α to describe the influence of local inhomogeneity on angular diameter distance, and they obtained the angular diameter distance-redshift approximate relation (Dyer-Roeder equation) for locally inhomogeneous universe. Furthermore, the DistanceDuality (DD) relation, D L (z)(1 + z) −2 /D A (z) = 1, should be valid for all cosmological models that are described by Riemannian geometry, where D L and D A are, respectively, the luminosity and angular distance distances. Therefore, it is necessary to test whether if the Dyer-Roeder approximate equation can satisfy the Distance-Duality relation. In this paper, we use Union2.1 SNe Ia data to constrain the smoothness parameter α and test whether the Dyer-Roeder equation satisfies the DD relation. By using χ 2 minimization, we get α = 0.92 +0.08 −0.32 at 1σ and 0.92 +0.08 −0.65 at 2σ, and our results show that the Dyer-Roeder equation is in good consistency with the DD relation at 1σ.

show abstract

Section: Discussionmentioning

confidence: 99%

Constraining smoothness parameter and the DD relation of Dyer-Roeder equation with supernovae

Yang¹,

Yu²,

Zhang

2013

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…In the above I am considering that the observation of luminosity distance is perfect. That is not the case in practice as a number of effects are changing the apparent luminosity such as gravitational lensing, Integrated Sachs-Wolfe effect and gravitational redshift and peculiar velocities (Sasaki 1987;Pyne & Birkinshaw 2004;Bonvin et al 2006). For the moment we will neglect all these effects, keeping in mind that in data they will eventually have to be inserted into the likelihood analysis of luminosity distances.…”

Section: The Flow Modelmentioning

confidence: 99%

Bayesian 3D velocity field reconstruction with virbius

Lavaux

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

I describe a new Bayesian based algorithm to infer the full three dimensional velocity field from observed distances and spectroscopic galaxy catalogues. In addition to the velocity field itself, the algorithm reconstructs true distances, some cosmological parameters and specific non-linearities in the velocity field. The algorithm takes care of selection effects, miscalibration issues and can be easily extended to handle direct fitting of, e.g., the inverse Tully-Fisher relation. I first describe the algorithm in details alongside its performances. This algorithm is implemented in the VIRBIuS (VelocIty Reconstruction using Bayesian Inference Software) software package. I then test it on different mock distance catalogues with a varying complexity of observational issues. The model proved to give robust measurement of velocities for mock catalogues of 3,000 galaxies. I expect the core of the algorithm to scale to tens of thousands galaxies. It holds the promises of giving a better handle on future large and deep distance surveys for which individual errors on distance would impede velocity field inference.

show abstract

“…Previous work has examined perturbations to the luminosity distance in detail [5][6][7][8][9]. Reference [10] considers the total source count to up to a certain redshift in a specific cosmological model, but does not give results for counts as a function of flux or magnitude limit.…”

Section: Introductionmentioning

confidence: 99%

Linear power spectrum of observed source number counts

Challinor¹,

2011

View full text Add to dashboard Cite

We relate the observable number of sources per solid angle and redshift to the underlying proper source density and velocity, background evolution and line-of-sight potentials. We give an exact result in the case of linearized perturbations assuming general relativity. This consistently includes contributions of the source density perturbations and redshift distortions, magnification, radial displacement, and various additional linear terms that are small on sub-horizon scales. In addition we calculate the effect on observed luminosities, and hence the result for sources observed as a function of flux, including magnification bias and radial-displacement effects. We give the corresponding linear result for a magnitude-limited survey at low redshift, and discuss the angular power spectrum of the total count distribution. We also calculate the cross-correlation with the CMB polarization and temperature including Doppler source terms, magnification, redshift distortions and other velocity effects for the sources, and discuss why the contribution of redshift distortions is generally small. Finally we relate the result for source number counts to that for the brightness of line radiation, for example 21-cm radiation, from the sources.

show abstract

The luminosity distance in perturbed FLRW space-times

Cited by 63 publications

References 13 publications

Constraining smoothness parameter and the DD relation of Dyer-Roeder equation with supernovae

Constraining smoothness parameter and the DD relation of Dyer-Roeder equation with supernovae

Bayesian 3D velocity field reconstruction with virbius

Linear power spectrum of observed source number counts

Contact Info

Product

Resources

About