Cosmic distance-duality relation test using type Ia supernovae and the baryon acoustic oscillation

Wu, Puxun; Li, Zheng‐Xiang; Liu, Xiaoliang; Yu, Hongwei

doi:10.1103/physrevd.92.023520

Cited by 32 publications

(35 citation statements)

References 42 publications

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“…The mismatch between the empirical sound horizon and the ΛCDM-determined sound horizon could arise due to a violation of one of the two assumptions underlying the distance-duality relation. See [52,53] for constraints on violations of the distance-duality relation from the combination of supernova and BAO data.…”

Section: Violation Of the Distance Duality Relationmentioning

confidence: 99%

Hubble constant hunter’s guide

2020

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Measurements of the Hubble constant, and more generally measurements of the expansion rate and distances over the interval 0 < z < 1, appear to be inconsistent with the predictions of the standard cosmological model (ΛCDM) given observations of cosmic microwave background temperature and polarization anisotropies. Here we consider a variety of types of departures from ΛCDM that could, in principle, restore concordance among these datasets, and we explain why we find almost all of them unlikely to be successful. We single out the set of solutions that increase the expansion rate in the decade of scale factor expansion just prior to recombination as the least unlikely. These solutions are themselves tightly constrained by their impact on photon diffusion and on the gravitational driving of acoustic oscillations of the modes that begin oscillating during this epoch -modes that project on to angular scales that are very well measured. We point out that a general feature of such solutions is a residual to fits to ΛCDM, like the one observed in Planck power spectra. This residual drives the modestly significant inferences of angular-scale dependence to the matter density and anomalously high lensing power, puzzling aspects of a data set that is otherwise extremely well fit by ΛCDM. I. INTRODUCTIONEstimates of the Hubble constant from a distance ladder approach are generally higher than those derived from cosmic microwave background (CMB) data, assuming the standard "ΛCDM" cosmological model [2]. The SH 0 ES team calibrates a supernova sample with Cepheids and finds H 0 = 74.03 ± 1.42 km/s/Mpc [3, hereafter R19].Compared with the value inferred from Planck CMB temperature and polarization power spectra plus CMB lensing, assuming ΛCDM, H 0 = 67.27 ± 0.60 km/s/Mpc, there is a 4.4 σ discrepancy. The most recent result from strong-lensing time delays, from the H 0 LiCoW team [4,5], assuming the standard cosmological model and a prior of Ω m ∈ [0.05, 0.5], of H 0 = 76.8 ± 2.5 km/s/Mpc is consistent with R19 and discrepant with the ΛCDM Planck value at 3.1 σ. The Carnegie-Chicago Hubble Project have used their own Hubble flow set of supernovae that they have calibrated with the tip of the red giant branch method. They find H 0 = 69.8 ± 0.8(stat) ± 1.7(sys) km/s/Mpc [6], which at the 2 σ level is consistent with all of these results.Bernal et al. [7] showed that in addition to a discrepancy in the Hubble constant, there is a discrepancy in the comoving sound horizon at the end of the baryon drag epoch, r drag s . They used Cepheid-calibrated supernovae [8,9] to infer distances out to redshifts with precise measurements of the baryon acoustic oscillation feature [10][11][12]. With these distances, they could convert the BAO angles to inferences of r drag s . Using supernova data to control the shape of D(z) they obtained relatively model-independent inferences of this empirically- * with apologies to Gunion et al. [1]

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Section: Violation Of the Distance Duality Relationmentioning

confidence: 99%

Hubble constant hunter’s guide

2020

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“…Moreover, it is straightforward to show that J vanishes, and the usual DRR of Riemannian geometry is preserved in the form of Eq. (18). In other words, we have shown that Riemannian geometry is a sufficient condition for the validity of the usual DRR, but not a necessary one.…”

Section: Application: Two Simple Casesmentioning

confidence: 73%

“…For general relativity (GR), of course η = 1. Observational constraints on its value have been extensively explored in the recent literature [4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19][20].…”

Section: Introductionmentioning

confidence: 99%

How does light move in a generic metric-affine background?

et al. 2017

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Light is the richest information retriever for most physical systems, particularly so for astronomy and cosmology, in which gravitation is of paramount importance, and also for solid state defects and metamaterials, in which some effects can be mimicked by non-Euclidean or even non-Riemannian geometries. Thus, it is expedient to probe light motion in geometrical backgrounds alternative to that of general relativity. Here we investigate this issue in generic metric-affine theories and derive (i) the expression, in the geometrical optics (eikonal) limit, for light trajectories, showing that they still are null (extremal) geodesics and thus, in general, no longer autoparallels, (ii) a generic formula to obtain the relation between source (galaxy) and reception (observer) angular size (area) distances, generalizing Etherington's original distance reciprocity relation (DRR), and then applying it to two particular representative non-Riemannian geometries. First in metric-compatible, completely antisymmetric torsion geometries, the generalized DRR is not changed at all, and then in Weyl integrable spacetimes, the generalized DRR assumes a specially simple expression.

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“…Holanda et al [85] parametrized the redshift dependence of η(z) in two distinct forms, η(z) = 1 + η 0 z(P1) and η(z) = 1 + η 0 z/(1 + z)(P2) and investigated the η 0 parameter by employing the luminosity distance D L measurements from Type Ia supernovae (SNe Ia) and diameter distance D A from galaxy clusters [86,87]. Several other authors have also tested the DDR relation using different observations: SNe Ia plus cosmic microwave background (CMB) and barion acoustic oscillations (BAO) [88], SNe Ia plus H(z) data [77,[89][90][91], gas mass fraction of galaxy clusters and SNe Ia [92,93], CMB spectrum [94], gammaray burst (GRB) plus H(z) [95], SNe Ia plus BAO [96], gas mass fraction plus H(z) [97], gravitational lensing plus SNe Ia [98], SNe Ia and radio galaxy plus CMB [99]. Most of the above authors obtain no significant deviation in DDR relation, although, roughly the scatter in η 0 parameter is observed as ±0.1 to ±0.…”

Section: Methodsmentioning

confidence: 99%

Constraining axionlike particles using the distance-duality relation

Tiwari¹

2017

Phys. Rev. D

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One of the fundamental results used in observational cosmology is the distance duality relation (DDR), which relates the luminosity distance, DL, with angular diameter distance, DA, at a given redshift z. We employ the observed limits of this relation to constrain the coupling of axion like particles (ALPs) with photons. With our detailed 3D ALP-photon mixing simulation in standard ΛCDM universe and latest DDR limits observed in Holand & Barros (2016) we limit the coupling constant g φ ≤ 6 × 10 −13 GeV −1 nG B Mpc for ALPs of mass ≤ 10 −15 eV. The DDR observations can provide very stringent constraint on ALPs mixing in future. Also any deviation in DDR can be conventionally explained as photons decaying to axions or vice-versa.

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Cosmic distance-duality relation test using type Ia supernovae and the baryon acoustic oscillation

Cited by 32 publications

References 42 publications

Hubble constant hunter’s guide

Hubble constant hunter’s guide

How does light move in a generic metric-affine background?

Constraining axionlike particles using the distance-duality relation

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