Isotropic vs. anisotropic components of BAO data: a tool for model selection

Haridasu, Balakrishna S.; Luković, Vladimir V.; Vittorio, N.

doi:10.1088/1475-7516/2018/05/033

Cited by 28 publications

(15 citation statements)

References 83 publications

(201 reference statements)

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“…The statistical estimate obtained here is in agreement with the CMB P16 and local R18 at 1.41σ and 2.60σ, respectively. Very similar inference was also made with a model-dependent analysis in [80]. When we include the R18 measurement in our analysis we find H 0 = 71.40 +0.30+1.65(sys) −0.30 km/s Mpc −1 and r d = 141.29 +1.31 −1.31−2.63(sys) Mpc.…”

Section: Conclusion and Future Prospectssupporting

confidence: 86%

An improved model-independent assessment of the late-time cosmic expansion

Haridasu

Luković

Moresco

et al. 2018

J. Cosmol. Astropart. Phys.

Self Cite

140

105

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In the current work, we have implemented an extension of the standard Gaussian Process formalism, namely the Multi-Task Gaussian Process with the ability to perform a joint learning of several cosmological data simultaneously. We have utilised the "low-redshift" expansion rate data from Supernovae Type-Ia (SN), Baryon Acoustic Oscillations (BAO) and Cosmic Chronometers (CC) data in a joint analysis. We have tested several possible models of covariance functions and find very consistent estimates for cosmologically relevant parameters. In the current formalism, we also find provisions for heuristic arguments which allow us to select the best-suited kernel for the reconstruction of expansion rate data. We also utilised our method to account for systematics in CC data and find an estimate of H 0 = 68.52 +0.94+2.51(sys) −0.94 km/s Mpc −1 and a corresponding r d = 145.61 +2.82 −2.82−4.3(sys)Mpc as our primary result. Subsequently, we find constraints on the present deceleration parameter q 0 = −0.52 ± 0.06 and the transition redshift z T = 0.64 +0.12 −0.09 . All the estimated cosmological parameters are found to be in good agreement with the standard ΛCDM scenario. Including the local model-independent H 0 estimate to the analysis we find H 0 = 71.40 +0.30+1.65(sys) −0.30 km/s Mpc −1 and the corresponding r d = 141.29 +1.31 −1.31−2.63(sys) Mpc. Also, the constraints on r d H 0 remain consistent throughout our analysis and also with the model-dependent CMB estimate. Using the Om(z) diagnostic, we find that the concordance model is very consistent within the redshift range z 2 and mildly discrepant for z 2.

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Section: Conclusion and Future Prospectssupporting

confidence: 86%

An improved model-independent assessment of the late-time cosmic expansion

Haridasu

Luković

Moresco

et al. 2018

J. Cosmol. Astropart. Phys.

Self Cite

140

105

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“…It is worth noting here that a tension seems to persist between the local measurement values and the lower value obtained from Planck, i.e., H 0 = 66.93 ± 0.62 km s −1 Mpc −1 . This tension has been the subject of numerous discussions in recent literature offering different perspectives (Bernal et al 2016;Lin and Ishak 2017b,a;Luković et al 2018;Wang et al 2017;Haridasu et al 2017;Zhang et al 2018;Gómez-Valent and Amendola 2018;Abbott et al 2017b). As we discuss further below in some of the sub-sections (see e.g., Sect.…”

Section: Local Measurements Of the Hubble Constant Or Measurements Of...mentioning

confidence: 89%

Testing general relativity in cosmology

2018

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We review recent developments and results in testing general relativity (GR) at cosmological scales. The subject has witnessed rapid growth during the last two decades with the aim of addressing the question of cosmic acceleration and the dark energy associated with it. However, with the advent of precision cosmology, it has also become a well-motivated endeavor by itself to test gravitational physics at cosmic scales. We overview cosmological probes of gravity, formalisms and parameterizations for testing deviations from GR at cosmological scales, selected modified gravity (MG) theories, gravitational screening mechanisms, and computer codes developed for these tests. We then provide summaries of recent cosmological constraints on MG parameters and selected MG models. We supplement these cosmological constraints with a summary of implications from the recent binary neutron star merger event. Next, we summarize some results on MG parameter forecasts with and without astrophysical systematics that will dominate the uncertainties. The review aims at providing an overall picture of the subject and an entry point to students and researchers interested in joining the field. It can also serve as a quick reference to recent results and constraints on testing gravity at cosmological scales.

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“…Other probes based on the baryon acoustic oscillations (BAO) combined with data independent of CMB and SNIa provide H 0 = 67.2 +1.2 −1.0 km s −1 Mpc −1 by Abbott et al (2018) (BAO and Dark Energy Survey Year 1 clustering and weak-lensing data combined with Big Bang nucleosynthesis information), H 0 = 66.98±1.18 km s −1 Mpc −1 from Addison et al (2018) (BAO from galaxy and Lyα forest with an estimate of primordial deuterium abundance). At the same time, BAO in combination with other CMB measurements from the Wilkinson Microwave Anisotropy Probe (WMAP), the South-Pole Telescope (SPT), the Atacama Cosmology Telescope(ACT), and SNIa data provide H 0 = 69.6±0.7 km s −1 Mpc −1 from Bennett et al (2014) or in combination with observational Hubble datasets and SNIa data H 0 = 69.4 ± 1.7 km s −1 Mpc −1 from Haridasu et al (2018).…”

Section: Comparison With Other Cosmological Probesmentioning

confidence: 94%

Deriving the Hubble constant usingPlanckandXMM-Newtonobservations of galaxy clusters

Kozmanyan

Bourdin

Mazzotta

et al. 2019

A&A

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The possibility of determining the value of the Hubble constant using observations of galaxy clusters in X-ray and microwave wavelengths through the Sunyaev Zel'dovich (SZ) effect has long been known. Previous measurements have been plagued by relatively large errors in the observational data and severe biases induced, for example, by cluster triaxiality and clumpiness. The advent of Planck allows us to map the Compton parameter y, that is, the amplitude of the SZ effect, with unprecedented accuracy at intermediate cluster-centric radii, which in turn allows performing a detailed spatially resolved comparison with X-ray measurements. Given such higher quality observational data, we developed a Bayesian approach that combines informed priors on the physics of the intracluster medium obtained from hydrodynamical simulations of massive clusters with measurement uncertainties. We applied our method to a sample of 61 galaxy clusters with redshifts up to z < 0.5 observed with Planck and XMM-Newton and find H 0 = 67 ± 3km s −1 Mpc −1 .

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Isotropic vs. anisotropic components of BAO data: a tool for model selection

Cited by 28 publications

References 83 publications

An improved model-independent assessment of the late-time cosmic expansion

An improved model-independent assessment of the late-time cosmic expansion

Testing general relativity in cosmology

Deriving the Hubble constant usingPlanckandXMM-Newtonobservations of galaxy clusters

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