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Title: Integrated cosmological probes: Extended analysis

Authors:
; ;
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1353138
Resource Type:
Journal Article: Publisher's Accepted Manuscript
Journal Name:
Physical Review D
Additional Journal Information:
Journal Volume: 95; Journal Issue: 8; Related Information: CHORUS Timestamp: 2017-04-25 22:10:46; Journal ID: ISSN 2470-0010
Publisher:
American Physical Society
Country of Publication:
United States
Language:
English

Citation Formats

Nicola, Andrina, Refregier, Alexandre, and Amara, Adam. Integrated cosmological probes: Extended analysis. United States: N. p., 2017. Web. doi:10.1103/PhysRevD.95.083523.
Nicola, Andrina, Refregier, Alexandre, & Amara, Adam. Integrated cosmological probes: Extended analysis. United States. doi:10.1103/PhysRevD.95.083523.
Nicola, Andrina, Refregier, Alexandre, and Amara, Adam. Tue . "Integrated cosmological probes: Extended analysis". United States. doi:10.1103/PhysRevD.95.083523.
@article{osti_1353138,
title = {Integrated cosmological probes: Extended analysis},
author = {Nicola, Andrina and Refregier, Alexandre and Amara, Adam},
abstractNote = {},
doi = {10.1103/PhysRevD.95.083523},
journal = {Physical Review D},
number = 8,
volume = 95,
place = {United States},
year = {Tue Apr 25 00:00:00 EDT 2017},
month = {Tue Apr 25 00:00:00 EDT 2017}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record at 10.1103/PhysRevD.95.083523

Citation Metrics:
Cited by: 3works
Citation information provided by
Web of Science

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  • Assessing the consistency of parameter constraints derived from different cosmological probes is an important way to test the validity of the underlying cosmological model. In an earlier work [1], we computed constraints on cosmological parameters for ΛCDM from an integrated analysis of CMB temperature anisotropies and CMB lensing from Planck, galaxy clustering and weak lensing from SDSS, weak lensing from DES SV as well as Type Ia supernovae and Hubble parameter measurements. In this work, we extend this analysis and quantify the concordance between the derived constraints and those derived by the Planck Collaboration as well as WMAP9, SPT andmore » ACT. As a measure for consistency, we use the Surprise statistic [2], which is based on the relative entropy. In the framework of a flat ΛCDM cosmological model, we find all data sets to be consistent with one another at a level of less than 1σ. We highlight that the relative entropy is sensitive to inconsistencies in the models that are used in different parts of the analysis. In particular, inconsistent assumptions for the neutrino mass break its invariance on the parameter choice. When consistent model assumptions are used, the data sets considered in this work all agree with each other and ΛCDM, without evidence for tensions.« less
  • We review, compare and extend recent studies searching for evidence for a preferred cosmological axis. We start from the Union2 SnIa dataset and use the hemisphere comparison method to search for a preferred axis in the data. We find that the hemisphere of maximum accelerating expansion rate is in the direction (l,b) = (309°{sup +23°}{sub −3°},18°{sup +11°}{sub −10°}) (Ω{sub 0m} = 0.19) while the hemisphere of minimum acceleration is in the opposite direction (l,b) = (129°{sup +23°}{sub −3°},−18°{sup +10°}{sub −11°}) (Ω{sub 0m} = 0.30). The level of anisotropy is described by the normalized difference of the best fit values ofmore » Ω{sub 0m} between the two hemispheres in the context of ΛCDM fits. We find a maximum anisotropy level in the Union2 data of ΔΩ{sub 0mmax} / Ω{sub 0m} = 0.43±0.06. Such a level does not necessarily correspond to statistically significant anisotropy because it is reproduced by about 30% of simulated isotropic data mimicking the best fit Union2 dataset. However, when combined with the axes directions of other cosmological observations (bulk velocity flow axis, three axes of CMB low multipole moments and quasar optical polarization alignment axis), the statistical evidence for a cosmological anisotropy increases dramatically. We estimate the probability that the above independent six axes directions would be so close in the sky to be less than 1%. Thus either the relative coincidence of these six axes is a very large statistical fluctuation or there is an underlying physical or systematic reason that leads to their correlation.« less
  • We present a global measurement of the integrated Sachs-Wolfe (ISW) effect obtained by cross correlating all relevant large-scale galaxy data sets with the cosmic microwave background radiation map provided by the Wilkinson Microwave Anisotropy Probe. With these measurements, the overall ISW signal is detected at the {approx}4.5{sigma} level. We also examine the cosmological implications of these measurements, particularly the dark energy equation of state w, its sound speed c{sub s}, and the overall curvature of the Universe. The flat {lambda}CDM model is a good fit to the data and, assuming this model, we find that the ISW data constrain {omega}{submore » m}=0.20{sub -0.11}{sup +0.19} at the 95% confidence level. When we combine our ISW results with the latest baryon oscillation and supernovae measurements, we find that the result is still consistent with a flat {lambda}CDM model with w=-1 out to redshifts z>1.« less
  • The first cosmological results from the ESSENCE supernova survey (Wood-Vasey et al. 2007) are extended to a wider range of cosmological models including dynamical dark energy and non-standard cosmological models. We fold in a greater number of external data sets such as the recent Higher-z release of high-redshift supernovae (Riess et al. 2007) as well as several complementary cosmological probes. Model comparison statistics such as the Bayesian and Akaike information criteria are applied to gauge the worth of models. These statistics favor models that give a good fit with fewer parameters. Based on this analysis, the preferred cosmological model ismore » the flat cosmological constant model, where the expansion history of the universe can be adequately described with only one free parameter describing the energy content of the universe. Amongst the more exotic models that provide good fits to the data, we note a preference for models whose best-fit parameters reduce them to the cosmological constant model.« less
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