Baryon Acoustic Oscillation Data Research Articles

Model-independent Test for the Cosmic Distance–Duality Relation with Pantheon and eBOSS DR16 Quasar Sample

In this Paper, we carry out a new model-independent cosmological test for the cosmic distance–duality relation (CDDR) by combining the latest five baryon acoustic oscillation (BAO) measurements and the Pantheon type Ia supernova (SNIa) sample. Particularly, the BAO measurement from the extended Baryon Oscillation Spectroscopic Survey data release 16 quasar sample at effective redshift z = 1.48 is used, and two methods, i.e., a compressed form of the Pantheon sample and the artificial neural network combined with the binning SNIa method, are applied to overcome the redshift-matching problem. Our results suggest that the CDDR is compatible with the observations, and the high-redshift BAO and SNIa data can effectively strengthen the constraints on the violation parameters of CDDR with the confidence interval decreasing by more than 20%. In addition, we find that the compressed form of observational data can provide a more rigorous constraint on the CDDR, and thus can be generalized to the applications of other actual observational data with limited sample size in the test for CDDR.

The Pantheon+ Analysis: Cosmological Constraints

We present constraints on cosmological parameters from the Pantheon+ analysis of 1701 light curves of 1550 distinct Type Ia supernovae (SNe Ia) ranging in redshift from z = 0.001 to 2.26. This work features an increased sample size from the addition of multiple cross-calibrated photometric systems of SNe covering an increased redshift span, and improved treatments of systematic uncertainties in comparison to the original Pantheon analysis, which together result in a factor of 2 improvement in cosmological constraining power. For a flat ΛCDM model, we find Ω M = 0.334 ± 0.018 from SNe Ia alone. For a flat w 0CDM model, we measure w 0 = −0.90 ± 0.14 from SNe Ia alone, H 0 = 73.5 ± 1.1 km s−1 Mpc−1 when including the Cepheid host distances and covariance (SH0ES), and w 0 = when combining the SN likelihood with Planck constraints from the cosmic microwave background (CMB) and baryon acoustic oscillations (BAO); both w 0 values are consistent with a cosmological constant. We also present the most precise measurements to date on the evolution of dark energy in a flat w 0 w a CDM universe, and measure w a = from Pantheon+ SNe Ia alone, H 0 = 73.3 ± 1.1 km s−1 Mpc−1 when including SH0ES Cepheid distances, and w a = when combining Pantheon+ SNe Ia with CMB and BAO data. Finally, we find that systematic uncertainties in the use of SNe Ia along the distance ladder comprise less than one-third of the total uncertainty in the measurement of H 0 and cannot explain the present “Hubble tension” between local measurements and early universe predictions from the cosmological model.

The First Direct Measurement of Gravitational Potential Decay Rate at Cosmological Scales and Improved Dark Energy Constraint

The integrated Sachs–Wolfe (ISW) effect probes the decay rate (DR) of large-scale gravitational potential and therefore provides a unique constraint on dark energy (DE). However, its constraining power is degraded by the ISW measurement, which relies on cross-correlating with the large-scale structure (LSS) and suffers from uncertainties in galaxy bias and matter clustering. In combination with lensing-LSS cross correlation, DR can be isolated in a way free of uncertainties in galaxy bias and matter clustering. We applied this proposal to the combination of the Data Release 8 galaxy catalog of DESI imaging surveys and Planck cosmic microwave background maps. We achieved the first DR measurement, with a total significance of 3.2σ. We verified the measurements at three redshift bins ([0.2, 0.4), [0.4, 0.6), [0.6, 0.8]), with two LSS tracers (the “low-density points” and the conventional galaxy positions). Despite its relatively low signal-to-noise ratio, the addition of DR significantly improves dark energy constraints, over Sloan Digital Sky Survey baryon acoustic oscillation (BAO) data alone or Pantheon supernovae (SNe) compilation alone. For flat wCDM cosmology, the improvement in the precision of Ω m is a factor of 1.8 over BAO and 1.5 over SNe. For the DE equation of state w, the improvement factor is 1.3 over BAO and 1.4 over SNe. These improvements demonstrate DR as a useful cosmological probe, and therefore we advocate its usage in future cosmological analysis.

CMB lensing from Planck PR4 maps

We reconstruct the Cosmic Microwave Background (CMB) lensing potential on the latest Planck CMB PR4 (NPIPE) maps, which include slightly more data than the 2018 PR3 release, and implement quadratic estimators using more optimal filtering. We increase the reconstruction signal to noise by almost 20%, constraining the amplitude of the CMB-marginalized lensing power spectrum in units of the Planck 2018 best-fit to 1.004 ± 0.024 (68% limits), which is the tightest constraint on the CMB lensing power spectrum to date. For a base ΛCDM cosmology we find σ 8 Ωm 0.25 = 0.599 ± 0.016 from CMB lensing alone in combination with weak priors and element abundance observations. Combination with baryon acoustic oscillation data gives tight 68% constraints on individual ΛCDM parameters σ m = 0.814 ± 0.016, H 0 = 68.1+1.0 -1.1 km s-1 Mpc-1, Ωm = 0.313+0.014 -0.016. Planck polarized maps alone now constrain the lensing power to 7%.

KiDS and Euclid: Cosmological implications of a pseudo angular power spectrum analysis of KiDS-1000 cosmic shear tomography

We present a tomographic weak lensing analysis of the Kilo Degree Survey Data Release 4 (KiDS-1000), using a new pseudo angular power spectrum estimator (pseudo-Cℓ) under development for the ESA Euclid mission. Over 21 million galaxies with shape information are divided into five tomographic redshift bins, ranging from 0.1 to 1.2 in photometric redshift. We measured pseudo-Cℓ using eight bands in the multipole range 76 < ℓ < 1500 for auto- and cross-power spectra between the tomographic bins. A series of tests were carried out to check for systematic contamination from a variety of observational sources including stellar number density, variations in survey depth, and point spread function properties. While some marginal correlations with these systematic tracers were observed, there is no evidence of bias in the cosmological inference. B-mode power spectra are consistent with zero signal, with no significant residual contamination from E/B-mode leakage. We performed a Bayesian analysis of the pseudo-Cℓ estimates by forward modelling the effects of the mask. Assuming a spatially flat ΛCDM cosmology, we constrained the structure growth parameter S8 = σ8(Ωm/0.3)1/2 = 0.754−0.029+0.027. When combining cosmic shear from KiDS-1000 with baryon acoustic oscillation and redshift space distortion data from recent Sloan Digital Sky Survey (SDSS) measurements of luminous red galaxies, as well as the Lyman-α forest and its cross-correlation with quasars, we tightened these constraints to S8 = 0.771−0.032+0.006. These results are in very good agreement with previous KiDS-1000 and SDSS analyses and confirm a ∼3σ tension with early-Universe constraints from cosmic microwave background experiments.

Running vacuum versus holographic dark energy: a cosmographic comparison

We perform a comparative study of different types of dynamical dark energy models (DDEs) using the cosmographic method. Among the models being examined herein we have the Running Vacuum models (RVMs), which have demonstrated considerable ability to fit the overall cosmological data at a level comparable to the standard cosmological model, Lambda CDM, and capable of alleviating the sigma _8 and H_0 tensions. At the same time we address a variety of Holographic dark energy models (HDEs) with different options for the time (redshift)-varying model parameter c=c(z). We deal with the HDEs under the double assumption of fixed and evolving holographic length scale and assess which one is better. Both types of DDEs (RVMs and HDEs) are confronted with the most robust cosmographic data available, namely the Pantheon sample of supernovae data (SnIa), the baryonic acoustic oscillations data (BAOs) extracted from measurement of the power spectrum and bispectrum of the BOSS data release, and the cosmic chronometer measurements of the Hubble rate (CCHs) at different redshifts obtained from spectroscopic observations of passively evolving galaxies. Using these data samples we assess the viability of the mentioned DDEs and compare them with the concordance Lambda CDM model. From our cosmographic analysis we conclude that the RVMs fare comparably well to the Lambda CDM, a fact which adds up more credit to their sound phenomenological status. In contrast, while some of the HDEs are favored using the current Hubble horizon as fixed holographic length, they become highly unfavoured in the more realistic case when the holographic length is dynamical and evolves as the Hubble horizon.

Improved constraints on primordial gravitational waves in light of the H0 tension and BICEP/Keck data

The Hubble tension that the standard $\Lambda$CDM model is suffering from can be resolved with pre-recombination early dark energy. We present the first constraint on the tensor-to-scalar ratio $r$ in corresponding Hubble-tension-free cosmologies using the most recent BICEP/Keck cosmic microwave background (CMB) B-mode polarization data. We find, combining BICEP/Keck with Planck18 CMB and baryon acoustic oscillation data, that the models with larger Hubble constant $H_0$ will have tighter upper bound on $r$, and resolution $H_0\sim73$ km/s/Mpc of the Hubble tension tightens the upper bound to $r<0.028\ (95\%\text{C.L.})$, $25\%$ tighter than the $\Lambda$CDM constraint $r<0.036$. We clarify the origin of this tightening bound.

Quasar cosmology: dark energy evolution and spatial curvature

ABSTRACT We analyse some open debates in cosmology in light of the most updated quasar (QSO) sample, covering a wide redshift range up to $\mathit{ z}$ ∼ 7.5, combined with type Ia supernovae (SNe) and baryon acoustic oscillations (BAOs). Indeed, extending the cosmological analyses with high-redshift data is key to distinguishing between different cosmological models that are degenerate at low redshifts, and allowing better constraints on a possible dark energy (DE) evolution. Also, we discuss combinations of BAO, SNe, and QSO data to understand their compatibility and implications for extensions of the standard cosmological model. Specifically, we consider a flat and non-flat ΛCDM cosmology, a flat and non-flat DE model with a constant DE equation of state parameter (w), and four flat DE models with variable w, namely the Chevallier–Polarski–Linder and Jassal–Bagla–Padmanabhan models, and an ‘exponential’, and Barboza–Alcaniz parametrizations. We find that a joint analysis of QSO+SNe with BAO is only possible in the context of a flat Universe. Indeed BAO confirms the flatness condition assuming a curved geometry, whilst SNe + QSO show evidence of a closed space. We also find ΩM,0 = 0.3 in all data sets assuming a flat ΛCDM model. Yet, all the other models show a statistically significant deviation at 2-3 σ with the combined SNe + SO + BAO data set. In the models where DE density evolves with time, SNe + QSO + BAO data always prefer ΩM,0 &amp;gt; 0.3, w0 &amp;lt; −1 and wa &amp;gt; 0. This DE phantom behaviour is mainly driven by SNe + QSO, while BAO are closer to the flat ΛCDM model.

Constraining decaying dark matter with BOSS data and the effective field theory of large-scale structures

We update cosmological constraints on two decaying dark matter models in light of BOSS-DR12 data analyzed under the effective field theory of large-scale structures (EFTofLSS) formalism, together with Planck, Pantheon and other BOSS measurements of the baryonic acoustic oscillation (BAO). In the first model, a fraction ${f}_{\mathrm{dcdm}}$ of cold dark matter (CDM) decays into dark radiation (DR) with a lifetime $\ensuremath{\tau}$. In the second model (recently suggested as a potential resolution to the ${S}_{8}$ tension), all the CDM decays with a lifetime $\ensuremath{\tau}$ into DR and a massive warm dark matter (WDM) particle, with a fraction $ϵ$ of the CDM rest mass energy transferred to the DR. Using numerical codes from the recent literature, we perform the first calculation of the mildly nonlinear (matter and galaxy) power spectra with the EFTofLSS for these two models. In the case of DR products, we obtain the constraints ${f}_{\mathrm{dcdm}}\ensuremath{\lesssim}0.022$ (95% C.L.) for lifetimes shorter than the age of the Universe, and $\ensuremath{\tau}/{f}_{\mathrm{dcdm}}\ensuremath{\gtrsim}250\text{ }\text{ }\mathrm{Gyr}$ in the long-lived regime assuming ${f}_{\mathrm{dcdm}}\ensuremath{\rightarrow}1$. We show that Planck data contributes the most to these constraints, with EFTofBOSS providing a marginal improvement over conventional BAO and redshift space distortions ($f{\ensuremath{\sigma}}_{8}$) data. In the case of DR and WDM decay products, we find that EFTofBOSS data significantly improves the constraints at 68% C.L. on the CDM lifetime with a ${S}_{8}$ prior from KiDS-1000. We show that, in order to fit EFTofBOSS data while lowering ${S}_{8}$ to match KiDS-1000, the best-fit model has a longer lifetime $\ensuremath{\tau}=120\text{ }\text{ }\mathrm{Gyr}$, with a larger kick velocity ${v}_{\mathrm{kick}}/c\ensuremath{\simeq}ϵ\ensuremath{\simeq}1.2%$, than that without EFTofBOSS ($\ensuremath{\tau}=43\text{ }\text{ }\mathrm{Gyr}$, $ϵ=0.6%$). We anticipate that future surveys will provide exquisite constraints on such models.

On the distribution of Bayesian evidence

ABSTRACT We look at the distribution of the Bayesian evidence for mock realizations of supernova and baryon acoustic oscillation data. The ratios of Bayesian evidence of different models are often used to perform model selection. The significance of these Bayes factors is then interpreted using scales such as the Jeffreys or Kass &amp; Raftery scale. First, we demonstrate how to use the evidence itself to validate the model, that is to say how well a model fits the data, regardless of how well other models perform. The basic idea is that if, for some real data set, a model’s evidence lies outside the distribution of evidence that result when the same fiducial model that generates the data sets is used for the analysis, then the model in question is robustly ruled out. Further, we show how to assess the significance of a hypothetically computed Bayes factor. We show that the range of the distribution of Bayes factors can greatly depend on the models in question and also the number of data points in the data set. Thus, we have demonstrated that the significance of Bayes factors needs to be calculated for each unique data set.

Brane inflation driven by an arctan potential: CMB constraints and reheating

We investigate the early universe evolution in the context of brane inflation driven by a supergravity-inspired arctan potential. We performed a slow-roll and a semi-analytical reheating analyses and obtained constraints on the inflationary parameters in agreement with Planck 2018 data. We also employed a Markov Chain Monte Carlo analysis to perform a parameter estimation of the cosmological parameters, obtaining results in good agreement with the currently available cosmic microwave background and baryon acoustic oscillation data. This work establishes the general theoretical predictions of the arctan model, with the results of the statistical analysis corroborating its observational viability.

A cosmological underdensity does not solve the Hubble tension

A potential solution to the Hubble tension is the hypothesis that the Milky Way is located near the center of a matter underdensity. We model this scenario through the Lemaître-Tolman-Bondi formalism with the inclusion of a cosmological constant (ΛLTB) and consider a generalized Gaussian parametrization for the matter density profile. We constrain the underdensity and the background cosmology with a combination of data sets: the Pantheon Sample of type Ia supernovae (both the full catalogue and a redshift-binned version of it), a collection of baryon acoustic oscillations data points and the distance priors extracted from the latest Planck data release. The analysis with the binned supernovae suggests a preference for a -13 % density drop with a size of approximately 300 Mpc, interestingly matching the prediction for the so-called KBC void already identified on the basis of independent analyses using galaxy distributions. The constraints obtained with the full Pantheon Sample are instead compatible with a homogeneous cosmology and we interpret this radically different result as a cautionary tale about the potential bias introduced by employing a binned supernova data set. We quantify the level of improvement on the Hubble tension by analyzing the constraints on the B-band absolute magnitude of the supernovae, which provides the calibration for the local measurements of H 0. Since no significant difference is observed with respect to an analogous fit performed with a standard ΛCDM cosmology, we conclude that the potential presence of a local underdensity does not resolve the tension and does not significantly degrade current supernova constraints on H 0.

Revisiting a non-parametric reconstruction of the deceleration parameter from combined background and the growth rate data

The cosmic deceleration parameter q has been reconstructed in a non-parametric way using various combinations of recent observational datasets. The Pantheon compilation of the Supernova (SN) distance modulus data, the Cosmic Chronometer (CC) measurements of the Hubble parameter including the full systematics and the Baryon Acoustic Oscillation (BAO) data have been considered in this work. The redshift z t , where the transition from a past decelerated to a late-time accelerated phase of evolution occurs, is estimated from the reconstructed q . The possible effect of a non-zero spatial curvature from the Planck 2020 estimate is checked. The outcome of including different H 0 measurements from recent Planck 2020 and Riess 2021 probes having a maximum discrepancy at the 4 . 2 σ level, is investigated. Results indicate that the transition from a past decelerated phase to the late-time accelerated phase occurs within the redshift range 0 . 5 < z < 1 . The reconstructed q is observed to have a non-monotonic evolution in case of the combined CC and SN data for z > 1 , which becomes oscillatory on introducing the BAO data. To investigate the effect of matter perturbations, the growth rate data from the Redshift-Space Distortions (RSD) are utilized in reconstructing q . Using the O m ( z ) diagnostic, we draw inferences on the validity of Λ CDM as a consistency check. The Λ CDM model is well consistent and included at the 2 σ level in the domain of all the reconstructions.

Fluctuations in the Ginzburg–Landau Theory of Dark Energy: Internal (In)consistencies in the Planck Data Set

In this work, predictions of the Ginzburg–Landau theory of dark energy (GLT) for cosmic microwave background (CMB) lensing are studied. We find that the time and scale dependence of the dark energy fluctuations in this semiphenomenological model is favored by data in several ways. First, unlike ΛCDM, ℓ ≤ 801 and ℓ > 801 ranges of the CMB angular power spectrum are consistent in this framework. Second, the lensing amplitude A L is completely consistent with unity when GLT is confronted with CMB data, even without including CMB lensing data. Therefore the lensing anomaly is absent in this model. Although the background evolution of dark energy in this model is able to reconcile the H 0 inferred from CMB with that directly measured through observing nearby standard candles, the inclusion of Baryon Acoustic Oscillations (BAO) data brings the inferred H 0 close to what ΛCDM predicts and hence the Hubble tension is not fully eased. However, this does not affect the posterior on A L and the lensing anomaly is still absent.

Testing f(R) gravity models with quasar x-ray and UV fluxes

Recently, active galactic nuclei (AGN) have been proposed as ``standardizable candles,'' thanks to an observed nonlinear relation between their x-ray and optical-ultraviolet (UV) luminosities, which provides an independent measurement of their distances. In this paper, we use these observables for the first time to estimate the parameters of $f(R)$ gravity models (specifically, the Hu-Sawicki and the exponential models) together with the cosmological parameters. The importance of these types of modified gravity theories lies in the fact that they can explain the late time accelerated expansion of the universe without the inclusion of a dark energy component. We have also included other observable data to the analyses such as estimates of the Hubble parameter $H(z)$ from cosmic chronometers (CCs), the Pantheon Type Ia (SnIa) supernovae compilation, and baryon acoustic oscillation (BAO) measurements. The $1\ensuremath{\sigma}$ inferred constraints using all datasets are $b\ensuremath{\le}0.276$, ${\mathrm{\ensuremath{\Omega}}}_{m}=0.30{4}_{\ensuremath{-}0.011}^{+0.010}$, and ${H}_{0}=67.55{3}_{\ensuremath{-}0.936}^{+1.242}$ for the Hu-Sawicki model, and $b=0.78{5}_{\ensuremath{-}0.606}^{+0.409}\text{ }$ ${\mathrm{\ensuremath{\Omega}}}_{m}=0.30{5}_{\ensuremath{-}0.010}^{+0.011}$ and ${H}_{0}=68.34{8}_{\ensuremath{-}0.760}^{+0.959}$ for the exponential one, but we stress that for both $f(R)$ models results within $2\ensuremath{\sigma}$ are consistent with the $\mathrm{\ensuremath{\Lambda}}$ cold dark matter (CDM) model. Our results show that the allowed space parameter is restricted when both AGN and BAO data are added to CC and SnIa data, with the BAO dataset being the most restrictive one. We can conclude that both the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model and small deviations from general relativity given by the $f(R)$ models studied in this paper are allowed by the considered observational datasets.

Impact of $$H_0$$ priors on f(T) late time cosmology

We present a detailed analysis of the impact of $$H_0$$ priors from recent surveys in the literature on the late time cosmology of five f(T) cosmological models using cosmic chronometers, the Pantheon data set, and baryonic acoustic oscillation data. In this work, we use three recently reported values of $$H_0$$ that have contributed to the recent $$H_0$$ tension problem. We find that these priors have a strong response in these analyses in terms of all the cosmological parameters. In general, our analyses give much higher values of $$H_0$$ when considered against equivalent analyses without priors while, by and large, giving lower values of the matter density parameter. We close with a cross-analysis of each of our model, data set and prior combination choices.

Tsallis holographic dark energy reconsidered

We consider the interacting Tsallis Holographic Dark Energy (THDE), with the Granda–Oliveros (GO) scale as the infrared (IR) cutoff, as dynamical vacuum. We analytically solved for the Hubble parameter, in a spatially flat FLRW universe with dark energy and matter as components, and the solution traces the evolutionary path from the prior decelerated to the late accelerated epoch. Without interaction, the model predicts a varLambda CDM like behavior with an effective cosmological constant. We used Pantheon Supernovae type Ia, observational Hubble data (OHD), cosmic microwave background (CMB), and baryon acoustic oscillation (BAO) data to constrain the free parameters of the model. The estimated values of the cosmological parameters were consistent with observational results. We analyzed the behavior of the model using the statefinder and omega ^prime _{e}-omega _{e} plane where omega _{e} and omega ^prime _{e} corresponds to the effective equation of state and its evolution, respectively. The model shows a quintessence behavior in general, and the model trajectory ends in a point that corresponds to the de Sitter phase. We performed a dynamical analysis of the model, concluding that the prior decelerated and late accelerated phases are unstable and stable equilibria, respectively. We also investigated the thermodynamical nature of the model and found that the generalized second law remains valid in the dynamical vacuum treatment of the model.

Linear Nash-Greene fluctuations on the evolution of S_8 and H_0 tensions

We present the perturbation equations in an embedded four space-time from the linear Nash-Greene fluctuations of background metric. In the context of a five-dimensional bulk, we show that the cosmological perturbations are only propagated by the gravitational tensorial field equation. In Newtonian conformal gauge, we study the matter density evolution in sub-horizon regime and on how such scale may be affected by the extrinsic curvature. We apply a joint likelihood analysis to the data by means of the Markov Chain Monte Carlo (MCMC) method for parameter estimation using a pack of recent datasets as the Pantheon Supernovae type Ia, the Baryon Acoustic Oscillations (BAO) from DR12 galaxy sample and Dark Energy Survey (DESY1). We discuss the tensions on the Hubble constant H_0 and the growth amplitude factor S_8 of the observations from Planck 2018 Cosmic Microwave Background (CMB) and the local measurements of H_0 with Hubble Space Telescope (HST) photometry and Gaia EDR3. As a result, we obtain an alleviation below sim 1sigma in the contours (S_8-varOmega _m) at 68.4% confidence level (CL) when compared with DESY1 data. On the other hand, the H_0 tension persists with sim 2.6sigma at 68.4% CL and 1.95sigma at 95.7% CL, aggravated with the inclusion of BAO data.

DGP and DGP-like cosmologies from f(Q) actions

In this work we explore and test new formulations of cosmological scenarios in $f(Q)$ theories. In these settings, the nonmetricity scalar ($Q$) is the main source of gravity and Friedmann equations are modified to account for the associated degrees of freedom. This work focuses first on the derivation, and then theoretical and observational analysis of two such (new) exact cosmological models; they both display a nonstandard behavior in which an additional parameter encoding nonmetricity effects acts in the fashion of a screened cosmological constant. One of the new settings has the same background evolution as the well know DGP cosmological model, while the other resembles the former considerably, although its origin is purely phenomenological. We use the Markov Chain Montecarlo method combined with standard statistical techniques to perform observational astrophysical tests relying upon background data, specifically these are type Ia supernovae luminosities and direct Hubble data (from cosmic clocks), along with cosmic microwave background shift and baryon acoustic oscillations data. In addition, we compute some of the cosmographic parameters and other discriminators with the purpose of refining our knowledge about these models in the light of their theoretical and observational signatures, and this allows for a better comparison with the (concordance) $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ setup. We conclude that these scenarios do not show signatures indicating a departure from the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ behavior.

Using lower-redshift, non-CMB, data to constrain the Hubble constant and other cosmological parameters

Abstract We use updated Hubble parameter and baryon acoustic oscillation data, as well as other lower-redshift Type Ia supernova, Mg ii reverberation-measured quasar, quasar angular size, H ii starburst galaxy, and Amati-correlated gamma-ray burst data, to jointly constrain cosmological parameters in six cosmological models. The joint analysis provides model-independent determinations of the Hubble constant, H0 = 69.7 ± 1.2 $\rm {km \ s^{-1} \ Mpc^{-1}}$, and the current non-relativistic matter density parameter, Ωm0 = 0.295 ± 0.017. These error bars are factors of 2.2 and 2.3 larger than the corresponding error bars in the flat ΛCDM model from Planck TT,TE,EE+lowE+lensing cosmic microwave background anisotropy data. Based on the deviance information criterion (DIC), the flat ΛCDM model is most favored but mild dark energy dynamics and a little spatial curvature are not ruled out.