1712.00677
The $H_0$ and $\sigma_8$ tensions and the scale invariant spectrum
Benetti, Graef, Alcaniz
In a previous communication showed that a joint analysis of CMB data and the current measurement of the local expansion rate favors a model with a scale invariant spectrum HZ over the minimal LambdaCDM scenario provided that the effective number of relativistic degrees of freedom, N_eff, is taken as a free parameter. Such a result is basically obtained due to the HST value of the Hubble constant, H0=73.24±1.74 km/s/Mpc (68% CL), as the CMB data alone discard the HZ+N_eff model. Although such a model is not physically motivated by current scenarios of the early universe, observations pointing to a scale invariant spectrum may indicate that the origin of cosmic perturbations lies in an unknown physical process. Here, extend the previous results performing a Bayesian analysis using joint CMB, HST and BAO measurements. In order to take into account the well-known tension on the value of the fluctuation amplitude parameter, sigma_8, also consider Cluster Number counts (CN) and WL data. Use two different sample of BAO data, which are obtained using 2pt spatial (BAO 2PCF) and angular (BAO 2PACF) correlation functions. The results show that a joint CMB+HST+BAO 2PACF favors the former model, even when an extended dataset with NC [CN?] and WL is considered.
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