The expansion rate of the intermediate universe in light of Planck

We use cosmology-independent measurements of the expansion history in the redshift range 0.1 less than or similar to z < 1.2 and compare them with the Cosmic Microwave Background-derived expansion history predictions. The motivation is to investigate if the tension between the local (cosmology independent) Hubble constant H-0 value and the Planck-derived H-0 is also present at other redshifts. We conclude that there is no tension between Planck and cosmology independent-measurements of the Hubble parameter H(z) at 0.1 less than or similar to z < 1.2 for the Lambda CDM model (odds of tension are only 1:15, statistically not significant). Considering extensions of the Lambda CDM model does not improve these odds (actually makes them worse), thus favouring the simpler model over its extensions. On the other hand the H(z) data are also not in tension with the local H-0 measurements but the combination of all three data-sets shows a highly significant tension (odds similar to 1:400). Thus the new data deepen the mystery of the mismatch between Planck and local H-0 measurements, and cannot univocally determine whether it is an effect localised at a particular redshift. Having said this, we find that assuming the NGC4258 maser distance as the correct anchor for H-0, brings the odds to comfortable values. Further, using only the expansion history measurements we constrain, within the Lambda CDM model, H-0 = 68.5 +/- 3.5 and Omega(m) = 0.32 +/- 0.05 (at 68% confidence) without relying on any CMB prior. We also address the question of how smooth the expansion history of the Universe is given the cosmology independent data and conclude that there is no evidence for deviations from smoothness on the expansion history, neither variations with time in the value of the equation of state of dark energy. (C) 2014 The Authors. Published by Elsevier B.V.