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 < 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 H0 value and the Planck-derived H0 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 < z < 1.2 for the
LCDM model (odds of tension are only 1:15, statistically not significant).
Considering extensions of the LCDM 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 H0 measurements
but the combination of all three data-sets shows a highly significant tension
(odds ~ 1:400). Thus the new data deepen the mystery of the mismatch between
Planck and local H0 measurements, and cannot univocally determine wether 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 H0, brings the
odds to comfortable values.
  Further, using only the expansion history measurements we constrain, within
the LCDM model, H0 = 68.5 +- 3.5 and Omega_m = 0.32 +- 0.05 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.
