A More Accurate and Competitive Estimative of $H_0$ in Intermediate
  Redshifts
  In order to clarify the tension between estimates of the Hubble Constant
($H_0$) from local ($z \ll 1$) and global ($z \gg 1$) measurements, Lima and
Cunha (LC) proposed a new method to measure $H_0$ in intermediate redshifts ($z
\approx 1$), which were obtained $H_0 = 74.1 \pm 2.2$ km s$^{-1} $Mpc$^{-1}$
($1 \sigma$), in full agreement to local measurements via Supernovae/Cepheid
dataset. However, Holanda \textit{et al.} (2014) affirm that a better
understanding of the morphology of galaxy clusters in LC framework is needed to
a more robust and accurate determination of $H_0$. Moreover, that kind of
sample has been strongly questioned in the literature. In this context, (i) we
investigated if the sample of galaxy clusters used by LC has a relevant role in
their results, then (ii) we perform a more accurate and competitive
determination of $H_0$ in intermediate redshifts, free of unknown systematic
uncertainties. First, we found that the exclusion of the sample of galaxy
clusters from the determination initially proposed by LC leads to significantly
different results. Finally, we performed a new determination in $H_0$, where we
obtained $H_0 = 68.00 \pm 2.20$ km s$^{-1}$ Mpc$^{-1}$ ($1 \sigma$) with
statistical and systematic errors and $H_0 = 68.71^{+1.37}_{-1.45}$ km s$^{-1}$
Mpc$^{-1}$ ($1 \sigma$) with statistical errors only. Contrary to those
obtained by LC, these values are in full harmony with the global measurements
via Cosmic Microwave Background (CMB) radiation and to the other recent
estimates of $H_0$ in intermediate redshifts.
