  The masses and radii of exoplanets are fundamental quantities needed for
their characterisation. Studying the different populations of exoplanets is
important for understanding the demographics of the different planetary types,
which can then be linked to planetary formation and evolution. We present an
updated exoplanet catalog based on reliable, robust and as much as possible
accurate mass and radius measurements of transiting planets up to 120
$M_{\oplus}$. The resulting mass-radius (M-R) diagram shows two distinct
populations, corresponding to rocky and volatile-rich exoplanets which overlap
in both mass and radius. The rocky exoplanet population shows a relatively
small density variability and ends at mass of $\sim25 M_{\oplus}$, possibly
indicating the maximum core mass that can be formed. We use the composition
line of pure-water to separate the two populations, and infer two new empirical
M-R relations based on this data: $ M = (0.9 \pm 0.06) \ R^{(3.45 \pm 0.12)}$
for the rocky population, and $ M = (1.74 \pm 0.38) \ R^{(1.58 \pm 0.10)}$ for
the volatile-rich population. While our results for the two regimes are in
agreement with previous studies, the new M-R relations better match the
population in the transition-region from rocky to volatile-rich exoplanets,
which correspond to a mass range of 5-25 $M_{\oplus}$ and a radius range of 2-3
$R_{\oplus}$.
