  In a recent paper (Crida et al. 2018, accepted on April 19), we presented a
method to derive the mass and radius of a transiting exoplanet and their
intrinsic correlation, that we applied to 55 Cnc e. We wrote: "More precise
observations of the transit would be very useful in this particular case and
would allow to increase significantly the gain on the planetary density
precision." Three months later, Bourrier et al. (2018) published new
observations of the system. Additionally, Gaia's DR2 was released on April 25,
2018. The purpose of this research note is solely to implement these precise
new data in our pipeline to provide an up-to-date result of our model. We find
$R_p = 1.947\pm 0.038\,R_\oplus$ and $M_p = 8.59\pm 0.43\,M_\oplus$. We also
double the precision on the planetary density ($\rho_p = 1.164\pm
0.062\,\rho_\oplus$), which allows us to refine the estimates for all interior
parameters of interest. In particular, we now find that the radius of the
gaseous envelope is $0.03\pm 0.02\,R_p$.
