Hydrodynamical modelling of Type IIb SNe
We present HYDE, a new one-dimensional hydrodynamical code, and use it to construct a grid of supernova (SN) models based on solar-metallicity bare helium-core models evolved to the verge of core-collapse with MESA STAR. This grid is suited to model Type IIb SNe, which progenitor stars are thought to have lost all but a tiny fraction of their hydrogen envelopes. Using an automated procedure we fit the bolometric lightcurves and photospheric velocities for a large sample of (17) Type IIb SNe to the grid of SN models. We find that the distribution of initial masses for the sample can be reasonably well described by a standard Salpeter IMF, although there is an under-population in the >25 M$_\odot$ range. The fractions of SNe with initial masses <15 M$_\odot$ and <20 M$_\odot$ are 56 and 81 percent, respectively, suggesting either the binary channel to dominate the production of Type IIb SNe or a flaw in our understanding of single-star mass-loss. We find correlations between the explosion energy, initial mass and mass of $^{56}$Ni; the explosion energy increases with initial mass and the mass of $^{56}$Ni increases with explosion energy. The method used allows us to determine the errors in the model parameters arising from the observed quantities and the degeneracy of the solution. We find that an error in the distance and extinction propagates mainly to the derived mass of $^{56}$Ni, whereas an error in the photospheric velocity propagates mainly to the derived helium-core mass and explosion energy. Fits using the bolometric lightcurve alone are completely degenerate along the M$_{\mathrm{ej}}^{2}$/E$_{\mathrm{ej}}$=const curve, whereas fits using also the photospheric velocities are quite robust for well-sampled SNe. Finally, we provide a description and tests of the HYDE code, and a discussion of the limitations of the method used.