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A set of hydrodynamical models based on stellar evolutionary progenitors isused to study the nature of SN 2011dh. Our modeling suggests that a largeprogenitor star ---with R ~200 Rsun---, is needed to reproduce the early lightcurve of SN 2011dh. This is consistent with the suggestion that the yellowsuper-giant star detected at the location of the SN in deep pre-explosionimages is the progenitor star. From the main peak of the bolometric light curveand expansion velocities we constrain the mass of the ejecta to be ~2 Msun, theexplosion energy to be E= 6-10 x 10^50 erg, and the 56Ni mass to beapproximately 0.06 Msun. The progenitor star was composed of a helium core of 3to 4 Msun and a thin hydrogen-rich envelope of ~0.1 M_sun with a main sequencemass estimated to be in the range of 12--15 Msun. Our models rule outprogenitors with helium-core masses larger than 8 Msun, which correspond toM_ZAMS > 25 Msun. This suggests that a single star evolutionary scenario for SN2011dh is unlikely.

The Type IIb Supernova 2011dh from a Supergiant Progenitor