Abstract

Observations spanning a large wavelength range, from X-ray to radio, of the Type IIb supernova (SN) 2011hs are presented, covering its evolution during the first year after explosion. The optical light curve presents a narrower shape and a fainter luminosity at peak than previously observed for Type IIb SNe. High expansion velocities are measured from the broad absorption H i and He i lines. From the comparison of the bolometric light curve and the time evolution of the photospheric velocities with hydrodynamical models, we found that SN 2011hs is consistent with the explosion of a 3-4 M-circle dot He-core progenitor star, corresponding to a main-sequence mass of 12-15 M-circle dot, that ejected a mass of Ni-56 of about 0.04 M-circle dot, with an energy of E = 8.5 x 10(50) ERG. Such a low-mass progenitor scenario is in full agreement with the modelling of the nebular spectrum taken at similar to 215 d from maximum. From the modelling of the adiabatic cooling phase, we infer a progenitor radius of approximate to 500-600 R-circle dot, clearly pointing to an extended progenitor star. The radio light curve of SN 2011hs yields a peak luminosity similar to that of SN 1993J, but with a higher mass-loss rate and a wind density possibly more similar to that of SN 2001ig. Although no significant deviations from a smooth decline have been found in the radio light curves, we cannot rule out the presence of a binary companion star.