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We present the spectroscopic and photometric evolution of the nearby (z =0.059) spectroscopically confirmed type Ic supernova, SN 2010bh, associatedwith the soft, long-duration gamma-ray burst (X-ray flash) GRB 100316D.Intensive follow-up observations of SN 2010bh were performed at the ESO VeryLarge Telescope (VLT) using the X-shooter and FORS2 instruments. Owing to thedetailed temporal coverage and the extended wavelength range (3000--24800 A),we obtained an unprecedentedly rich spectral sequence among the hypernovae,making SN 2010bh one of the best studied representatives of this SN class. Wefind that SN 2010bh has a more rapid rise to maximum brightness (8.0 +/- 1.0rest-frame days) and a fainter absolute peak luminosity (L_bol~3e42 erg/s) thanpreviously observed SN events associated with GRBs. Our estimate of the ejected(56)Ni mass is 0.12 +/- 0.02 Msun. From the broad spectral features we measureexpansion velocities up to 47,000 km/s, higher than those of SNe 1998bw (GRB980425) and 2006aj (GRB 060218). Helium absorption lines He I lambda5876 and HeI 1.083 microm, blueshifted by ~20,000--30,000 km/s and ~28,000--38,000 km/s,respectively, may be present in the optical spectra. However, the lack ofcoverage of the He I 2.058 microm line prevents us from confirming suchidentifications. The nebular spectrum, taken at ~186 days after the explosion,shows a broad but faint [O I] emission at 6340 A. The light-curve shape andphotospheric expansion velocities of SN 2010bh suggest that we witnessed ahighly energetic explosion with a small ejected mass (E_k ~ 1e52 erg and M_ej ~3 Msun). The observed properties of SN 2010bh further extend the heterogeneityof the class of GRB supernovae.

The Highly Energetic Expansion of SN2010bh Associated with GRB 100316D