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Long-duration gamma-ray bursts (GRBs) at z < 1 are in most cases found to beaccompanied by bright, broad-lined Type Ic supernovae (SNe Ic-BL). Thehighest-energy GRBs are mostly located at higher redshifts, where theassociated SNe are hard to detect observationally. Here we present early andlate observations of the optical counterpart of the very energetic GRB 130427A.Despite its moderate redshift z = 0.3399+/-0.0002, GRB 130427A is at the highend of the GRB energy distribution, with an isotropic-equivalent energy releaseof Eiso ~ 9.6x10^53 erg, more than an order of magnitude more energetic thanother GRBs with spectroscopically confirmed SNe. In our dense photometricmonitoring, we detect excess flux in the host-subtracted r-band light curve,consistent with what expected from an emerging SN, ~0.2 mag fainter than theprototypical SN 1998bw. A spectrum obtained around the time of the SN peak(16.7 days after the GRB) reveals broad undulations typical of SNe Ic-BL,confirming the presence of a SN, designated SN 2013cq. The spectral shape andearly peak time are similar to those of the high expansion velocity SN 2010bhassociated with GRB 100316D. Our findings demonstrate that high-energylong-duration GRBs, commonly detected at high redshift, can also be associatedwith SNe Ic-BL, pointing to a common progenitor mechanism.

Discovery of the broad-lined Type Ic SN 2013cq associated with the very energetic GRB 130427A