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Core-collapse supernova (SN) explosions mark the end of the tumultuous lifeof massive stars. Determining the nature of their progenitors is a crucial steptowards understanding the properties of SNe. Until recently, no progenitor hasbeen directly detected for SN of type Ibc, which are believed to come frommassive stars that lose their hydrogen envelope through stellar winds and frombinary systems where the companion has stripped the H envelope from theprimary. Here we analyze recently reported observations of iPTF13bvn, whichcould possibly be the first detection of a SN Ib progenitor based onpre-explosion images. Very interestingly, the recently published Geneva modelsof single stars can reproduce the observed photometry of the progenitorcandidate and its mass-loss rate, confirming a recently proposed scenario. Wefind that a single WR star with initial mass in the range 31-35 Msun fits theobserved photometry of the progenitor of iPTF13bvn. The progenitor likely has aluminosity of log (L/Lsun)~5.55, surface temperature ~45000 K, and mass of~10.9 Msun at the time of explosion. Our non-rotating 32 Msun modeloverestimates the derived radius of the progenitor, although this could likelybe reconciled with a fine-tuned model of a more massive (between 40 and 50Msun), hotter, and luminous progenitor. Our models indicate a very uncertainejecta mass of ~8 Msun, which is higher than the average of the SN Ib ejectamass that is derived from the lightcurve (2-4 Msun). This possibly high ejectamass could produce detectable effects in the iPTF13bvn lightcurve and spectrum.If the candidate is indeed confirmed to be the progenitor, our results suggestthat stars with relatively high initial masses (>30 Msun) can produce visibleSN explosions at their deaths and do not collapse directly to a black hole.

Progenitors of supernova Ibc: a single Wolf-Rayet star as the possible progenitor of the SN Ib iPTF13bvn