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The core collapse supernova (CCSN) rate provides a strong lower limit for thestar formation rate (SFR). Progress in using it as a cosmic SFR tracer requiressome confidence that it is consistent with more conventional SFR diagnostics inthe nearby Universe. This paper compares standard SFR measurements based onHalpha, FUV and TIR galaxy luminosities with the observed CCSN rate in the samegalaxy sample. The comparison can be viewed from two perspectives. Firstly, byadopting an estimate of the minimum stellar mass to produce a CCSN one candetermine a SFR from SN numbers. Secondly, the radiative SFRs can be assumed tobe robust and then the SN statistics provide a constrain on the minimum stellarmass for CCSN progenitors. The novel aspect of this study is that Halpha, FUVand TIR luminosities are now available for a complete galaxy sample within thelocal 11Mpc volume and the number of discovered SNe in this sample within thelast 13 years is high enough to perform a meaningful statistical comparison. Weexploit the multi-wavelength dataset from 11HUGS, a volume-limited surveydesigned to provide a census of SFR in the local Volume. Assuming a lower limitfor CCSN progenitors of 8 Msun, the CCSN rate matches the SFR from the FUVluminosity. However the SFR based on Halpha luminosity is lower than these twoestimates by a factor of nearly 2. If we assume that the FUV or Halpha basedluminosities are a true reflection of the SFR, we find that the minimum massfor CCSN progenitors is 8 +/- 1 Msun, and 6 +/- 1 Msun, respectively. Theestimate of the minimum mass for CCSN progenitors obtained exploiting FUV datais in good agreement with that from the direct detection of CCSN progenitors.The concordant results by these independent methods point toward a constraintof 8 +/- 1 Msun on the lower mass limit for progenitor stars of CCSNe.

A comparison between star formation rate diagnostics and rate of core collapse supernovae within 11 Mpc