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tokens: that the progenitor was enshrouded in a dusty cocoon of material that was lost close to the explosion. If the SN was not an electron capture SN it would have been the explosion of a 11 M ⊙ red supergiant. However 2008S has little in common with other such SN from progenitors in this mass range (Smartt 2015 ; Davies Beasor 2018 ). In conclusion using the new distance to determine the luminosity of the progenitor we find it more likely than before that SN 2008S was an electron capture event. It also was likely to have been the result of a binary interaction which was suggested by Podsiadlowski et al. ( 2004 ) to be the most likely channel for such core-collapse events. While SN 2008S is at the minimum mass for a core-collapse SNe, N6946-BH1 is at the maximum mass for a core-collapse of a red supergiant. This star was observed to rapidly fade with a light curve that was in agreement with a source powered by a feeding black hole (Adams et al. 2017 ). When the nature of the progenitor was examined this study assumed a distance of 5.95 Mpc. Therefore again this increases the suggested progenitor luminosity from log ( L/L ⊙ ) = 5.3 to 5.5. As shown in Fig. 1 this increase in the luminosity implied a mass for the progenitor star or 24 M ⊙ that is above the predicted mass limit for the formation of a black hole. This is also consistent with the mass estimated from the surrounding stellar population by Murphy et al. ( 2018 ). Again while it is only one event tension between the mass estimates for black hole formation and the luminosity of the observed progenitor stars are reduced by this study. We note that this result is in agreement with the work of Murphy et al. ( 2018 ). 4 CONCLUSIONS We have re-evaluated the distance to NGC 6946. The value of 5.9 Mpc is incorrect and should not be used in future studies. We used the observed SN rate to estimate the star formation rate and thus the FUV luminosity of the galaxy. Using the standard candel method we derive a distance of 7.9 ± 4.0 Mpc. This is consistent with the more recent distances estimated by Anand et al. ( 2018 ) and Murphy et al. ( 2018 ) of 7.72 ± 0.32 Mpc and 7.83 ± 0.29 Mpc, respectively. We strongly recommend that all future studies concerning NGC 6946 use the updated distance of 7.72 ± 0.32 Mpc from Anand et al. ( 2018 ). Their distance is consistent with the distance of Murphy et al. ( 2018 ) but Anand et al. ( 2018 ) took additional steps to reduce contamination and is therefore preferred. We re-evaluated the nature of the five progenitors of observed core collapse events in NGC 6946 using the distance of 7.72 ± 0.32 Mpc. We found that the mass constraints change significantly. The two most significant changes are: first, that the observed progenitor of SN 2008S is now more consistent with predictions for the progenitors of electron capture SNe. We suggest that SN 2008S was an electron capture SN with the progenitor having experienced a binary interaction before explosion. Second, the