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We show that it is not possible to determine the final mass $M_{\rm fin}$ ofa red supergiant (RSG) at the pre-supernova (SN) stage from its luminosity $L$and effective temperature $T_{\rm eff}$ alone. Using a grid of stellar models,we demonstrate that for a given value of $L$ and $T_{\rm eff}$, a RSG can havea range of $M_{\rm fin}$ as wide as 3 to $45~\mathrm{M}_{\odot}$. While theprobability distribution within these limits is not flat, any individualdetermination of $M_{\rm fin}$ for a RSG will be degenerate. This makes itdifficult to determine its evolutionary history and to map $M_{\rm fin}$ to aninitial mass. Single stars produce a narrower range that is difficult toaccurately determine without making strong assumptions about mass loss,convection, and rotation. Binaries would produce a wider range of RSG $M_{\rmfin}$. However, the final Helium core mass M$_{\rm He-core}$ is well determinedby the final luminosity and we find $\log (\mathrm{M}_{\rm He-core}/M_{\odot})= 0.659 \log (L/\mathrm{L}_{\odot}) -2.630$ Using this relationship, we deriveM$_{\rm He-core}$ for directly imaged SN progenitors and one failed SNcandidate. The value of $M_{\rm fin}$ for stripped star progenitors of SNe IIbis better constrained by $L$ and $T_{\rm eff}$ due to the dependence of $T_{\rmeff}$ on the envelope mass $M_{\rm env}$ for $M_{\rm env} \lesssim1~$M$_{\odot}$. Given the initial mass function, our results apply to themajority of progenitors of core collapse SNe, failed SNe and direct collapseblack holes.

The Uncertain Masses of Progenitors of Core Collapse Supernovae and Direct Collapse Black Holes