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We report the first detection of a credible progenitor system for a Type Icsupernova (SN Ic), SN 2017ein. We present spectra and photometry of the SN,finding it to be similar to carbon-rich, low-luminosity SNe Ic. Using apost-explosion Keck adaptive optics image, we precisely determine the positionof SN 2017ein in pre-explosion \hst\ images, finding a single source coincidentwith the SN position. This source is marginally extended, and is consistentwith being a stellar cluster. However, under the assumption that the emissionof this source is dominated by a single point source, we perform point-spreadfunction photometry, and correcting for line-of-sight reddening, we find it tohave $M_{\rm F555W} = -7.5\pm0.2$ mag and $m_{\rm F555W}-m_{\rmF814W}$=$-0.67\pm0.14$ mag. This source is bluer than the main sequence andbrighter than almost all Wolf-Rayet stars, however it is similar to some WC+O-and B-star binary systems. Under the assumption that the source is dominated bya single star, we find that it had an initial mass of $55\substack{+20-15}M_{\odot}$. We also examined binary star models to look for systems that matchthe overall photometry of the pre-explosion source and found that thebest-fitting model is a $80$+$48 M_{\odot}$ close binary system in which the$80 M_{\odot}$ star is stripped and explodes as a lower mass star. Late-timephotometry after the SN has faded will be necessary to cleanly separate theprogenitor star emission from the additional coincident emission.

A Potential Progenitor for the Type Ic Supernova 2017ein