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SN 2014C was an unprecedented supernova (SN) that displayed a metamorphosisfrom Type Ib to Type IIn over $\sim$200 days. This transformation is consistentwith a helium star having exploded in a cavity surrounded by a dense shell ofthe progenitor's stripped hydrogen envelope. For at least 5 yearspost-explosion, the ejecta continued to interact with an outer, extendedcomponent of circumstellar medium (CSM) that was ejected even before the denseshell. It is still unclear, however, what kind of progenitor could haveundergone such a complicated mass-loss history before it produced this peculiarSN. In this paper, we report a new analysis of SN 2014C's host star clusterbased on data from the Hubble Space Telescope (HST). By carefully fitting itsspectral energy distribution (SED), we derive a precise cluster age of20.0$^{+3.5}_{-2.6}$ Myr, which corresponds to the progenitor's lifetimeassuming coevolution. Combined with binary stellar evolution models, we findthat SN 2014C's progenitor may have been an $\sim$11-$M_\odot$ star in arelatively wide binary system. The progenitor's envelope was partially strippedby Case C or Case BC mass transfer via binary interaction, followed by aviolent eruption that ejected the last hydrogen layer before terminalexplosion. Thus, SN 2014C, in common with SNe 2006jc and 2015G, may be a thirdexample that violent eruptions, with mass-loss rates matching luminous bluevariable (LBV) giant eruptions, can also occur in much lower-mass massive starsif their envelopes are partially or completely stripped in interactingbinaries.

The changing-type SN 2014C may come from an 11-$M_\odot$ star stripped by binary interaction and violent eruption