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We present Hubble Space Telescope imaging of a pre-explosion counterpart toSN 2019yvr obtained 2.6 years before its explosion as a type Ib supernova (SNIb). Aligning to a post-explosion Gemini-S/GSAOI image, we demonstrate thatthere is a single source consistent with being the SN 2019yvr progenitorsystem, the second SN Ib progenitor candidate after iPTF13bvn. We also analyzedpre-explosion Spitzer/IRAC imaging, but we do not detect any counterparts atthe SN location. SN 2019yvr was highly reddened, and comparing its spectra andphotometry to those of other, less extinguished SNe Ib we derive$E(B-V)=0.51\substack{+0.27\\-0.16}$ mag for SN 2019yvr. Correcting photometryof the pre-explosion source for dust reddening, we determine that this sourceis consistent with a $\log(L/L_{\odot}) = 5.3 \pm 0.2$ and $T_{\mathrm{eff}} =6800\substack{+400\\-200}$ K star. This relatively cool photospherictemperature implies a radius of 320$\substack{+30\\-50} R_{\odot}$, much largerthan expectations for SN Ib progenitor stars with trace amounts of hydrogen butin agreement with previously identified SN IIb progenitor systems. Thephotometry of the system is also consistent with binary star models thatundergo common envelope evolution, leading to a primary star hydrogen envelopemass that is mostly depleted but seemingly in conflict with the SN Ibclassification of SN 2019yvr. SN 2019yvr had signatures of strong circumstellarinteraction in late-time ($>$150 day) spectra and imaging, and so we considereruptive mass loss and common envelope evolution scenarios that explain the SNIb spectroscopic class, pre-explosion counterpart, and dense circumstellarmaterial. We also hypothesize that the apparent inflation could be caused by aquasi-photosphere formed in an extended, low-density envelope or circumstellarmatter around the primary star.

A Cool and Inflated Progenitor Candidate for the Type Ib Supernova 2019yvr at 2.6 Years Before Explosion