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SN 2019yvr is the second Type Ib supernova (SN) with a possible directdetection of its progenitor (system); however, the spectral energy distribution(SED) of the pre-explosion source appears much cooler and overluminous than anexpected helium-star progenitor. Using Hubble Space Telescope (HST) images andMUSE integral-field-unit (IFU) spectroscopy, we find the SN environmentcontains three episodes of star formation; the low ejecta mass suggests the SNprogenitor is most likely from the oldest population, corresponding to aninitial mass of 10.4$^{+1.5}_{-1.3}$ $M_\odot$. The pre-explosion SED can bereproduced by two components, one for the hot and compact SN progenitor and onefor a cool and inflated yellow hypergiant (YHG) companion that dominates thebrightness. Thus, SN 2019yvr could possibly be the first Type Ib/c SN for whichthe progenitor's binary companion is directly detected on pre-explosion images.Both the low progenitor mass and the YHG companion suggest significant binaryinteraction during their evolution. Similar to SN 2014C, SN 2019yvr exhibits ametamorphosis from Type Ib to Type IIn, showing signatures of interaction withhydrogen-rich circumstellar material (CSM) at >150 days; our result supportsenhanced pre-SN mass loss as an important process for hydrogen-poor stars atthe low mass end of core-collapse SN progenitors.

An environmental analysis of the Type Ib SN 2019yvr and the possible presence of an inflated binary companion