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We present the results of a detailed, systematic stellar evolution study ofbinary mergers for blue supergiant (BSG) progenitors of Type II supernovae. Inparticular, these are the first evolutionary models that can simultaneouslyreproduce nearly all observational aspects of the progenitor of SN 1987A,$\text{Sk}-69\,^{\circ}202$, such as its position in the HR diagram, theenrichment of helium and nitrogen in the triple-ring nebula, and its lifetimebefore its explosion. The merger model, based on the one proposed byPodsiadlowski 1992 et al. and Podsiadlowski 2007 et al., consists of a mainsequence secondary star that dissolves completely in the common envelope of theprimary red supergiant at the end of their merger. We empirically explore alarge initial parameter space, such as primary masses ($15\,\text{M}_{\odot}$,$16\,\text{M}_{\odot}$, and $17\,\text{M}_{\odot}$), secondary masses($2\,\text{M}_{\odot}$, $3\,\text{M}_{\odot}$, ..., $8\,\text{M}_{\odot}$) anddifferent depths up to which the secondary penetrates the He core of theprimary during the merger. The evolution of the merged star is continued untiljust before iron-core collapse and the surface properties of the 84pre-supernova models ($16\,\text{M}_{\odot}-23\,\mathrm{M}_{\odot}$) computedhave been made available in this work. Within the parameter space studied, themajority of the pre-supernova models are compact, hot BSGs with effectivetemperature $>12\,\text{kK}$ and radii of$30\,\text{R}_{\odot}-70\,\mathrm{R}_{\odot}$ of which six match nearly all theobservational properties of $\text{Sk}-69\,^{\circ}202$.

The quest for blue supergiants: binary merger models for the evolution of the progenitor of SN 1987A