The Progenitor of the S147 Supernova Remnant

Abstract

The supernova remnant (SNR) S147 contains the pulsar PSR J0538+2817 and a likely unbound binary companion, HD 37424. It is the only good Galactic candidate for a binary unbound by a core-collapse supernova (SN). Using Gaia DR3 parallaxes and photometry, we select the stars local to SNR S147 in a cylinder with a projected radius of $100$ pc and a parallax range of $0.614<\varpi <0.787$ mas (a length of $\simeq 360$ pc). We individually model the most luminous of these stars. The two most luminous single stars are the unbound binary companion, HD 37424, and HD 37367, with estimated masses of $(13.51\pm 0.05)M_{\odot }$ and $(14.30\pm 0.09)M_{\odot }$, respectively. The two most luminous binary systems are the spectroscopic binary HD 37366 and the eclipsing binary ET Tau that have primary masses of $(20.9\pm 0.12)M_{\odot }$ and $(16.7\pm 0.09)M_{\odot }$, respectively. We model the Gaia color-magnitude diagram (CMD) of this local stellar population using both single stars and a model consisting of noninteracting binaries using Solar metallicity PARSEC isochrones. For both models, the estimated age distributions of the $439$ $M_G<0$ mag stars favor a high mass progenitor of $21.5M_{\odot }-41.1M_{\odot }$ for the SN.

13 pages, 13 figures, submitted to ApJ October 1st, 2025

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