The Progenitor of the S147 Supernova Remnant
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| Format: | Preprint |
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2025
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| _version_ | 1866912942393393152 |
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| author | Cruz-Cruz, Elvira Kochanek, Christopher S. |
| author_facet | Cruz-Cruz, Elvira Kochanek, Christopher S. |
| contents | 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 $(13.51\pm0.05) M_{\odot}$ and $(14.30\pm0.09) M_{\odot}$, respectively. The two most luminous binary systems are the spectroscopic binary HD 37366 and the eclipsing binary ET Tau that have primary masses of $(20.9\pm0.12) M_{\odot}$ and $(16.7\pm0.09) M_{\odot}$, 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. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2510_02132 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Progenitor of the S147 Supernova Remnant Cruz-Cruz, Elvira Kochanek, Christopher S. High Energy Astrophysical Phenomena Solar and Stellar Astrophysics 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 $(13.51\pm0.05) M_{\odot}$ and $(14.30\pm0.09) M_{\odot}$, respectively. The two most luminous binary systems are the spectroscopic binary HD 37366 and the eclipsing binary ET Tau that have primary masses of $(20.9\pm0.12) M_{\odot}$ and $(16.7\pm0.09) M_{\odot}$, 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. |
| title | The Progenitor of the S147 Supernova Remnant |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2510.02132 |