Exclusion of a direct progenitor detection for the Type Ic SN 2017ein based on late-time observations
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arXiv
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| Auteurs principaux: | , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866911202013085696 |
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| author | Zhao, Yi-Han Sun, Ning-Chen Wu, Junjie Niu, Zexi Hong, Xinyi Huang, Yinhan Maund, Justyn R. Xi, Qiang Xiang, Danfeng Liu, Jifeng |
| author_facet | Zhao, Yi-Han Sun, Ning-Chen Wu, Junjie Niu, Zexi Hong, Xinyi Huang, Yinhan Maund, Justyn R. Xi, Qiang Xiang, Danfeng Liu, Jifeng |
| contents | To date, SN 2017ein is the only Type Ic supernova with a directly identified progenitor candidate. This candidate points to a very massive ($>$45 $M_\odot$) Wolf-Rayet progenitor, but its disappearance after the explosion of SN 2017ein remains unconfirmed. In this work, we revisit SN 2017ein in late-time images acquired by the Hubble Space Telescope (HST) at 2.4--3.8 yrs after peak brightness. We find this source has not disappeared and its brightness and color remain almost the same as in the pre-explosion images. Thus, we conclude that the pre-explosion source is not the genuine progenitor of SN 2017ein. We exclude the possibility that it is a companion star of the progenitor, since it has a much lower extinction than SN 2017ein; its color is also inconsistent with a star cluster, indicated by the newly added magnitude limit in F336W, apart from F555W and F814W. We suggest, therefore, this source is an unrelated star in chance alignment with SN 2017ein. Based on the low ejecta mass, we propose that SN 2017ein is most likely originated from a moderately massive star with $M_{\rm ini}$ $\sim$ 8--20 $M_\odot$, stripped by binary interaction, rather than a very massive Wolf-Rayet progenitor. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2411_17969 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Exclusion of a direct progenitor detection for the Type Ic SN 2017ein based on late-time observations Zhao, Yi-Han Sun, Ning-Chen Wu, Junjie Niu, Zexi Hong, Xinyi Huang, Yinhan Maund, Justyn R. Xi, Qiang Xiang, Danfeng Liu, Jifeng High Energy Astrophysical Phenomena Solar and Stellar Astrophysics To date, SN 2017ein is the only Type Ic supernova with a directly identified progenitor candidate. This candidate points to a very massive ($>$45 $M_\odot$) Wolf-Rayet progenitor, but its disappearance after the explosion of SN 2017ein remains unconfirmed. In this work, we revisit SN 2017ein in late-time images acquired by the Hubble Space Telescope (HST) at 2.4--3.8 yrs after peak brightness. We find this source has not disappeared and its brightness and color remain almost the same as in the pre-explosion images. Thus, we conclude that the pre-explosion source is not the genuine progenitor of SN 2017ein. We exclude the possibility that it is a companion star of the progenitor, since it has a much lower extinction than SN 2017ein; its color is also inconsistent with a star cluster, indicated by the newly added magnitude limit in F336W, apart from F555W and F814W. We suggest, therefore, this source is an unrelated star in chance alignment with SN 2017ein. Based on the low ejecta mass, we propose that SN 2017ein is most likely originated from a moderately massive star with $M_{\rm ini}$ $\sim$ 8--20 $M_\odot$, stripped by binary interaction, rather than a very massive Wolf-Rayet progenitor. |
| title | Exclusion of a direct progenitor detection for the Type Ic SN 2017ein based on late-time observations |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2411.17969 |