Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations
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 _⊙ ) Wolf–Rayet (WR) progenitor, but its disappearance after the explosion of SN 2017ein remains unconfirmed. In this work, we revisit SN 2017ein in la...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/adad5d |
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| author | Yi-Han Zhao Ning-Chen Sun Junjie Wu Zexi Niu Xinyi Hong Yinhan Huang Justyn R. Maund Qiang Xi Danfeng Xiang Jifeng Liu |
| author_facet | Yi-Han Zhao Ning-Chen Sun Junjie Wu Zexi Niu Xinyi Hong Yinhan Huang Justyn R. Maund Qiang Xi Danfeng Xiang Jifeng Liu |
| author_sort | Yi-Han Zhao |
| collection | DOAJ |
| description | 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 _⊙ ) Wolf–Rayet (WR) 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 at 2.4–3.8 yr after peak brightness. We find this source has not disappeared, and its brightness and color remain almost the same as in the preexplosion images. Thus, we conclude that the preexplosion source is not the genuine progenitor of SN 2017ein. It is not much likelier to be a companion star of the progenitor since it has a much lower extinction than SN 2017ein; its color also seems 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 _ini ∼ 8–20 M _⊙ , stripped by binary interaction, rather than a very massive WR progenitor. |
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| id | doaj-art-1a1f4fb1ccd04e89bcf0dd521aa38d60 |
| institution | Kabale University |
| issn | 2041-8205 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Letters |
| spelling | doaj-art-1a1f4fb1ccd04e89bcf0dd521aa38d602025-02-06T05:38:50ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019801L610.3847/2041-8213/adad5dExclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time ObservationsYi-Han Zhao0https://orcid.org/0009-0005-9841-1434Ning-Chen Sun1https://orcid.org/0000-0002-4731-9698Junjie Wu2Zexi Niu3https://orcid.org/0000-0002-3651-0681Xinyi Hong4https://orcid.org/0009-0002-2074-0148Yinhan Huang5Justyn R. Maund6https://orcid.org/0000-0003-0733-7215Qiang Xi7Danfeng Xiang8Jifeng Liu9School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China ; sunnc@ucas.ac.cn; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China ; sunnc@ucas.ac.cn; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing, 102206, People’s Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China ; sunnc@ucas.ac.cn; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China ; sunnc@ucas.ac.cn; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China ; sunnc@ucas.ac.cn; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of ChinaSchool of Mathematical Sciences, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaDepartment of Physics, Royal Holloway, University of London , Egham, TW20 0EX, UKSchool of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China ; sunnc@ucas.ac.cn; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of ChinaBeijing Planetarium, Beijing Academy of Sciences and Technology , Beijing 100044, People’s Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China ; sunnc@ucas.ac.cn; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing, 102206, People’s Republic of China; New Cornerstone Science Laboratory, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100012, People’s Republic of ChinaTo date, SN 2017ein is the only Type Ic supernova with a directly identified progenitor candidate. This candidate points to a very massive (>45 M _⊙ ) Wolf–Rayet (WR) 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 at 2.4–3.8 yr after peak brightness. We find this source has not disappeared, and its brightness and color remain almost the same as in the preexplosion images. Thus, we conclude that the preexplosion source is not the genuine progenitor of SN 2017ein. It is not much likelier to be a companion star of the progenitor since it has a much lower extinction than SN 2017ein; its color also seems 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 _ini ∼ 8–20 M _⊙ , stripped by binary interaction, rather than a very massive WR progenitor.https://doi.org/10.3847/2041-8213/adad5dCore-collapse supernovaeSupernovaeType Ic supernovaeStellar evolutionMassive starsTime domain astronomy |
| spellingShingle | Yi-Han Zhao Ning-Chen Sun Junjie Wu Zexi Niu Xinyi Hong Yinhan Huang Justyn R. Maund Qiang Xi Danfeng Xiang Jifeng Liu Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations The Astrophysical Journal Letters Core-collapse supernovae Supernovae Type Ic supernovae Stellar evolution Massive stars Time domain astronomy |
| title | Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations |
| title_full | Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations |
| title_fullStr | Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations |
| title_full_unstemmed | Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations |
| title_short | Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations |
| title_sort | exclusion of a direct progenitor detection for the type ic sn 2017ein based on late time observations |
| topic | Core-collapse supernovae Supernovae Type Ic supernovae Stellar evolution Massive stars Time domain astronomy |
| url | https://doi.org/10.3847/2041-8213/adad5d |
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