Chandra’s Insights into SN 2023ixf
We report Chandra-ACIS observations of supernova (SN) 2023ixf in M101 on day 13 and 86 since the explosion. The X-rays in both epochs are characterized by high-temperature plasma from the forward shocked region as a result of circumstellar interaction. We are able to constrain the absorption column...
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/ad275d |
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| author | Poonam Chandra Roger A. Chevalier Keiichi Maeda Alak K. Ray Nayana A. J. |
| author_facet | Poonam Chandra Roger A. Chevalier Keiichi Maeda Alak K. Ray Nayana A. J. |
| author_sort | Poonam Chandra |
| collection | DOAJ |
| description | We report Chandra-ACIS observations of supernova (SN) 2023ixf in M101 on day 13 and 86 since the explosion. The X-rays in both epochs are characterized by high-temperature plasma from the forward shocked region as a result of circumstellar interaction. We are able to constrain the absorption column density at both Chandra epochs, which is much larger than that due to the Galactic and host absorption column, and we attribute it to absorption by the circumstellar matter in the immediate vicinity of SN 2023ixf. Combining our column density measurements with the published measurement on day 4, we show that the column density declines as t ^−2 between day 4 to day 13 and then evolves as t ^−1 . The unabsorbed 0.3–10 keV luminosity evolves as t ^−1 during the Chandra epochs. On the Chandra first epoch observation, when the SN was 13 days old, we detect the Fe K α fluorescent line at 6.4 keV indicating presence of cold material in the vicinity of the supernova. The line is absent on day 86, consistent with the decreased column density by a factor of 7 between the two epochs. Our analysis indicates that during 10–1.5 yr before explosion, the progenitor was evolving with a constant mass-loss rate of 5.6 × 10 ^−4 M _⊙ yr ^−1 . |
| format | Article |
| id | doaj-art-ca261daf029540b79b466112612f89ba |
| institution | DOAJ |
| issn | 2041-8205 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Letters |
| spelling | doaj-art-ca261daf029540b79b466112612f89ba2025-08-20T02:52:42ZengIOP PublishingThe Astrophysical Journal Letters2041-82052024-01-019631L410.3847/2041-8213/ad275dChandra’s Insights into SN 2023ixfPoonam Chandra0https://orcid.org/0000-0002-0844-6563Roger A. Chevalier1https://orcid.org/0000-0002-9117-7244Keiichi Maeda2https://orcid.org/0000-0003-2611-7269Alak K. Ray3https://orcid.org/0000-0003-2404-0018Nayana A. J.4https://orcid.org/0000-0002-8070-5400National Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USA; National Centre for Radio Astrophysics , TIFR, Ganeshkhind Pune 411007, IndiaDepartment of Astronomy, University of Virginia , Charlottesville, VA 22904-4325, USADepartment of Astronomy, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502 JapanHomi Bhabha Centre for Science Education , TIFR, Mumbai 400088, IndiaDepartment of Astronomy, University of California , Berkeley, CA 94720-3411, USAWe report Chandra-ACIS observations of supernova (SN) 2023ixf in M101 on day 13 and 86 since the explosion. The X-rays in both epochs are characterized by high-temperature plasma from the forward shocked region as a result of circumstellar interaction. We are able to constrain the absorption column density at both Chandra epochs, which is much larger than that due to the Galactic and host absorption column, and we attribute it to absorption by the circumstellar matter in the immediate vicinity of SN 2023ixf. Combining our column density measurements with the published measurement on day 4, we show that the column density declines as t ^−2 between day 4 to day 13 and then evolves as t ^−1 . The unabsorbed 0.3–10 keV luminosity evolves as t ^−1 during the Chandra epochs. On the Chandra first epoch observation, when the SN was 13 days old, we detect the Fe K α fluorescent line at 6.4 keV indicating presence of cold material in the vicinity of the supernova. The line is absent on day 86, consistent with the decreased column density by a factor of 7 between the two epochs. Our analysis indicates that during 10–1.5 yr before explosion, the progenitor was evolving with a constant mass-loss rate of 5.6 × 10 ^−4 M _⊙ yr ^−1 .https://doi.org/10.3847/2041-8213/ad275dCircumstellar matterSupernovaeStellar mass lossX-ray transient sources |
| spellingShingle | Poonam Chandra Roger A. Chevalier Keiichi Maeda Alak K. Ray Nayana A. J. Chandra’s Insights into SN 2023ixf The Astrophysical Journal Letters Circumstellar matter Supernovae Stellar mass loss X-ray transient sources |
| title | Chandra’s Insights into SN 2023ixf |
| title_full | Chandra’s Insights into SN 2023ixf |
| title_fullStr | Chandra’s Insights into SN 2023ixf |
| title_full_unstemmed | Chandra’s Insights into SN 2023ixf |
| title_short | Chandra’s Insights into SN 2023ixf |
| title_sort | chandra s insights into sn 2023ixf |
| topic | Circumstellar matter Supernovae Stellar mass loss X-ray transient sources |
| url | https://doi.org/10.3847/2041-8213/ad275d |
| work_keys_str_mv | AT poonamchandra chandrasinsightsintosn2023ixf AT rogerachevalier chandrasinsightsintosn2023ixf AT keiichimaeda chandrasinsightsintosn2023ixf AT alakkray chandrasinsightsintosn2023ixf AT nayanaaj chandrasinsightsintosn2023ixf |