Evidence for Charge Exchange Emission in Supernova Remnant N132D from XRISM/Resolve Observations
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arXiv
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| Natura: | Preprint |
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2025
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| _version_ | 1866915227912634368 |
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| author | Gu, Liyi Yamaguchi, Hiroya Foster, Adam Katsuda, Satoru Uchida, Hiroyuki Sawada, Makoto Porter, Frederick Scott Williams, Brian J. Petre, Robert Bamba, Aya Terada, Yukikatsu Agarwal, Manan Decourchelle, Anne Guainazzi, Matteo Kelley, Richard Kilbourne, Caroline Loewenstein, Michael Matsumoto, Hironori Miller, Eric D. Ohshiro, Yuken Plucinsky, Paul Suzuki, Hiromasa Tashiro, Makoto Vink, Jacco Ezoe, Yuichiro Behar, Ehud Smith, Randall |
| author_facet | Gu, Liyi Yamaguchi, Hiroya Foster, Adam Katsuda, Satoru Uchida, Hiroyuki Sawada, Makoto Porter, Frederick Scott Williams, Brian J. Petre, Robert Bamba, Aya Terada, Yukikatsu Agarwal, Manan Decourchelle, Anne Guainazzi, Matteo Kelley, Richard Kilbourne, Caroline Loewenstein, Michael Matsumoto, Hironori Miller, Eric D. Ohshiro, Yuken Plucinsky, Paul Suzuki, Hiromasa Tashiro, Makoto Vink, Jacco Ezoe, Yuichiro Behar, Ehud Smith, Randall |
| contents | XRISM has delivered one of its first light observations on N132D, the X-ray brightest supernova remnant in the Large Magellanic Cloud. Utilizing 193 ks of high-resolution X-ray spectroscopy data, we conduct a comprehensive search for charge exchange emission. By incorporating a charge exchange model into our spectral analysis, we observe an improvement in the fits of two weak features at 2.41 keV and 2.63 keV. These features, with a combined significance of 99.6%, are consistent with transitions from highly ionized silicon ions in high Rydberg states, which are unique indicators of charge exchange. Our analysis constrains the charge exchange flux to no more than 4% of the total source flux within the 1.7-3.0 keV band, and places an upper limit on the charge exchange interaction velocity at 450 km/s. This result supports ongoing shock-cloud interactions within N132D and highlights the unique capabilities of XRISM to probe the complex physical processes at play. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_03223 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Evidence for Charge Exchange Emission in Supernova Remnant N132D from XRISM/Resolve Observations Gu, Liyi Yamaguchi, Hiroya Foster, Adam Katsuda, Satoru Uchida, Hiroyuki Sawada, Makoto Porter, Frederick Scott Williams, Brian J. Petre, Robert Bamba, Aya Terada, Yukikatsu Agarwal, Manan Decourchelle, Anne Guainazzi, Matteo Kelley, Richard Kilbourne, Caroline Loewenstein, Michael Matsumoto, Hironori Miller, Eric D. Ohshiro, Yuken Plucinsky, Paul Suzuki, Hiromasa Tashiro, Makoto Vink, Jacco Ezoe, Yuichiro Behar, Ehud Smith, Randall High Energy Astrophysical Phenomena Atomic Physics XRISM has delivered one of its first light observations on N132D, the X-ray brightest supernova remnant in the Large Magellanic Cloud. Utilizing 193 ks of high-resolution X-ray spectroscopy data, we conduct a comprehensive search for charge exchange emission. By incorporating a charge exchange model into our spectral analysis, we observe an improvement in the fits of two weak features at 2.41 keV and 2.63 keV. These features, with a combined significance of 99.6%, are consistent with transitions from highly ionized silicon ions in high Rydberg states, which are unique indicators of charge exchange. Our analysis constrains the charge exchange flux to no more than 4% of the total source flux within the 1.7-3.0 keV band, and places an upper limit on the charge exchange interaction velocity at 450 km/s. This result supports ongoing shock-cloud interactions within N132D and highlights the unique capabilities of XRISM to probe the complex physical processes at play. |
| title | Evidence for Charge Exchange Emission in Supernova Remnant N132D from XRISM/Resolve Observations |
| topic | High Energy Astrophysical Phenomena Atomic Physics |
| url | https://arxiv.org/abs/2504.03223 |