The XRISM First Light Observation: Velocity Structure and Thermal Properties of the Supernova Remnant N132D
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866914971200258048 |
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| author | XRISM Collaboration |
| author_facet | XRISM Collaboration |
| contents | We present an initial analysis of the X-Ray Imaging and Spectroscopy Mission (XRISM) first-light observation of the supernova remnant (SNR) N132D in the Large Magellanic Cloud. The Resolve microcalorimeter has obtained the first high-resolution spectrum in the 1.6-10 keV band, which contains K-shell emission lines of Si, S, Ar, Ca, and Fe. We find that the Si and S lines are relatively narrow, with a broadening represented by a Gaussian-like velocity dispersion of $σ_v \sim 450$ km s$^{-1}$. The Fe He$α$ lines are, on the other hand, substantially broadened with $σ_v \sim 1670$ km s$^{-1}$. This broadening can be explained by a combination of the thermal Doppler effect due to the high ion temperature and the kinematic Doppler effect due to the SNR expansion. Assuming that the Fe He$α$ emission originates predominantly from the supernova ejecta, we estimate the reverse shock velocity at the time when the bulk of the Fe ejecta were shock heated to be $-1000 \lesssim V_{\rm rs}~[{\rm km s}^{-1}] \lesssim 3300$ (in the observer frame). We also find that Fe Ly$α$ emission is redshifted with a bulk velocity of $\sim 890$ km s$^{-1}$, substantially larger than the radial velocity of the local interstellar medium surrounding N132D. These results demonstrate that high-resolution X-ray spectroscopy is capable of providing constraints on the evolutionary stage, geometry, and velocity distribution of SNRs. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_14301 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The XRISM First Light Observation: Velocity Structure and Thermal Properties of the Supernova Remnant N132D XRISM Collaboration High Energy Astrophysical Phenomena We present an initial analysis of the X-Ray Imaging and Spectroscopy Mission (XRISM) first-light observation of the supernova remnant (SNR) N132D in the Large Magellanic Cloud. The Resolve microcalorimeter has obtained the first high-resolution spectrum in the 1.6-10 keV band, which contains K-shell emission lines of Si, S, Ar, Ca, and Fe. We find that the Si and S lines are relatively narrow, with a broadening represented by a Gaussian-like velocity dispersion of $σ_v \sim 450$ km s$^{-1}$. The Fe He$α$ lines are, on the other hand, substantially broadened with $σ_v \sim 1670$ km s$^{-1}$. This broadening can be explained by a combination of the thermal Doppler effect due to the high ion temperature and the kinematic Doppler effect due to the SNR expansion. Assuming that the Fe He$α$ emission originates predominantly from the supernova ejecta, we estimate the reverse shock velocity at the time when the bulk of the Fe ejecta were shock heated to be $-1000 \lesssim V_{\rm rs}~[{\rm km s}^{-1}] \lesssim 3300$ (in the observer frame). We also find that Fe Ly$α$ emission is redshifted with a bulk velocity of $\sim 890$ km s$^{-1}$, substantially larger than the radial velocity of the local interstellar medium surrounding N132D. These results demonstrate that high-resolution X-ray spectroscopy is capable of providing constraints on the evolutionary stage, geometry, and velocity distribution of SNRs. |
| title | The XRISM First Light Observation: Velocity Structure and Thermal Properties of the Supernova Remnant N132D |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2408.14301 |