The XRISM first-light observation: Velocity structure and thermal properties of the supernova remnant N 132D

Abstract We present an initial analysis of the X-Ray Imaging and Spectroscopy Mission (XRISM) first-light observation of the supernova remnant (SNR) N 132D 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 $\sigma _v \sim 450$ km s$^{-1}$. However, the Fe He$\alpha$ lines are substantially broadened with $\sigma _v \sim 1670$ 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$\alpha$ 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 $-1000 \lesssim V_{\rm rs}$ (km s$^{-1}$) $\lesssim 3300$ (in the observer frame). We also find that Fe Ly$\alpha$ 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 N 132D. These results demonstrate that high-resolution X-ray spectroscopy is capable of providing constraints on the evolutionary stage, geometry, and velocity distribution of SNRs.

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Journal
Publications of the Astronomical Society of Japan
Published
2024-10-10
DOI
https://doi.org/10.1093/pasj/psae080
Citations
32
Primary Topic
Astrophysics and Cosmic Phenomena
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article
Field-Weighted Citation Impact
21.11

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article

The XRISM first-light observation: Velocity structure and thermal properties of the supernova remnant N 132D

Lía Corrales, Yutaka Fujita, Chris Done, Katsuhiro Hayashi et al.
32 citations
Publications of the Astronomical Society of Japan
Astrophysics and Cosmic Phenomena
21.11
article

The XRISM first-light observation: Velocity structure and thermal properties of the supernova remnant N 132D

Lía Corrales, Yutaka Fujita, Chris Done, Katsuhiro Hayashi, Aya Kubota, Kyoko Matsushita, Kouichi Hagino, M. Shidatsu, M. Audard, J. S. Kaastra, Yuken Ohshiro, Satoshi Eguchi, Hirokazu Odaka, Luigi Gallo, Hideki Uchiyama, Hirofumi Noda, Y. Terada, K. Mukai, María Díaz Trigo, Aya Bamba, Eric D. Miller, Yoshiaki Kanemaru, J. M. Mïller, Ryuichi Fujimoto, Javier A. García, T. R. Kallman, Anna Ogorzałek, A. Simionescu, Megan E. Eckart, S. Paltani, Edmund Hodges‐Kluck, Erin Kara, Renata Cumbee, Hiroyuki Uchida, Hironori Matsumoto, Hiromasa Suzuki, A. E. Hornschemeier, Irina Zhuravleva, Mai Takeo, Gregory V. Brown, Adam Foster, Laura Brenneman, Masahiro Tsujimoto, Yoshitomo Maeda, Liyi Gu, Noriko Y. Yamasaki, D. McCammon, Toru Tamagawa, K. Yamaoka, Jan‐Uwe Ness, Michael Loewenstein, Naomi Ota, M. Guainazzi, Kosuke Sato, Takaaki Tanaka, Satoru Katsuda, Tsunefumi Mizuno, Robert Petre, M. Yamauchi, Ikuyuki Mitsuishi, Teruaki Enoto, Takeshi Go Tsuru, Isamu Hatsukade, Hiroshi Murakami, Ken Ebisawa, Maurice A. Leutenegger, Takashi Okajima, Manan Agarwal, Paul Plucinsky, F. S. Porter, D. Eckert, Maxim Markevitch, R. F. Mushotzky, Natalie Hell, Kumiko Nobukawa, Takayuki Hayashi, Ralf Ballhausen, Mihoko Yukita, B. R. McNamara, Masayoshi Nobukawa, Misaki Mizumoto, Rozenn Boissay-Malaquin, François Mernier, Shunji Kitamoto, T. Yoneyama, Shin Watanabe, Toshiki Sato, E. Costantini, H. Takahashi, Yuusuke Uchida, A. Tanimoto, Caroline A. Kilbourne, Shoji Ogawa, Satoshi Yamada, Shogo Kobayashi, Nagomi Uchida, Yohko Tsuboi, Shinya Yamada, Ehud Behar, Katja Pottschmidt, Shinichiro Uno, Yoshihiro Ueda, Kumi Ishikawa, Hiromi Seta, Koji Mori, Randall W. Smith, Hiroshi Nakajima, Hisamitsu Awaki, Hiroya Yamaguchi, Richard L. Kelley, Hiroshi Tsunemi, Jacco Vink, Yuichi Terashima, Akihiro Furuzawa, Yuichiro Ezoe, Makoto Sawada, Keisuke Tamura, M. Ishida, Yuto Ichinohe, Tessei Yoshida, Yoshitaka Ishisaki, Yasushi Fukazawa, Kenji Hamaguchi, Takayoshi Kohmura, Kazuhiro Nakazawa, Andrew Szymkowiak, Tadayasu Dotani, Kotaro Fukushima, Makoto Tashiro, Shigeo Yamauchi, Tahir Yaqoob, Brian J. Williams
article en
32 citations

Abstract

Abstract We present an initial analysis of the X-Ray Imaging and Spectroscopy Mission (XRISM) first-light observation of the supernova remnant (SNR) N 132D 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 $\sigma _v \sim 450$ km s$^{-1}$. However, the Fe He$\alpha$ lines are substantially broadened with $\sigma _v \sim 1670$ 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$\alpha$ 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 $-1000 \lesssim V_{\rm rs}$ (km s$^{-1}$) $\lesssim 3300$ (in the observer frame). We also find that Fe Ly$\alpha$ 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 N 132D. These results demonstrate that high-resolution X-ray spectroscopy is capable of providing constraints on the evolutionary stage, geometry, and velocity distribution of SNRs.

Publications of the Astronomical Society of JapanVol. 76(6)
Kagoshima University (JP), Hiroshima University (JP), University of Geneva (CH), University of Miyazaki (JP), Kumamoto Gakuen University (JP), Leiden University (NL), California Institute of Technology (US), Nihon Fukushi University (JP), Vassar College (US), Lawrence Livermore National Laboratory (US), Shizuoka University (JP), Goddard Space Flight Center (US), Rikkyo University (JP), University of Wisconsin–Madison (US), Pioneer (United States) (US), Johns Hopkins University (US), Nara University of Education (JP), University of Waterloo (CA), Konan University (JP), Tokyo University of Science (JP), Meiji University (JP), Shibaura Institute of Technology (JP), Technion – Israel Institute of Technology (IL), Durham University (GB), Tohoku University (JP), Kanto Gakuin University (JP), Kyoto University (JP), University of Michigan (US), University of Teacher Education Fukuoka (JP), Japan Aerospace Exploration Agency (JP), European Space Agency (FR), Yale Cancer Center (US), Tohoku Gakuin University (JP), Yale University (US), University of Chicago (US), European Space Astronomy Centre (ES), Pioneer (Japan) (JP), RIKEN (JP), Center for Astrophysics Harvard & Smithsonian (US), Fujita Health University Hospital (JP), Astrophysics Science Division (US), Institute of Space and Astronautical Science (JP), Astronomical Institute of the Slovak Academy of Sciences (SK), RIKEN Nishina Center (JP), Ehime University (JP), Leiden Observatory, European Space Research and Technology Centre (NL), Space Research Organisation Netherlands (NL), Nagoya University (JP), Massachusetts Institute of Technology (US), Saint Mary's University (CA), University of Maryland, College Park (US), Tokyo Metropolitan University (JP), Saitama University (JP), The University of Tokyo (JP), University of Maryland, Baltimore County (US), University of Amsterdam (NL), Kindai University (JP), Chuo University (JP), The University of Osaka (JP), Nara Women's University (JP)
National Science Foundation, U.S. Department of Energy, National Aeronautics and Space Administration, Alfred P. Sloan Foundation, Kagoshima University, Goddard Space Flight Center, Canadian Space Agency, Science and Technology Facilities Council, Japan Society for the Promotion of Science, RIKEN, Lawrence Livermore National Laboratory
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Astrophysics and Cosmic Phenomena
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