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XRISM forecast for the Coma cluster: stormy, with a steep power spectrum

Fuente: arXiv

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Autori principali:	XRISM Collaboration, Audard, Marc, Awaki, Hisamitsu, Ballhausen, Ralf, Bamba, Aya, Behar, Ehud, Boissay-Malaquin, Rozenn, Brenneman, Laura, Brown, Gregory V., Corrales, Lia, Costantini, Elisa, Cumbee, Renata, Trigo, Maria Diaz, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Eckert, Dominique, Eguchi, Satoshi, Enoto, Teruaki, Ezoe, Yuichiro, Foster, Adam, Fujimoto, Ryuichi, Fujita, Yutaka, Fukazawa, Yasushi, Fukushima, Kotaro, Furuzawa, Akihiro, Gallo, Luigi, Garcia, Javier A., Gu, Liyi, Guainazzi, Matteo, Hagino, Kouichi, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hell, Natalie, Hodges-Kluck, Edmund, Hornschemeier, Ann, Ichinohe, Yuto, Ishi, Daiki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Timothy, Kara, Erin, Katsuda, Satoru, Kanemaru, Yoshiaki, Kelley, Richard, Kilbourne, Caroline, Kitamoto, Shunji, Kobayashi, Shogo, Kohmura, Takayoshi, Kubota, Aya, Leutenegger, Maurice, Loewenstein, Michael, Maeda, Yoshitomo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian, Mernier, Francois, Miller, Eric D., Miller, Jon M., Mitsuishi, Ikuyuki, Mizumoto, Misaki, Mizuno, Tsunefumi, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard, Nakajima, Hiroshi, Nakazawa, Kazuhiro, Ness, Jan-Uwe, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogawa, Shoji, Ogorzalek, Anna, Okajima, Takashi, Ota, Naomi, Paltani, Stephane, Petre, Robert, Plucinsky, Paul, Porter, Frederick S., Pottschmidt, Katja, Sato, Kosuke, Sato, Toshiki, Sawada, Makoto, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall, Suzuki, Hiromasa, Szymkowiak, Andrew, Takahashi, Hiromitsu, Takeo, Mai, Tamagawa, Toru, Tamura, Keisuke, Tanaka, Takaaki, Tanimoto, Atsushi, Tashiro, Makoto, Terada, Yukikatsu, Terashima, Yuichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Tumer, Aysegul, Uchida, Hiroyuki, Uchida, Nagomi, Uchida, Yuusuke, Uchiyama, Hideki, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shinichiro, Vink, Jacco, Watanabe, Shin, Williams, Brian J., Yamada, Satoshi, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yoneyama, Tomokage, Yoshida, Tessei, Yukita, Mihoko, Zhuravleva, Irina, Fabian, Andrew, Nelson, Dylan, Okabe, Nobuhiro, Pillepich, Annalisa, Potter, Cicely, Regamey, Manon, Sakai, Kosei, Shishido, Mona, Truong, Nhut, Wik, Daniel R., ZuHone, John
Natura:	Preprint
Pubblicazione:	2025
Soggetti:	High Energy Astrophysical Phenomena Astrophysics of Galaxies
Accesso online:	Acceder al recurso
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author	XRISM Collaboration Audard, Marc Awaki, Hisamitsu Ballhausen, Ralf Bamba, Aya Behar, Ehud Boissay-Malaquin, Rozenn Brenneman, Laura Brown, Gregory V. Corrales, Lia Costantini, Elisa Cumbee, Renata Trigo, Maria Diaz Done, Chris Dotani, Tadayasu Ebisawa, Ken Eckart, Megan E. Eckert, Dominique Eguchi, Satoshi Enoto, Teruaki Ezoe, Yuichiro Foster, Adam Fujimoto, Ryuichi Fujita, Yutaka Fukazawa, Yasushi Fukushima, Kotaro Furuzawa, Akihiro Gallo, Luigi Garcia, Javier A. Gu, Liyi Guainazzi, Matteo Hagino, Kouichi Hamaguchi, Kenji Hatsukade, Isamu Hayashi, Katsuhiro Hayashi, Takayuki Hell, Natalie Hodges-Kluck, Edmund Hornschemeier, Ann Ichinohe, Yuto Ishi, Daiki Ishida, Manabu Ishikawa, Kumi Ishisaki, Yoshitaka Kaastra, Jelle Kallman, Timothy Kara, Erin Katsuda, Satoru Kanemaru, Yoshiaki Kelley, Richard Kilbourne, Caroline Kitamoto, Shunji Kobayashi, Shogo Kohmura, Takayoshi Kubota, Aya Leutenegger, Maurice Loewenstein, Michael Maeda, Yoshitomo Markevitch, Maxim Matsumoto, Hironori Matsushita, Kyoko McCammon, Dan McNamara, Brian Mernier, Francois Miller, Eric D. Miller, Jon M. Mitsuishi, Ikuyuki Mizumoto, Misaki Mizuno, Tsunefumi Mori, Koji Mukai, Koji Murakami, Hiroshi Mushotzky, Richard Nakajima, Hiroshi Nakazawa, Kazuhiro Ness, Jan-Uwe Nobukawa, Kumiko Nobukawa, Masayoshi Noda, Hirofumi Odaka, Hirokazu Ogawa, Shoji Ogorzalek, Anna Okajima, Takashi Ota, Naomi Paltani, Stephane Petre, Robert Plucinsky, Paul Porter, Frederick S. Pottschmidt, Katja Sato, Kosuke Sato, Toshiki Sawada, Makoto Seta, Hiromi Shidatsu, Megumi Simionescu, Aurora Smith, Randall Suzuki, Hiromasa Szymkowiak, Andrew Takahashi, Hiromitsu Takeo, Mai Tamagawa, Toru Tamura, Keisuke Tanaka, Takaaki Tanimoto, Atsushi Tashiro, Makoto Terada, Yukikatsu Terashima, Yuichi Tsuboi, Yohko Tsujimoto, Masahiro Tsunemi, Hiroshi Tsuru, Takeshi Tumer, Aysegul Uchida, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchiyama, Hideki Ueda, Shutaro Ueda, Yoshihiro Uno, Shinichiro Vink, Jacco Watanabe, Shin Williams, Brian J. Yamada, Satoshi Yamada, Shinya Yamaguchi, Hiroya Yamaoka, Kazutaka Yamasaki, Noriko Yamauchi, Makoto Yamauchi, Shigeo Yaqoob, Tahir Yoneyama, Tomokage Yoshida, Tessei Yukita, Mihoko Zhuravleva, Irina Fabian, Andrew Nelson, Dylan Okabe, Nobuhiro Pillepich, Annalisa Potter, Cicely Regamey, Manon Sakai, Kosei Shishido, Mona Truong, Nhut Wik, Daniel R. ZuHone, John
author_facet	XRISM Collaboration Audard, Marc Awaki, Hisamitsu Ballhausen, Ralf Bamba, Aya Behar, Ehud Boissay-Malaquin, Rozenn Brenneman, Laura Brown, Gregory V. Corrales, Lia Costantini, Elisa Cumbee, Renata Trigo, Maria Diaz Done, Chris Dotani, Tadayasu Ebisawa, Ken Eckart, Megan E. Eckert, Dominique Eguchi, Satoshi Enoto, Teruaki Ezoe, Yuichiro Foster, Adam Fujimoto, Ryuichi Fujita, Yutaka Fukazawa, Yasushi Fukushima, Kotaro Furuzawa, Akihiro Gallo, Luigi Garcia, Javier A. Gu, Liyi Guainazzi, Matteo Hagino, Kouichi Hamaguchi, Kenji Hatsukade, Isamu Hayashi, Katsuhiro Hayashi, Takayuki Hell, Natalie Hodges-Kluck, Edmund Hornschemeier, Ann Ichinohe, Yuto Ishi, Daiki Ishida, Manabu Ishikawa, Kumi Ishisaki, Yoshitaka Kaastra, Jelle Kallman, Timothy Kara, Erin Katsuda, Satoru Kanemaru, Yoshiaki Kelley, Richard Kilbourne, Caroline Kitamoto, Shunji Kobayashi, Shogo Kohmura, Takayoshi Kubota, Aya Leutenegger, Maurice Loewenstein, Michael Maeda, Yoshitomo Markevitch, Maxim Matsumoto, Hironori Matsushita, Kyoko McCammon, Dan McNamara, Brian Mernier, Francois Miller, Eric D. Miller, Jon M. Mitsuishi, Ikuyuki Mizumoto, Misaki Mizuno, Tsunefumi Mori, Koji Mukai, Koji Murakami, Hiroshi Mushotzky, Richard Nakajima, Hiroshi Nakazawa, Kazuhiro Ness, Jan-Uwe Nobukawa, Kumiko Nobukawa, Masayoshi Noda, Hirofumi Odaka, Hirokazu Ogawa, Shoji Ogorzalek, Anna Okajima, Takashi Ota, Naomi Paltani, Stephane Petre, Robert Plucinsky, Paul Porter, Frederick S. Pottschmidt, Katja Sato, Kosuke Sato, Toshiki Sawada, Makoto Seta, Hiromi Shidatsu, Megumi Simionescu, Aurora Smith, Randall Suzuki, Hiromasa Szymkowiak, Andrew Takahashi, Hiromitsu Takeo, Mai Tamagawa, Toru Tamura, Keisuke Tanaka, Takaaki Tanimoto, Atsushi Tashiro, Makoto Terada, Yukikatsu Terashima, Yuichi Tsuboi, Yohko Tsujimoto, Masahiro Tsunemi, Hiroshi Tsuru, Takeshi Tumer, Aysegul Uchida, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchiyama, Hideki Ueda, Shutaro Ueda, Yoshihiro Uno, Shinichiro Vink, Jacco Watanabe, Shin Williams, Brian J. Yamada, Satoshi Yamada, Shinya Yamaguchi, Hiroya Yamaoka, Kazutaka Yamasaki, Noriko Yamauchi, Makoto Yamauchi, Shigeo Yaqoob, Tahir Yoneyama, Tomokage Yoshida, Tessei Yukita, Mihoko Zhuravleva, Irina Fabian, Andrew Nelson, Dylan Okabe, Nobuhiro Pillepich, Annalisa Potter, Cicely Regamey, Manon Sakai, Kosei Shishido, Mona Truong, Nhut Wik, Daniel R. ZuHone, John
contents	The XRISM Resolve microcalorimeter array measured the velocities of hot intracluster gas at two positions in the Coma galaxy cluster: 3'x3' squares at the center and at 6' (170 kpc) to the south. We find the line-of-sight velocity dispersions in those regions to be sigma_z=208+-12 km/s and 202+-24 km/s, respectively. The central value corresponds to a 3D Mach number of M=0.24+-0.015 and the ratio of the kinetic pressure of small-scale motions to thermal pressure in the intracluster plasma of only 3.1+-0.4%, at the lower end of predictions from cosmological simulations for merging clusters like Coma, and similar to that observed in the cool core of the relaxed cluster A2029. Meanwhile, the gas in both regions exhibits high line-of-sight velocity differences from the mean velocity of the cluster galaxies, Delta v_z=450+-15 km/s and 730+-30 km/s, respectively. A small contribution from an additional gas velocity component, consistent with the cluster optical mean, is detected along a sightline near the cluster center. The combination of the observed velocity dispersions and bulk velocities is not described by a Kolmogorov velocity power spectrum of steady-state turbulence; instead, the data imply a much steeper effective slope (i.e., relatively more power at larger linear scales). This may indicate either a very large dissipation scale resulting in the suppression of small-scale motions, or a transient dynamic state of the cluster, where large-scale gas flows generated by an ongoing merger have not yet cascaded down to small scales.
format	Preprint
id	arxiv_https___arxiv_org_abs_2504_20928
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	XRISM forecast for the Coma cluster: stormy, with a steep power spectrum XRISM Collaboration Audard, Marc Awaki, Hisamitsu Ballhausen, Ralf Bamba, Aya Behar, Ehud Boissay-Malaquin, Rozenn Brenneman, Laura Brown, Gregory V. Corrales, Lia Costantini, Elisa Cumbee, Renata Trigo, Maria Diaz Done, Chris Dotani, Tadayasu Ebisawa, Ken Eckart, Megan E. Eckert, Dominique Eguchi, Satoshi Enoto, Teruaki Ezoe, Yuichiro Foster, Adam Fujimoto, Ryuichi Fujita, Yutaka Fukazawa, Yasushi Fukushima, Kotaro Furuzawa, Akihiro Gallo, Luigi Garcia, Javier A. Gu, Liyi Guainazzi, Matteo Hagino, Kouichi Hamaguchi, Kenji Hatsukade, Isamu Hayashi, Katsuhiro Hayashi, Takayuki Hell, Natalie Hodges-Kluck, Edmund Hornschemeier, Ann Ichinohe, Yuto Ishi, Daiki Ishida, Manabu Ishikawa, Kumi Ishisaki, Yoshitaka Kaastra, Jelle Kallman, Timothy Kara, Erin Katsuda, Satoru Kanemaru, Yoshiaki Kelley, Richard Kilbourne, Caroline Kitamoto, Shunji Kobayashi, Shogo Kohmura, Takayoshi Kubota, Aya Leutenegger, Maurice Loewenstein, Michael Maeda, Yoshitomo Markevitch, Maxim Matsumoto, Hironori Matsushita, Kyoko McCammon, Dan McNamara, Brian Mernier, Francois Miller, Eric D. Miller, Jon M. Mitsuishi, Ikuyuki Mizumoto, Misaki Mizuno, Tsunefumi Mori, Koji Mukai, Koji Murakami, Hiroshi Mushotzky, Richard Nakajima, Hiroshi Nakazawa, Kazuhiro Ness, Jan-Uwe Nobukawa, Kumiko Nobukawa, Masayoshi Noda, Hirofumi Odaka, Hirokazu Ogawa, Shoji Ogorzalek, Anna Okajima, Takashi Ota, Naomi Paltani, Stephane Petre, Robert Plucinsky, Paul Porter, Frederick S. Pottschmidt, Katja Sato, Kosuke Sato, Toshiki Sawada, Makoto Seta, Hiromi Shidatsu, Megumi Simionescu, Aurora Smith, Randall Suzuki, Hiromasa Szymkowiak, Andrew Takahashi, Hiromitsu Takeo, Mai Tamagawa, Toru Tamura, Keisuke Tanaka, Takaaki Tanimoto, Atsushi Tashiro, Makoto Terada, Yukikatsu Terashima, Yuichi Tsuboi, Yohko Tsujimoto, Masahiro Tsunemi, Hiroshi Tsuru, Takeshi Tumer, Aysegul Uchida, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchiyama, Hideki Ueda, Shutaro Ueda, Yoshihiro Uno, Shinichiro Vink, Jacco Watanabe, Shin Williams, Brian J. Yamada, Satoshi Yamada, Shinya Yamaguchi, Hiroya Yamaoka, Kazutaka Yamasaki, Noriko Yamauchi, Makoto Yamauchi, Shigeo Yaqoob, Tahir Yoneyama, Tomokage Yoshida, Tessei Yukita, Mihoko Zhuravleva, Irina Fabian, Andrew Nelson, Dylan Okabe, Nobuhiro Pillepich, Annalisa Potter, Cicely Regamey, Manon Sakai, Kosei Shishido, Mona Truong, Nhut Wik, Daniel R. ZuHone, John High Energy Astrophysical Phenomena Astrophysics of Galaxies The XRISM Resolve microcalorimeter array measured the velocities of hot intracluster gas at two positions in the Coma galaxy cluster: 3'x3' squares at the center and at 6' (170 kpc) to the south. We find the line-of-sight velocity dispersions in those regions to be sigma_z=208+-12 km/s and 202+-24 km/s, respectively. The central value corresponds to a 3D Mach number of M=0.24+-0.015 and the ratio of the kinetic pressure of small-scale motions to thermal pressure in the intracluster plasma of only 3.1+-0.4%, at the lower end of predictions from cosmological simulations for merging clusters like Coma, and similar to that observed in the cool core of the relaxed cluster A2029. Meanwhile, the gas in both regions exhibits high line-of-sight velocity differences from the mean velocity of the cluster galaxies, Delta v_z=450+-15 km/s and 730+-30 km/s, respectively. A small contribution from an additional gas velocity component, consistent with the cluster optical mean, is detected along a sightline near the cluster center. The combination of the observed velocity dispersions and bulk velocities is not described by a Kolmogorov velocity power spectrum of steady-state turbulence; instead, the data imply a much steeper effective slope (i.e., relatively more power at larger linear scales). This may indicate either a very large dissipation scale resulting in the suppression of small-scale motions, or a transient dynamic state of the cluster, where large-scale gas flows generated by an ongoing merger have not yet cascaded down to small scales.
title	XRISM forecast for the Coma cluster: stormy, with a steep power spectrum
topic	High Energy Astrophysical Phenomena Astrophysics of Galaxies
url	https://arxiv.org/abs/2504.20928