Banner image placeholder
Banner image

A XRISM/Resolve View of the Dynamics in the Hot Gaseous Atmosphere of M87


Journal article


M. Audard, H. Awaki, R. Ballhausen, A. Bamba, E. Behar, R. Boissay-Malaquin, L. Brenneman, G. V. Brown, Lia Corrales, E. Costantini, R. Cumbee, M. Díaz Trigo, C. Done, T. Dotani, K. Ebisawa, M. Eckart, D. Eckert, Satoshi Eguchi, T. Enoto, Y. Ezoe, A. Foster, R. Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, A. Furuzawa, L. Gallo, Javier A. García, Liyi Gu, M. Guainazzi, Kouichi Hagino, Kenji Hamaguchi, I. Hatsukade, K. Hayashi, T. Hayashi, N. Hell, E. Hodges-Kluck, A. Hornschemeier, Y. Ichinohe, D. Ishi, Manabu Ishida, K. Ishikawa, Y. Ishisaki, J. Kaastra, T. Kallman, Erin Kara, S. Katsuda, Y. Kanemaru, Rich Kelley, C. Kilbourne, S. Kitamoto, S. Kobayashi, T. Kohmura, A. Kubota, M. Leutenegger, M. Loewenstein, Yoshitomo Maeda, M. Markevitch, Hironori Matsumoto, K. Matsushita, D. McCammon, Brian McNamara, F. Mernier, Eric D. Miller, Jon M. Miller, I. Mitsuishi, M. Mizumoto, T. Mizuno, K. Mori, K. Mukai, Hiroshi Murakami, R. Mushotzky, H. Nakajima, K. Nakazawa, J. Ness, K. Nobukawa, M. Nobukawa, Hirofumi Noda, H. Odaka, S. Ogawa, A. Ogorzałek, T. Okajima, Naomi Ota, S. Paltani, R. Petre, P. Plucinsky, F. Porter, K. Pottschmidt, Kousuke Sato, Toshiki Sato, Makoto Sawada, H. Seta, M. Shidatsu, A. Simionescu, Randall K. Smith, Hiromasa Suzuki, A. Szymkowiak, H. Takahashi, M. Takeo, T. Tamagawa, Keisuke Tamura, Takaaki Tanaka, A. Tanimoto, M. Tashiro, Y. Terada, Y. Terashima, Y. Tsuboi, Masahiro Tsujimoto, H. Tsunemi, T. Tsuru, Ayşegül Tümer, Hiroyuki Uchida, N. Uchida, Y. Uchida, H. Uchiyama, S. Ueda, Y. Ueda, S. Uno, J. Vink, S. Watanabe, Brian J. Williams, S. Yamada, S. Yamada, Hiroya Yamaguchi, K. Yamaoka, N. Yamasaki, M. Yamauchi, S. Yamauchi, T. Yaqoob, T. Yoneyama, Tessei Yoshida, M. Yukita, I. Zhuravleva, M. Charbonneau, N. Dizdar, M. Fujita, Daisuke Ito, Jessica Martin, H. McCall, H. Russell, J. Zuhone
Astrophysical Journal, 2025

Semantic Scholar ArXiv DOI
Cite

Cite

APA   Click to copy
Audard, M., Awaki, H., Ballhausen, R., Bamba, A., Behar, E., Boissay-Malaquin, R., … Zuhone, J. (2025). A XRISM/Resolve View of the Dynamics in the Hot Gaseous Atmosphere of M87. Astrophysical Journal.


Chicago/Turabian   Click to copy
Audard, M., H. Awaki, R. Ballhausen, A. Bamba, E. Behar, R. Boissay-Malaquin, L. Brenneman, et al. “A XRISM/Resolve View of the Dynamics in the Hot Gaseous Atmosphere of M87.” Astrophysical Journal (2025).


MLA   Click to copy
Audard, M., et al. “A XRISM/Resolve View of the Dynamics in the Hot Gaseous Atmosphere of M87.” Astrophysical Journal, 2025.


BibTeX   Click to copy

@article{m2025a,
  title = {A XRISM/Resolve View of the Dynamics in the Hot Gaseous Atmosphere of M87},
  year = {2025},
  journal = {Astrophysical Journal},
  author = {Audard, M. and Awaki, H. and Ballhausen, R. and Bamba, A. and Behar, E. and Boissay-Malaquin, R. and Brenneman, L. and Brown, G. V. and Corrales, Lia and Costantini, E. and Cumbee, R. and Trigo, M. Díaz and Done, C. and Dotani, T. and Ebisawa, K. and Eckart, M. and Eckert, D. and Eguchi, Satoshi and Enoto, T. and Ezoe, Y. and Foster, A. and Fujimoto, R. and Fujita, Yutaka and Fukazawa, Yasushi and Fukushima, Kotaro and Furuzawa, A. and Gallo, L. and García, Javier A. and Gu, Liyi and Guainazzi, M. and Hagino, Kouichi and Hamaguchi, Kenji and Hatsukade, I. and Hayashi, K. and Hayashi, T. and Hell, N. and Hodges-Kluck, E. and Hornschemeier, A. and Ichinohe, Y. and Ishi, D. and Ishida, Manabu and Ishikawa, K. and Ishisaki, Y. and Kaastra, J. and Kallman, T. and Kara, Erin and Katsuda, S. and Kanemaru, Y. and Kelley, Rich and Kilbourne, C. and Kitamoto, S. and Kobayashi, S. and Kohmura, T. and Kubota, A. and Leutenegger, M. and Loewenstein, M. and Maeda, Yoshitomo and Markevitch, M. and Matsumoto, Hironori and Matsushita, K. and McCammon, D. and McNamara, Brian and Mernier, F. and Miller, Eric D. and Miller, Jon M. and Mitsuishi, I. and Mizumoto, M. and Mizuno, T. and Mori, K. and Mukai, K. and Murakami, Hiroshi and Mushotzky, R. and Nakajima, H. and Nakazawa, K. and Ness, J. and Nobukawa, K. and Nobukawa, M. and Noda, Hirofumi and Odaka, H. and Ogawa, S. and Ogorzałek, A. and Okajima, T. and Ota, Naomi and Paltani, S. and Petre, R. and Plucinsky, P. and Porter, F. and Pottschmidt, K. and Sato, Kousuke and Sato, Toshiki and Sawada, Makoto and Seta, H. and Shidatsu, M. and Simionescu, A. and Smith, Randall K. and Suzuki, Hiromasa and Szymkowiak, A. and Takahashi, H. and Takeo, M. and Tamagawa, T. and Tamura, Keisuke and Tanaka, Takaaki and Tanimoto, A. and Tashiro, M. and Terada, Y. and Terashima, Y. and Tsuboi, Y. and Tsujimoto, Masahiro and Tsunemi, H. and Tsuru, T. and Tümer, Ayşegül and Uchida, Hiroyuki and Uchida, N. and Uchida, Y. and Uchiyama, H. and Ueda, S. and Ueda, Y. and Uno, S. and Vink, J. and Watanabe, S. and Williams, Brian J. and Yamada, S. and Yamada, S. and Yamaguchi, Hiroya and Yamaoka, K. and Yamasaki, N. and Yamauchi, M. and Yamauchi, S. and Yaqoob, T. and Yoneyama, T. and Yoshida, Tessei and Yukita, M. and Zhuravleva, I. and Charbonneau, M. and Dizdar, N. and Fujita, M. and Ito, Daisuke and Martin, Jessica and McCall, H. and Russell, H. and Zuhone, J.}
}

Abstract

The XRISM/Resolve microcalorimeter directly measured the gas velocities in the core of the Virgo Cluster, the closest example of active galactic nucleus (AGN) feedback in a cluster. This proximity allows us to resolve the kinematic impact of feedback on scales down to 5 kpc. Our spectral analysis reveals a high velocity dispersion of σv=262−38+45 km s−1 near the AGN, which steeply declines to ∼60 km s−1 between 5 and 25 kpc in the northwest direction. The observed line-of-sight bulk velocity in all regions is broadly consistent with the central galaxy, M87, with a mild trend toward blueshifted motions at larger radii. Systematic uncertainties have been carefully assessed and do not affect the measurements. The central velocities, if attributed entirely to isotropic turbulence, correspond to a transonic intracluster medium at sub-6 kpc scales with 3D Mach number 0.69-0.11+0.14 and a nonthermal pressure fraction of 21-5+7% . Simple models of weak shocks and sound waves and calculations assuming isotropic turbulence both support the hypothesis that the velocity field reflects a mix of shock-driven expansion and turbulence. Compared to other clusters observed by XRISM to date, M87’s central region stands out as the most kinematically disturbed, exhibiting both the highest velocity dispersion and the largest 3D Mach number, concentrated at the smallest physical scales.


Share

Text Only Owlstown
QR Code
Translate to