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Probable Detection of a Cooler Gas Component in the Perseus Cluster with XRISM


Journal article


J. Meunier, B. McNamara, A. Simionescu, F. Mernier, I. Zhuravleva, Congyao Zhang, Annie Heinrich, J. Hlavacek-Larrondo, F. Porter, B. Vigneron, J. Zuhone, E. Bellomi, Ian Drury, M. Eckart, R. Fujimoto, Y. Fujita, L. Gu, I. Hatsukade, Y. Ichinohe, Y. Kanemaru, T. Kitaguchi, S. Kitamoto, S. Kobayashi, T. Kohmura, Hironori Matsumoto, K. Matsushita, K. Migkas, I. Mitsuishi, K. Mori, H. Nakajima, Hirofumi Noda, A. Ogorzałek, Naomi Ota, Lior Shefler, N. Truong, A. Tumer, N. Uchida, Y. Uchida, S. Ueda
2026

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APA   Click to copy
Meunier, J., McNamara, B., Simionescu, A., Mernier, F., Zhuravleva, I., Zhang, C., … Ueda, S. (2026). Probable Detection of a Cooler Gas Component in the Perseus Cluster with XRISM.


Chicago/Turabian   Click to copy
Meunier, J., B. McNamara, A. Simionescu, F. Mernier, I. Zhuravleva, Congyao Zhang, Annie Heinrich, et al. “Probable Detection of a Cooler Gas Component in the Perseus Cluster with XRISM” (2026).


MLA   Click to copy
Meunier, J., et al. Probable Detection of a Cooler Gas Component in the Perseus Cluster with XRISM. 2026.


BibTeX   Click to copy

@article{j2026a,
  title = {Probable Detection of a Cooler Gas Component in the Perseus Cluster with XRISM},
  year = {2026},
  author = {Meunier, J. and McNamara, B. and Simionescu, A. and Mernier, F. and Zhuravleva, I. and Zhang, Congyao and Heinrich, Annie and Hlavacek-Larrondo, J. and Porter, F. and Vigneron, B. and Zuhone, J. and Bellomi, E. and Drury, Ian and Eckart, M. and Fujimoto, R. and Fujita, Y. and Gu, L. and Hatsukade, I. and Ichinohe, Y. and Kanemaru, Y. and Kitaguchi, T. and Kitamoto, S. and Kobayashi, S. and Kohmura, T. and Matsumoto, Hironori and Matsushita, K. and Migkas, K. and Mitsuishi, I. and Mori, K. and Nakajima, H. and Noda, Hirofumi and Ogorzałek, A. and Ota, Naomi and Shefler, Lior and Truong, N. and Tumer, A. and Uchida, N. and Uchida, Y. and Ueda, S.}
}

Abstract

We present an analysis of the temperature structure of the Perseus cluster atmosphere using XRISM Resolve observations. The average temperature rises from 3.3 keV near the nucleus of NGC 1275 to 8 keV at 10 arcmin (210 kpc), which is consistent with Chandra and XMM measurements. The velocity and velocity dispersion profiles are broadly consistent with those in arXiv:2509.04421. While the gas at altitudes beyond $\sim60$ kpc can be modeled as a single temperature plasma, we find evidence for more than one gas phase in the inner $\sim60$ kpc. The hotter gas component, traced primarily by the Fe He$\alpha$ line, has a velocity dispersion of $\lesssim140$ km s$^{-1}$. We detect a cooler, $\sim1.87-2.43$ keV, gas component with a velocity dispersion of $\sim300-400$ km s$^{-1}$ and a bulk velocity of $\sim 21-213$ km s$^{-1}$ with respect to the central galaxy. These ranges reflect large systematic uncertainties associated with modeling spatial-spectral mixing and the bright central point source. Potential low energy gain variations may add additional uncertainties. The cooler component is identified by broad wings in prominent emission lines, most notably S Ly$\alpha$ and Fe He$\alpha$. This cooler component's Mach number $\sim0.73-0.96$ and non-thermal pressure fraction of $\sim22.9-33.7\%$ are much higher than found for the hotter gas. The cooler gas may be associated with merging halos along the line of sight which formed the cool, sloshing spiral and/or cooling gas being disturbed by the radio jets and lobes.


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