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Vigorous turbulence driven by quasar-mode feedback in a cluster core

Satoshi YamadaFrontier Research Institute for Interdisciplinary Sciences, Tohoku University, Sendai, JapanShutaro UedaAdvanced Research Center for Space Science and Technology, College of Science and Engineering, Kanazawa University, Kanazawa, JapanHirofumi NodaAstronomical Institute, Graduate School of Science, Tohoku University, Sendai, JapanYutaka FujitaDepartment of Physics, Graduate School of Science, Tokyo Metropolitan University, Tokyo, JapanMisaki MizumotoScience Education Research Unit, University of Teacher Education Fukuoka, Fukuoka, JapanKentaro NagamineKavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, JapanClaudio RicciKavli Institute for Astronomy and Astrophysics, Peking University, Beijing, ChinaShoji OgawaFaculty of Science and Technology, Tokyo University of Science, Noda, JapanT. KawamuroRIKEN Cluster for Pioneering Research, Wako, JapanShinya YamadaAstronomical Institute, Graduate School of Science, Tohoku University, Sendai, JapanYuichi TerashimaDepartment of Physics, Faculty of Science, Ehime University, Ehime, JapanYoshihiro UedaDepartment of Astronomy, Kyoto University, Kyoto, Japan

2026en

ABI

Аннотация

Abstract Quasars are among the most luminous objects. They are powered by accretion onto supermassive black holes. They are thought to impact cosmological evolution primarily through energetic winds, known as quasar-mode feedback, yet the efficiency and spatial extent of this process remain poorly constrained. Here we present X-Ray Imaging and Spectroscopy Mission (XRISM) observations of H1821+643—the nearest galaxy cluster with a central quasar (redshift z = 0.297)—which was a rare opportunity to directly probe quasar-mode feedback in the intracluster medium. High-resolution spectroscopy reveals exceptionally broadened Fe XXV emission lines from the intracluster medium, with a velocity dispersion of approximately 300 km s −1 , far exceeding values observed in nearby cluster cores. These lines originate predominantly at radii of 20–100 kpc from the centre. Assuming that turbulence from a quasar-driven shock led to the broadening of the lines, the energy injected by the quasar beyond galactic scales (≳20 kpc) is estimated to be ≳1–10% of its radiative energy. Notably, this feedback efficiency exceeds previous multiwavelength estimates by orders of magnitude (≲0.01%) and reaches the levels required by the latest cosmological hydrodynamical simulations. This finding of vigorous turbulence indicates that quasar-mode feedback plays a central role in regulating galaxy and cluster evolution at high redshift.

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DOI: 10.1038/s41550-026-02939-x

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