Препринт

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

Julian MeunierWaterloo Centre for Astrophysics , Department of Physics & Astronomy , University of Waterloo , Ontario N2L 3G1 , CanadaBrian R. McNamaraWaterloo Centre for Astrophysics , Department of Physics & Astronomy , University of Waterloo , Ontario N2L 3G1 , CanadaAurora SimionescuSRON Space Research Organisation Netherlands , Niels Bohrweg 4 , 2333 CA , Leiden , The NetherlandsFrançois MernierIrina ZhuravlevaDepartment of Astronomy and Astrophysics , University of Chicago , Chicago , IL 60637 , USACongyao ZhangDepartment of Theoretical Physics and Astrophysics , Masaryk University , Brno 61137 , CzechiaAnnie HeinrichDepartment of Astronomy and Astrophysics , University of Chicago , Chicago , IL 60637 , USAJulie Hlavacek-LarrondoUniversité de MontréalFrederick S. PorterNASA / Goddard Space Flight Center , Greenbelt , MD 20771 , USABenjamin VigneronUniversité de MontréalJohn ZuHoneCenter for Astrophysics | Harvard & Smithsonian , Cambridge , MA 02138 , USAElena BellomiCenter for Astrophysics | Harvard & Smithsonian , Cambridge , MA 02138 , USAIan DruryDepartment of Physics and Astronomy , The University of Georgia , Athens , GA 30602 , USAMegan E. EckartLawrence Livermore National Laboratory , CA 94550 , USARyuichi FujimotoInstitute of Space and Astronautical Science (ISAS) , Japan Aerospace Exploration Agency (JAXA) , Kanagawa 252-5210 , JapanYutaka FujitaDepartment of Physics , Tokyo Metropolitan University , Tokyo 192-0397 , JapanLiyi GuSRON Netherlands Institute for Space Research , Leiden , The NetherlandsIsamu HatsukadeFaculty of Engineering , University of Miyazaki , Miyazaki 889-2192 , JapanYuto IchinoheRIKEN Nishina Center , Saitama 351-0198 , JapanYoshiaki KanemaruInstitute of Space and Astronautical Science (ISAS) , Japan Aerospace Exploration Agency (JAXA) , Kanagawa 252-5210 , JapanTakao KitaguchiRIKEN Nishina Center , Saitama 351-0198 , JapanShunji KitamotoDepartment of Physics , Rikkyo University , Tokyo 171-8501 , JapanShogo KobayashiFaculty of Physics , Tokyo University of Science , Tokyo 162-8601 , JapanTakayoshi KohmuraFaculty of Science and Technology , Tokyo University of Science , Chiba 278-8510 , JapanHironori MatsumotoDepartment of Earth and Space Science , Osaka University , Osaka 560-0043 , JapanKyoko MatsushitaFaculty of Physics , Tokyo University of Science , Tokyo 162-8601 , JapanK. MigkasSRON Netherlands Institute for Space Research , Leiden , The NetherlandsIkuyuki MitsuishiDepartment of Physics , Nagoya University , Aichi 464-8602 , JapanKoji MoriFaculty of Engineering , University of Miyazaki , Miyazaki 889-2192 , JapanHiroshi NakajimaCollege of Science and Engineering , Kanto Gakuin University , Kanagawa 236-8501 , JapanHirofumi NodaAstronomical Institute , Tohoku University , Miyagi 980-8578 , JapanAnna OgorzalekNaomi OtaDepartment of Physics , Nara Women's University , Nara 630-8506 , JapanLior SheflerDepartment of Physics and Astronomy , The University of Georgia , Athens , GA 30602 , USANhut TruongAyşegül TümerNagomi UchidaInstitute of Space and Astronautical Science (ISAS) , Japan Aerospace Exploration Agency (JAXA) , Kanagawa 252-5210 , JapanYuusuke UchidaFaculty of Science and Technology , Tokyo University of Science , Chiba 278-8510 , JapanShutaro Ueda

2026

ABI

Аннотация

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$α$ 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$α$ and Fe He$α$. 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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