X-ray metal line emission from the hot circumgalactic medium: probing the effects of supermassive black hole feedback

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Authors

TRUONG Nhut PILLEPICH Annalisa NELSON Dylan BOGDAN Akos SCHELLENBERGER Gerrit CHAKRABORTY Priyanka FORMAN William R KRAFT Ralph MARKEVITCH Maxim OGORZALEK Anna OPPENHEIMER Benjamin D SARKAR Arnab VEILLEUX Sylvain VOGELSBERGER Mark WANG Q Daniel WERNER Norbert ZHURAVLEVA Irina ZUHONE John

Year of publication 2023
Type Article in Periodical
Magazine / Source Monthly Notices of the Royal Astronomical Society
MU Faculty or unit

Faculty of Science

Citation
Web
Doi http://dx.doi.org/10.1093/mnras/stad2216
Keywords galaxies: evolution; galaxies: formation; galaxies: haloes; quasars: super massive black holes; X-rays: galaxies
Description We derive predictions from state-of-the-art cosmological galaxy simulations for the spatial distribution of the hot circumgalactic medium (CGM, [0.1-1]R-200c) through its emission lines in the X-ray soft band ([0.3-1.3] keV). In particular, we compare IllustrisTNG, EAGLE, and SIMBA and focus on galaxies with stellar mass 10(10-11.6) M-circle dot at z = 0. The three simulation models return significantly different surface brightness radial profiles of prominent emission lines from ionized metals such as O VII(f), O VIII, and Fe XVII as a function of galaxy mass. Likewise, the three simulations predict varying azimuthal distributions of line emission with respect to the galactic stellar planes, with IllustrisTNG predicting the strongest angular modulation of CGM physical properties at radial range greater than or similar to 0.3-0.5 R-200c. This anisotropic signal is more prominent for higher energy lines, where it can manifest as X-ray eROSITA-like bubbles. Despite different models of stellar and supermassive black hole (SMBH) feedback, the three simulations consistently predict a dichotomy between star-forming and quiescent galaxies at the Milky Way and Andromeda mass range, where the former are X-ray brighter than the latter. This is a signature of SMBH-driven outflows, which are responsible for quenching star formation. Finally, we explore the prospect of testing these predictions with a microcalorimeter-based X-ray mission concept with a large field of view. Such a mission would probe the extended hot CGM via soft X-ray line emission, determine the physical properties of the CGM, including temperature, from the measurement of line ratios, and provide critical constraints on the efficiency and impact of SMBH feedback on the CGM.
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