Kavli Affiliate: Mark Vogelsberger
| First 5 Authors: Nhut Truong, Annalisa Pillepich, Dylan Nelson, Ákos Bogdán, Gerrit Schellenberger
| Summary:
We derive predictions from state-of-the-art cosmological galaxy simulations
for the spatial distribution of the hot circumgalactic medium (CGM, ${rm
[0.1-1]R_{200c}}$) 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 $10^{10-11.6}, MSUN$ at $z=0$. The three
simulation models return significantly different surface brightness radial
profiles of prominent emission lines from ionized metals such as OVII(f),
OVIII, and FeXVII 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
${gtrsim0.3-0.5,R_{200c}}$. 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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