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The hot component of the circum-galactic medium (CGM) around star forminggalaxies is detected as diffuse X-ray emission. The X-ray spectra from the CGMdepend on the temperature and metallicity of the emitting plasma, providingimportant information about the feeding and feedback of the galaxy. Theobserved spectra are commonly fitted using simple 1-Temperature (1-T) or 2-Tmodels. However, the actual temperature distribution of the gas can be complexbecause of the interaction between galactic outflows and halo gas. Here wedemonstrate this by analysing 3-D hydrodynamical simulations of the CGM with arealistic outflow model. We investigate the physical properties of thesimulated hot CGM, which shows a broad distribution in density, temperature,and metallicity. By constructing and fitting the simulated spectra, we showthat, while the 1-T and 2-T models are able to fit the synthesized spectrareasonably well, the inferred temperature(s) does not bear much physicalmeaning. Instead, we propose a log-normal distribution as a more physicalmodel. The log-normal model better fits the simulated spectra while reproducingthe gas temperature distribution. We also show that when the star formationrate is high, the spectra inside the bi-conical outflows are distinct from thatoutside, as outflows are generally hotter and more metal-enriched. Finally, weproduce mock spectra for future missions with the eV-level spectral resolution,such as Athena, Lynx, HUBS and XRISM.

X-ray Spectra of Circumgalactic Medium Around Star-Forming Galaxies: Connecting Simulations to Observations