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The hot, X-ray-emitting phase of the circumgalactic medium in galaxies isbelieved to be the reservoir of baryons from which gas flows onto the centralgalaxy and into which feedback from AGN and stars inject mass, momentum,energy, and metals. These effects shape the velocity fields of the hot gas,which can be observed by X-ray IFUs via the Doppler shifting and broadening ofemission lines. In this work, we analyze the gas kinematics of the hotcircumgalactic medium of Milky Way-mass disk galaxies from the TNG50 simulationwith synthetic observations to determine how future instruments can probe thisvelocity structure. We find that the hot phase is often characterized byoutflows outward from the disk driven by feedback processes, radial inflowsnear the galactic plane, and rotation, though in other cases the velocity fieldis more disorganized and turbulent. With a spectral resolution of $\sim$1 eV,fast and hot outflows ($\sim$200-500 km s$^{-1}$) can be measured, depending onthe orientation of the galaxy on the sky. The rotation velocity of the hotphase ($\sim$100-200 km s$^{-1}$) can be measured using line shifts in edge-ongalaxies, and is slower than that of colder gas phases but similar to stellarrotation velocities. By contrast, the slow inflows ($\sim$50-100 km s$^{-1}$)are difficult to measure in projection with these other components. We findthat the velocity measured is sensitive to which emission lines are used.Measuring these flows will help constrain theories of how the gas in thesegalaxies forms and evolves.

Properties of the Line-of-Sight Velocity Field in the Hot and X-ray Emitting Circumgalactic Medium of Nearby Simulated Disk Galaxies