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We present an in-depth analysis of gas morphologies for a sample of 25 MilkyWay-like galaxies from the IllustrisTNG TNG50 simulation. We constrain themorphology of cold, warm, hot gas, and gas particles as a whole using a LocalShell Iterative Method (LSIM) and explore its observational implications bycomputing the hard-to-soft X-ray ratio, which ranges between$10^{-3}$-$10^{-2}$ in the inner $\sim 50 \rm kpc$ of the distribution and$10^{-5}$-$10^{-4}$ at the outer portion of the hot gas distribution. We groupgalaxies into three main categories: simple, stretched, and twisted. Thesecategories are based on the radial reorientation of the principal axes of thereduced inertia tensor. We find that a vast majority ($77\%$) of the galaxiesin our sample exhibit twisting patterns in their radial profiles. Additionally,we present detailed comparisons between 1) the gaseous distributions belongingto individual temperature regimes, 2) the cold gas distributions and stellardistributions, and 3) the gaseous distributions and dark matter (DM) halos. Wefind a strong correlation between the morphological properties of the cold gasand stellar distributions. Furthermore, we find a correlation between gaseousdistributions with DM halo that increases with gas temperature, implying thatwe may use the warm-hot gaseous morphology as a tracer to probe the DMmorphology. Finally, we show gaseous distributions exhibit significantly moreprolate morphologies than the stellar distributions and DM halos, which wehypothesize is due to stellar and AGN feedback.

Gas Morphology of Milky Way-like Galaxies in the TNG50 Simulation: Signals of Twisting and Stretching