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Understanding what shapes the cold gas component of galaxies, which bothprovides the fuel for star formation and is strongly affected by the subsequentstellar feedback, is a crucial step towards a better understanding of galaxyevolution. Here, we analyse the HI properties of a sample of 46 Milky Wayhalo-mass galaxies, drawn from cosmological simulations (EMP-Pathfinder andFIREbox). This set of simulations comprises galaxies evolved self-consistentlyacross cosmic time with different baryonic sub-grid physics: three differentstar formation models [constant star formation efficiency (SFE) with differentstar formation eligibility criteria, and an environmentally-dependent,turbulence-based SFE] and two different feedback prescriptions, where only onesub-sample includes early stellar feedback. We use these simulations to assessthe impact of different baryonic physics on the HI content of galaxies. We findthat the galaxy-wide HI properties agree with each other and with observations.However, differences appear for small-scale properties. The thin HI discsobserved in the local Universe are only reproduced with a turbulence-dependentSFE and/or early stellar feedback. Furthermore, we find that the morphology ofHI discs is particularly sensitive to the different physics models: galaxiessimulated with a turbulence-based SFE have discs that are smoother and morerotationally symmetric, compared to those simulated with a constant SFE;galaxies simulated with early stellar feedback have more regular discs thansupernova-feedback-only galaxies. We find that the rotational asymmetry of theHI discs depends most strongly on the underlying physics model, making this apromising observable for understanding the physics responsible for shaping theinterstellar medium of galaxies.

HI discs of L$_{\ast}$ galaxies as probes of the baryonic physics of galaxy evolution