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We present a new halo model of neutral hydrogen (HI) calibrated to galaxyformation simulations at redshifts $z\sim0.1$ and $z\sim1.0$ that we employ toinvestigate the constraining power of interferometric HI intensity mapping onHI astrophysics. We demonstrate that constraints on the small-scale HI powerspectrum can break the degeneracy between the HI density $\Omega_{\rm HI}$ andthe HI bias $b_{\rm HI}$. For $z\sim0.1$, we forecast that an accuratemeasurement of $\Omega_{\rm HI}$ up to 6% level precision and the large-scaleHI bias $b_{\rm HI}^0$ up to 1% level precision can be achieved using SquareKilometre Array (SKA) pathfinder data from MeerKAT and Australian SKAPathfinder (ASKAP). We also propose a new description of the HI shot noise inthe halo model framework in which a scatter of the relation between the HI massof galaxies and their host halo mass is taken into account. Furthermore, giventhe number density of HI galaxies above a certain HI mass threshold, futuresurveys will also be able to constrain the HI mass function using only the HIshot noise. This will lead to constraints at the 10% level using the standardSchechter function. This technique will potentially provide a new way ofmeasuring the HI Mass Function, independent from existing methods. We predictthat the SKA will be able to further improve the low-redshift constraints by afactor of 3, as well as pioneering measurements of HI astrophysics at higherredshifts.

Extracting HI Astrophysics from Interferometric Intensity Mapping