  Dark matter (DM) halo angular momentum is very challenging to determine from
observations of galaxies. In this study, we present a new hybrid method of
estimating the dimensionless halo angular momentum, halo spin of a gas-rich
dwarf barred galaxy UGC5288 using N-Body/SPH simulations. We forward model the
galaxy disk properties: stellar and gas mass, surface densities, disk
scalelengths, bar length and bar ellipticity from observations. We use the HI
rotation curve to constrain the DM halo density profile and further use the bar
properties to determine the models that best represent the observed baryonic
disk. We compare the halo spin profile from our models to the halo spin
profiles of similar mass dwarf galaxy analogues of UGC5288 in the TNG50
simulations. The halo spin profile from our simulated models matches within
ballpark values of the median spin profile of UGC5288 analogues in the TNG50
simulations, although there are some uncertainties due to the DM halo
evolutionary history.
