  Dark matter (DM) halo properties are extensively studied in cosmological
simulations but are very challenging to estimate from observations. The DM halo
density profile of observed galaxies is modelled using multiple probes that
trace the dark matter potential. However, the angular momentum distribution of
DM halos is still a subject of debate. In this study we investigate a method
for estimating the halo spin and halo concentration of low surface brightness
(LSB), gas-rich dwarf barred galaxy UGC 5288, by forward modelling disk
properties derived from observations - stellar and gas surface densities, disk
scale length, HI rotation curve, bar length and bar ellipticity. We combine
semi-analytical techniques, N-body/SPH and cosmological simulations to model
the DM halo of UGC 5288 with both a cuspy Hernquist profile and a flat-core
pseudo-isothermal profile. We find that the best match with observations is a
pseudo-isothermal halo model with a core radius of $r_{c} = 0.23$ kpc, and halo
spin of $\lambda$= 0.08 at the virial radius. Although our findings are
consistent with previous core radius estimates of the halo density profile of
UGC 5288, as well as with the halo spin profiles of similar mass analogues of
UGC5288 in the high-resolution cosmological-magneto-hydrodynamical simulation
TNG50, there still remain some uncertainties as we are limited in our knowledge
of the formation history of the galaxy. Additionally, we find that the inner
halo spin ($ r< 10$ kpc) in barred galaxies is different from the unbarred
ones, and the halo spin shows weak correlations with bar properties.
