  Neutral atomic gas (HI) effectively traces galactic dynamics across mid to
large galactocentric radii. However, its limitations in observing small-scale
changes within the central few kiloparsecs, coupled with the often observed HI
deficit in galactic centers, necessitates using molecular gas emission as a
preferred tracer in these regions. Understanding the dynamics of both neutral
atomic and molecular gas is crucial for a more complete understanding of how
galaxies evolve, funnel gas from the outer disk into their central parts, and
eventually form stars. In this work we aim to quantify the dynamics of both,
the neutral atomic and molecular gas, in the nearby spiral galaxies NGC 1512,
NGC 4535, and NGC 7496 using new MeerKAT-HI observations together with ALMA CO
(2-1) observations from the PHANGS collaboration. We use the analysis tool
3D-Barolo to fit tilted ring models to the HI and CO observations. A combined
approach of using the HI to constrain the true disk orientation parameters
before applying these to the CO datasets is tested. This paper sets
expectations for the results of the upcoming high-resolution HI coverage of
many galaxies in the PHANGS-ALMA sample using MeerKAT or VLA, to establish a
robust methodology for characterizing galaxy orientations and deriving dynamics
from combining new HI with existing CO data.
