2025RAA....25g5001L

To address the disk-halo degeneracy problem, we investigate the nearby barred spiral galaxy NGC 1097. We construct mass models using 3.6 and 4.5 μm near-infrared photometric images from the S⁴G survey, constrained by rotation curves derived from CO(J = 2-1) data from the PHANGS-ALMA survey. These models serve as inputs for a suite of hydrodynamic simulations, where we systematically test the influence of key parameters including the disk mass scaling factor (f_M), bar pattern speed (Ω_b), and gas sound speed (c_s). By comparing the CO(2-1) kinematic maps in the bar region with those from the simulations, we perform a standard χ² analysis to identify the best-fit model. The best-fit model reproduces the observed morphological and kinematic gas features of the galaxy, indicating that NGC 1097 likely hosts a maximal disk with a slowly rotating bar. We also test the influence of a boxy/peanut-shaped (B/P) bulge by incorporating a double-peaked vertical density profile into the model. This B/P structure tends to weaken the bar's non-axisymmetric potential and necessitate a higher bar pattern speed to reproduce the observed gas morphology.