Dynamical Simulations of NGC 2523 and NGC 4245

TL;DR

This paper uses dynamical simulations and observational data to estimate the bar pattern speeds in two barred galaxies, NGC 2523 and NGC 4245, confirming consistency between different measurement methods.

Contribution

It introduces a method combining sticky-particle simulations with near-infrared imaging to estimate galaxy bar pattern speeds, validated against the Tremaine-Weinberg method.

Findings

Both methods yield consistent pattern speeds within errors.

Inner rings serve as resonance features to constrain models.

Simulations match observed morphologies effectively.

Abstract

We present dynamical simulations of NGC 2523 and NGC 4245, two barred galaxies (types SB(r)b and SB(r)0/a, respectively) with prominent inner rings. Our goal is to estimate the bar pattern speeds in these galaxies by matching a sticky-particle simulation to the $B$-band morphology, using near-infrared $K_s$-band images to define the gravitational potentials. We compare the pattern speeds derived by this method with those derived in our previous paper using the well-known Tremaine-Weinberg continuity equation method. The inner rings in these galaxies, which are likely to be resonance features, help to constrain the dynamical models. We find that both methods give the same pattern speeds within the errors.