Orbit-based structural decomposition and stellar population recovery for edge-on barred galaxies

In our previous paper, we developed an orbit-superposition method for edge-on barred galaxies, and constructed dynamical models based on different mock observations of three galaxies from the Auriga simulations. In this study, we adopt 12 cases with side-on bars (three simulated galaxies, each with four different projections). We decompose these galaxies into different structures combining the kinematic and morphological properties of stellar orbits, and compare the model-predicted components to their true counterparts in the simulations. Our models can identify (BP/X-shaped) bars, spheroidal bulges, thin disks, and spatially diffuse stellar halos. The mass fractions of bars and disks are well constrained with absolute biases |fmodel-fₜᵣᵤₑ|≤0.15. The mass fractions of halos are recovered with |fmodel-fₜᵣᵤₑ|≤0.03. For the bulge components, 10 of 12 cases have |fmodel-fₜᵣᵤₑ|≤0.05, while the other two cases have |fmodel-fₜᵣᵤₑ|≤0.10. Then, by tagging the stellar orbits with ages and metallicities, we derive the chemical properties of each structure. For stellar ages, our models recover the negative gradients in the bars and disks, but exhibit relatively larger uncertainties for age gradients in the bulges and halos. The mean stellar ages of all components are constrained with absolute biases |tmodel-tₜᵣᵤₑ|1\,Gyr. For stellar metallicities, our models reproduce the steep negative gradients of the bars and bulges, and all different kinds of metallicity gradients in the disks and halos. Except for the bulge in the simulated galaxy Au-18, the mean stellar metallicities of all other components are constrained with absolute biases |Zmodel-Zₜᵣᵤₑ|≤0.5\,Z_.