# Chemodynamical Modelling of the Galactic Bulge and Bar

## TL;DR

This paper introduces a chemodynamical model of the Milky Way's bulge and bar, integrating metallicity data to analyze stellar populations and their dynamics, revealing distinct properties of metal-rich and metal-poor stars.

## Contribution

It extends the Made-to-Measure method to include stellar metallicity, enabling detailed chemodynamical modeling of the galactic bulge, bar, and inner disk.

## Key findings

- Metal-rich stars are strongly barred with disk-like dynamics.
- Metal-poor stars show diverse kinematic behaviors, indicating multiple stellar populations.
- The model reproduces observed vertex deviations in the bulge.

## Abstract

We present the first self-consistent chemodynamical model fitted to reproduce data for the galactic bulge, bar and inner disk. We extend the Made-to-Measure method to an augmented phase-space including the metallicity of stars, and show its first application to the bar region of the Milky Way. Using data from the ARGOS and APOGEE (DR12) surveys, we adapt the recent dynamical model from Portail et al. to reproduce the observed spatial and kinematic variations as a function of metallicity, thus allowing the detailed study of the 3D density distributions, kinematics and orbital structure of stars in different metallicity bins. We find that metal-rich stars with [Fe/H] > -0.5 are strongly barred and have dynamical properties that are consistent with a common disk origin. Metal-poor stars with [Fe/H] < -0.5 show strong kinematic variations with metallicity, indicating varying contributions from the underlying stellar populations. Outside the central kpc, metal-poor stars are found to have the density and kinematics of a thick disk while in the inner kpc, evidence for an extra concentration of metal-poor stars is found. Finally, the combined orbit distributions of all metallicities in the model naturally reproduce the observed vertex deviations in the bulge. This paper demonstrates the power of Made-to-Measure chemodynamical models, that when extended to other chemical dimensions will be very powerful tools to maximize the information obtained from large spectroscopic surveys such as APOGEE, GALAH and MOONS.