Three Models of the Gravitational Potential of the Milky Way

TL;DR

This paper refines axisymmetric models of the Milky Way's gravitational potential using extensive observational data, resulting in two- and three-component models that improve understanding of stellar and cluster dynamics.

Contribution

It introduces new two- and three-component models of the Galaxy's gravitational potential based on a refined rotation curve derived from diverse stellar and galactic data.

Findings

Constructed rotation curve from masers, Cepheids, and other stars.

Developed two- and three-component potential models.

Validated models against Illustris TNG50 simulations.

Abstract

The parameters of an axisymmetric model for the gravitational potential of the Galaxy have been refined. The basic curve of the Galaxy's rotation in a distance interval of $R:0-190$ kpc was constructed using the velocities of masers, classical Cepheids, Red Clump stars, Blue Horizontal Branch stars, halo stars, globular clusters, and dwarf satellite galaxies of the Milky Way. The rotation curve was selected in such a way that there would be no dominant burst of circular velocities in the central ($R<2$ kpc) region of the Galaxy. As a result, we constructed two two-component models of the galactic potential, which include contributions from the disk and the halo of invisible matter, as well as a three-component model with a small-mass bulge added in advance. These models can be useful in studying the long-term orbital evolution of stars and open and globular star clusters in the central ($R<4$ kpc) region of the Galaxy. The constructed models were tested for self-consistency by comparing their rotation curves with a set of model curves generated with the Illustris TNG50 software package.