Self-consistent modelling of our Galaxy with Gaia data

Abstract

Galaxy models are fundamental to exploiting surveys of our Galaxy. There is now a significant body of work on axisymmetric models. A model can be defined by giving the DF of each major class of stars and of dark matter. Then the self-consistent gravitational potential is determined. Other modelling techniques are briefly considered before an overview of some early work on non-axisymmetric models.

8 pages, 1 figure to appear in proceedings of IAU Symposium 330, eds. Recio-Blanco, de Laverny & Brown

References in corpus (11)

• Dynamical modelling of the Galactic bulge and bar: the Milky Way's bar pattern speed, stellar, and dark matter mass distribution
• Constraining the Galaxy's dark halo with RAVE stars
• NMAGIC: Fast Parallel Implementation of a Chi-Squared-Made-to-Measure Algorithm for Modelling Observational Data
• Action-based distribution functions for spheroidal galaxy components
• A centrally heated dark halo for our Galaxy
• Bringing the Galaxy's dark halo to life
• Characterizing stellar halo populations II: The age gradient in blue horizontal-branch stars
• A fast algorithm for estimating actions in triaxial potentials
• Modelling the Milky Way's globular cluster system
• The structural evolution of galaxies with both thin and thick discs
• Managing resonant trapped orbits in our Galaxy

Cited by in corpus (4)

• Anatomy of Eddington-like inversion methods in the context of dark matter searches
• $\gamma$-ray and $\nu$ searches for dark matter subhalos in the Milky Way with a baryonic potential
• Axion Structure Formation I: The Co-motion Picture
• Dynamical Models of the Milky Way in Action Space with LAMOST DR8 and GAIA EDR3