Galactoseismology in the GAIA Era
arXiv:1608.04150 · doi:10.1017/S1743921316011078
Abstract
The GAIA satellite will provide unprecedented phase-space information for our Galaxy and enable a new era of Galactic dynamics. We may soon see successful realizations of Galactoseismology, i.e., inferring the characteristics of the Galactic potential and sub-structure from a dynamical analysis of observed perturbations in the gas or stellar disk of the Milky Way. Here, we argue that to maximally take advantage of the GAIA data and other complementary surveys, it is necessary to build comprehensive models for both the stars and the gas. We outline several key morphological puzzles of the Galactic disk and proposed solutions that may soon be tested.
arXiv comment3 pages, 1 figure, proceedings for Galaxy Outskirts conference
References in corpus (14)
- The Field of Streams: Sagittarius and its Siblings
- The Ghost of Sagittarius and Lumps in the Halo of the Milky Way
- Extremely Inefficient Star Formation in the Outer Disks of Nearby Galaxies
- The Kinematics, Orbit, and Survival of the Sagittarius Dwarf Spheroidal Galaxy
- Galactoseismology: Discovery of Vertical Waves in the Galactic Disk
- Rings and Radial Waves in the Disk of the Milky Way
- The Spiral Structure of the Outer Milky Way in Hydrogen
- Tidal Streams as Probes of the Galactic Potential
- Substructure in bulk velocities of Milky Way disk stars
- The Role of Gas In Maintaining Quasi-Steady Spiral Structure In Stellar Disks
- Tidal Imprints of a Dark Sub-Halo on the Outskirts of the Milky Way II. Perturber Azimuth
- Spitzer, Gaia, and the Potential of the Milky Way
- Incorporating Streams into Milky Way Models
- Clustered Cepheid Variables 90 kiloparsec from the Galactic Center