Probabilistic distribution functions

Abstract

Observed clusters should be modelled by considering the distribution function to be a random variable that quantifies the degree of excitation of the system's normal modes. A system of canonical coordinates for the space of DFs is identified so DFs can be weighted in a consistent way.

arXiv comment5 pages. Submitted to MNRAS

References in corpus (6)

• Gaia Data Release 2. Summary of the contents and survey properties
• A dynamically young and perturbed Milky Way disk
• Footprints of the Sagittarius dwarf galaxy in the $Gaia$ data set
• Does NGC 6397 contain an intermediate-mass black hole or a more diffuse inner subcluster?
• Constraining black hole masses from stellar kinematics by summing over all possible distribution functions
• Relaxation of spherical stellar systems

Cited by in corpus (1)

• Modes of a stellar system I: ergodic systems