Observations of ’classical’ dwarf spheroidal kinematics

Abstract: I introduce a statistical model for the purpose of characterizing the spatial, 
kinematic and spectral index distributions of the stellar populations in 
pressure-supported dwarf galaxies based on spectroscopic measurements of individual 
stars.  This model allows for up to two chemo-dynamically independent stellar 
components.  Where two components are detected, estimates of their different 
half-light radii and velocity dispersions provide an estimate of the slope of the mass 
profile in which both components are embedded.  I discuss the application of this 
model to the Milky Way's `classical' dwarf spheroidal satellites.