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: http://www.stsci.edu/~marel/abstracts/abs_R14.html
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A simple algorithm is presented for the calculation of the projected
line-of-sight velocity profiles (VPs) of non-rotating anisotropic
spherical dynamical models with a phase-space distribution function of
the Osipkov-Merritt type. The velocity distribution in these models is
isotropic inside the anisotropy radius r_a and becomes increasingly
radially biased at larger radii. VP shape parameters are presented for
a family of models in which the luminous mass density has a power-law
cusp rho_L = r^{-gamma} at small radii and a power-law fall-off rho_L
= r^{-4} at large radii. Self-consistent models and models in which
the luminous matter is embedded in a dark halo are discussed. The
effects of changes in the cusp slope gamma and in the anisotropy
radius r_a are documented, and the area in the (gamma, r_a)-plane that
contains physical models is delineated. The shapes of the VPs of the
models show a considerable (and observable) variation with projected
galactocentric radius. These models will be useful for interpreting
the data on the VP shapes of elliptical galaxies that are now becoming
available.
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Last modified December 8, 1998.
Roeland van der Marel,
marel@stsci.edu.
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