  The halo masses of nearby individual elliptical galaxies can be estimated by
using the kinematics of their stars, planetary nebulae, and globular clusters
-- ideally in combination. With currently improving coverage of galaxies of
ordinary luminosities and morphologies, systematic trends may be identified.
Bright, boxy ellipticals show strong signatures of dark matter, while faint,
disky ones typically do not. The former result is problematic for the MOND
theory of gravity, and the latter is a challenge to explain in the LCDM
paradigm of galaxy formation.
