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Multi-object and multi-fiber spectrographs on 4 and 8 meter telescopes makeit possible to use extragalactic planetary nebulae (PNe) in the outer halos ofearly-type galaxies as kinematical tracers, where classical techniques based onintegrated stellar light fail. Until now, published PNe radial velocity samplesare small, with only a few tens of radial velocity measurements (except for afew cases like NGC 5128 or M31), causing uncertainties in the mass and angularmomentum estimates based on these data. To quantify these uncertainties, wehave made equilibrium models for spherical galaxies, with and without darkmatter, and via Montecarlo simulations we produce radial velocity samples withdifferent sizes. We then apply, to these discrete radial velocity fields, thesame standard kinematical analysis as it is commonly done with small samples ofobserved PNe radial velocities. By comparison of the inferred quantities withthose computed from the analytical model, we test for systematic biases andestablish a robust procedure to infer the angular momentum distribution andradial velocity dispersion profiles from such samples.Comment: 18 pages, 26 figures, A&A 2001, in pres

Planetary nebulae as mass tracers of their parent galaxies: Biases in the estimate of the kinematical quantities