  In this paper we adopt a method to analyse absorption line spectra from
elliptical galaxies that determines the dynamics of the galaxy and at the same
time offers a way to study the stellar populations in that galaxy by a direct
fit to the spectra. The result of the modelling is a distribution function for
each stellar population that is considered in the fit. The method is described
in detail in an accompanying paper.
  This paper reports on a dynamical stellar population study in NGC3258, based
on spectra in two different wavelength regions, the near-IR Ca II triplet
around 8600A and the Ca H and K lines around 3900A. These absorption lines have
discriminating power toward various stellar types.
  The dynamical model shows an increase in dwarfs (represented by G2V stars)
toward the centre. Most of the rotation in the model is delivered by the giants
(represented by M1III stars). Moreover, the different models that were
considered indicate that establishing a potential for a galaxy is dependent on
the wavelength range used for the modelling.
