  We study the use of parallax microlensing to separate the effects of the mass
function of dark massive halo objects (MHOs or `machos') on the one hand and
their spatial distribution and kinematics on the other. This disentanglement is
supposed to allow a much better determination of the two than could be achieved
entirely on the basis of the durations of events. We restrict our treatment to
the same class of power-law spherical models for the halo of MHOs studied in a
previous paper (astro-ph/9609187). Whereas the duration-based error in the
average MHO mass, \mu exceeds (at N=100 events) \mu by a factor of 2 or more,
parallax microlensing remarkably brings it down to 15-20% of \mu, regardless of
the shape of the mass function. In addition, the slope \alpha of the mass
function, dn/d\mu\propto\mu^{\alpha}, can be inferred relatively accurately
(\sigma_{\alpha} < 0.4) for a broader range, -3 <\alpha < 0. The improvement in
the inference of the halo structure is also significant: the index \gamma of
the density profile (\rho\sim R^{-\gamma}) can be obtained with the error
\sigma_{\gamma} <0.4. While in a typical situation the errors for the
parameters specifying the velocity dispersion profile are of about the same
magnitude as the parameters themselves, virtually all the uncertainty is
`concentrated' in linear combinations of the parameters that may have little
influence on the profile and thus allow its reasonably accurate inference.
