  We have studied the angular distribution of the magnetic field vector in the
solar internetwork employing high-quality data (noise level $\sigma \approx
3\times 10^{-4}$ in units of the quiet-Sun intensity) at different latitudes
recorded with the Hinode/SP instrument. Instead of applying traditional
inversion codes of the radiative transfer equation to retrieve the magnetic
field vector at each spatial point on the solar surface and studying the
resulting distribution of the magnetic field vector, we surmised a theoretical
distribution function of the magnetic field vector and used it to obtain the
theoretical histograms of the Stokes profiles. These histograms were then
compared to the observed ones. Any mismatch between them was ascribed to the
theoretical distribution of the magnetic field vector, which was subsequently
modified to produce a better fit to the observed histograms. With this method
we find that Stokes profiles with signals above $2\times 10^{-3}$ (in units of
the continuum intensity) cannot be explained by an isotropic distribution of
the magnetic field vector. We also find that the differences between the
histograms of the Stokes profiles observed at different latitudes cannot be
explained in terms of line-of-sight effects. However, they can be explained by
a distribution of the magnetic field vector that inherently varies with
latitude. We note that these results are based on a series of assumptions that,
although briefly discussed in this paper, need to be considered in more detail
in the future.
