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We have studied the angular distribution of the magnetic field vector in thesolar internetwork employing high-quality data (noise level $\sigma \approx3\times 10^{-4}$ in units of the quiet-Sun intensity) at different latitudesrecorded with the Hinode/SP instrument. Instead of applying traditionalinversion codes of the radiative transfer equation to retrieve the magneticfield vector at each spatial point on the solar surface and studying theresulting distribution of the magnetic field vector, we surmised a theoreticaldistribution function of the magnetic field vector and used it to obtain thetheoretical histograms of the Stokes profiles. These histograms were thencompared to the observed ones. Any mismatch between them was ascribed to thetheoretical distribution of the magnetic field vector, which was subsequentlymodified to produce a better fit to the observed histograms. With this methodwe find that Stokes profiles with signals above $2\times 10^{-3}$ (in units ofthe continuum intensity) cannot be explained by an isotropic distribution ofthe magnetic field vector. We also find that the differences between thehistograms of the Stokes profiles observed at different latitudes cannot beexplained in terms of line-of-sight effects. However, they can be explained bya distribution of the magnetic field vector that inherently varies withlatitude. 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 detailin the future.

Inferring the magnetic field vector in the quiet Sun. III. Disk variation of the Stokes profiles and isotropism of the magnetic field