  There are various indications that the most primitive small bodies (P, D-type
asteroids, comets) have surfaces made of intimate mixtures of opaque minerals
and other components (silicates, carbonaceous compounds, etc.) in the form of
sub-micrometre-sized grains, smaller than the wavelength at which they are
observed, so-called hyperfine grains. Here, we investigate how the Vis-NIR-MIR
spectral and V-band polarimetric properties of surfaces made of hyperfine
grains are influenced by the relative abundance of such hyperfine materials,
having strongly different optical indexes. Mixtures of grains of olivine and
iron sulfide (or anthracite), as analogues of silicates and opaque minerals
present on small bodies, were prepared at different proportions. The
measurements reveal that these mixtures of hyperfine grains have spectral and
polarimetric Vis-NIR properties varying in strongly nonlinear ways. When
present at even a few percent, opaque components dominate the Vis-NIR spectral
and polarimetric properties, and mask the silicate bands at these wavelengths.
The Vis-NIR spectral slope ranges from red (positive slope), for pure opaque
material, to blue (negative slope) as the proportion of silicates increases,
which is reminiscent of the range of spectral slopes observed on P, D, X, C-
and B-types asteroids. The spectra of the darkest mixtures in the Vis-NIR
exhibit the absorption bands of Si-O in olivine around 10 m in the MIR, which
is observed in emission for several small bodies. This work shows that both the
contrasted optical indexes of the components, and the dispersion or aggregation
(depending on their relative proportions) of their hyperfine grains, induce
different light scattering regimes in the Vis-NIR and MIR, as observed for
primitive small bodies. The optical separation of hyperfine grains seems to be
a major parameter controlling the optical properties of these objects.
