  We present an in-depth study of the reflectance spectra of 39 equilibrated
and 41 unequilibrated ordinary chondrites. We demonstrate that consistent
measuring conditions are vital for the direct comparison of spectral features
between chondrites, otherwise hampering any conclusions. We include a
comparison with a total of 466 S-type asteroid reflectance spectra. We analyze
(i) if a difference between EOCs and UOCs as well as between H, L and LL can be
seen, (ii) if it is possible to identify unequilibrated and equilibrated S-type
asteroid surfaces and (iii) if we can further constrain the match between OCs
and S-type asteroids all based on reflectance spectra. We checked the
classification of the 31 Antarctic UOCs analyzed in the present work, using
petrography and magnetic measurements, and evidenced that 74% of them were
misclassified. Reflectance spectra were compared between EOCs and UOCs as well
as between H, L and LL chondrites using a set of spectral features including
band depths and positions, peak reflectance values, spectral slopes and the
Ol/(Ol + Px) ratio. UOCs and EOCs reflectance spectra show no clear-cut
dichotomy, but a continuum with some EOCs showing stronger absorption bands and
peak reflectance values, while others are comparable to UOCs. We show by the
example of 6 EOCs that their band depths decrease with decreasing grain size.
Based on reflectance spectra alone, it is thus highly challenging to
objectively identify an unequilibrated from an equilibrated S-type surface.
There is no clear distinction of the chemical groups: only LL EOCs of
petrographic type > 4 can be distinguished from H and L through less deep 2-mic
band depths and 1-mic band positions at longer wavelengths. Lastly, an
anti-correlation between the diameter of the asteroids and their 1000 nm band
depth is found indicating that larger sized S-type asteroids show finer grained
surfaces.
