  Non-differentiated asteroids are among the most primitive objects in our
Solar System, having escaped intense heating mechanisms. To help us understand
the information contained in reflectance spectra measured on asteroids, we
analyzed meteorites in the laboratory. We present an in-depth analysis of a
large set of reflectance spectra: 23 CV3, 15 CO3, 4 CR2 and 31 Unequilibrated
Ordinary Chondrites (UOCs). Each of the samples has a well characterized
thermal history . Variations in the reflectance spectra are observed between
and within each chondrite group. UOCs systematically exhibit deeper absorption
features, distinguishing them from carbonaceous chondrites. The CR2 samples
presented in this study are easily distinguished from type 3 chondrites by
exhibiting the 1 {\mu}m band at lower wavelengths. CV and CO chondrites exhibit
comparable mineralogical compositions and can, therefore, not be distinguished
solely based on their spectral features. In the case of CV chondrites, the 1
{\mu}m band depth increases with increasing metamorphic grade, while among CO
chondrites, the spectra exhibit increasing visual slopes. By comparing the
chondrite spectra with the spectra of various end member asteroids we are able
to suggest several possible genetic links to the studied chondrites.
