  In the next decade, two rovers will characterize in situ the mineralogy of
rocks on Mars, using for the first time near-infrared reflectance
spectrometers: SuperCam onboard the Mars 2020 rover and MicrOmega onboard the
ExoMars rover, although this technique is predominantly used in orbit for
mineralogical investigations. Until successful completion of sample-return
missions from Mars, Martian meteorites are currently the only samples of the
red planet available for study in terrestrial laboratories and comparison with
in situ data. However, the current spectral database available for these
samples does not represent their diversity and consists primarily of spectra
acquired on finely crushed samples, albeit grain size is known to greatly
affect spectral features. We measured the reflected light of a broad Martian
meteorite suite as a means to catalogue and characterize their spectra between
0.4 and 3 microns. These measurements are achieved using a point spectrometer
acquiring data comparable to SuperCam, and an imaging spectrometer producing
hyperspectral cubes similarly to MicrOmega. Our results indicate that point
spectrometry is sufficient to discriminate the different Martian meteorites
families, to identify their primary petrology based on band parameters, and to
detect their low content in alteration minerals. However, significant spectral
mixing occurs in the point measurements, even at spot sizes down to a few
millimeters, and imaging spectroscopy is needed to correctly identify the
various mineral phases in the meteorites. Bidirectional spectral measurements
confirm their non-Lambertian behavior, with backward and suspected forward
scattering peaks. With changing observation geometry, the main absorption
strengths show variations up to 10-15 percents. All the spectra presented are
provided in the supplementary data for further comparison with in situ and
orbital measurements.
