All Figures

	Figure 1: NIR spectra of the nine observed asteroids, with theirs errorbars. The spectra were normalized to 1.25 m and offset for visibility ( left panel). Continuum subtracted spectra are presented in the right panel.
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In the text

	Figure 2: The spectrum of 497 Iva in the visible region, with errorbars. This spectrum exhibits monotonic behavior with a slightly positive slope. The edge of the spectrum is less reliable because of limitations of the instrument and detector (http://www.tng.iac.es/instruments/lrs/).
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In the text

	Figure 3: Modified Gaussian Model applied to asteroid 766 Moguntia. Two absorption bands (light green) associated with olivine were used to model the experimental data, by using free parameters option. The error between the real spectrum and the best fit is presented in red. The best fit (turquoise) suggests a surface dominated by olivine minerals.
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In the text

	Figure 4: NIR spectrum of 766 Moguntia (in black) is plotted together with the best fit (red diamonds) obtained using the Shkuratov model (derived composition: 100% olivine with Mg number = ).
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In the text

	Figure 5: NIR spectrum of 766 Moguntia presents a trend very similar to the asteroid 221 Eos, classified as a K class member.
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In the text

	Figure 6: Spectra of the asteroids presented here and the inferred meteorites (in blue). The legend describing the meteorites corresponds to the best fit, in order, from the top to the bottom. The asteroid visible spectra complement our NIR spectra as discussed in the text.
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In the text