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The surface composition of S-type asteroids can be determined using bandparameters extracted from their near-infrared (NIR) spectra (0.7-2.50 $\mu$m)along with spectral calibrations derived from laboratory samples. In the past,these empirical equations have been obtained by combining NIR spectra ofmeteorite samples with information about their composition and mineralabundance. For these equations to give accurate results, the characteristics ofthe laboratory spectra they are derived from should be similar to those ofasteroid spectral data (i.e., similar signal-to-noise ratio (S/N) andwavelength range). Here we present new spectral calibrations that can be usedto determine the mineral composition of ordinary chondrite-like S-typeasteroids. Contrary to previous work, the S/N of the ordinary chondrite spectraused in this study has been decreased to recreate the S/N typically observedamong asteroid spectra, allowing us to obtain more realistic results. Inaddition, the new equations have been derived for five wavelength rangesencompassed between 0.7 and 2.50 $\mu$m, making it possible to determine thecomposition of asteroids with incomplete data. The new spectral calibrationswere tested using band parameters measured from the NIR spectrum of asteroid(25143) Itokawa, and comparing the results with laboratory measurements of thereturned samples. We found that the spectrally derived olivine and pyroxenechemistry, which are given by the molar contents of fayalite (Fa) andferrosilite (Fs), are in excellent agreement with the mean values measured fromthe samples (Fa$_{28.6\pm1.1}$ and Fs$_{23.1\pm2.2}$), with a maximumdifference of 0.6 mol\% for Fa and 1.4 mol\% for Fs.

A new method for deriving composition of S-type asteroids from noisy and incomplete near-infrared spectra