Intensity of the crystalline olivine and pyroxene (enstatite) emissivity features (Table 4) for centaurs (blue) and Jupiter trojans (red). We did not analyze the ~11.2 μm feature because credible data at shorter wavelengths for an accurate estimation of its strength are lacking (this pertains to our targets, not to Jupiter trojans). The wavelength positions of enstatite and olivine as a function of Mg number were retrieved from (Koike et al. 2003; Bowey et al. 2007; Hofmeister & Pitman 2007; Kelley & Wooden 2009; Hamilton 2010; Bowey et al. 2020). The position of the ~13.7 μm (enstatite) feature does not vary significantly with composition. Hence, the composition of crystalline olivine and crystalline pyroxene is best determined from the remaining peaks. We cannot rule out the possibility that the position of the ~11.9 μm olivine feature in the Jupiter trojan spectra is partially biased by insufficient correction for the well-known ~12.2 μm MRS spectral leak.