Mineralogical analysis of the Eos family from near-infrared spectra

The aim of this work is to analyze the mineralogy of the Eos family, which exhibits considerable taxonomic diversity. Its biggest fragment, (221) Eos has previously been associated, through direct spectral comparisons, with such diverse mineralogies as CV/CO and achondrite meteorites [Burbine, T.H., Binzel, R.P., Bus, S.J., Clark, B.E., 2001. Meteorit. Planet. Sci. 36, 245–253; Mothé-Diniz, T., Carvano, J.M., 2005. Astron. Astrophys. 174, 54–80]. In order to perform such analysis we obtained spectra of 30 family members in the 0.8–2.5 μm range, and used three different methods of mineralogical inference: direct spectral comparison with meteorites, intimate mixing using Hapkeʹs theory, and fitting absorption features with the MGM. Although the direct comparison failed to yield good matches—the best candidates being R-chondrites—both mixing model and MGM analysis suggest that the bulk of the family is dominated by forsteritic ( Fa ∼ 20 ) olivine, with a minor component of orthopyroxene. This composition can be compatible with what would be expected from the partial differentiation of a parent-body with an original composition similar to ordinary chondrites, which probably formed and differentiated closer to the Sun than the present location of the family. A CK-like composition is also possible, from the inferred mineralogy, as well as from the similarities of the spectra in the NIR.