Spectral reflectance properties of carbonaceous chondrites: 1. CI chondrites

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The Compositional Structure of the Asteroid Belt (2015, background): “ as a function of size is not yet understood. Possible explanations could include space weathering (Lantz et al., 2013, Brunetto et al., 2014), compositional differences, or grain size effects (e.g., Cloutis et al., 2011a,b). Additionally, among the smallest asteroids (D <~15 km) we find very red”
Density of asteroids (2012, background): “These features were interpreted as evidences for aqueous alteration, similar to that experienced by CI/CM parent bodies (Cloutis et al., 2011a,b).”
Ion irradiation of carbonaceous chondrites: A new view of space weathering on primitive asteroids (2017, result): “55 in the following text) is 12, 15 and 17 % respectively (see Table 2 for the whole values), in agreement with literature data on CV and CO chondrites [Cloutis et al., 2012b,a] (though pellet spectra tend to be brighter than the powder ones; see Append.”
Modal mineralogy of CI and CI-like chondrites by X-ray diffraction (2015, background): “A signiﬁcant fraction of C-type asteroids appear to have dehydrated surfaces with spectral features similar to those of the thermally metamorphosed CI-like chondrites (Hiroi et al., 1993, 1996; Osawa et al., 2005; Cloutis et al., 2012).”