Insights into the origins of Phobos and Deimos based on a spectral comparison with small bodies and Martian materials

Open Access

Fig. 2

VIS slope, NIR slope, and albedo of featureless asteroid types (i.e., B-, C-, M-, P-, D-, and Z-type objects) in comparison with Phobos blue unit, Phobos red unit, and the spectral parameters of Deimos. The spectral slopes for the Martian moons were computed on the spectra obtained by Fraeman et al. (2014), and the albedos were taken from Fornasier et al. (2024) for Phobos and from Thomas et al. (1996) for Deimos.

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