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Photometric lightcurves were also obtained for 14 of them during the Spitzerobservations to provide the context of the observations and reliable estimatesof their absolute magnitudes. The extracted mid-IR spectra were analyzed usinga modified standard thermal model (STM) and a thermophysical model (TPM) thattakes into account the shape and geometry of the large primary at the time ofthe Spitzer observation. We derived a reliable estimate of the size, albedo,and beaming factor for each of these asteroids, representing three maintaxonomic groups: C, S, and X. For large (volume-equivalent system diameter Deq$\lt$ 130 km) binary asteroids, the TPM analysis indicates a low thermalinertia ($\Gamma$ < $\sim$100 J s-1/2K-1m-2) and their emissivity spectradisplay strong mineral features, implying that they are covered with a thicklayer of thermally insulating regolith. The smaller (surface-equivalent systemdiameter Deff $\lt$17 km) asteroids also show some emission lines of minerals,but they are significantly weaker, consistent with regoliths with coarsergrains, than those of the large binary asteroids. The average bulk densities ofthese multiple asteroids vary from 0.7-1.7 g/cm3 (P-, C- type) to $\sim$2 g/cm3(S-type). The highest density is estimated for the M-type (22) Kalliope (3.2$\pm$ 0.9 g/cm3). The spectral energy distributions (SED) and emissivityspectra, made available as a supplement document, could help to constrain thesurface compositions of these asteroids.

Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations