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We present a comparison of our results from ground-based observations ofasteroid (21) Lutetia with imaging data acquired during the flyby of theasteroid by the ESA Rosetta mission. This flyby provided a unique opportunityto evaluate and calibrate our method of determination of size, 3-D shape, andspin of an asteroid from ground-based observations. We present our 3-Dshape-modeling technique KOALA which is based on multi-dataset inversion. Wecompare the results we obtained with KOALA, prior to the flyby, on asteroid(21) Lutetia with the high-spatial resolution images of the asteroid taken withthe OSIRIS camera on-board the ESA Rosetta spacecraft, during its encounterwith Lutetia. The spin axis determined with KOALA was found to be accurate towithin two degrees, while the KOALA diameter determinations were within 2% ofthe Rosetta-derived values. The 3-D shape of the KOALA model is also confirmedby the spectacular visual agreement between both 3-D shape models (KOALA pre-and OSIRIS post-flyby). We found a typical deviation of only 2 km at localscales between the profiles from KOALA predictions and OSIRIS images, resultingin a volume uncertainty provided by KOALA better than 10%. Radiometrictechniques for the interpretation of thermal infrared data also benefit greatlyfrom the KOALA shape model: the absolute size and geometric albedo can bederived with high accuracy, and thermal properties, for example the thermalinertia, can be determined unambiguously. We consider this to be a validationof the KOALA method. Because space exploration will remain limited to only afew objects, KOALA stands as a powerful technique to study a much larger set ofsmall bodies using Earth-based observations.

Shape modeling technique KOALA validated by ESA Rosetta at (21) Lutetia