The rubble pile structure of Itokawa indicates that the later has been formed by the catastrophic disruption of a significantly larger parent body. In earlier studies (AO1, 3 and 7), we successfully analyzed a total of 9 regolith dust particles recovered by the Hayabusa space probe from the rubble pile asteroid 25143 Itokawa, using a workflow of microstructural analysis by electron backscatter diffraction (EBSD), element mapping by time-of-flight secondary ion mass spectrometry (ToF-SIMS ± atom probe) and ⁴⁰Ar/³⁹Ar geochronology. We showed that Itokawa must have formed before or at ca. ≥ 4. 2 Ga and that during the breakup of Itokawa’s parent body, part of the asteroid experienced minimum to negligible shock pressure and temperature increase. Here, we propose to continue our quest to understand the bombardment history of Itokawa with the so far seemingly elusive goal of precisely pinpointing the age and nature of the catastrophic breakup of Itokawa’s parent body and better understand the effect of impact on rubble pile asteroids. Only through a larger number of ⁴⁰Ar/³⁹Ar ages obtained on individual particles coupled with careful particle characterizations via EBSD measurements, will we be able to achieve these goals.