Largest main belt asteroids data

We subsequently performed a detailed shape analysis and constrained the density of each target using available mass estimates including our own mass estimates in the case of multiple systems. The analysis of the reconstructed shapes allowed us to identify two families of objects as a function of their diameters, namely "spherical" and "elongated" bodies. A difference in rotation period appears to be the main origin of this bimodality.

In addition, all but one object (216 Kleopatra) are located along the Maclaurin sequence with large volatile-rich bodies being the closest to the latter. Our results further reveal that the primaries of most multiple systems possess a rotation period of shorter than 6h and an elongated shape (c/a<=0.65). Densities in our sample range from ~1.3g/cm^3^ (87 Sylvia) to ~4.3g/cm^3^ (22 Kalliope).

Furthermore, the density distribution appears to be strongly bimodal with volatile poor ({rho}>=2.7g/cm^3^) and volatile-rich ({rho}>=2.2g/cm^3^) bodies. Finally, our survey along with previous observations provides evidence in support of the possibility that some C-complex bodies could be intrinsically related to IDP-like P- and D-type asteroids, representing different layers of a same body (C: core; P/D: outer shell).

We therefore propose that P/ D-types and some C-types may have the same origin in the primordial trans-Neptunian disk.