  Asteroid 2008TC3 was a Near Earth Asteroid that impacted the Earth on 2008
October 7. Meteorites were produced by the break-up of 2008TC3 in the high
atmosphere and at present, about 600 meteorites - called Almahata Sitta -
coming from 2008TC3 have been recovered. A mineralogical study of Almahata
Sitta fragments shows that the asteroid 2008TC3 was made of meteorites of
different types (ureilites, H, L, and E chondrites). Understanding the origin
of this body and how it was put together remain a challenge. Here we perform a
detailed spectroscopical and dynamical investigation to show that the most
likely source region of 2008TC3 is in the inner Main Belt at low inclination
(i<8 degrees). We show that asteroids with spectroscopic classes that can be
associated with the different meteorite types of Almahata Sitta are present in
the region of the Main Belt that includes the Nysa-Polana family and objects of
the Background at low inclination. Searching for a possible scenario of
formation for 2008TC3, we show that there is little chance that 2008TC3 was
formed by low velocity collisions between asteroids of different mineralogies,
in the current asteroid belt. It seems more likely that the heterogeneous
composition of 2008TC3 was a inherited from a time when the asteroid belt was
in a different dynamical state, most likely in the very early Solar System.
Because ureilites are fragments of a large, thermally metamorphosed asteroid,
this suggests that the phases of collisional erosion (the break-up of the
ureilite parent-body) and collisional accretion (the formation of the parent
body of 2008TC3) overlapped for some time in the primordial asteroid belt.
