2002 TX300 is classified as a classical Kuiper belt object and follows an orbit very similar to that of Haumea: highly inclined (26°) and moderately eccentric (e ~0.12), far from Neptune's perturbations (perihelion at ~37 AU).

[12] The artist's diagram was largely based on the concept that 2002 TX300, with an absolute magnitude (H) of 3.4,[1] may have an albedo around 0.08,[10] which resulted in an overly optimistic diameter estimate of around 1,000 kilometres (620 mi).

[5] In 2008, it was considered to be a dwarf planet candidate based on its small lightcurve amplitude (which would imply a spheroidal shape) and the assumption that it was larger than 450 kilometres (280 mi) in diameter.

[4] The spectrum in the visible and near-infrared rages is very similar to that of Charon, characterized by neutral to blue slope (1%/1000 Å) with deep (60%) water absorption bands at 1.5 and 2.0 μm.

Common physical characteristics with the dwarf planet Haumea together with similar orbit elements[20] led to suggestion that 2002 TX300 was a member of the Haumean collisional family.

The object, together with other members of the family ((19308) 1996 TO66, (24835) 1995 SM55, (120178) 2003 OP32 and (145453) 2005 RR43), would be created from ice mantle ejected from the proto-Haumea as result of a collision with another large (around 1,660 kilometres (1,030 mi)) body.