| Minorplanet: | yes |
| Background: |
|
| Discovered: | 23 September 2003 |
| Epoch: | 4 September 2017 (JD 2458000.5) |
| Uncertainty: | 4 |
| Observation Arc: | 10.12 yr (3,698 days) |
| Perihelion: | 39.231 AU |
| Semimajor: | 42.489 AU |
| Eccentricity: | 0.0767 |
| Period: | 276.96 yr (101,159 days) |
| Mean Motion: | / day |
| Inclination: | 28.619° |
| Asc Node: | 176.34° |
| Arg Peri: | 191.81° |
| Dimensions: | km |
| Density: | 0.8–2.7 g/cm3 |
| Rotation: | h 7.5 h |
| Spectral Type: | B−R |
| Albedo: | 0.05–0.50 |
| Abs Magnitude: | 6.2 |
is a classical trans-Neptunian object and member of Haumea family from the Kuiper belt located in the outermost regions of the Solar System, approximately 300 kilometers in diameter. It was first observed on 23 September 2003, by astronomers of the Canada–France Ecliptic Plane Survey at Mauna Kea Observatories on Hawaii. The surface of is made of water ice.
is a classical Kuiper belt object (cubewano) belonging to the hot population. Its size estimated to lie between 150 and 450 km based on a range of plausible albedos. The object has a large light curve amplitude of about 0.85, which indicates that it has an extremely elongated shape or is a contact binary.[1] In the former case the density of is estimated at 0.86 g/cm3 and its axis ratios at 0.55 and 0.41. If is a contact binary, which is actually more likely, the density is estimated at 2.67 g/cm3. In the latter case, the components are also thought to be unequal in size with the mass ratio of about 0.3 and axis ratios of about 0.8 and 0.5, respectively, for the primary and secondary components.
was identified as a member of the Haumea family, which is defined based on a common pattern of IR water-ice absorption, neutral visible spectrum and the clustering of the orbital elements. The Haumea family members including,,, and others all appear to be collisional fragments broken off of the dwarf planet .