AuthorPike, Rosemary E.
Proudfoot, Benjamin C. N.
Bannister, Michele T.
Gladman, Brett J.
Kavelaars, J. J.
AffiliationUniv Arizona, Lunar & Planetary Lab
MetadataShow full item record
PublisherNATURE PUBLISHING GROUP
CitationPike, R.E., Proudfoot, B.C.N., Ragozzine, D. et al. A dearth of small members in the Haumea family revealed by OSSOS. Nat Astron 4, 89–96 (2020). https://doi.org/10.1038/s41550-019-0867-z
Rights© The Author(s), under exclusive licence to Springer Nature Limited 2019
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractAn extensive survey to search for members of the only known Kuiper belt family, named after the parent body Haumea, found no family members fainter than absolute magnitude H-r = 7.9, significantly brighter than the detection limit (H-r = 9.5). This lack of small members is inconsistent with a catastrophic disruption as the origin of the Haumea family. While collisional families are common in the asteroid belt, only one is known in the Kuiper belt, linked to the dwarf planet Haumea. The characterization of Haumea's family helps to constrain its origin and, more generally, the collisional history of the Kuiper belt. However, the size distribution of the Haumea family is difficult to constrain from the known sample, which is affected by discovery biases. Here, we use the Outer Solar System Origins Survey (OSSOS) Ensemble to look for Haumea family members. In this OSSOS XVI study we report the detection of three candidates with small ejection velocities relative to the family formation centre. The largest discovery, 2013 UQ(15), is conclusively a Haumea family member, with a low ejection velocity and neutral surface colours. Although the OSSOS Ensemble is sensitive to Haumea family members to a limiting absolute magnitude (H-r) of 9.5 (inferred diameter of ~90 km), the smallest candidate is significantly larger, H-r = 7.9. The Haumea family members larger than similar or equal to 20 km in diameter must be characterized by a shallow H-distribution slope in order to produce only these three large detections. This shallow size distribution suggests that the family formed in a graze-and-merge scenario, not a catastrophic collision.
Note6 month embargo; published online: 26 August 2019
VersionFinal accepted manuscript