Editing Classical Kuiper belt object (section)

== Families ==
The first known [[collisional family]] in the classical Kuiper belt—a group of objects thought to be remnants from the breakup of a single body—is the [[Haumea family]].<ref name="BrownBarkume2007">
{{cite journal |last1=Brown |first1=Michael E. |last2=Barkume |first2=Kristina M. |last3=Ragozzine |first3=Darin |last4=Schaller |first4=Emily L. |year=2007 |title=A collisional family of icy objects in the Kuiper belt |journal=Nature |volume=446 |issue=7133 |pages=294–6 |bibcode=2007Natur.446..294B |doi=10.1038/nature05619 |pmid=17361177 |s2cid=4430027 |url=https://authors.library.caltech.edu/34346/2/nature05619-s1.pdf |archive-url=https://web.archive.org/web/20180723192004/https://authors.library.caltech.edu/34346/2/nature05619-s1.pdf |archive-date=2018-07-23 |url-status=live}}</ref> It includes Haumea, its moons, {{mpl|2002 TX|300}} and seven smaller bodies.{{efn|As of 2008. The four brightest objects of the family are situated on the graphs ''inside'' the circle representing Haumea.{{clarify|reason=What graphs is this note referring to?|date=July 2023}}}} The objects not only follow similar orbits but also share similar physical characteristics. Unlike many other KBO their surface contains large amounts of water ice (H<sub>2</sub>O) and no or very little [[tholin]]s.<ref name="Pinilla-Alonso2009">
{{cite journal |last1=Pinilla-Alonso |first1=N. |last2=Brunetto |first2=R. |last3=Licandro |first3=J. |last4=Gil-Hutton |first4=R. |last5=Roush |first5=T. L. |last6=Strazzulla |first6=G. |year=2009 |title=The surface of (136108) Haumea ({{mp|2003 EL|61}}), the largest carbon-depleted object in the trans-Neptunian belt |journal=Astronomy and Astrophysics |volume=496 |issue=2 |pages=547 |arxiv=0803.1080 |bibcode=2009A&A...496..547P |doi=10.1051/0004-6361/200809733|s2cid=15139257 }}</ref> The surface composition is inferred from their neutral (as opposed to red) colour and deep absorption at 1.5 and 2. [[micrometre|μm]] in [[infrared]] [[electromagnetic spectrum|spectrum]].<ref name="Pinilla-Alonso2007">
{{cite journal |last1=Pinilla-Alonso |first1=N. |last2=Licandro |first2=J. |last3=Gil-Hutton |first3=R. |last4=Brunetto |first4=R. |year=2007 |title=The water ice rich surface of (145453) 2005 RR<sub>43</sub>: a case for a carbon-depleted population of TNOs? |journal=Astronomy and Astrophysics |volume=468 |issue=1 |pages=L25–L28 |arxiv=astro-ph/0703098 |bibcode=2007A&A...468L..25P |doi=10.1051/0004-6361:20077294|s2cid=18546361 }}</ref> Several other collisional families might reside in the classical Kuiper belt.<ref name=chiang>{{cite journal |last1=Chiang |first1=E.-I. |title=A Collisional Family in the Classical Kuiper Belt |journal=[[The Astrophysical Journal]] |date=July 2002 |volume=573 |issue=1 |pages=L65–L68 |arxiv=astro-ph/0205275 |doi=10.1086/342089 |bibcode=2002ApJ...573L..65C |s2cid=18671789 }}</ref><ref name=pairs>{{cite journal |last1=de la Fuente Marcos |first1=Carlos |last2=de la Fuente Marcos |first2=Raúl |title=Dynamically correlated minor bodies in the outer Solar system |journal=[[Monthly Notices of the Royal Astronomical Society]] |date=11 February 2018 |volume=474 |issue=1 |pages=838–846 |arxiv=1710.07610 |doi=10.1093/mnras/stx2765 |doi-access=free |bibcode=2018MNRAS.474..838D|s2cid=73588205 }}</ref>