Editing Jupiter trojan (section)

=== Dynamical families and binaries ===
Discerning [[collisional family|dynamical families]] within the Jupiter trojan population is more difficult than it is in the asteroid belt, because the Jupiter trojans are locked within a far narrower range of possible positions. This means that clusters tend to overlap and merge with the overall swarm. By 2003 roughly a dozen dynamical families were identified. Jupiter-trojan families are much smaller in size than families in the asteroid belt; the largest identified family, the Menelaus group, consists of only eight members.<ref name=Jewitt2004/>

In 2001, [[617 Patroclus]] was the first Jupiter trojan to be identified as a [[Minor-planet moon|binary asteroid]].<ref name="Merline">{{cite web|last=Merline|first=W. J.|date=2001|url=http://cbat.eps.harvard.edu/iauc/07700/07741.html#Item2|title=IAUC 7741: 2001fc; S/2001 (617) 1; C/2001 T1, C/2001 T2|access-date=25 October 2010|archive-url=https://web.archive.org/web/20110719210034/http://cbat.eps.harvard.edu/iauc/07700/07741.html#Item2|archive-date=19 July 2011|url-status=live}}</ref> The binary's orbit is extremely close, at 650&nbsp;km, compared to 35,000&nbsp;km for the primary's [[Hill sphere]].<ref name=Marchis2006/> The largest Jupiter trojan—[[624 Hektor]]— is probably a [[contact binary (asteroid)|contact binary]] with a moonlet.<ref name=Jewitt2004/><ref name=IAUC8732>{{cite web|url=http://cbat.eps.harvard.edu/iauc/08700/08732.html#Item1|title=IAUC 8732: S/2006 (624) 1|access-date=23 July 2006|archive-url=https://web.archive.org/web/20110719210046/http://cbat.eps.harvard.edu/iauc/08700/08732.html#Item1|archive-date=19 July 2011|url-status=live}} (Satellite Discovery)</ref><ref name=Lacerda2007/>