View source for Detached object

{{Short description|Dynamical class of minor planets}}

[[File:TheTransneptunians 500AU.svg|thumb|upright=1.35|[[Trans-Neptunian object]]s plotted by their distance and [[Orbital inclination|inclination]]. Objects beyond a distance of 100&nbsp;[[astronomical unit|AU]] display their [[Minor planet designation|designation]].

{{legend2|#ff0000|border=1px solid #333|[[Resonant trans-Neptunian object|Resonant TNO]] &amp; [[Plutino]]}}<br />
{{legend2|#0000ff|border=1px solid #000|[[Cubewanos]] (classical KBO)}}<br />
{{legend2|#999|border=1px solid #222|[[Scattered disc object]]}}<br />
{{legend2|#ffffff|border=1px solid #666|'''Detached object'''}}
]]

'''Detached objects''' are a [[Orbital mechanics|dynamical]] class of [[minor planet]]s in the outer reaches of the [[Solar System]] and belong to the broader family of [[trans-Neptunian object]]s (TNOs). These objects have orbits whose points of closest approach to the Sun ([[apsis|perihelion]]) are sufficiently distant from the [[Gravitational two-body problem|gravitational influence]] of [[Neptune]] that they are only moderately affected by Neptune and the other known planets: This makes them appear to be "detached" from the rest of the Solar System, except for their attraction to the Sun.<ref name=lykawka>
{{cite journal |author1=Lykawka, P.S. |author2=Mukai, T. |title=An outer planet beyond Pluto and the origin of the trans-Neptunian belt architecture  |journal=Astronomical Journal |year = 2008 |volume=135 |issue=4 |pages=1161–1200 |doi=10.1088/0004-6256/135/4/1161 |bibcode=2008AJ....135.1161L |arxiv=0712.2198|s2cid=118414447 }}</ref><ref name="Jewitt2006">{{cite book |author1-link=David Jewitt |first1=D. |last1=Jewitt |first2=A. |last2=Delsanti |contribution=The Solar System Beyond the Planets |title=Solar System Update: Topical and Timely Reviews in Solar System Sciences |edition=Springer-Praxis |isbn=3-540-26056-0 |year=2006 |publisher=Springer |url=http://www.ifa.hawaii.edu/faculty/jewitt/papers/2006/DJ06.pdf <!-- Preprint of the article (pdf) --> |archive-url=https://web.archive.org/web/20070129151907/http://www.ifa.hawaii.edu/faculty/jewitt/papers/2006/DJ06.pdf |archive-date=January 29, 2007 |df=dmy-all}}</ref>

In this way, detached objects differ substantially from most other known TNOs, which form a loosely defined set of populations that have been [[Perturbation (astronomy)|perturbed]] to varying degrees onto their current orbit by gravitational encounters with the [[giant planets]], predominantly Neptune. Detached objects have larger perihelia than these other TNO populations, including the objects in [[orbital resonance]] with Neptune, such as [[Pluto]], the [[classical Kuiper belt object]]s in non-resonant orbits such as [[Makemake (dwarf planet)|Makemake]], and the [[scattered disk|scattered disk object]]s like [[Eris (dwarf planet)|Eris]].

Detached objects have also been referred to in the scientific literature as '''extended scattered disc objects''' (E-SDO),<ref name="Gladman">{{cite journal |last1=Gladman |first1=B. |display-authors=etal |year=2002 |title=Evidence for an extended scattered disk |journal=Icarus |volume=157 |issue=2 |pages=269–279 |doi=10.1006/icar.2002.6860 |bibcode=2002Icar..157..269G |arxiv=astro-ph/0103435 |s2cid=16465390 }}</ref> '''distant detached objects''' (DDO),<ref name="Gomez 2006" >{{cite journal |bibcode=2006Icar..184..589G |title=A distant planetary-mass solar companion may have produced distant detached objects |journal=Icarus |volume=184 |issue=2 |pages=589–601 |publisher=Elsevier |doi=10.1016/j.icarus.2006.05.026 |year=2006 |first1=Rodney S. |last1=Gomes |last2=Matese |first2=J. |last3=Lissauer |first3=Jack}}
</ref> or '''scattered–extended''', as in the formal classification by the [[Deep Ecliptic Survey]].<ref name="DES_Elliot2006" >{{cite journal
|author1=Elliot, J.L. |author2=Kern, S.D. |author3=Clancy, K.B. |author4=Gulbis, A.A.S. |author5=Millis, R.L. |author6=Buie, M.W. |author7=Wasserman, L.H. |author8=Chiang, E.I. |author9=Jordan, A.B. |author10=Trilling, D.E. |author11=Meech, K.J. |title=The Deep Ecliptic Survey: A search for Kuiper belt objects and centaurs. II. Dynamical classification, the Kuiper belt plane, and the core population |journal=The Astronomical Journal |volume=129 |issue=2 |pages=1117–1162 |year=2006 |url=http://occult.mit.edu/_assets/documents/publications/Elliot2005AJ129.1117.pdf |bibcode=2005AJ....129.1117E  |doi=10.1086/427395|doi-access=free }}</ref> This reflects the dynamical gradation that can exist between the orbital parameters of the scattered disk and the detached population.

At least nine such bodies have been securely identified,<ref name="LykDyn">{{cite journal |author1=Lykawka, Patryk Sofia  |author2=Mukai, Tadashi |date=July 2007 |title=Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation |journal=Icarus |volume=189 |issue=1 |pages=213–232 |doi=10.1016/j.icarus.2007.01.001 |bibcode=2007Icar..189..213L}}</ref> of which the largest, most distant, and best known is [[90377 Sedna|Sedna]]. Those with large semi-major axes and high perihelion orbits similar to that of Sedna are termed [[sednoid]]s. As of 2024, there are three known sednoids: Sedna, [[2012 VP113|2012 VP<sub>113</sub>]], and [[541132 Leleākūhonua|Leleākūhonua]].<ref>{{Cite journal |last1=Huang 黄 |first1=Yukun 宇坤 |last2=Gladman |first2=Brett |date=2024-02-01 |title=Primordial Orbital Alignment of Sednoids |journal=The Astrophysical Journal Letters |volume=962 |issue=2 |pages=L33 |doi=10.3847/2041-8213/ad2686 |doi-access=free |arxiv=2310.20614 |bibcode=2024ApJ...962L..33H |issn=2041-8205}}</ref> These objects exhibit a highly statistically significant asymmetry between the distributions of object pairs with small ascending and descending nodal distances that might be indicative of a response to external perturbations; asymmetries such as this one are sometimes attributed to perturbations induced by unseen planets.<ref name=nodes-2021>{{cite journal |last1=de la Fuente Marcos |first1=Carlos |last2=de la Fuente Marcos |first2=Raúl |title=Peculiar orbits and asymmetries in extreme trans-Neptunian space | journal=[[Monthly Notices of the Royal Astronomical Society]] |url=https://academic.oup.com/mnras/article-abstract/506/1/633/6307523|volume=506 |issue=1 |pages=633–649 |arxiv=2106.08369 |bibcode=2021MNRAS.506..633D |doi=10.1093/mnras/stab1756|date=1 September 2021|doi-access=free }}</ref><ref name=nodes-2022>{{cite journal |last1=de la Fuente Marcos |first1=Carlos |last2=de la Fuente Marcos |first2=Raúl |title=Twisted extreme trans-Neptunian orbital parameter space: statistically significant asymmetries confirmed |journal=Monthly Notices of the Royal Astronomical Society Letters |url=https://academic.oup.com/mnrasl/article-abstract/512/1/L6/6524836 |volume=512 |issue=1 |pages=L6–L10 |arxiv=2202.01693 |bibcode=2022MNRAS.512L...6D |doi=10.1093/mnrasl/slac012 |date=1 May 2022|doi-access=free }}</ref>

== Orbits ==

Detached objects have perihelia much larger than Neptune's aphelion. They often have highly [[ellipse|elliptical]], very large orbits with [[semi-major axis|semi-major axes]] of up to a few hundred [[astronomical unit]]s (AU, the radius of Earth's orbit). Such orbits cannot have been created by gravitational [[Perturbation (astronomy)|scattering]] by the [[giant planet]]s, not even Neptune. Instead, a number of explanations have been put forward, including an ''encounter with a passing star''<ref name=Morbidelli2004>{{cite journal |journal=The Astronomical Journal |issue=5 |volume=128 |pages=2564–2576 |date=November 2004 |title=Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects {{mp|2000 CR|105}} and {{mp|2003 VB|12}} |first1=Alessandro |last1=Morbidelli |doi=10.1086/424617 |last2=Levison |first2=Harold F. |bibcode=2004AJ....128.2564M |arxiv=astro-ph/0403358|s2cid=119486916 }}</ref> or a [[Planets beyond Neptune|''distant planet-sized object'']],<ref name="Gomez 2006"/> or ''Neptune migration'' (which may once have had a much more eccentric orbit, from which it could have tugged the objects to their current orbit)<ref name=Gladman2001>{{cite journal |doi=10.1006/icar.2002.6860 |title=Evidence for an extended scattered disk |arxiv=astro-ph/0103435 |bibcode=2002Icar..157..269G |volume=157 |issue=2|journal=Icarus |pages=269–279 |year=2002 |last1=Gladman |first1=B. |last2=Holman |first2=M. |last3=Grav |first3=T. |last4=Kavelaars |first4=J. |last5=Nicholson |first5=P. |last6=Aksnes |first6=K. |last7=Petit |first7=J.-M.|s2cid=16465390 }}</ref><ref name=12thplanet>{{cite web |url=http://www.grantchronicles.com/12thplanetmk.htm |title=Mankind's Explanation: 12th Planet}}</ref><ref name=sciencenews>{{cite web |url=https://www.sciencenews.org/article/comets-odd-orbit-hints-hidden-planet?mode=magazine&context=293 |title=A comet's odd orbit hints at hidden planet |date=4 April 2001 }}</ref><ref name=spaceref>{{cite web |url=http://www.spaceref.com/news/viewnews.html?id=309 |title=Is There a Large Planet Orbiting Beyond Neptune? }}{{Dead link|date=January 2024 |bot=InternetArchiveBot |fix-attempted=yes }}</ref><ref name=sciencemag>{{cite web |url=https://www.science.org/content/article/signs-hidden-planet |title=Signs of a Hidden Planet?}}</ref> 
or [[Rogue planet|''ejected rogue planets'']] (present in the early Solar System that were ejected).<ref name=Gladman2006>{{cite journal |doi=10.1086/505214 |title=Production of the Extended Scattered Disk by Rogue Planets|bibcode = 2006ApJ...643L.135G |volume=643 |issue=2 |journal=The Astrophysical Journal |pages=L135–L138 |citeseerx=10.1.1.386.5256 |year=2006 |last1=Gladman |first1=Brett |last2=Chan |first2=Collin |s2cid=2453782 }}</ref><ref name=findPlanet9>{{cite web |url=http://www.findplanetnine.com/2016/01/the-long-and-winding-history-of-planet-x.html |title=The long and winding history of Planet X |access-date=2016-02-09 |archive-date=2016-02-15 |archive-url=https://web.archive.org/web/20160215164442/http://www.findplanetnine.com/2016/01/the-long-and-winding-history-of-planet-x.html |url-status=dead }}</ref><ref>{{Cite journal |last1=Huang |first1=Yukun |last2=Gladman |first2=Brett |last3=Beaudoin |first3=Matthew |last4=Zhang |first4=Kevin |date=October 2022 |title=A Rogue Planet Helps to Populate the Distant Kuiper Belt |journal=The Astrophysical Journal Letters |language=en |volume=938 |issue=2 |pages=L23 |doi=10.3847/2041-8213/ac9480 |doi-access=free |arxiv=2209.09399 |bibcode=2022ApJ...938L..23H |issn=2041-8205}}</ref>

The classification suggested by the [[Deep Ecliptic Survey]] team introduces a formal distinction between ''scattered-near'' objects (which could be scattered by Neptune) and ''scattered-extended'' objects (e.g. [[90377 Sedna]]) using a [[Tisserand's parameter]] value of 3.<ref name="DES_Elliot2006" />

The [[Planet Nine]] hypothesis suggests that the orbits of several detached objects can be explained by the gravitational influence of a large, unobserved planet between 200&nbsp;AU and 1200&nbsp;AU from the Sun and/or the influence of Neptune.<ref name=TAJ201601>{{cite journal |title=Evidence for a distant giant planet in the Solar system |first1=Konstantin |last1=Batygin |first2=Michael E. |last2=Brown |date=20 January 2016 |journal=[[The Astronomical Journal]] |volume=151 |number=2 |page=22 |doi=10.3847/0004-6256/151/2/22 |arxiv=1601.05438 |bibcode = 2016AJ....151...22B|s2cid=2701020 |doi-access=free }}</ref>

== Classification ==
{{TNO}}

Detached objects are one of four distinct dynamical classes of TNO; the other three classes are [[classical Kuiper-belt object]]s, [[Resonant trans-Neptunian object|resonant object]]s, and [[scattered disc|scattered-disc objects]] (SDO).<ref>{{Cite book |last1=Gladman |first1=B. |url=https://ui.adsabs.harvard.edu/abs/2008ssbn.book...43G |title=Nomenclature in the Outer Solar System |last2=Marsden |first2=B. G. |last3=Vanlaerhoven |first3=C. |date=2008-01-01|bibcode=2008ssbn.book...43G }}</ref> [[Sednoid]]s also belong to detached objects. Detached objects generally have a perihelion distance greater than 40&nbsp;AU, deterring strong interactions with Neptune, which has an approximately circular orbit about 30&nbsp;AU from the Sun. The boundary between the scattered and detached regions can be defined using an analytical resonance overlap criterion.<ref>{{Cite journal |last1=Batygin |first1=Konstantin |last2=Mardling |first2=Rosemary A. |last3=Nesvorný |first3=David |date=2021-10-01 |title=The Stability Boundary of the Distant Scattered Disk |journal=The Astrophysical Journal |volume=920 |issue=2 |pages=148 |doi=10.3847/1538-4357/ac19a4 |doi-access=free |arxiv=2111.00305 |bibcode=2021ApJ...920..148B |issn=0004-637X}}</ref><ref>{{Cite journal |last1=Hadden |first1=Sam |last2=Tremaine |first2=Scott |date=2023-11-09 |title=Scattered disc dynamics: the mapping approach |url=https://academic.oup.com/mnras/article/527/2/3054/7408612 |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=527 |issue=2 |pages=3054–3075 |doi=10.1093/mnras/stad3478 |issn=0035-8711|doi-access=free }}</ref>

The discovery of [[90377 Sedna]] in 2003, together with a few other objects discovered around that time such as {{mpl|(148209) 2000 CR|105}} and {{mpl|(612911) 2004 XR|190}}, has motivated discussion of a category of distant objects that may also be inner [[Oort cloud]] objects or (more likely) transitional objects between the scattered disc and the inner Oort cloud.<ref name="Jewitt2006"/>

Although Sedna is officially considered a scattered-disc object by the MPC, its discoverer [[Michael E. Brown]] has suggested that because its [[perihelion]] distance of 76&nbsp;AU is too distant to be affected by the gravitational attraction of the outer planets it should be considered an inner-Oort-cloud object rather than a member of the scattered disc.<ref name=Sedna>{{cite web |title=Sedna (The coldest most distant place known in the solar system; possibly the first object in the long-hypothesized Oort cloud) |last=Brown |first=Michael E. |author-link=Michael E. Brown |publisher=California Institute of Technology, Department of Geological Sciences |url=http://www.gps.caltech.edu/~mbrown/sedna/ |access-date=2008-07-02 |df=dmy-all}}</ref> This classification of Sedna as a detached object is accepted in recent publications.<ref name="Jewitt2008">{{cite book |author1-link=David Jewitt |first1=D. |last1=Jewitt |first2=A. |last2=Moro-Martın |first3=P. |last3=Lacerda |contribution=The Kuiper belt and other debris disks |title=Astrophysics in the Next Decade |publisher=Springer Verlag |year=2009 |url=http://www.ifa.hawaii.edu/faculty/jewitt/papers/2008/JML08.pdf <!-- Preprint of the article -->}}</ref>

This line of thinking suggests that the lack of a significant gravitational [[Perturbation (astronomy)|interaction]] with the outer planets creates an extended–outer group starting somewhere between Sedna (perihelion 76&nbsp;AU) and more conventional SDOs like {{mpl-|15874|1996 TL|66}} (perihelion 35 AU), which is listed as a scattered–near object by the Deep Ecliptic Survey.<ref name=1996TL66>{{cite web |author=Buie, Marc W. |author-link=Marc W. Buie |date=2007-12-28 |title=Orbit fit and astrometric record for 15874 |publisher=SwRI |department=Space Science Department |url=http://www.boulder.swri.edu/~buie/kbo/astrom/15874.html |access-date=2011-11-12 |df=dmy-all}}</ref>

=== Influence of Neptune ===
One of the problems with defining this extended category is that weak resonances may exist and would be difficult to prove due to chaotic planetary perturbations and the current lack of knowledge of the orbits of these distant objects. They have [[orbital period]]s of more than 300 years and most have only been observed over a short observation [[Arc (geometry)|arc]] of a couple years. Due to their great distance and slow movement against background stars, it may be decades before most of these distant orbits are determined well enough to confidently confirm or [[Orbital resonance#Coincidental 'near' ratios of mean motion|rule out a resonance]]. Further improvement in the orbit and potential resonance of these objects will help to understand the [[Formation and evolution of the Solar System#Planetary migration|migration of the giant planets]] and the formation of the Solar System. For example, simulations by Emel'yanenko and Kiseleva in 2007 show that many distant objects could be in [[Resonant trans-Neptunian object|resonance with Neptune]]. They show a 10% likelihood that 2000 CR<sub>105</sub> is in a 20:1 resonance, a 38% likelihood that 2003 QK<sub>91</sub> is in a 10:3 resonance, and an 84% likelihood that {{mpl|(82075) 2000 YW|134}} is in an 8:3 resonance.<ref name=Emel2008>{{cite journal |last=Emel'yanenko |first=V.V. |title=Resonant motion of trans-Neptunian objects in high-eccentricity orbits |journal=Astronomy Letters |volume=34 |issue=4 |pages=271–279 |year=2008 |bibcode=2008AstL...34..271E |doi=10.1134/S1063773708040075|s2cid=122634598 }}(subscription required)</ref> The [[List of possible dwarf planets|likely dwarf planet]] {{mpl|(145480) 2005 TB|190}} appears to have less than a 1% likelihood of being in a 4:1 resonance.<ref name="Emel2008"/>

=== Influence of hypothetical planet(s) beyond Neptune ===
Mike Brown—who made the [[Planet Nine]] hypothesis—makes an observation that "all of the known distant objects which are pulled even a little bit away from the Kuiper seem to be clustered under the influence of this hypothetical planet (specifically, objects with semimajor axis > 100 AU and perihelion > 42 AU)".<ref name=Brownplanet9>{{cite web |url=http://www.findplanetnine.com/2016/02/why-i-believe-in-planet-nine.html |author=Mike Brown |title=Why I believe in Planet Nine |author-link=Michael E. Brown}}</ref>
Carlos de la Fuente Marcos and Ralph de la Fuente Marcos have calculated that some of the statistically significant [[Commensurability (astronomy)|commensurabilities]] are compatible with the Planet Nine hypothesis; in particular, a number of objects{{efn|60 minor planets with a semi-major axis greater than 150&nbsp;AU and [[perihelion]] greater than 30&nbsp;AU are known.<ref name=mpcq30a150>{{cite web |url=http://minorplanetcenter.net/db_search/show_by_properties?perihelion_distance_min=30&semimajor_axis_min=150 |title=Minor Planets with semi-major axis greater than 150&nbsp;AU and perihelion greater than 30&nbsp;AU}}</ref>}} which are called [[extreme trans-Neptunian object]] ('''ETNOs''')<ref name="Marcos2014">{{cite journal |author1=C. de la Fuente Marcos |author2=R. de la Fuente Marcos |title=Extreme trans-Neptunian objects and the Kozai mechanism: Signalling the presence of trans-Plutonian planets |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=443 |issue=1 |pages=L59–L63 |arxiv=1406.0715 |bibcode=2014MNRAS.443L..59D |doi=10.1093/mnrasl/slu084 |date=September 1, 2014 |doi-access=free |s2cid=118622180 |df=dmy-all}}</ref> may be trapped in the 5:3 and 3:1 mean-motion resonances with a putative Planet Nine with a semimajor axis ~700&nbsp;AU.<ref name=Marcos2016>{{cite journal |doi=10.1093/mnrasl/slw077|title=Commensurabilities between ETNOs: a Monte Carlo survey |arxiv=1604.05881 |bibcode=2016MNRAS.460L..64D |first1=Carlos |last1=de la Fuente Marcos |first2=Raúl |last2=de la Fuente Marcos |journal=Monthly Notices of the Royal Astronomical Society: Letters |volume=460 |issue=1 |pages=L64–L68 |date=21 July 2016|doi-access=free |s2cid=119110892 }}</ref>

== Possible detached objects ==
{{See also|Sednoid|Extreme trans-Neptunian object}}
{{Update|date=October 2023|demospace=section|type=section}}

This is a list of known objects by discovery date that could not be easily scattered by Neptune's current orbit and therefore are likely to be detached objects, but that lie inside the perihelion gap of ≈50–75&nbsp;AU that defines the [[sednoid]]s.<ref>{{cite web|date=10 September 2013 |title=How many dwarf planets are there in the outer solar system? (updates daily) |publisher=California Institute of Technology |author=Michael E. Brown |url=http://www.gps.caltech.edu/~mbrown/dps.html |access-date=2013-05-27 |quote=Diameter: 242km |url-status=dead |archive-url=https://web.archive.org/web/20111018154917/http://www.gps.caltech.edu/~mbrown/dps.html |archive-date=2011-10-18 |df=dmy-all |author-link=Michael E. Brown }}</ref><ref name=mpcfilter>{{cite web |url=http://minorplanetcenter.net/db_search/show_by_properties?perihelion_distance_min=40&aphelion_distance_min=60&perihelion_distance_max=55 |title=objects with perihelia between 40–55 AU and aphelion more than 60 AU}}</ref><ref name=mpcfilter1b>{{cite web |url=http://minorplanetcenter.net/db_search/show_by_properties?perihelion_distance_min=40&aphelion_distance_min=100&perihelion_distance_max=55 |title=objects with perihelia between 40–55&nbsp;AU and aphelion more than 100&nbsp;AU}}</ref><ref name=mpcfilter2>{{cite web |url=http://minorplanetcenter.net/db_search/show_by_properties?perihelion_distance_min=40&semimajor_axis_min=50&perihelion_distance_max=55 |title=objects with perihelia between 40–55&nbsp;AU and semi-major axis more than 50&nbsp;AU}}</ref><ref name=mpcfilter3>{{cite web |url=http://minorplanetcenter.net/db_search/show_by_properties?perihelion_distance_min=40&eccentricity_min=0.5&perihelion_distance_max=55 |title=objects with perihelia between 40–55&nbsp;AU and eccentricity more than 0.5}}</ref><ref name=mpcfilter4>{{cite web |url=http://minorplanetcenter.net/db_search/show_by_properties?perihelion_distance_min=37&eccentricity_min=0.5&perihelion_distance_max=40 |title=objects with perihelia between 37–40&nbsp;AU and eccentricity more than 0.5}}</ref>

Objects listed below have a perihelion of more than 40&nbsp;AU, and a [[Semi-major and semi-minor axes|semi-major axis]] of more than 47.7&nbsp;AU (the 1:2 resonance with Neptune, and the approximate outer limit of the Kuiper Belt):<ref>{{cite web |title=MPC list of ''q'' > 40 and ''a'' > 47.7 |url=http://minorplanetcenter.net/db_search/show_by_properties?perihelion_distance_min=40&semimajor_axis_min=47.7 |publisher=[[Minor Planet Center]] |access-date=7 May 2018}}</ref>

{| class="wikitable sortable collapsible" style="text-align: center; font-size: 0.9em;"
|-
! data-sort-type="number" width=130 | [[Minor planet designation|Designation]]
! data-sort-type="number" | Diameter<ref name="johnstonsarchive" /><br />(km)
! data-sort-type="number" | [[Absolute magnitude#Solar System bodies (H)|H]]
! data-sort-type="number" | [[Perihelion|q]]<br />(AU)
! data-sort-type="number" | [[Semi-major axis|a]]<br />(AU)
! data-sort-type="number" | [[Aphelion|Q]]<br />(AU)
! data-sort-type="number" | [[Argument of perihelion|ω]] (°)
! data-sort-type="number" | Discovery<br />Year
! Discoverer
! class="unsortable" | Notes & Refs
|-
| data-sort-value="148209" | {{mpl-|148209|2000 CR|105}}
| 243
| 6.3
| 44.252
| 221.2
| 398
| 316.93
| 2000
| [[Marc William Buie|M. W. Buie]]
|<ref name=abc>{{cite journal |author1=E. L. Schaller |author2=M. E. Brown |title=Volatile loss and retention on Kuiper belt objects |journal=Astrophysical Journal |volume=659 |issue=1 |pages=I.61–I.64 |year=2007|url=http://www.gps.caltech.edu/~mbrown/papers/ps/volatiles.pdf|access-date=2008-04-02|doi=10.1086/516709 |bibcode=2007ApJ...659L..61S|s2cid=10782167 }}</ref>
|-
| data-sort-value="082075" | {{mpl-|82075|2000 YW|134}}
| 216
| 4.7 
| 41.207
| 57.795
| 74.383
| 316.481
| 2000
| [[Spacewatch]]
| ≈3:8 Neptune resonance 
|-
| {{mpl|2001 FL|193}}
| 81 
| 8.7
|40.29
|50.26
|60.23
|108.6
|2001 
| [[Rhiannon Lynne Allen|R. L. Allen]], [[Gary Bernstein (astronomer)|G. Bernstein]], [[Renu Malhotra|R. Malhotra]]
| orbit extremely poor, might not be a TNO
|-
| data-sort-value="P2001K077A" | {{mpl|2001 KA|77}}
| 634
| 5.0
| 43.41
| 47.74
| 52.07
| 120.3
| 2001
| [[Marc William Buie|M. W. Buie]]
| borderline [[Cubewano|classical KBO]]
|-
| data-sort-value="P2002C154P" | {{mpl|2002 CP|154}}
| 222
| 6.5
| 42
| 52
| 62
| 50
| 2002
| [[Marc William Buie|M. W. Buie]]
| orbit fairly poor, but definitely a detached object
|-
| data-sort-value="P2003U291Y" | {{mpl|2003 UY|291}}
| 147
| 7.4
| 41.19
| 48.95
| 56.72
| 15.6
| 2003
| [[Marc William Buie|M. W. Buie]]
| borderline [[Cubewano|classical KBO]]
|-
| data-sort-value="090377" | [[90377 Sedna|Sedna]]
| 995
| 1.5
| 76.072
| 483.3
| 890
| 311.61
| 2003
| [[Michael E. Brown|M. E. Brown]], [[Chad Trujillo|C. A. Trujillo]], [[David L. Rabinowitz|D. L. Rabinowitz]]
| Sednoid
|-
| data-sort-value="P2004P112D" | {{mpl|2004 PD|112}}
| 267
| 6.1
| 40
| 70
| 90
| 40
| 2004
| [[Marc William Buie|M. W. Buie]]
| orbit very poor, might not be a detached object
|-
| data-sort-value="474640" | [[474640 Alicanto|Alicanto]]
| 222
| 6.5
| 47.308
| 315
| 584
| 326.925
| 2004
| [[Cerro Tololo Inter-American Observatory|Cerro Tololo]] (unspecified)
|<ref name=VN112>{{cite web |first=Marc W. |last=Buie |date=2007-11-08 |df=dmy-all |title=Orbit Fit and Astrometric record for 04VN112 |publisher=SwRI (Space Science Department) |url=http://www.boulder.swri.edu/~buie/kbo/astrom/04VN112.html |access-date=2008-07-17 |url-status=dead |archive-url=https://web.archive.org/web/20100818145946/http://www.boulder.swri.edu/~buie/kbo/astrom/04VN112.html |archive-date=2010-08-18 |author-link=Marc W. Buie }}</ref><ref name=jpldata04VN112>{{cite web |title=JPL Small-Body Database Browser: (2004 VN112) |url=http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2004VN112 |access-date=2015-02-24}}</ref><ref name="cen_sdo">{{cite web |url=http://www.minorplanetcenter.net/iau/lists/Centaurs.html|title=List Of Centaurs and Scattered-Disk Objects |access-date=2011-07-05 |df=dmy-all |quote=Discoverer: CTIO}}</ref>
|-
| data-sort-value="P2004X190R" | {{mpl|2004 XR|190}}
| 612
| 4.1
| 51.085
| 57.336
| 63.586
| 284.93
| 2004
| [[Rhiannon Lynne Allen|R. L. Allen]], [[Brett J. Gladman|B. J. Gladman]], [[John J. Kavelaars|J. J. Kavelaars]]<br />[[Jean-Marc Petit|J.-M. Petit]], [[Joel W. Parker|J. W. Parker]], [[Phil Nicholson|P. Nicholson]]
| very high inclination; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination of 2004 XR<sub>190</sub> to obtain a very high perihelion<ref name="abc"/><ref>{{cite journal |author1=R. L. Allen |author2=B. Gladman | title = Discovery of a low-eccentricity, high-inclination Kuiper Belt object at 58 AU | journal = The Astrophysical Journal | year = 2006 | volume = 640 |issue=1 |doi=10.1086/503098 |arxiv=astro-ph/0512430 |bibcode = 2006ApJ...640L..83A | pages=L83–L86|s2cid=15588453 }}</ref><ref name="Like Buffy">{{cite journal |title=Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects with Moderate Semimajor Axes and Eccentricities |journal=The Astrophysical Journal Letters |first1=Scott S. |last1=Sheppard |first2=Chadwick |last2=Trujillo |first3=David J. |last3=Tholen |volume=825 |issue=1 |page=L13 |date=July 2016 |doi=10.3847/2041-8205/825/1/L13 |bibcode=2016ApJ...825L..13S |arxiv=1606.02294|s2cid=118630570 |doi-access=free }}</ref>
|-
| data-sort-value="P2005C081G" | {{mpl|2005 CG|81}}
| 267
| 6.1
| 41.03
| 54.10
| 67.18
| 57.12
| 2005
| [[Canada France Ecliptic Plane Survey|CFEPS]]
| —
|-
| data-sort-value="385607" | {{mpl-|385607|2005 EO|297}}
| 161
| 7.2
| 41.215
| 62.98
| 84.75
| 349.86
| 2005
| [[Marc William Buie|M. W. Buie]]
| —
|-
| data-sort-value="145480" | {{mpl-|145480|2005 TB|190}}
| 372
| 4.5
| 46.197
| 75.546
| 104.896
| 171.023
| 2005
| [[Andrew C. Becker|A. C. Becker]], [[Andrew W. Puckett|A. W. Puckett]], [[Jeremy Martin Kubica|J. M. Kubica]]
| Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion<ref name="Like Buffy"/>
|-
| data-sort-value="P2006A101O" | {{mpl|2006 AO|101}}
| 168
| 7.1
| —
| —
| —
| —
| 2006
| [[Mauna Kea Observatories|Mauna Kea]] (unspecified)
| orbit extremely poor, might not be a TNO
|-
| data-sort-value="278361" | {{mpl-|278361|2007 JJ|43}}
| 558
| 4.5
| 40.383
| 48.390
| 56.397
| 6.536
| 2007
| [[Palomar Observatory|Palomar]] (unspecified)
| borderline [[Cubewano|classical KBO]]
|-
| data-sort-value="P2007L038E" | {{mpl|2007 LE|38}}
| 176
| 7.0
| 41.798
| 54.56
| 67.32
| 53.96
| 2007
| [[Mauna Kea Observatories|Mauna Kea]] (unspecified)
| —
|-
| data-sort-value="P2008S291T" | {{mpl|2008 ST|291}}
| 640
| 4.2
| 42.27
| 99.3
| 156.4
| 324.37
| 2008
| [[Megan Schwamb|M. E. Schwamb]], [[Michael E. Brown|M. E. Brown]], [[David L. Rabinowitz|D. L. Rabinowitz]]
| ≈1:6 Neptune resonance
|-
| data-sort-value="P2009K036X" | {{mpl|2009 KX|36}}
| 111
| 8.0
| —
| 100
| 100
| —
| 2009
| [[Mauna Kea Observatories|Mauna Kea]] (unspecified)
| orbit extremely poor, might not be a TNO
|-
| data-sort-value="P2010D093N" | {{mpl-|523635|2010 DN|93}}
| 486
| 4.7
| 45.102
| 55.501
| 65.90
| 33.01
| 2010
| [[Pan-STARRS]]
| ≈2:5 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion<ref name="Like Buffy"/>
|-
| data-sort-value="P2010E065R" | {{mpl|2010 ER|65}}
| 404
| 5.0
| 40.035
| 99.71
| 159.39
| 324.19
| 2010
| [[David L. Rabinowitz|D. L. Rabinowitz]], [[Suzanne W. Tourtellotte|S. W. Tourtellotte]]
| —
|-
| data-sort-value="P2010G174B" | {{mpl|2010 GB|174}}
| 222
| 6.5
| 48.8
| 360
| 670
| 347.7
| 2010
| [[Mauna Kea Observatories|Mauna Kea]] (unspecified)
| —
|-
| data-sort-value="P2012F084H" | {{mpl|2012 FH|84}}
| 161
| 7.2
| 42
| 56
| 70
| 10
| 2012
| [[Las Campanas Observatory|Las Campanas]] (unspecified)
| —
|-
| data-sort-value="P2012V113P" | {{mpl|2012 VP|113}}
| 702
| 4.0
| 80.47
| 256
| 431
| 293.8
| 2012
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]]
| Sednoid
|-
| data-sort-value="P2013Q028Q" | {{mpl|2013 FQ|28}}
| 280
| 6.0
| 45.9
| 63.1
| 80.3
| 230
| 2013
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]]
| ≈1:3 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion<ref name="Like Buffy"/>
|-
| data-sort-value="P2013F028T" | {{mpl|2013 FT|28}}
| 202
| 6.7
| 43.5
| 310
| 580
| 40.3
| 2013
| [[Scott S. Sheppard|S. S. Sheppard]]
| —
|-
| data-sort-value="496315" | {{mpl-|496315|2013 GP|136}}
| 212
| 6.6
| 41.061
| 155.1
| 269.1
| 42.38
| 2013
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="P2013G136Q" | {{mpl|2013 GQ|136}}
| 222
| 6.5
| 40.79
| 49.06
| 57.33
| 155.3
| 2013
| [[Outer Solar System Origins Survey|OSSOS]]
| borderline [[Cubewano|classical KBO]]
|-
| data-sort-value="P2013G138G" | {{mpl|2013 GG|138}}
| 212
| 6.6
| 46.64
| 47.792
| 48.946
| 128
| 2013
| [[Outer Solar System Origins Survey|OSSOS]]
| borderline [[Cubewano|classical KBO]]
|-
| data-sort-value="500876" | {{mpl-|500876|2013 JD|64}}
| 111
| 8.0
| 42.603
| 73.12
| 103.63
| 178.0
| 2013
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="500880" | {{mpl-|500880|2013 JJ|64}}
| 147
| 7.4
| 44.04
| 48.158
| 52.272
| 179.8
| 2013
| [[Outer Solar System Origins Survey|OSSOS]]
| borderline [[Cubewano|classical KBO]]
|-
| data-sort-value="P2013S099Y" | {{mpl|2013 SY|99}}
| 202
| 6.7
| 50.02
| 694
| 1338
| 32.1
| 2013
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="P2013S100K" | {{mpl|2013 SK|100}}
| 134
| 7.6
| 45.468
| 61.61
| 77.76
| 11.5
| 2013
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="505478" | {{mpl-|505478|2013 UT|15}}
| 255
| 6.3
| 43.89
| 195.7
| 348
| 252.33
| 2013
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="P2013U017B" | {{mpl|2013 UB|17}}
| 176
| 7.0
| 44.49
| 62.31
| 80.13
| 308.93
| 2013
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="P2013V024D" | {{mpl|2013 VD|24}}
| 128
| 7.8
| 40
| 50
| 70
| 197
| 2013
| [[Dark Energy Survey]]
| orbit very poor, might not be a detached object
|-
| data-sort-value="P2013Y151J" | {{mpl|2013 YJ|151}}
| 336
| 5.4
| 40.866
| 72.35
| 103.83
| 141.83
| 2013
| [[Pan-STARRS]]
| —
|-
| data-sort-value="P2014E051Z" | {{mpl|2014 EZ|51}}
| 770
| 3.7
| 40.70
| 52.49
| 64.28
| 329.84
| 2014
| [[Pan-STARRS]]
| —
|-
| data-sort-value="P2014F069C" | {{mpl|2014 FC|69}}
| 533
| 4.6
| 40.28
| 73.06
| 105.8
| 190.57
| 2014
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]]
|
|-
| data-sort-value="P2014F071Z" | {{mpl|2014 FZ|71}}
| 185
| 6.9
| 55.9
| 76.2
| 96.5
| 245
| 2014
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]]
| ≈1:4 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a very high perihelion<ref name="Like Buffy"/>
|-
| data-sort-value="P2014F072C" | {{mpl|2014 FC|72}}
| 509
| 4.5
| 51.670
| 76.329
| 100.99
| 32.85
| 2014
| [[Pan-STARRS]]
|  ≈1:4 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a very high perihelion<ref name="Like Buffy"/>
|-
| data-sort-value="P2014J080M" | {{mpl|2014 JM|80}}
| 352
| 5.5
| 46.00
| 63.00
| 80.01
| 96.1
| 2014
| [[Pan-STARRS]]
| ≈1:3 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion<ref name="Like Buffy"/>
|-
| data-sort-value="P2014J080S" | {{mpl|2014 JS|80}}
| 306
| 5.5
| 40.013
| 48.291
| 56.569
| 174.5
| 2014
| [[Pan-STARRS]]
| borderline [[Cubewano|classical KBO]]
|-
| data-sort-value="P2014O394J" | {{mpl|2014 OJ|394}}
| 423
| 5.0
| 40.80
| 52.97
| 65.14
| 271.60
| 2014
| [[Pan-STARRS]]
| in 3:7 Neptune resonance
|-
| data-sort-value="P2014Q441R" | {{mpl|2014 QR|441}}
| 193
| 6.8
| 42.6
| 67.8
| 93.0
| 283
| 2014
| [[Dark Energy Survey]]
| —
|-
| data-sort-value="P2014S349R" | {{mpl|2014 SR|349}}
| 202
| 6.6
| 47.6
| 300
| 540
| 341.1
| 2014
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]]
| —
|-
| data-sort-value="P2014S349S" | {{mpl|2014 SS|349}}
| 134
| 7.6
| 45
| 140
| 240
| 148
| 2014
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]]
| ≈2:10 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion<ref name="Like 2014SS349">{{cite journal |title=New Extreme Trans-Neptunian Objects: Towards a Super-Earth in the Outer Solar System |journal=Astrophysical Journal |volume=152 |issue=6 |pages=221 |first1=Scott S. |last1=Sheppard |first2=Chad |last2=Trujillo |date=August 2016 |doi= 10.3847/1538-3881/152/6/221 |arxiv=1608.08772 |bibcode=2016AJ....152..221S|s2cid=119187392 |doi-access=free }}</ref>
|-
| data-sort-value="P2014S373T" | {{mpl|2014 ST|373}}
| 330
| 5.5
| 50.13
| 104.0
| 157.8
| 297.52
| 2014
| [[Dark Energy Survey]]
| —
|-
| data-sort-value="P2014U228T" | {{mpl|2014 UT|228}}
| 154
| 7.3
| 43.97
| 48.593
| 53.216
| 49.9
| 2014
| [[Outer Solar System Origins Survey|OSSOS]]
| borderline [[Cubewano|classical KBO]]
|-
| data-sort-value="P2014U230A" | {{mpl|2014 UA|230}}
| 222
| 6.5
| 42.27
| 55.05
| 67.84
| 132.8
| 2014
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="P2014U231O" | {{mpl|2014 UO|231}}
| 97
| 8.3
| 42.25
| 55.11
| 67.98
| 234.56
| 2014
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="P2014W509K" | {{mpl|2014 WK|509}}
| 584
| 4.0
| 40.08
| 50.79
| 61.50
| 135.4
| 2014
| [[Pan-STARRS]]
| —
|-
| data-sort-value="P2014W556B" | {{mpl|2014 WB|556}}
| 147
| 7.4
| 42.6
| 280
| 520
| 234
| 2014
| [[Dark Energy Survey]]
| —
|-
| data-sort-value="P2015A281L" | {{mpl|2015 AL|281}}
| 293
| 6.1
| 42
| 48
| 54
| 120
| 2015
| [[Pan-STARRS]]
| borderline [[Cubewano|classical KBO]]<br />orbit very poor, might not be a detached object
|-
| data-sort-value="495603" | {{mpl-|495603|2015 AM|281}}
| 486
| 4.8
| 41.380
| 55.372
| 69.364
| 157.72
| 2015
| [[Pan-STARRS]]
| —
|-
| data-sort-value="487581" | {{mpl-|487581|2015 BE|519}}
| 352
| 5.5
| 44.82
| 47.866
| 50.909
| 293.2
| 2015
| [[Pan-STARRS]]
| borderline [[Cubewano|classical KBO]]
|-
| data-sort-value="P2015F345J" | {{mpl|2015 FJ|345}}
| 117
| 7.9
| 51
| 63.0
| 75.2
| 78
| 2015
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]]
| ≈1:3 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a very high perihelion<ref name="Like Buffy"/>
|-
| data-sort-value="P2015G050P" | {{mpl|2015 GP|50}}
| 222
| 6.5
| 40.4
| 55.2
| 70.0
| 130
| 2015
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]]
| —
|-
| data-sort-value="P2015K162H" | {{mpl|2015 KH|162}}
| 671
| 3.9
| 41.63
| 62.29
| 82.95
| 296.805
| 2015
| [[Scott S. Sheppard|S. S. Sheppard]], [[David J. Tholen|D. J. Tholen]], [[Chad Trujillo|C. A. Trujillo]]
| —
|-
| data-sort-value="P2015K163G" | {{mpl|2015 KG|163}}
| 101
| 8.3
| 40.502
| 826
| 1610
| 32.06
| 2015
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="P2015K163H" | {{mpl|2015 KH|163}}
| 117
| 7.9
| 40.06
| 157.2
| 274
| 230.29
| 2015
| [[Outer Solar System Origins Survey|OSSOS]]
| ≈1:12 Neptune resonance
|-
| data-sort-value="P2015K172E" | {{mpl|2015 KE|172}}
| 106
| 8.1
| 44.137
| 133.12
| 222.1
| 15.43
| 2015
| [[Outer Solar System Origins Survey|OSSOS]]
| 1:9 Neptune resonance
|-
| data-sort-value="P2015K172G" | {{mpl|2015 KG|172}}
| 280
| 6.0
| 42
| 55
| 69
| 35
| 2015
| [[Rhiannon Lynne Allen|R. L. Allen]]<br />D. James<br />[[David Herrera (astronomer)|D. Herrera]]
|  orbit fairly poor, might not be a detached object
|-
| data-sort-value="P2015K174Q" | {{mpl|2015 KQ|174}}
| 154
| 7.3
| 49.31
| 55.40
| 61.48
| 294.0
| 2015
| [[Mauna Kea Observatories|Mauna Kea]] (unspecified)
| ≈2:5 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a very high perihelion<ref name="Like Buffy"/>
|-
| data-sort-value="P2015R245X" | {{mpl|2015 RX|245}}
| 255
| 6.2
| 45.5
| 410
| 780
| 65.3
| 2015
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|-
| data-sort-value="P2015T387G" | [[541132 Leleākūhonua|Leleākūhonua]]
| 300
| 5.5
| 65.02
| 1042
| 2019
| 118.0
| 2015
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]], [[David J. Tholen|D. J. Tholen]]
| Sednoid
|-
| {{mpl|2017 DP|121}}|| 161 ||7.2 ||40.52||50.48||60.45||217.9||2017 || || —
|-
| {{mpl|2017 FP|161}}|| 168 ||7.1 ||40.88||47.99||55.1||218||2017 || || borderline classical KBO
|-
| data-sort-value="P2017S132N" | {{mpl|2017 SN|132}}
| 97
| 5.8
| 40.949
| 79.868
| 118.786
| 148.769
| 2017
| [[Scott S. Sheppard|S. S. Sheppard]], [[Chad Trujillo|C. A. Trujillo]], [[David J. Tholen|D. J. Tholen]]
| 
|-
| data-sort-value="P2018V035M" | {{mpl|2018 VM|35}}
| 134
| 7.6
| 45.289
| 240.575
| 435.861
| 302.008
| 2018
| [[Mauna Kea Observatories|Mauna Kea]] (unspecified)
| 
|}

The following objects can also be generally thought to be detached objects, although with slightly lower perihelion distances of 38–40 AU.

{| class="wikitable sortable collapsible" style="text-align:center; font-size: 0.9em;"
|-
! width=130 | [[Minor planet designation|Designation]]
! data-sort-type="number" | Diameter<ref name="johnstonsarchive" /><br />(km)
! data-sort-type="number" | [[Absolute magnitude#Solar System bodies (H)|H]]
! data-sort-type="number" | [[Perihelion|q]]<br />(AU)
! data-sort-type="number" | [[Semi-major axis|a]]<br />(AU)
! data-sort-type="number" | [[Aphelion|Q]]<br />(AU)
! data-sort-type="number" | [[Argument of perihelion|ω]] (°)
! data-sort-type="number" | Discovery<br />Year
! Discoverer
! class="unsortable" | Notes & Refs
|-
| data-sort-value="506479" | {{mpl-|506479|2003 HB|57}}
| 147
| 7.4
| 38.116
| 166.2
| 294
| 11.082
| 2003
| [[Mauna Kea Observatories|Mauna Kea]] (unspecified)
| —
|-
| data-sort-value="P2003S422S" | {{mpl|2003 SS|422}}
| 168
| data-slort-value="7.2" | 7.04
| 39.574
| 198.181
| 356.788
| 206.824
| 2003
| [[Cerro Tololo Inter-American Observatory|Cerro Tololo]] (unspecified)
| —
|-
| data-sort-value="P2005R052H" | {{mpl|2005 RH|52}}
| 128
| 7.8
| 38.957
| 152.6
| 266.3
| 32.285
| 2005
| [[Canada France Ecliptic Plane Survey|CFEPS]]
| —
|-
| data-sort-value="P2007T434C" | {{mpl|2007 TC|434}}
| 168
| 7.0
| 39.577
| 128.41
| 217.23
| 351.010
| 2007
| [[Las Campanas Observatory|Las Campanas]] (unspecified)
| 1:9 Neptune resonance
|-
| data-sort-value="P2012F084L" | {{mpl|2012 FL|84}}
| 212
| 6.6
| 38.607
| 106.25
| 173.89
| 141.866
| 2012
| [[Pan-STARRS]]
| —
|-
| data-sort-value="P2014F072L" | {{mpl|2014 FL|72}}
| 193
| 6.8
| 38.1
| 104
| 170
| 259.49
| 2014
| [[Cerro Tololo Inter-American Observatory|Cerro Tololo]] (unspecified)
| —
|-
| data-sort-value="P2014J080W" | {{mpl|2014 JW|80}}
| 352
| 5.5
| 38.161
| 142.62
| 247.1
| 131.61
| 2014
| [[Pan-STARRS]]
| —
|-
| data-sort-value="P2014Y050K" | {{mpl-|523778|2014 YK|50}}
| 293
| 5.6
| 38.972
| 120.52
| 202.1
| 169.31
| 2014
| [[Pan-STARRS]]
| —
|-
|{{mpl|2015 DM|319}}
|
|8.78
|39.491
|272.302
|505.113
|43.227
|2015
|[[Outer Solar System Origins Survey|OSSOS]]
|
|-
| data-sort-value="P2015G050T" | {{mpl|2015 GT|50}}
| 88
| 8.6
| 38.46
| 333
| 627
| 129.3
| 2015
| [[Outer Solar System Origins Survey|OSSOS]]
| —
|}

== See also ==
* [[Classical Kuiper belt object]]
* [[List of Solar System objects by greatest aphelion]]
* [[List of trans-Neptunian objects]]
* [[Extreme trans-Neptunian object]]
* [[Planets beyond Neptune]]

== Notes ==
{{notelist|1}}

== References ==
{{reflist|25em|refs=

<ref name="johnstonsarchive">{{cite web
  |title      = List of Known Trans-Neptunian Objects
  |publisher  = Johnston's Archive
  |date       = 7 October 2018
  |url        = http://www.johnstonsarchive.net/astro/tnoslist.html
  |access-date = 23 October 2018}}</ref>

}} <!-- end of reflist -->

{{Dwarf planets}}
{{Small Solar System bodies}}
{{Solar System}}
{{Portal bar|Astronomy|Spaceflight|Outer space|Solar system}}
{{Good article}}

[[Category:Scattered disc and detached objects| ]]
[[Category:Oort cloud]]
[[Category:Solar System]]