View source for Neptune trojan

{{Short description|Asteroid orbiting the Sun near one of the stable Lagrangian points of Neptune}}
[[Image:NTrojans Plutinos 55AU.svg|thumb|265px|Neptune's {{L4|nolink=yes}} trojans with plutinos for reference.
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{{TNO}}

'''Neptune trojans''' are bodies that orbit the [[Sun]] near one of the stable [[Lagrangian point]]s of [[Neptune]], similar to the [[Trojan (astronomy)|trojans]] of other planets. They therefore have approximately the same orbital period as Neptune and follow roughly the same orbital path. Thirty-one Neptune trojans are currently known, of which 27 orbit near the Sun–Neptune {{L4}} Lagrangian point 60° ahead of Neptune<ref name=mpctrojans/> and four orbit near Neptune's {{L5}} region 60° behind Neptune.<ref name=mpctrojans/> The Neptune trojans are termed 'trojans' by analogy with the [[Jupiter trojan]]s.

The discovery of {{mpl|2005 TN|53}} in a high-inclination (>25°) orbit was significant, because it suggested a "thick" cloud of trojans<ref name=sheppard2006>{{cite journal
 |last        = Sheppard
 |first       = Scott S.
 |author2     = Trujillo, Chadwick A.
 |title       = A Thick Cloud of Neptune Trojans and Their Colors
 |doi         = 10.1126/science.1127173
 |journal     = Science
 |volume      = 313
 |issue       = 5786
 |pages       = 511–514
 |date        = June 2006
 |url         = http://www.dtm.ciw.edu/users/sheppard/pub/Sheppard06NepTroj.pdf
 |access-date  = 2008-02-26
 |pmid        = 16778021
 |bibcode     = 2006Sci...313..511S
 |s2cid = 35721399
 |url-status     = live
 |archive-url  = https://web.archive.org/web/20100716005454/http://www.dtm.ciw.edu/users/sheppard/pub/Sheppard06NepTroj.pdf
 |archive-date = 2010-07-16
}}</ref> ([[Jupiter trojan]]s have inclinations up to 40°<ref name=Jewitt2000>{{cite journal
 | last=Jewitt
 | first=David C.
 |author2=Trujillo, Chadwick A. |author3=Luu, Jane X.
  | title=Population and size distribution of small Jovian Trojan asteroids|date=2000|journal=The Astronomical Journal
 | volume=120
 | issue=2
 | pages=1140–7
 | doi=10.1086/301453
 | bibcode=2000AJ....120.1140J|arxiv = astro-ph/0004117 | s2cid=119450236
 }}</ref>), which is indicative of freeze-in capture instead of in situ or collisional formation.<ref name=sheppard2006/> It is suspected that large (radius ≈ 100&nbsp;km) Neptune trojans could outnumber [[Jupiter trojan]]s by an [[order of magnitude]].<ref name=Chiang2005>
E. I. Chiang and Y. Lithwick
''Neptune Trojans as a Testbed for Planet Formation'',
The Astrophysical Journal, '''628''', pp. 520–532   [http://www.arxiv.org/abs/astro-ph/0502276  Preprint]</ref><ref name=Sheppard>{{cite web
 |date        = 30 January 2007
 |title       = Neptune May Have Thousands of Escorts
 |author      = David Powell
 |publisher   = Space.com
 |url         = http://www.space.com/scienceastronomy/070130_st_neptune_trojans.html
 |access-date  = 2007-03-08
 |url-status     = live
 |archive-url  = https://web.archive.org/web/20080815161200/http://www.space.com/scienceastronomy/070130_st_neptune_trojans.html
 |archive-date = 15 August 2008
}}</ref>

In 2010, the discovery of the first known {{L5}} Neptune trojan, {{mpl|2008 LC|18}}, was announced.<ref name=LC18>{{cite web
 |date        = 2010-08-12
 |title       = Trojan Asteroid Found in Neptune's Trailing Gravitational Stability Zone
 |publisher   = Carnegie Institution of Washington
 |author      = Scott S. Sheppard
 |url         = http://www.dtm.ciw.edu/users/sheppard/L5trojan/
 |access-date  = 2007-12-28
 |url-status     = live
 |archive-url  = https://web.archive.org/web/20100815095616/http://www.dtm.ciw.edu/users/sheppard/L5trojan/
 |archive-date = 2010-08-15
}}</ref> Neptune's trailing {{L5|nolink=yes}} region is currently very difficult to observe because it is along the line of sight to the [[Galactic Center|center of the Milky Way]], an area of the sky crowded with stars.

== Discovery and exploration ==
In 2001, the first Neptune trojan was discovered, {{mpl|(612243) 2001 QR|322}}, near Neptune's {{L4|nolink=yes}} region, and with it the fifth{{efn|After the [[asteroid belt]], the [[Jupiter trojan]]s, the [[trans-Neptunian object]]s and the [[Mars trojan]]s.}} known populated stable reservoir of small bodies in the Solar System. In 2005, the discovery of the high-inclination trojan {{mpl|2005 TN|53}} has indicated that the Neptune trojans populate thick clouds, which has constrained their possible origins (see below).

On August 12, 2010, the first {{L5|nolink=yes}} trojan, {{mpl|2008 LC|18}}, was announced.<ref name=LC18/> It was discovered by a dedicated survey that scanned regions where the light from the stars near the [[Galactic Center]] is obscured by dust clouds.<ref name=2008LC18/> This suggests that large {{L5|nolink=yes}} trojans are as common as large {{L4|nolink=yes}} trojans, to within uncertainty,<ref name=2008LC18/> further constraining models about their origins (see below).

It would have been possible for the ''[[New Horizons]]'' spacecraft to investigate {{L5|nolink=yes}} Neptune trojans discovered by 2014, when it passed through this region of space en route to [[Pluto]].<ref name=Sheppard/> Some of the patches where the light from the Galactic Center is obscured by dust clouds are along ''New Horizons''{{'}}s flight path, allowing detection of objects that the spacecraft could image.<ref name=2008LC18/> {{mpl|2011 HM|102}}, the highest-inclination Neptune trojan known, was just bright enough for ''New Horizons'' to observe it in end-2013 at a distance of 1.2 AU.<ref name=2011HM102-IH>{{cite web
 |last        = Parker
 |first       = Alex
 |title       = Citizen "Ice Hunters" help find a Neptune Trojan target for New Horizons
 |work        = www.planetary.org/blogs
 |publisher   = [[The Planetary Society]]
 |date        = 2012-10-09
 |url         = http://www.planetary.org/blogs/guest-blogs/20121009-parker-neptune-trojan-ice-hunters.html
 |access-date  = 2012-10-09
 |url-status     = live
 |archive-url  = https://web.archive.org/web/20121101020405/http://www.planetary.org/blogs/guest-blogs/20121009-parker-neptune-trojan-ice-hunters.html
 |archive-date = 2012-11-01
}}</ref> However, ''New Horizons'' may not have had sufficient downlink bandwidth, so it was eventually decided to give precedence to the preparations for the Pluto flyby.<ref name="Stern, Alan">{{cite web|author=Stern, Alan|date=May 1, 2006|title=Where Is the Centaur Rocket?|work=The PI's Perspective|url=http://pluto.jhuapl.edu/overview/piPerspectives/piPerspective_5_1_2006_2.php|publisher=Johns Hopkins APL|access-date=June 11, 2006|archive-url=https://web.archive.org/web/20060901204154/http://pluto.jhuapl.edu/overview/piPerspectives/piPerspective_5_1_2006_2.php|archive-date=September 1, 2006|url-status=dead}}</ref><ref name="Parker">{{cite news |last=Parker |first=Alex |url=http://www.planetary.org/blogs/guest-blogs/2013/0430-2011hm102-new-neptune-companion.html |title=2011 HM102: A new companion for Neptune |work=The Planetary Society |date=April 30, 2013 |access-date=October 7, 2014 |url-status=dead |archive-url=https://web.archive.org/web/20141009183627/http://www.planetary.org/blogs/guest-blogs/2013/0430-2011hm102-new-neptune-companion.html |archive-date=October 9, 2014 }}</ref>

== Dynamics and origin ==
[[Image:Neptunian Trojans.gif|right|thumb|330px|An animation showing the path of six of Neptune's {{L4|nolink=yes}} trojans in a [[rotating frame]] with a period equal to [[Neptune]]'s orbital period. Neptune is held stationary. (Click to view.)]]

The orbits of Neptune trojans are highly stable; Neptune may have retained up to 50% of the original post-migration trojan population over the age of the Solar System.<ref name=sheppard2006/> Neptune's {{L5|nolink=yes}} can host stable trojans equally well as its {{L4|nolink=yes}}.<ref name=2008LC18potunstable/> Neptune trojans can [[Libration|librate]] up to 30° from their associated Lagrangian points with a 10,000-year period.<ref name=2008LC18/> Neptune trojans that escape enter orbits similar to [[centaur (minor planet)|centaurs]].<ref name=2008LC18potunstable/> Although Neptune cannot currently capture stable trojans,<ref name=sheppard2006/> roughly 2.8% of the centaurs within 34 AU are predicted to be Neptune [[Co-orbital configuration|co-orbitals]]. Of these, 54% would be in [[horseshoe orbit]]s, 10% would be [[quasi-satellite]]s, and 36% would be trojans (evenly split between the {{L4|nolink=yes}} and {{L5|nolink=yes}} groups).<ref name="AlexandersenGladman2013">{{Cite journal | last1 = Alexandersen | first1 = M. | last2 = Gladman | first2 = B. | last3 = Greenstreet | first3 = S. | last4 = Kavelaars | first4 = J. J. | last5 = Petit | first5 = J. -M. | last6 = Gwyn | first6 = S. | doi = 10.1126/science.1238072 | title = A Uranian Trojan and the Frequency of Temporary Giant-Planet Co-Orbitals | journal = Science | volume = 341 | issue = 6149 | pages = 994–997 | year = 2013 | pmid =  23990557| arxiv = 1303.5774|bibcode = 2013Sci...341..994A | s2cid = 39044607 }}</ref>

The unexpected high-inclination trojans are the key to understanding the origin and evolution of the population as a whole.<ref name=2008LC18potunstable>Horner, J., Lykawka, P. S., Bannister, M. T., & Francis, P. [https://arxiv.org/ftp/arxiv/papers/1202/1202.3279.pdf 2008 LC18: a potentially unstable Neptune Trojan] Accepted to appear in [[Monthly Notices of the Royal Astronomical Society]]</ref> The existence of high-inclination Neptune trojans points to a capture during planetary migration instead of in situ or collisional formation.<ref name=sheppard2006/><ref name=2008LC18/> The estimated equal number of large {{L5|nolink=yes}} and {{L4|nolink=yes}} trojans indicates that there was no gas drag during capture and points to a common capture mechanism for both {{L4|nolink=yes}} and {{L5|nolink=yes}} trojans.<ref name=2008LC18/> The capture of Neptune trojans during a migration of the planets occurs via process similar to the chaotic capture of Jupiter trojans in the Nice model. When Uranus and Neptune are near but not in a mean-motion resonance the locations where Uranus passes Neptune can circulate with a period that is in resonance with the libration periods of Neptune trojans. This results in repeated perturbations that increase the libration of existing trojans causing their orbits to become unstable.<ref name="Kortenkamp_etal_2004">{{cite journal|last1=Kortenkamp|first1=Stephen J.|last2=Malhotra|first2=Renu|last3=Michtchenko|first3=Tatiana|title=Survival of Trojan-type companions of Neptune during primordial planet migration|journal=Icarus|date=2004|volume=167|issue=2|pages=347–359|doi=10.1016/j.icarus.2003.09.021|arxiv=astro-ph/0305572|bibcode = 2004Icar..167..347K |s2cid=2046901}}</ref> This process is reversible allowing new trojans to be captured when the planetary migration continues.<ref name="Nesvorny_Vokroulicky_2009">{{cite journal|last1=Nesvorný|first1=David|last2=Vokrouhlický|first2=David|title=Chaotic Capture of Neptune Trojans|journal=The Astronomical Journal|date=2009|volume=137|issue=6|pages=5003–5011|doi=10.1088/0004-6256/137/6/5003|bibcode = 2009AJ....137.5003N |citeseerx=10.1.1.693.4387|s2cid=54186674 }}</ref> For high-inclination trojans to be captured the migration must have been slow,<ref name="Gomes_Nesvorny_2016">{{cite journal|last1=Gomes|first1=R.|last2=Nesvorny|first2=D.|title=Neptune trojan formation during planetary instability and migration|journal=Astronomy & Astrophysics|date=2016|volume=592|page=A146|doi=10.1051/0004-6361/201527757|bibcode=2016A&A...592A.146G|doi-access=free}}</ref> or their inclinations must have been acquired previously.<ref name="Parker_2015">{{cite journal|last1=Parker|first1=Alex|title=The intrinsic Neptune Trojan orbit distribution: Implications for the primordial disk and planet migration|journal=Icarus|date=2015|volume=247|pages=112–125|doi=10.1016/j.icarus.2014.09.043|arxiv=1409.6735|bibcode = 2015Icar..247..112P |s2cid=119203006}}</ref>

== Colors ==
The first four discovered Neptune trojans have similar colors.<ref name=sheppard2006/> They are modestly red, slightly redder than the gray Kuiper belt objects, but not as extremely red as the high-perihelion cold [[classical Kuiper belt object]]s.<ref name=sheppard2006/> This is similar to the colors of the blue lobe of the [[centaur (minor planet)|centaur]] color distribution, the [[Jupiter trojan]]s, the irregular satellites of the gas giants, and possibly the [[comet]]s, which is consistent with a similar origin of these populations of [[small Solar System body|small Solar System bodies]].<ref name=sheppard2006/>

The Neptune trojans are too faint to efficiently observe spectroscopically with current technology, which means that a large variety of surface compositions are compatible with the observed colors.<ref name=sheppard2006/>

Several Neptunian Trojans have been observed to have very-red colors similar to cold [[classical Kuiper belt object]]s.<ref name="Bolin2023">{{cite journal
  |title      = Keck, gemini, and palomar 200-inch visible photometry of red and very-red neptunian trojans
  |display-authors = etal
  |first1     = B. T. |last1 = Bolin
  |first2     = C. |last2 = Fremling
  |first3     = A. |last3 = Morbidelli
  |first4     = K. S. |last4 = Noll
  |first5     = J. |last5 = van Roestel
  |first6     = E. K. |last6 = Deibert
  |date       = February 2023
  |journal    = [[Monthly Notices of the Royal Astronomical Society: Letters]]
  |volume     = 521
  |issue      = 1
  |pages      = L29–L33
  |url        = https://academic.oup.com/mnrasl/article-abstract/521/1/L29/7036802
  |doi        = 10.1093/mnrasl/slad018
  |doi-access = free
 |arxiv      = 2302.04280}}</ref>

== Naming ==

In 2015, the [[International Astronomical Union|IAU]] adopted a new naming scheme for Neptune trojans, which are to be named after [[Amazons]], with no differentiation between objects in L4 and L5.<ref name="Amazons">{{cite web|url=https://www.iau.org/static/science/scientific_bodies/working_groups/97/wg-sbn-triennial-report-2015-2018.pdf|title=DIVISION F / Working Group for Small Body Nomenclature Working Group for Small Body Nomenclature. THE TRIENNIAL REPORT (2015 Sept 1 – 2018 Feb 15)|date=10 April 2018|access-date=25 August 2018|publisher=IAU|author1=Ticha, J.|display-authors=etal}}</ref> The Amazons were an all-female warrior tribe that fought in the [[Trojan War]] on the side of the Trojans against the Greeks. As of 2019, the named Neptune trojans are [[385571 Otrera]] (after [[Otrera]], the first [[Amazons|Amazonian]] queen in [[Greek mythology]]) and [[385695 Clete]] (after [[Clete (Amazon)|Clete]], an Amazon and the attendant to the Amazons' queen [[Penthesilea]], who led the Amazons in the Trojan war).<ref name="MPC-Otrera">{{cite web|title=385571 Otrera (2004 UP10)|work=Minor Planet Center|url=http://www.minorplanetcenter.net/db_search/show_object?object_id=385571|date=30 November 2015|access-date = 4 August 2017}}</ref><ref name="MPC-Clete">{{cite web|title=385695 Clete (2005 TO74)|work=Minor Planet Center|url=http://www.minorplanetcenter.net/db_search/show_object?object_id=385695|date=18 May 2019|access-date = 10 June 2019}}</ref>

== Members ==

The amount of high-inclination objects in such a small sample, in which relatively fewer high-inclination Neptune trojans are known due to observational biases,<ref name=sheppard2006/> implies that high-inclination trojans may significantly outnumber low-inclination trojans.<ref name=2008LC18potunstable/> The ratio of high- to low-inclination Neptune trojans is estimated to be about 4:1.<ref name=sheppard2006/> Assuming albedos of 0.05, there are an expected {{val|400|+250|-200}} Neptune trojans with radii above 40&nbsp;km in Neptune's {{L4|nolink=yes}}.<ref name=sheppard2006/> This would indicate that large Neptune trojans are 5 to 20 times more abundant than [[Jupiter trojan]]s, depending on their albedos.<ref name=sheppard2006/> There may be relatively fewer smaller Neptune trojans, which could be because these fragment more readily.<ref name=sheppard2006/> Large {{L5|nolink=yes}} trojans are estimated to be as common as large {{L4|nolink=yes}} trojans.<ref name=2008LC18/>

{{mpl|(612243) 2001 QR|322}} and {{mpl|2008 LC|18}} display significant dynamical instability.<ref name=2008LC18potunstable/> This means they could have been captured after planetary migration, but may as well be a long-term member that happens not to be perfectly dynamically stable.<ref name=2008LC18potunstable/>

As of September 2023, 31 Neptune trojans are known, of which 27 orbit near the [[Sun]]–[[Neptune]] {{L4}} [[Lagrangian point]] 60° ahead of Neptune,<ref name=mpctrojans/> 4 orbit near Neptune's {{L5}} region 60° behind Neptune, and one orbits on the opposite side of Neptune ({{L3}}) but frequently changes location relative to Neptune to L4 and L5.<ref name=mpctrojans/> These are listed in the following table. It is constructed from the list of Neptune trojans maintained by the [[International Astronomical Union|IAU]] [[Minor Planet Center]]<ref name=mpctrojans>{{cite web
 |title       = List Of Neptune Trojans
 |publisher   = Minor Planet Center
 |url         = http://www.minorplanetcenter.org/iau/lists/NeptuneTrojans.html
 |access-date  = 2012-08-09
 |url-status     = live
 |archive-url  = https://archive.today/20120525133119/http://www.minorplanetcenter.org/iau/lists/NeptuneTrojans.html
 |archive-date = 2012-05-25
}}</ref> and with diameters from Sheppard and Trujillo's paper on {{mpl|2008 LC|18}},<ref name=2008LC18>{{cite journal
 |last        = Sheppard
 |first       = Scott S.
 |author-link  = Scott S. Sheppard
 |author2     = Trujillo, Chadwick A.
 |title       = Detection of a Trailing (L5) Neptune Trojan
 |journal     = [[Science (journal)|Science]]
 |volume      = 329
 |issue       = 5997
 |pages       = 1304
 |publisher   = [[American Association for the Advancement of Science|AAAS]]
 |date        = 2010-08-12
 |doi         = 10.1126/science.1189666
 |pmid        = 20705814
 |bibcode     = 2010Sci...329.1304S
|s2cid = 7657932
 |doi-access= free
 }}</ref> unless otherwise noted.

=== L3 Members ===


{| class="wikitable sortable plainrowheaders" style="text-align: center; margin-right: 0;"
|-
! scope="col" | [[Astronomical naming conventions|Name]]
! scope="col" | [[Provisional designation in astronomy|Prov.<br />designation]]
! scope="col" | [[Lagrangian point|Lagrangian<br />point]]
! scope="col" | [[Perihelion|q]] ({{small|[[Astronomical unit|AU]]}})
! scope="col" | [[Aphelion|Q]] ({{small|[[Astronomical unit|AU]]}})
! scope="col" | [[Orbital eccentricity|e]]
! scope="col" | [[Inclination|i]] ([[Degree (angle)|°]])
! scope="col" | [[Absolute magnitude|Abs. mag]]
! scope="col" | [[Diameter]]{{efn|assuming an albedo of 0.05}}<br />([[Kilometre|km]])
! scope="col" | {{small|Year of<br />identification}}
! scope="col" class="unsortable" | Notes
! scope="col" class="unsortable" | [[Minor Planet Center|MPC]]
|-
! scope=row style=text-align:center colspan=2 | {{mpl|316179|2010 EN|65}}
| {{L3}} || 21.109 || 40.613 || 0.310 || 19.2 || 7.2 || {{sort|220|~220}} || 2010 || Jumping trojan  || {{MPC|316179}}
|}

=== L4 Members ===

{| class="wikitable sortable plainrowheaders" style="text-align: center; margin-right: 0;"
|-
! scope="col" | [[Astronomical naming conventions|Name]]
! scope="col" | [[Provisional designation in astronomy|Prov.<br />designation]]
! scope="col" | [[Lagrangian point|Lagrangian<br />point]]
! scope="col" | [[Perihelion|q]] ({{small|[[Astronomical unit|AU]]}})
! scope="col" | [[Aphelion|Q]] ({{small|[[Astronomical unit|AU]]}})
! scope="col" | [[Orbital eccentricity|e]]
! scope="col" | [[Inclination|i]] ([[Degree (angle)|°]])
! scope="col" | [[Absolute magnitude|Abs. mag]]
! scope="col" | [[Diameter]]{{efn|assuming an albedo of 0.05}}<br />([[Kilometre|km]])
! scope="col" | {{small|Year of<br />identification}}
! scope="col" class="unsortable" | Notes
! scope="col" class="unsortable" | [[Minor Planet Center|MPC]]
|-
! scope=row style=text-align:center | [[385571 Otrera]] ||scope=row| {{mp|2004 UP|10}}
| {{L4}} || 29.318 || 30.942 || 0.031 || 1.4 || 8.8 || {{sort|100|~100}} || 2004 || First Neptune trojan numbered and named || {{MPC|385571}}
|-
! scope=row style=text-align:center | [[385695 Clete]] ||scope=row| {{mp|2005 TO|74}}
| {{L4}} || 28.469 || 31.771 || 0.052 || 5.3 || 8.3 || {{sort|130|~130}} || 2005 || – || {{MPC|385695}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|527604|2007 VL|305}}
| {{L4}} || 28.130 || 32.028 || 0.065 || 28.1 || 8.5 || {{sort|120|~120}} || 2007 || – || {{MPC|2007+VL305}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|(530664) 2011 SO|277}}
| {{L4}} || 29.622 || 30.503 || 0.009 || 9.6 || 7.8 || {{sort|170|~170}} || 2016 || – || {{MPC|2011+SO277}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|(530930) 2011 WG|157}}
| {{L4}} || 29.064 || 30.878 || 0.025 || 22.3 || 7.3 || {{sort|210|~210}} || 2016 || – || {{MPC|2011+WG157}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|612243|2001 QR|322}}
| {{L4}} || 29.404 || 31.011 || 0.031 || 1.3 || 8.1 || {{sort|140|~140}} || 2001 || First Neptune trojan discovered, unstable Trojan
|-
! scope=row style=text-align:center colspan=2 | {{mpl|613490|2006 RJ|103}}
| {{L4}} || 29.077 || 31.014 || 0.028 || 8.2 || 7.6 || {{sort|180|~180}} || 2006 || – || {{MPC|2006+RJ103}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2005 TN|53}}
| {{L4}} || 28.092 || 32.162 || 0.067 || 25.0 || 9.0 || {{sort|090|~90}} || 2005 || First high-inclination trojan discovered<ref name=sheppard2006/> || {{MPC|2005+TN53}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|666739|2010 TS|191}}
| {{L4}} || 28.608 || 31.253 || 0.048 || 6.6 || 8.1 || {{sort|140|~140}} || 2016 || – || {{MPC|2010+TS191}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2010 TT|191}}
| {{L4}} || 27.913 || 32.189 || 0.070 || 4.3 || 7.8 || {{sort|160|~160}} || 2016 || – || {{MPC|2010+TT191}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2012 UV|177}}
| {{L4}} || 27.806 || 32.259 || 0.072 || 20.8 || 9.3 || {{sort|080|~80}}<ref name=AbsMagCon>{{cite web|url=http://www.physics.sfasu.edu/astro/asteroids/sizemagnitude.html|title=Conversion of Absolute Magnitude to Diameter|website=www.physics.sfasu.edu|access-date=29 April 2018|url-status=live|archive-url=https://web.archive.org/web/20100323180835/http://www.physics.sfasu.edu/astro/asteroids/sizemagnitude.html|archive-date=23 March 2010}}</ref> || 2014 || – || {{MPC|2012+UV177}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2012 UD|185}}
| {{L4}} || 28.794 || 31.538 || 0.042 || 28.4 || 7.6 || {{sort|180|~180}} || 2019 || – || {{MPC|2012+UD185}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2013 RL|124}}
| {{L4}} || 29.366 || 30.783 || 0.028 || 10.1 || 8.8 || {{sort|100|~100}} || 2020 || – || {{MPC|2013+RL124}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2013 RC|158}}
| {{L4}} || 28.611  || 31.784 || 0.053 || 7.5 || 8.9 || {{sort|100|~100}} || 2021 || – || {{MPC|2013+RC158}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2013 TZ|187}}
| {{L4}} || 28.092 || 32.135 || 0.066 || 13.1 || 8.2 || {{sort|140|~140}} || 2020 || – || {{MPC|2013+TZ187}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2013 TK|227}}
| {{L4}} || 27.787 || 32.683 || 0.081 || 18.6 || 9.6 || {{sort|70|~70}} || 2021 || – || {{MPC|2013+TK227}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2013 VX|30}}
| {{L4}} || 27.563 || 32.525 || 0.087 || 31.3 || 8.3 || {{sort|130|~130}} || 2018 || – || {{MPC|2013+VX30}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2014 QO|441}}
| {{L4}} || 26.961 || 33.215 || 0.101 || 18.8 || 8.3 || {{sort|130|~130}}<ref name=AbsMagCon/> || 2014 || Most eccentric stable Neptune trojan<ref>{{cite journal|title=Observation of Two New L4 Neptune Trojans in the Dark Energy Survey Supernova Fields|first1=D. W.|last1=Gerdes|first2=R. J.|last2=Jennings|first3=G. M.|last3=Bernstein|first4=M.|last4=Sako|first5=F.|last5=Adams|first6=D.|last6=Goldstein|first7=R.|last7=Kessler|first8=T.|last8=Abbott|first9=F. B.|last9=Abdalla|first10=S.|last10=Allam|first11=A.|last11=Benoit-Lévy|first12=E.|last12=Bertin|first13=D.|last13=Brooks|first14=E.|last14=Buckley-Geer|author14-link=Elizabeth Buckley-Geer|first15=D. L.|last15=Burke|first16=D.|last16=Capozzi|first17=A. Carnero|last17=Rosell|first18=M. Carrasco|last18=Kind|first19=J.|last19=Carretero|first20=C. E.|last20=Cunha|first21=C. B.|last21=D'Andrea|first22=L. N.|last22=da Costa|first23=D. L.|last23=DePoy|first24=S.|last24=Desai|first25=J. P.|last25=Dietrich|first26=P.|last26=Doel|first27=T. F.|last27=Eifler|first28=A. Fausti|last28=Neto|first29=B.|last29=Flaugher|author29-link= Brenna Flaugher |first30=J.|last30=Frieman|first31=E.|last31=Gaztanaga|first32=D.|last32=Gruen|first33=R. A.|last33=Gruendl|first34=G.|last34=Gutierrez|first35=K.|last35=Honscheid|first36=D. J.|last36=James|first37=K.|last37=Kuehn|first38=N.|last38=Kuropatkin|first39=O.|last39=Lahav|first40=T. S.|last40=Li|first41=M. A. G.|last41=Maia|first42=M.|last42=March|first43=P.|last43=Martini|first44=C. J.|last44=Miller|first45=R.|last45=Miquel|first46=R. C.|last46=Nichol|first47=B.|last47=Nord|first48=R.|last48=Ogando|first49=A. A.|last49=Plazas|first50=A. K.|last50=Romer|first51=A.|last51=Roodman|first52=E.|last52=Sanchez|first53=B.|last53=Santiago|first54=M.|last54=Schubnell|first55=I.|last55=Sevilla-Noarbe|first56=R. C.|last56=Smith|first57=M.|last57=Soares-Santos|author57-link=Marcelle Soares-Santos|first58=F.|last58=Sobreira|first59=E.|last59=Suchyta|first60=M. E. C.|last60=Swanson|first61=G.|last61=Tarlé|first62=J.|last62=Thaler|first63=A. R.|last63=Walker|first64=W.|last64=Wester|first65=Y.|last65=Zhang|date=28 January 2016|journal=The Astronomical Journal|volume=151|issue=2|pages=39|doi=10.3847/0004-6256/151/2/39|arxiv=1507.05177|bibcode=2016AJ....151...39G|s2cid=55326461 |doi-access=free }}</ref> || {{MPC|2014+QO441}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2014 QP|441}}
| {{L4}} || 28.137 || 31.971 || 0.067 || 19.4 || 9.3 || {{sort|80|~80}} || 2015 || – || {{MPC|2014+QP441}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2014 RO|74}}
| {{L4}} || 28.426 || 31.614 || 0.050 || 29.5 || 8.4 || {{sort|120|~120}} || 2020 || – || {{MPC|2014+RO74}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2014 SC|374}}
| {{L4}} || 27.038 || 33.060 || 0.096 || 33.7 || 8.2 || {{sort|140|~140}} || 2020 || – || {{MPC|2014+SC374}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2014 UU|240}}
| {{L4}} || 28.661 || 31.457 || 0.045 || 35.8 || 8.2 || {{sort|140|~140}} || 2018 || – || {{MPC|2014+UU240}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2014 YB|92}}
| {{L4}} || 27.309 || 33.243 || 0.098 || 30.8 || 8.6 || {{sort|110|~110}} || 2021 || – || {{MPC|2014+YB92}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2015 RW|277}}
| {{L4}} || 27.742 || 32.236 || 0.074 || 30.8 || 10.2 || {{sort|050|~50}} || 2018 || – || {{MPC|2015+RW277}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2015 VV|165}}
| {{L4}} || 27.513 || 32.497 || 0.086 || 16.9 || 9.0 || {{sort|090|~90}} || 2018 || – || {{MPC|2015+VV165}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2015 VW|165}}
| {{L4}} || 28.488 || 31.488 || 0.049 || 5.0 || 8.4 || {{sort|120|~120}} || 2018 || – || {{MPC|2015+VW165}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2015 VX|165}}
| {{L4}} || 27.612 || 32.327 || 0.073 || 17.2 || 9.2 || {{sort|090|~90}} || 2018 || – || {{MPC|2015+VX165}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2015 VU|207}}
| {{L4}} || 29.211 || 31.174 || 0.033 || 38.9 || 7.3 || {{sort|210|~210}} || 2021 || Highest known inclination || {{MPC|2015+VU207}}
|}

=== L5 Members ===

{| class="wikitable sortable plainrowheaders" style="text-align: center; margin-right: 0;"
|-
! scope="col" | [[Astronomical naming conventions|Name]]
! scope="col" | [[Provisional designation in astronomy|Prov.<br />designation]]
! scope="col" | [[Lagrangian point|Lagrangian<br />point]]
! scope="col" | [[Perihelion|q]] ({{small|[[Astronomical unit|AU]]}})
! scope="col" | [[Aphelion|Q]] ({{small|[[Astronomical unit|AU]]}})
! scope="col" | [[Orbital eccentricity|e]]
! scope="col" | [[Inclination|i]] ([[Degree (angle)|°]])
! scope="col" | [[Absolute magnitude|Abs. mag]]
! scope="col" | [[Diameter]]{{efn|assuming an albedo of 0.05}}<br />([[Kilometre|km]])
! scope="col" | {{small|Year of<br />identification}}
! scope="col" class="unsortable" | Notes
! scope="col" class="unsortable" | [[Minor Planet Center|MPC]]
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2004 KV|18}}
| {{L5}} || 24.553 || 35.851 || 0.183 || 13.6 || 8.7 || {{sort|110|110}} || 2011 || Temporary Neptune trojan || {{MPC|2004+KV18}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2008 LC|18}}
| {{L5}} || 27.365 || 32.479 || 0.079 || 27.6 || 8.2 || {{sort|130|~130}} || 2008 || First {{L5|nolink=yes}} trojan discovered<ref name=2008LC18/> || {{MPC|2008+LC18}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2011 HM|102}}
| {{L5}} || 27.662 || 32.455 || 0.083 || 29.4 || 8.1 || {{sort|130|~130}} || 2012 || – || {{MPC|2011+HM102}}
|-
! scope=row style=text-align:center colspan=2 | {{mpl|2013 KY|18}}
| {{L5}} || 26.624 || 34.084 || 0.124 || 6.6 || 6.8 || {{sort|260|~260}} || 2016 || Stability uncertain || {{MPC|2013+KY18}}
|}


{{mpl|(613100) 2005 TN|74}}<ref name=MPC05T74N>[http://www.minorplanetcenter.net/iau/mpec/K05/K05U97.html MPEC 2005-U97 : 2005 TN74, 2005 TO74] Minor Planet Center</ref> and {{mpl|(309239) 2007 RW|10}}<ref name="EKOS55">{{cite web | title=Distant EKOs, 55 | url=http://www.boulder.swri.edu/ekonews/issues/past/n055/html/index.html | access-date=2012-07-24 | url-status=live | archive-url=https://web.archive.org/web/20130525030402/http://www.boulder.swri.edu/ekonews/issues/past/n055/html/index.html | archive-date=2013-05-25 }}</ref> were thought to be Neptune trojans at the time of their discovery, but further observations have disconfirmed their membership. {{mpl|2005 TN|74}} is currently thought to be in a 3:5 [[Resonant trans-Neptunian object|resonance]] with Neptune.<ref name=Buie05TN74>{{cite web|url=http://www.boulder.swri.edu/~buie/kbo/astrom/05TN74.html|title=Orbit and Astrometry for 05TN74|website=www.boulder.swri.edu|access-date=29 April 2018|url-status=live|archive-url=https://web.archive.org/web/20180429165723/http://www.boulder.swri.edu/~buie/kbo/astrom/05TN74.html|archive-date=29 April 2018}}</ref> {{mp|(309239) 2007 RW|10}} is currently following a quasi-satellite loop around Neptune.<ref name="quasi">{{cite journal |author=de la Fuente Marcos |author2=de la Fuente Marcos |title=(309239) 2007 RW10: a large temporary quasi-satellite of Neptune |journal=Astronomy and Astrophysics Letters |volume=545 |pages=L9 |date=2012 |doi=10.1051/0004-6361/201219931 |arxiv=1209.1577 |bibcode=2012A&A...545L...9D|s2cid=118374080 }}</ref>

== See also ==
*[[Nice model]]
*[[Nice 2 model]]
*{{mpl|(309239) 2007 RW|10}}, a temporary [[quasi-satellite]] of [[Neptune]].

== Notes ==
{{notelist}}

== References ==
{{reflist|30em}}

== External links ==
* {{cite journal |first1=J. |last1=Horner |first2=P. S. |last2=Lykawka |title=Planetary Trojans – the main source of short period comets? |journal=[[International Journal of Astrobiology]] |volume=9 |year=2010 |issue=4 |pages=227–234 |doi=10.1017/S1473550410000212 |arxiv=1007.2541 |bibcode = 2010IJAsB...9..227H |s2cid=53982616 }}
* {{cite web|url=https://www.newscientist.com/article/dn9340-new-trojan-asteroid-hints-at-huge-neptunian-cloud.html|title=New Trojan asteroid hints at huge Neptunian cloud|publisher=New Scientist}}

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