View source for List of possible dwarf planets

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{{Use dmy dates|date=April 2020}}
[[File:Trans-Neptunians_Size_Albedo_Color.svg|thumb|upright=2|Comparison of sizes, albedo, and colors of various large trans-Neptunian objects with diameters greater than {{cvt|700|km|mi}}. The dark colored arcs represent uncertainties of the object's size.]]

The number of [[dwarf planet]]s in the [[Solar System]] is unknown. Estimates have run as high as 200 in the [[Kuiper belt]]<ref name=Brown>{{cite web|url=http://web.gps.caltech.edu/~mbrown/dwarfplanets/|author=Mike Brown|title=The Dwarf Planets|access-date=2008-01-20|author-link=Michael E. Brown}}</ref> and over 10,000 in the region beyond.<ref name=Stern2012>{{Cite web |url=http://pluto.jhuapl.edu/News-Center/PI-Perspectives.php?page=piPerspective_08_24_2012 |title=The Kuiper Belt at 20: Paradigm Changes in Our Knowledge of the Solar System |date=24 August 2012 |last1=Stern |first1=Alan |author-link=Alan Stern |website=[[Applied Physics Laboratory]] |quote=Today we know of more than a dozen dwarf planets in the solar system [and] it is estimated that the ultimate number of dwarf planets we will discover in the Kuiper Belt and beyond may well exceed 10,000.}}</ref>
However, consideration of the surprisingly low densities of many large trans-Neptunian objects, as well as spectroscopic analysis of their surfaces, suggests that the number of dwarf planets may be much lower, perhaps only nine among bodies known so far.<ref name="Grundy2019">{{cite journal |last1=Grundy |first1=W.M. |last2=Noll |first2=K.S. |last3=Buie |first3=M.W. |last4=Benecchi |first4=S.D. |last5=Ragozzine |first5=D. |last6=Roe |first6=H.G. |title=The mutual orbit, mass, and density of transneptunian binary Gǃkúnǁʼhòmdímà ({{mp|(229762) 2007 UK|126}}) |journal=Icarus |date=December 2019 |volume=334 |pages=30–38 |doi=10.1016/j.icarus.2018.12.037 |bibcode=2019Icar..334...30G |s2cid=126574999 |url=http://www2.lowell.edu/users/grundy/abstracts/preprints/2019.G-G.pdf |url-status=live |archive-url=https://web.archive.org/web/20190407045339/http://www2.lowell.edu/~grundy/abstracts/preprints/2019.G-G.pdf |archive-date=2019-04-07 }}</ref><ref name=JWST/> The [[International Astronomical Union]] (IAU) defines dwarf planets as being in [[hydrostatic equilibrium]], and notes six bodies in particular: {{dp|Ceres}} in the [[Solar System#Inner Solar System|inner Solar System]] and five in the trans-Neptunian region: {{dp|Pluto}}, {{dp|Eris}}, {{dp|Haumea}}, {{dp|Makemake}}, and {{dp|Quaoar}}.<ref>Accepted in a 2022–2023 annual report</ref> Only Pluto and Ceres have been confirmed to be in hydrostatic equilibrium, due to the results of the ''[[New Horizons]]'' and ''[[Dawn (spacecraft)|Dawn]]'' missions.<ref>{{cite web | url=https://www.nasa.gov/feature/jpl/what-s-inside-ceres-new-findings-from-gravity-data | title=What's Inside Ceres? New Findings from Gravity Data | date=2 August 2016 }}</ref> Eris is generally assumed to be a dwarf planet because it is similar in size to Pluto and even more massive. Haumea and Makemake were accepted as dwarf planets by the IAU for naming purposes and will keep their names if it turns out they are not dwarf planets. Smaller trans-Neptunian objects have been called dwarf planets if they appear to be solid bodies, which is a prerequisite for hydrostatic equilibrium: planetologists generally include at least {{dp|Gonggong}}, {{dp|Orcus}}, and {{dp|Sedna}}. Quaoar was labelled as a dwarf planet in a 2022–2023 annual report, though it does not appear to be in hydrostatic equilibrium. In practice the requirement for hydrostatic equilibrium is often loosened to include all gravitationally rounded objects, even by the IAU, as otherwise [[Mercury (planet)|Mercury]] would not be a planet.{{cn|date=May 2025}}

== Limiting values ==
[[Image:Ixion-Spitzer2007.gif|thumb|upright|Calculation of the diameter of [[28978 Ixion|Ixion]] depends on the [[Albedo#Astronomical albedo|albedo]] (the fraction of light that it reflects). Current estimates are that the albedo is 13–15%, a bit under the midpoint of the range shown here and corresponding to a diameter of 620 km.]]

Beside directly orbiting the Sun, the qualifying feature of a dwarf planet is that it have "sufficient mass for its self-gravity to overcome [[rigid body|rigid-body]] forces so that it assumes a [[hydrostatic equilibrium]] ([[ellipsoid|nearly round]]) shape".<ref name=iau2006>{{cite web |website=[[International Astronomical Union]] |title=IAU 2006 General Assembly: Result of the IAU Resolution votes |url=http://www.iau.org/iau0603.414.0.html |date=24 August 2006 |access-date=2008-01-26 |url-status=dead |archive-url=https://web.archive.org/web/20070103145836/http://www.iau.org/iau0603.414.0.html |archive-date=2007-01-03 |df=dmy-all}}</ref><ref>{{cite web|url=http://solarsystem.nasa.gov/planets/profile.cfm?Object=Dwarf&Display=OverviewLong |title=Dwarf Planets |website=[[NASA]] |access-date=2008-01-22 |archive-url=https://web.archive.org/web/20120723014035/http://solarsystem.nasa.gov/planets/profile.cfm?Object=Dwarf&Display=OverviewLong |archive-date=2012-07-23 |url-status=dead |df=dmy-all}}</ref><ref name=iau2008>{{cite press release |url=http://www.iau.org/public_press/news/release/iau0804 |title=Plutoid chosen as name for Solar System objects like Pluto |date=11 June 2008 |access-date=2008-06-15 |archive-url=https://web.archive.org/web/20110702012327/http://iau.org/public_press/news/detail/iau0804 |archive-date=2011-07-02 |url-status=dead |df=dmy-all}}</ref> Current observations are generally insufficient for a direct determination as to whether a body meets this definition. Often the only clues for trans-Neptunian objects (TNO) is a crude estimate of their diameters and albedos. Icy satellites as large as 1,500&nbsp;km in diameter have proven to not be in equilibrium, whereas dark objects in the outer solar system often have low densities that imply they are not even solid bodies, much less gravitationally controlled dwarf planets.

{{dp|Ceres}}, which has a significant amount of ice in its composition, is the only accepted dwarf planet in the [[asteroid belt]], though there are unexplained anomalies.<ref name=Vernazza2019>{{cite journal |title=A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea |url=https://www.eso.org/public/archives/releases/sciencepapers/eso1918/eso1918a.pdf |display-authors=etal |last1=Vernazza |first1=P. |last2=Jorda |first2=L. |last3=Ševeček |first3=P. |last4=Brož |first4=M. |last5=Viikinkoski |first5=M. |last6=Hanuš |first6=J. |journal=Nature Astronomy |volume=273 |issue=2 |pages=136–141 |doi=10.1038/s41550-019-0915-8 |hdl=10045/103308 |access-date=2019-10-28|year=2020 |bibcode=2020NatAs...4..136V |s2cid=209938346 |hdl-access=free}}</ref> [[4 Vesta]], the second-most-massive asteroid and one that is basaltic in composition, appears to have a fully differentiated interior and was therefore in equilibrium at some point in its history, but no longer is today.<ref name="Hubble">{{cite press release
  |author1=Savage, Don
  |author2=Jones, Tammy
  |author3= Villard, Ray
  |date=1995-04-19 |title=Asteroid or mini-planet? Hubble maps the ancient surface of Vesta
  |id= News Release STScI-1995-20
  |website=[[HubbleSite]]
  |url=http://hubblesite.org/newscenter/archive/releases/1995/20/image/c
  |access-date=2006-10-17 |df=dmy-all}}</ref> The third-most massive object, [[2 Pallas]], has a somewhat irregular surface and is thought to have only a partially differentiated interior; it is also less icy than Ceres. [[Michael E. Brown|Michael Brown]] has estimated that, because rocky objects such as Vesta are more rigid than icy objects, rocky objects below {{convert|900|km|mi}} in diameter may not be in hydrostatic equilibrium and thus not dwarf planets.<ref name=Brown /> The two largest icy outer-belt asteroids [[10 Hygiea]] and [[704 Interamnia]] are close to equilibrium, but in Hygiea's case this may be a result of its disruption and the re-aggregation of its fragments, while Interamnia is now somewhat away from equilibrium due to impacts.<ref name=Vernazza2019/><ref>{{cite journal|arxiv=1911.13049|doi=10.1051/0004-6361/201936639|title=(704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body|year=2020|last1=Hanuš|first1=J.|last2=Vernazza|first2=P.|last3=Viikinkoski|first3=M.|last4=Ferrais|first4=M.|last5=Rambaux|first5=N.|last6=Podlewska-Gaca|first6=E.|last7=Drouard|first7=A.|last8=Jorda|first8=L.|last9=Jehin|first9=E.|last10=Carry|first10=B.|last11=Marsset|first11=M.|last12=Marchis|first12=F.|last13=Warner|first13=B.|last14=Behrend|first14=R.|last15=Asenjo|first15=V.|last16=Berger|first16=N.|last17=Bronikowska|first17=M.|last18=Brothers|first18=T.|last19=Charbonnel|first19=S.|last20=Colazo|first20=C.|last21=Coliac|first21=J.-F.|last22=Duffard|first22=R.|last23=Jones|first23=A.|last24=Leroy|first24=A.|last25=Marciniak|first25=A.|last26=Melia|first26=R.|last27=Molina|first27=D.|last28=Nadolny|first28=J.|last29=Person|first29=M.|last30=Pejcha|first30=O.|s2cid=208512707|journal=Astronomy & Astrophysics|volume=633|pages=A65|bibcode=2020A&A...633A..65H|display-authors=29}}</ref>

Based on a comparison with the icy moons that have been visited by spacecraft, such as [[Mimas (moon)|Mimas]] (round at 400&nbsp;km in diameter) and [[Proteus (moon)|Proteus]] (irregular at 410–440&nbsp;km in diameter), Brown estimated that an icy body relaxes into hydrostatic equilibrium at a diameter somewhere between 200 and 400&nbsp;km.<ref name=Brown /> However, after Brown and Tancredi made their calculations, better determination of their shapes showed that Mimas and the other mid-sized ellipsoidal [[moons of Saturn]] up to at least [[Iapetus (moon)|Iapetus]] (which, at 1,471&nbsp;km in diameter, is approximately the same size as Haumea and Makemake) are no longer in hydrostatic equilibrium; they are also icier than TNOs are likely to be. They have equilibrium shapes that froze in place some time ago, and do not match the shapes that equilibrium bodies would have at their current rotation rates.<ref>{{cite web |url=http://www.planetary.org/blogs/emily-lakdawalla/2012/3389.html |title=Iapetus' peerless equatorial ridge |website=www.planetary.org |access-date=2 April 2018}}</ref> Thus [[Rhea (moon)|Rhea]], at 1528&nbsp;km in diameter, is the smallest body for which gravitational measurements are consistent with current hydrostatic equilibrium. Ceres, at 950&nbsp;km in diameter, is close to equilibrium, but some deviations from equilibrium shape remain unexplained.<ref name=EPSC>{{cite book|chapter-url=https://meetingorganizer.copernicus.org/EPSC2018/EPSC2018-645-1.pdf|display-authors=4|author1=Raymond, C.|author2=Castillo-Rogez, J.C.|author3=Park, R.S.|author4=Ermakov, A.|author5=Bland, M.T.|author6=Marchi, S.|author7=Prettyman, T.|author8=Ammannito, E.|author9=De Sanctis, M.C.|author10=Russell, C.T.|date=September 2018|chapter=Dawn Data Reveal Ceres' Complex Crustal Evolution|title=European Planetary Science Congress|volume=12|access-date=19 July 2020|archive-date=30 January 2020|archive-url=https://web.archive.org/web/20200130111631/https://meetingorganizer.copernicus.org/EPSC2018/EPSC2018-645-1.pdf|url-status=live}}</ref> Much larger objects, such as Earth's moon and the planet Mercury, are not near hydrostatic equilibrium today,<ref>{{cite journal |author1=Garrick |author2=Bethell |display-authors=etal |year=2014 |title=The tidal-rotational shape of the Moon and evidence for polar wander |journal=Nature |volume=512 |issue=7513 |pages=181–184|doi=10.1038/nature13639 |pmid=25079322 |bibcode=2014Natur.512..181G |s2cid=4452886 |url=https://escholarship.org/uc/item/0012r6g6 }}</ref><ref>{{cite book |via=Google Books |chapter-url=https://books.google.com/books?id=QzXZs_xSLk4C&q=Hydrostatic+equilibrium+mercury&pg=PA23 |title=Mercury |chapter=Hydrostatic equilibrium of Mercury|page=23|isbn = 9780387775395|last1 = Balogh|first1 = A.|last2 = Ksanfomality|first2 = Leonid|last3 = Steiger|first3 = Rudolf von|publisher = Springer Science & Business Media|date = 23 February 2008}}</ref><ref>{{cite journal|title=The low-degree shape of Mercury|display-authors=etal|first1=Mark E.|last1=Perry|first2=Gregory A.|last2=Neumann|first3=Roger J.|last3=Phillips|first4=Olivier S.|last4=Barnouin|first5=Carolyn M.|last5=Ernst|first6=Daniel S.|last6=Kahan|journal=Geophysical Research Letters|volume=42|issue=17|pages=6951–6958|date=September 2015|doi-access=free|doi=10.1002/2015GL065101|bibcode=2015GeoRL..42.6951P|s2cid=103269458}}</ref> though the Moon is composed primarily of silicate rock and Mercury of metal (in contrast to most dwarf planet candidates, which are ice and rock). Saturn's moons may have been subject to a thermal history that would have produced equilibrium-like shapes in bodies too small for gravity alone to do so. Thus, at present it is unknown whether any trans-Neptunian objects smaller than Pluto and Eris are in hydrostatic equilibrium.<ref name="Grundy2019"/> Nonetheless, it does not matter in practice, because the precise statement of hydrostatic equilibrium in the definition is universally ignored in favour of roundness and solidity.<ref name=Grundy2019/><ref name=plutokiller/>

The majority of mid-sized TNOs up to about {{Val|900|-|1000|u=km}} in diameter have significantly lower densities (~&nbsp;{{Val|1.0|-|1.2|u=g|up=ml}}) than larger bodies such as Pluto (1.86&nbsp;g/cm<sup>3</sup>). Brown had speculated that this was due to their composition, that they were almost entirely icy. However, Grundy et al.<ref name="Grundy2019"/> point out that there is no known mechanism or evolutionary pathway for mid-sized bodies to be icy while both larger and smaller objects are partially rocky. They demonstrated that at the prevailing temperatures of the Kuiper Belt, water ice is strong enough to support open interior spaces (interstices) in objects of this size; they concluded that mid-size TNOs have low densities for the same reason that smaller objects do—because they have not compacted under self-gravity into fully solid objects, and thus the typical TNO smaller than {{Val|900|-|1000|u=km}} in diameter is (pending some other formative mechanism) unlikely to be a dwarf planet.

=== <span id="Probable per Tancredi"></span>Assessment by Tancredi ===
In 2010, [[Gonzalo Tancredi]] presented a report to the IAU evaluating a list of 46 trans-Neptunian candidates for dwarf planet status based on [[light curve|light-curve]]-amplitude analysis and a calculation that the object was more than {{convert|450|km|mi}} in diameter. Some diameters were measured, some were best-fit estimates, and others used an assumed albedo of 0.10 to calculate the diameter. Of these, he identified 15 as dwarf planets by his criteria (including the 4 accepted by the IAU), with another 9 being considered possible. To be cautious, he advised the IAU to "officially" accept as dwarf planets the top three: Sedna, Orcus, and Quaoar.<ref name="tancredi-2010"/> Although the IAU had anticipated Tancredi's recommendations, by late 2023 only Quaoar had been accepted.{{Citation needed|date=May 2025}}

=== <span id="Probable per Brown"></span>Assessment by Brown ===
{| class="wikitable floatright" style="font-size: 0.9em; text-align: center; width: 350px; margin-top: 4px;"
! Brown's categories
! Min. {{big|[[Diameter|⌀]]}}
! Number of objects
|- style="background: #e0e0ff;"
| Nearly certain
| >&nbsp;900&nbsp;km
| 10
|- style="background: #e0ffff;"
| Highly likely
| 600–900&nbsp;km
| 17 (27 total)
|- style="background: #d0ffd0;"
| Likely
| 500–600&nbsp;km
| 41 (68 total)
|- style="background: #ffffd0;"
| Probably
| 400–500&nbsp;km
| 62 (130 total)
|- style="background: #ffe0c0;"
| Possibly
| 200–400&nbsp;km
| 611 (741 total)
|-
! colspan=3 style="text-align: left; font-size: 0.92em; font-weight: normal; padding: 6px 2px 4px 4px;" |''Source'': [[Michael E. Brown|Mike Brown]],<ref name="brown-list"/> as of October 22, 2020
|}

[[Michael E. Brown|Mike Brown]] considers 130<!--as of 22 October 2020, but these numbers haven't changed since 13 September 2019, and are only updated once or twice a year--> trans-Neptunian bodies to be "probably" dwarf planets, ranked them by estimated size.<ref name="brown-list"/> He does not consider asteroids, stating "in the asteroid belt Ceres, with a diameter of 900 km, is the only object large enough to be round."<ref name="brown-list"/>

The terms for varying degrees of likelihood he split these into:

*''Near certainty'': diameter estimated/measured to be over {{convert|900|km|mi}}. Sufficient confidence to say these must be in hydrostatic equilibrium, even if predominantly rocky. 10 objects as of 2020. 
*''Highly likely'': diameter estimated/measured to be over {{convert|600|km|mi}}. The size would have to be "grossly in error" or they would have to be primarily rocky to not be dwarf planets. 17 objects as of 2020. 
*''Likely'': diameter estimated/measured to be over {{convert|500|km|mi}}. Uncertainties in measurement mean that some of these will be significantly smaller and thus doubtful. 41 objects as of 2020. 
*''Probably'': diameter estimated/measured to be over {{convert|400|km|mi}}. Expected to be dwarf planets, if they are icy, and that figure is correct. 62 objects as of 2020. 
*''Possibly'': diameter estimated/measured to be over {{convert|200|km|mi}}. Icy moons transition from a round to irregular shape in the 200–400&nbsp;km range, suggesting that the same figure holds true for [[Kuiper belt|KBOs]]. Thus, some of these objects could be dwarf planets. 611 objects as of 2020. 
*''Probably not'': diameter estimated/measured to be under 200&nbsp;km. No icy moon under 200&nbsp;km is round, and the same may be true of KBOs. The estimated size of these objects would have to be in error for them to be dwarf planets.

Beside the five older accepted by the IAU plus Quaoar, the 'nearly certain' category includes {{dp|Gonggong}}, {{dp|Sedna}}, {{dp|Orcus}}, [[307261 Máni|Máni]], and {{dp|Salacia}}. Note that although Brown's site claims to be updated daily, these largest objects haven't been updated since late 2013, and indeed the current best diameter estimates for Salacia and Máni are less than 900&nbsp;km. (Orcus is just above the threshold.)<ref>[https://web.archive.org/web/20131113235927/http://www.gps.caltech.edu/~mbrown/dps.html How many dwarf planets are there in the outer solar system? (updates daily)], updated 2013-11-01</ref>

=== Assessment by Grundy et al. ===
[[File:TNO diameter-density plot - Rommel et al. 2025 Fig 1.jpg|thumb|upright=1.5|TNO densities (vertical axis) plotted by increasing diameter (horizontal axis). As the diameter of TNOs increase, their density increases as well. Salacia's density is now thought to be higher, closer to that of Orcus.]]
Grundy et al. propose that dark, low-density TNOs in the size range of approximately {{Val|400|-|1000|u=km}} are transitional between smaller, porous (and thus low-density) bodies and larger, denser, brighter, and geologically differentiated planetary bodies (such as dwarf planets). Bodies in this size range should have begun to collapse the interstitial spaces left over from their formation, but not fully, leaving some residual porosity.<ref name="Grundy2019" />

Many TNOs in the size range of about {{Val|400|-|1,000|u=km}} have oddly low densities, in the range of about {{Val|1.0|-|1.2|u=g/cm3}}, that are substantially less than those of dwarf planets such as Pluto, Eris and Ceres, which have densities closer to 2. Brown has suggested that large low-density bodies must be composed almost entirely of water ice since he presumed that bodies of this size would necessarily be solid. However, this leaves unexplained why TNOs both larger than 1,000&nbsp;km and smaller than 400&nbsp;km, and indeed comets, are composed of a substantial fraction of rock, leaving only this size range to be primarily icy. Experiments with water ice at the relevant pressures and temperatures suggest that substantial porosity could remain in this size range, and it is possible that adding rock to the mix would further increase resistance to collapsing into a solid body. Bodies with internal porosity remaining from their formation could be at best only partially differentiated, in their deep interiors (if a body had begun to collapse into a solid body, there should be evidence in the form of fault systems from when its surface contracted). The higher albedos of larger bodies are also evidence of full differentiation, as such bodies were presumably resurfaced with ice from their interiors. Grundy ''et al''.<ref name="Grundy2019"/> propose therefore that mid-size (<&nbsp;1,000&nbsp;km), low-density (<&nbsp;1.4 g/cm<sup>3</sup>) and low-albedo (<&nbsp;~0.2) bodies such as [[120347 Salacia|Salacia]], [[174567 Varda|Varda]], [[229762 Gǃkúnǁʼhòmdímà|Gǃkúnǁʼhòmdímà]], and {{mpl|55637|2002 UX|25}} are not differentiated planetary bodies like [[90482 Orcus|Orcus]], [[50000 Quaoar|Quaoar]], and [[Charon (moon)|Charon]]. The boundary between the two populations would appear to be in the range of about {{Val|900|-|1000|u=km}}, although Grundy et al. also suggest that {{val|600|-|700|u=km}} might constitute an upper limit to retaining significant porosity.<ref name="Grundy2019"/>

If Grundy et al.<ref name="Grundy2019"/> are correct, then very few known bodies in the outer Solar System are likely to have compacted into fully solid bodies, and thus to possibly have become dwarf planets at some point in their past or to still be dwarf planets at present. Pluto–Charon, Eris, Haumea, Gonggong, Makemake, Quaoar, and Sedna are either known (Pluto) or strong candidates (the others). Orcus is again just above the threshold by size, though it is bright.

There are a number of smaller bodies, estimated to be between 700 and 900&nbsp;km in diameter, for most of which not enough is known to apply these criteria. All of them are dark, mostly with albedos under 0.11, with brighter {{mpl|2013 FY|27}} (0.18) an exception; this suggests that they are not dwarf planets. However, Salacia and Varda may be dense enough to at least be solid. If Salacia were spherical and had the same albedo as its moon, it would have a density of between 1.4 and 1.6 g/cm<sup>3</sup>, calculated a few months after Grundy et al.'s initial assessment, though still an albedo of only 0.04.<ref name="Grundy2019-2">{{cite journal |last1=Grundy |first1=W.M. |last2=Noll |first2=K.S. |last3=Roe |first3=H.G. |last4=Buie |first4=M.W. |last5=Porter |first5=S.B. |last6=Parker |first6=A.H. |last7=Nesvorný |first7=D. |last8=Levison |first8=H.F. |last9=Benecchi |first9=S.D. |last10=Stephens |first10=D.C. |last11=Trujillo |first11=C.A. |display-authors=6 |title=Mutual orbit orientations of transneptunian binaries |journal=Icarus |date=December 2019 |volume=334 |pages=62–78 |doi=10.1016/j.icarus.2019.03.035 |bibcode=2019Icar..334...62G |s2cid=133585837 |url=http://www2.lowell.edu/~grundy/abstracts/preprints/2019.TNB_orbits.pdf |url-status=dead |archive-url=https://web.archive.org/web/20190407052940/http://www2.lowell.edu/~grundy/abstracts/preprints/2019.TNB_orbits.pdf |archive-date=2019-04-07 |df=dmy-all}}</ref> Varda might have a higher density of 1.78±0.06 g/cm<sup>3</sup> (a lower density of 1.23±0.04 g/cm<sup>3</sup> was considered possible though less probable), published the year after Grundy et al.'s initial assessment;<ref name="Souami2020">{{cite journal
  |display-authors = etal
  |first1     = D. |last1 = Souami
  |first2     = F. |last2 = Braga-Ribas
  |first3     = B. |last3 = Sicardy
  |first4     = B. |last4 = Morgado
  |first5     = J. L. |last5 = Ortiz
  |first6     = J. |last6 = Desmars
  |date       = August 2020
  |title      = A multi-chord stellar occultation by the large trans-Neptunian object (174567) Varda
  |journal = Astronomy & Astrophysics |volume = 643 |pages = A125 |doi = 10.1051/0004-6361/202038526 |arxiv     = 2008.04818
  |bibcode = 2020A&A...643A.125S |s2cid = 221095753 }}</ref> its albedo of 0.10 is close to Quaoar's.

=== Assessment by Emery et al. ===
In 2023, Emery et al. wrote that [[near-infrared]] [[spectroscopy]] by the [[James Webb Space Telescope]] (JWST) in 2022 suggests that Sedna, Gonggong and Quaoar internally melted and differentiated and are chemically evolved, like the larger dwarf planets Pluto, Eris, Haumea, and Makemake, but unlike "all smaller KBOs". This is because light hydrocarbons are present on their surfaces (e.g. [[ethane]], [[acetylene]], and [[ethylene]]), which implies that methane is continuously being resupplied, and that methane would likely come from internal geochemistry. On the other hand, the surfaces of Sedna, Gonggong and Quaoar have low abundances of CO and CO<sub>2</sub>, similar to Pluto, Eris and Makemake but in contrast to smaller bodies. This suggests that the threshold for dwarf planethood in the trans-Neptunian region is a diameter of ~1000&nbsp;km (thus including only Pluto, Eris, Haumea, Makemake, Gonggong, Quaoar and possibly Sedna).<ref name=JWST>{{cite journal|last1=Emery|first1=J. P. |first2=I. |last2=Wong |first3=R. |last3=Brunetto |first4=J. C. |last4=Cook |first5=N. |last5=Pinilla-Alonso |first6=J. A. |last6=Stansberry |first7=B. J. |last7=Holler |first8=W. M. |last8=Grundy |first9=S. |last9=Protopapa |first10=A. C. |last10=Souza-Feliciano |first11=E. |last11=Fernández-Valenzuela |first12=J. I. |last12=Lunine |first13=D. C. |last13=Hines |author-link=|date=2024|title=A Tale of 3 Dwarf Planets: Ices and Organics on Sedna, Gonggong, and Quaoar from JWST Spectroscopy|journal=Icarus |volume=414 |doi=10.1016/j.icarus.2024.116017 |arxiv=2309.15230|bibcode=2024Icar..41416017E }}</ref>

== <span id="list"></span>Likeliest dwarf planets ==
The assessments of the IAU, Tancredi et al., Brown, and Grundy et al. for some of potential dwarf planets are as follows. For the IAU, the acceptance criteria were for naming purposes; Quaoar was called a dwarf planet in a 2022–2023 IAU annual report.<ref name=report>{{cite report |title=Report of Division F "Planetary Systems and Astrobiology" Annual Report 2022-23 |date=2022–2023 |publisher=International Astronomical Union |archive-date=8 December 2023 |archive-url=https://web.archive.org/web/20231208112824/https://www.iau.org/static/science/scientific_bodies/divisions/f/division-f-annual-report-2022-2023.pdf |access-date=16 May 2025 |url=https://www.iau.org/static/science/scientific_bodies/divisions/f/division-f-annual-report-2022-2023.pdf}}</ref> An IAU question-and-answer press release from 2006 was more specific: it estimated that objects with mass above {{val|5|e=20|u=kg}} and [[List of Solar System objects by size#Larger than 400 km|diameter greater than 800&nbsp;km]] (800&nbsp;km across) would "normally" be in hydrostatic equilibrium ("the shape ... would normally be determined by self-gravity"), but that "all borderline cases would need to be determined by observation."<ref name="Q&A">{{cite web |title='Planet Definition' Questions & Answers Sheet |url=https://www.iau.org/static/archives/releases/doc/iau0601_q_answers.doc |publisher=International Astronomical Union |date=August 24, 2006 |access-date=October 16, 2021}}</ref> This is close to Grundy et al.'s suggestion for the approximate limit.

Several of these objects had not yet been discovered when Tancredi et al. did their analysis. Brown's sole criterion is diameter; he accepts significantly many more as "highly likely" to be dwarf planets, for which his threshold is 600&nbsp;km (see below). Grundy et al. did not determine which bodies were dwarf planets, but rather which could not be. A red [[Image:X mark.svg|15px|No]] marks objects that are not dense enough to be solid bodies; to this is added a question mark for the objects whose densities are not known (they are all dark, suggesting that they are not dwarf planets). Emery et al. suggest that Sedna, Quaoar, and Gonggong went through internal melting, differentiation, and chemical evolution like the larger dwarf planets, but that all smaller KBOs did not.<ref name=JWST/> The question of current equilibrium was not addressed; nonetheless, it is not generally taken seriously despite being in the definition. (Mercury is round but known to be out of equilibrium;<ref name="Mercury">Sean Solomon, Larry Nittler & Brian Anderson, eds. (2018) ''Mercury: The View after MESSENGER''. Cambridge Planetary Science series no. 21, Cambridge University Press. Chapter 3.</ref> it is universally considered as a planet according to the intent of the IAU and geophysical definitions, rather than to the letter.)<ref name=plutokiller>{{Cite tweet |user=plutokiller |last=Brown |first=Mike |number=1624127764969459713 |title=The real answer here is to not get too hung up on definitions, which I admit is hard when the IAU tries to make them sound official and clear, but, really, we all understand the intent of the hydrostatic equilibrium point, and the intent is clearly to include Merucry & the moon}}</ref> This would be relevant for Quaoar, as in 2024, Kiss et al. found that Quaoar has an ellipsoidal shape incompatible with hydrostatic equilibrium for its current spin. They hypothesised that Quaoar originally had a rapid rotation and was in hydrostatic equilibrium, but that its shape became "frozen in" and did not change as it spun down due to tidal forces from its moon [[Weywot]].<ref name="Kiss2024">{{cite journal
 |display-authors = etal
 |first1 = C. |last1 = Kiss
 |first2 = T. G. |last2 = Müller
 |first3 = G. |last3 = Marton
 |first4 = R. |last4 = Szakáts
 |first5 = A. |last5 = Pál
 |first6 = L. |last6 = Molnár
 |title      = The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
 |journal    = Astronomy & Astrophysics
 |date       = March 2024
 |volume     = 684
 |issue      = 
 |pages = A50 |doi        = 10.1051/0004-6361/202348054
 |arxiv      = 2401.12679
 |bibcode    = 2024A&A...684A..50K}}</ref> If so, this would resemble the situation of Saturn's moon [[Iapetus (moon)|Iapetus]], which is too oblate for its current spin.<ref name="Science News">Cowen, R. (2007). Idiosyncratic Iapetus, ''Science News'' vol. 172, pp. 104–106. [http://www.sciencenews.org/articles/20070818/bob8ref.asp references] {{Webarchive|url=https://web.archive.org/web/20071013165655/http://www.sciencenews.org/articles/20070818/bob8ref.asp |date=2007-10-13 }}</ref><ref name="Thomas2010">{{cite journal| doi = 10.1016/j.icarus.2010.01.025| last1 = Thomas| first1 = P. C.| date = July 2010| title = Sizes, shapes, and derived properties of the saturnian satellites after the Cassini nominal mission| journal = Icarus| volume = 208| issue = 1| pages = 395–401| url = http://www.ciclops.org/media/sp/2011/6794_16344_0.pdf| bibcode = 2010Icar..208..395T| access-date = 2015-09-25| archive-date = 2018-12-23| archive-url = https://web.archive.org/web/20181223003125/http://www.ciclops.org/media/sp/2011/6794_16344_0.pdf| url-status = dead}}</ref> Iapetus is generally still considered a [[planetary-mass moon]] nonetheless,<ref name=planetarysociety>Emily Lakdawalla et al., [https://www.planetary.org/worlds/what-is-a-planet What Is A Planet?] {{Webarchive|url=https://web.archive.org/web/20220122142140/https://www.planetary.org/worlds/what-is-a-planet |date=2022-01-22 }} The Planetary Society, 21 April 2020</ref> though not always.<ref name=ChenKipping>{{cite journal |last1=Chen |first1=Jingjing |last2=Kipping |first2=David |date=2016 |title=Probabilistic Forecasting of the Masses and Radii of Other Worlds |journal=The Astrophysical Journal |volume=834 |issue=1 |page=17 |doi= 10.3847/1538-4357/834/1/17|arxiv=1603.08614 |s2cid=119114880 |doi-access=free |bibcode=2017ApJ...834...17C }}</ref>

Two moons are included for comparison: Triton likely formed as a TNO before it was [[Capture of Triton|captured by Neptune]], and Charon is larger than some dwarf planet candidates.
{| class="wikitable sortable" style="text-align: center;"
|-
! rowspan="2" data-sort-type="number"| [[Minor-planet designation|Designation]]
! rowspan="2" data-sort-type="number"| Measured mean<br />[[diameter]] {{small|([[kilometre|km]])}}
! rowspan="2" data-sort-type="number"| [[Density]]<br />{{small|(g/cm<sup>3</sup>)}}
! rowspan="2" data-sort-type="number"| [[Albedo]]

! colspan="3" scope="col" | Identified as a dwarf planet
! rowspan="2"| Category
|-
! by Emery<br />et al.<ref name=JWST/>
! by Grundy<br />et al.<ref name="Grundy2019" /><ref name="Grundy2019-2" />
! by the IAU

|-
| ''[[Triton (moon)|N I Triton]]'' 
| {{val|2707|2}} || {{val|2.06}} || 0.60 to 0.95 
| colspan="3" |(likely in equilibrium)<ref>{{cite journal|title=The Shape of Triton from Limb Profiles|author=Thomas, P.C.|journal=Icarus|volume=148|issue=2|date=December 2000|pages=587–588|doi=10.1006/icar.2000.6511|bibcode=2000Icar..148..587T|doi-access=free}}</ref>
| (moon of Neptune)
|-
! style="text-align: left;" data-sort-value="134340" | {{dp|Pluto|134340 Pluto}}
| {{val|2376|3}} || {{val|1.854|0.006}} || 0.49 to 0.66 || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]]|| [[plutino]] ([[Plutino|2:3 resonant]])
|-
! style="text-align: left;" data-sort-value="136199" | {{dp|Eris|136199 Eris}}
| {{val|2326|12}} || {{val|2.43|0.05}} || 0.96 || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]] || [[Scattered disc|SDO]]
|-
! style="text-align: left;" data-sort-value="136108" | {{dp|Haumea|136108 Haumea}}
| {{val|1560|p=≈&nbsp;}} || {{val|2.018|p=≈&nbsp;}} || 0.51 || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]]<br />{{small|(naming rules)}} || resonant [[Classical Kuiper belt object|cubewano]]
|-
! style="text-align: left;" data-sort-value="136472" | {{dp|Makemake|136472 Makemake}}
| {{val|1430|38|22}} || {{val|1.9|0.2}} || 0.81 || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]]<br />{{small|(naming rules)}} || hot cubewano
|-
! style="text-align: left;" data-sort-value="225088" | {{dp|Gonggong|225088 Gonggong}}
| {{val|1230|50}} || {{val|1.74|0.16}} || 0.14 || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]] || [[Image:Commons-emblem-query.svg|15px|Maybe]] || [[resonant trans-Neptunian object|3:10 resonant]]
|-
| ''[[Charon (moon)|P I Charon]]'' 
| {{val|1212|1}} || {{val|1.70|0.02}} || 0.2 to 0.5 
| colspan="3" |(possibly in equilibrium)<ref>{{cite journal|title=On the asphericity of the figures of Pluto and Charon|author1=Kholshevnikovab, K.V.|author2=Borukhaa, M.A.|author3=Eskina, B.B.|author4=Mikryukov, D.V.|journal=Icarus|pages=104777|date=23 October 2019|volume=181|doi=10.1016/j.pss.2019.104777|s2cid=209958465}}</ref>
| (moon of Pluto)
|-
! style="text-align: left;" data-sort-value="50000" | {{dp|Quaoar|50000 Quaoar}} 
| {{val|1086|4}} || ≈&nbsp;1.7 || 0.11 || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]]<br />{{small|(2022–2023 annual report)<ref name=report/>}} || hot cubewano
|-
! style="text-align: left;" data-sort-value="1" | {{dp|Ceres|1 Ceres}}
| {{val|946|2}} || {{val|2.16|0.01}} || 0.09 
| colspan="2" |(close to equilibrium)<ref>{{cite book|chapter-url=https://meetingorganizer.copernicus.org/EPSC2018/EPSC2018-645-1.pdf|display-authors=4|author1=Raymond, C.|author2=Castillo-Rogez, J.C.|author3=Park, R.S.|author4=Ermakov, A.|author5=Bland, M.T.|author6=Marchi, S.|author7=Prettyman, T.|author8=Ammannito, E.|author9=De Sanctis, M.C.|author10=Russell, C.T.|date=September 2018|chapter=Dawn Data Reveal Ceres' Complex Crustal Evolution|title=European Planetary Science Congress|volume=12}}</ref>|| [[Image:Yes check.svg|15px|Yes]] 
| [[asteroid]]
|-
! style="text-align: left;" data-sort-value="90482" | {{dp|Orcus|90482 Orcus}} 
| {{val|910|50|40}} || {{val|1.4|0.2}} || 0.23 || [[Image:Commons-emblem-query.svg|15px|Maybe]]<br />{{small|(Not directly mentioned)}} || [[Image:Yes check.svg|15px|Yes]] || || plutino (2:3 resonant)
|-
! style="text-align: left;" data-sort-value="90377" | {{dp|Sedna|90377 Sedna}} 
| {{val|906|314|258}} ||? || 0.41 || [[Image:Yes check.svg|15px|Yes]] || [[Image:Yes check.svg|15px|Yes]] || || [[Detached object|detached]]
|-
! style="text-align: left;" data-sort-value="120347" | [[120347 Salacia]]
| {{val|846|21}} || {{val|1.50|0.12}} || 0.04 || [[Image:X mark.svg|15px|No]] || [[Image:Commons-emblem-query.svg|15px|Maybe]] || || hot cubewano
|-
! style="text-align: left;" data-sort-value="307261" | [[307261 Máni]]
| {{val|796|24}} ||? || 0.10 || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || hot cubewano
|-
! style="text-align: left;" data-sort-value="55565" | [[55565 Aya]]
| {{val|768|39}} ||? || 0.11 || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || hot cubewano
|-
! style="text-align: left;" data-sort-value="174567" | [[174567 Varda]]
| {{val|749|18}}|| {{val|1.78|0.06}}? or<br>{{val|1.23|0.04}}? || 0.10 || [[Image:X mark.svg|15px|No]] || [[Image:Commons-emblem-query.svg|15px|Maybe]] || || 4:7 resonant
|-
! style="text-align: left;" data-sort-value="532037" | {{mpl|532037|2013 FY|27}} 
| {{val|742|78|83}} || ? || 0.17 || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || SDO
|-
! style="text-align: left;" data-sort-value="208996" | [[208996 Achlys]] 
| {{val|723}} or {{val|772|12}} || {{val|0.76}} || 0.10 || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]] || || plutino (2:3 resonant)
|-
! style="text-align: left;" data-sort-value="28978" | [[28978 Ixion]]
| {{val|710|0.2}} || ? || 0.10 || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || plutino (2:3 resonant)
|-
! style="text-align: left;" data-sort-value="145452" | {{mpl|145452|2005 RN|43}}
| {{val|679|55|73}} || ? || {{val|0.107|0.029|0.018}} || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || hot cubewano
|-
! style="text-align: left;" data-sort-value="55637" | {{mpl|55637|2002 UX|25}}
| {{val|665|29}} or {{val|659|38}} || {{val|0.82|0.11}} || {{val|0.107|0.005|0.008}} or {{val|0.1|0.01}} || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]] || || hot cubewano
|-
! style="text-align: left;" data-sort-value="992018210618" | {{mpl|2018 VG|18}}
| {{val|656}} or {{val|500}} || ? || 0.12 || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || SDO
|-
! style="text-align: left;" data-sort-value="20000" | [[20000 Varuna]]
| {{val|654|154|102}} or {{val|668|154|86}} || ? || {{val|0.127|0.04|0.042}} || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || hot cubewano
|-
! style="text-align: left;" data-sort-value="992014202502" | {{mpl|2014 UZ|224}}
| {{val|635|65|72}} || ? || {{val|0.131|0.038|0.028}} || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || SDO
|-
! style="text-align: left;" data-sort-value="992012211503" | {{mpl|2012 VP|113}}
| {{val|574}}? || ? || 0.09 assumed || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || detached
|-
! style="text-align: left;" data-sort-value="528381" | {{mpl|528381|2008 ST|291}}
| {{val|549}} or {{val|584}} || ? || 0.09 assumed || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || || 1:6 resonant
|-
! style="text-align: left;" data-sort-value="523794" | {{mpl|523794|2015 RR|245}}
| {{val|500|p=≈}} || ? || 0.11 assumed || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]]? || [[Image:Commons-emblem-query.svg|15px|Maybe]]<br />{{small|(claimed without citation by [[American Geophysical Union|AGU]])<ref name=eos>{{Cite web |title=Six Things Dwarf Planets Have Taught Us About the Solar System |url=https://eos.org/articles/six-things-dwarf-planets-have-taught-us-about-the-solar-system |work=JoAnna Wendel |publisher=American Geophysical Union |date=27 January 2024}}</ref>}} <ref>{{Cite web |last=Hall |first=S. |date=2016-07-15 |title=New-Found Dwarf Planet Points to Solar System's Chaotic Past |url=http://eos.org/articles/new-found-dwarf-planet-points-to-solar-systems-chaotic-past |access-date=2024-07-16 |website=Eos |language=en-US}}</ref>|| SDO
|-
! style="text-align: left;" data-sort-value="15874" | {{mpl|15874|1996 TL|66}}
| {{val|339|20}} or {{val|575|115}} || ? || {{val|0.110|0.021|0.015}} || [[Image:X mark.svg|15px|No]] || [[Image:X mark.svg|15px|No]] || || SDO
|}

===Largest measured candidates===
{{See also|Category:Possible dwarf planets}}

The following [[trans-Neptunian object]]s have measured diameters at least {{convert|600|km|mi|-1}} to within measurement uncertainties; this was the threshold to be considered a "highly likely" [[dwarf planet]] in Brown's early assessment. Grundy et al. speculated that 600&nbsp;km to 700&nbsp;km diameter could represent "the upper limit to retain substantial internal pore space", and that objects around 900&nbsp;km could have collapsed interiors but fail to completely differentiate.<ref name=Grundy2019/> The two satellites of TNOs that surpass this threshold have also been included: Pluto's moon Charon and Eris' moon Dysnomia. The next largest TNO moon is Orcus' moon [[Vanth (moon)|Vanth]] at {{val|442.5|10.2|u=km}} and a poorly constrained {{val|87|8|e=18|u=kg}}, with an albedo of about 8%.

Ceres, generally accepted as a dwarf planet, is added for comparison. Also added for comparison is Triton, which is thought to have been a dwarf planet in the Kuiper belt before it was captured by Neptune.

Bodies with very poorly known sizes (e.g. {{mpl|2018 VG|18}} "Farout") have been excluded. Complicating the situation for poorly known bodies is that a body assumed to be a large single object might turn out to be a binary or ternary system of smaller objects, such as {{mpl-|532037|2013 FY|27}} or [[47171 Lempo|Lempo]]. A 2021 occultation of {{mpl-|612911|2004 XR|190}} ("Buffy") found a chord of 560&nbsp;km: if the body is approximately spherical, it is likely that the diameter is greater than 560&nbsp;km, but if it is elongated, the mean diameter may well be less. Explanations and sources for the measured masses and diameters can be found in the corresponding articles linked in column "Designation" of the table.

*Bodies with a nominal estimated diameter over 900&nbsp;km are bolded; they have general consensus as being dwarfs, per the previous section. Charon is also bolded, as it has sometimes been considered a possible dwarf in its own right; Triton is bolded as a former KBO that is still rounded and geologically active. 
*Bodies with estimated diameter between 700&nbsp;km and 900&nbsp;km are in bold italic; most are borderline possibilities, but in most cases are too poorly known for much certainty. They tend to be dark, suggesting that they are not dwarf planets, but some might be dense enough to be fully solid bodies.
*Other bodies, having estimated diameters below 700&nbsp;km, are unlikely to be dwarf planets on the basis of current evaluation, but may be transitional (partially compressed) bodies.
*A light-grey background indicates objects whose densities are believed to be higher than 1.5 g/cm<sup>3</sup>. Orcus and Sedna are on a medium-grey background due to uncertainties.
*Darkest of the three shades of grey indicates those bodies whose densities are believed to be lower than 1.5 g/cm<sup>3</sup>, and so if the data is correct cannot be dwarf planets.
*Satellites are on a pink background, as under the current definition a dwarf planet must directly orbit the Sun.

All of these categories are subject to change with further evidence.
<!--
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The Brown columns, Measured H, per-measured albedo, diameter per assumed albedo, and best diameter columns will all be automatically gathered by this process, as well as the ordering.
The other columns are manually gathered, so setting them here is good. You can also set Measured H.

The point is: don't spend hours trying to update this table to match Brown and the MPC when the mechanical process only takes a few minutes.
See the talk page for the mechanical process.

If you want to make a change to the table structure or presentation: If it's easy (for example, with a global edit, or column headers), go ahead and the process will be updated to match (a nice description of your change will help make the update easier). If it will take you a lot of work, describe what you want on the talk page and the process will be updated.
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{| class="wikitable sortable" style="text-align: center;"
|+Possible dwarf planets with measured sizes or masses<br>(satellites Triton, Charon, Dysnomia included for comparison)
|-
! data-sort-type="number"| [[Minor planet designation|Designation]]
! data-sort-type="number" | [[absolute magnitude|H]]
{{refn|name=mpc-tno}}{{refn|name=mpc-sdo}}
! data-sort-type="number" | Geometric<br />albedo{{efn|name=albedo|group=table}}
! data-sort-type="number" | Diameter<br />{{small|([[kilometre|km]])}}
!Method
! data-sort-type="number"| Mass{{efn|name=system_mass|group=table}}<br />{{small|([[Orders of magnitude (mass)|10<sup>18</sup>]]&nbsp;[[kilogram|kg]])}}
! data-sort-type="number"| Density<br />{{small|(g/cm<sup>3</sup>)}}
! Category
|-style="background:#ffb7c5"
| style="text-align: left;" data-sort-value="0.81" | '''[[Triton (moon)|Neptune I Triton]]''' || {{val|-1.2}} || data-sort-value="77.5%"| 60% to 95% || style="background: #e0e0ff;" | {{val|2707|2}}
|direct|| {{val|21390|28}} ||{{val|2.061}} || [[Moons of Neptune|satellite of Neptune]]
|-
| style="text-align: left;" data-sort-value="134340" | '''{{dp|Pluto|134340 Pluto}}''' || {{val|-0.45}} || data-sort-value="57.5%"| 49% to 66% || style="background: #e0e0ff;" | {{val|2377|3}}
|direct|| {{val|13030|30}} ||{{val|1.854|0.006}}|| [[Plutino|2:3 resonant]]
|-
| style="text-align: left;" data-sort-value="136199" | '''{{dp|Eris|136199 Eris}}''' || {{val|-1.21}}|| 96% || style="background: #e0e0ff;" | {{val|2326|12}} 
|occultation|| {{val|16466|85}} ||{{val|2.43|0.05}}|| [[Scattered disc|SDO]]
|-
| style="text-align: left;" data-sort-value="136108" | '''{{dp|Haumea|136108 Haumea}}''' || {{val|0.21}}|| 49% || style="background: #e0e0ff;" | {{val|1559}}
|occultation|| {{val|3986|43}}<!--total mass of Haumea's system is (4.006±0.040)×10^21 kg and total mass of known Haumea's satellites (Hiʻiaka and Namaka) is (1.969±0.258)×10^19 kg--> || {{val|2.018|p=≈&thinsp;}}|| [[cubewano]]
|-
| style="text-align: left;" data-sort-value="136472" | '''{{dp|Makemake|136472 Makemake}}''' || {{val|-0.21}}|| 83% || style="background: #e0e0ff;" | {{val|1429|38|20}} 
|occultation|| {{val|3100|p=≈&nbsp;}} ||{{val|1.9|0.2}}|| cubewano
|-
| style="text-align: left;" data-sort-value="225088" | '''{{dp|Gonggong|225088 Gonggong}}''' || {{val|1.86}} || 14% || style="background: #e0e0ff;" | {{val|1230|50}} 
|thermal|| {{val|1750|70}} ||{{val|1.74|0.16}}|| [[Resonant trans-Neptunian object#Other resonances|3:10 resonant]]
|-style="background:#ffb7c5"
| style="text-align: left;" data-sort-value="134340.5" | '''{{dp|Charon|134340 Pluto I Charon}}''' || {{val|1}} || data-sort-value="35%"| 20% to 50% || style="background: #e0e0ff;" | {{val|1212|1}}
|direct|| {{val|1586|15}} ||{{val|1.702|0.017}}|| [[Moons of Pluto|satellite of Pluto]]
|-
| style="text-align: left;" data-sort-value="50000" | '''{{dp|Quaoar|50000 Quaoar}}''' || {{val|2.42}} || 11% || style="background: #e0e0ff;" | {{val|1086|4}} 
|occultation|| {{val|1200|50}} ||{{val|1.7|-|1.8}}|| cubewano
|- 
| style="text-align: left;" data-sort-value="1" | '''{{dp|Ceres|1 Ceres}}''' || {{val|3.33}} || 9% || style="background: #e0e0ff;" | {{val|939.4|0.2}} 
|direct|| {{val|938.35|0.01}} ||{{val|2.16|0.01}}|| [[asteroid belt]]
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="90482" | '''{{dp|Orcus|90482 Orcus}}''' || {{val|2.18}} || 23% ± 2% || style="background: #e0e0ff;" | {{val|910|50|40}} 
|thermal|| {{val|548|10}}<!--mass of Orcus' system is (6.348±0.019)×10^20 kg and mass of Vanth is (8.7±0.8)×10^19 kg--> ||{{val|1.4|0.2}}|| 2:3 resonant
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="90377" | '''{{dp|Sedna|90377 Sedna}}''' || {{val|1.52}} || 41% || style="background: #e0e0ff;" | {{val|906|314|258}} 
|thermal||? ||?|| [[Detached object|detached]]
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="120347" | '''''[[120347 Salacia]]''''' || {{val|4.26}}|| 5% || style="background: #c0e0e0;" | {{val|846|21}} 
|thermal|| {{val|492|7}} ||{{val|1.5|0.12}}|| cubewano
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="307261" | '''''[[307261 Máni]]''''' || {{val|3.62}}|| 10% || style="background: #c0e0e0;" | {{val|796|24}} 
|occultation|| ||?|| cubewano
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="55565" | '''''[[55565 Aya]]''''' || {{val|3.47}}|| 11% || style="background: #c0e0e0;" | {{val|768|39|38}} 
|thermal|| ||?|| cubewano
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="174567" | '''''[[174567 Varda]]''''' || {{val|3.46}}|| 11% || style="background: #c0e0e0;" | {{val|749|18}}
|occultation|| {{val|245|6}} ||{{val|1.78|0.06}}? or<br>{{val|1.23|0.04}}?|| cubewano
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="532037" | '''''{{mpl|532037|2013 FY|27}}''''' || {{val|3.12}} || 18% || style="background: #c0e0e0;" | {{val|742|78|83}} 
|thermal|| ||?|| SDO
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="28978" | '''''[[28978 Ixion]]''''' || {{val|3.47}} || 10% || style="background: #c0e0e0;" | {{val|709.6|0.2}}
|occultation|| ||?|| 2:3 resonant
|- style="background: #cccccc;"
| style="text-align: left;" data-sort-value="208996" | [[208996 Achlys]] || {{val|3.77}} || 11% || style="background: #c0e0e0;" | {{val|707|24}} 
|occultation|| ||{{val|0.76}}|| 2:3 resonant
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="90568" | {{mpl|90568|2004 GV|9}} || {{val|3.99}}|| 8% || style="background: #c0e0e0;" | {{val|680|34}} 
|thermal|| ||?|| cubewano
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="145452" | {{mpl|145452|2005 RN|43}} || {{val|3.69}} || 11% || style="background: #c0e0e0;" | {{val|679|55|73}} 
|thermal|| ||?|| cubewano
|- style="background: #cccccc;"
| style="text-align: left;" data-sort-value="55637" | {{mpl|55637|2002 UX|25}} || {{val|3.85}} || 12% || style="background: #c0e0e0;" | {{val|659|38}}
|thermal|| {{val|125|3}} ||{{val|0.82|0.11}}|| cubewano
|- style="background: #cccccc;"
| style="text-align: left;" data-sort-value="229762" | {{dp|Gǃkúnǁʼhòmdímà|229762 Gǃkúnǁʼhòmdímà}}|| {{val|3.5}}|| 14% || style="background: #c0e0e0;" | {{val|655|14|13}}
|occultation|| {{val|136|3}} ||{{val|1.04|0.17}}|| SDO
|- style="background: #cccccc;"
| style="text-align: left;" data-sort-value="20000" | {{dp|Varuna|20000 Varuna}} || {{val|3.79}}|| 12% || style="background: #c0e0e0;" | {{val|654|154|102}}
|thermal|| ||{{val|0.992|0.086|0.015}}|| cubewano
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="145451" | {{mpl|145451|2005 RM|43}}|| {{val|4.63}}|| 11% || style="background: #c0e0e0; " | {{val|644}}
|occultation|| ||?|| SDO
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="992014202502" | {{mpl|2014 UZ|224}} || {{val|3.48}} || 14% || style="background: #c0e0e0;" | {{val|635|65|72}} 
|thermal|| ||?|| SDO
|-style="background:#ffb7c5"
| style="text-align: left;" data-sort-value="136199.5" | [[Dysnomia (moon)|136199 Eris I Dysnomia]] || {{val|5.6}} || data-sort-value="5%"| {{val|5|1}}% || style="background: #c0e0e0;" | {{val|615|60|50}} || thermal || <{{val|140}} || data-sort-value="{{val|0.7}}"| {{val|0.7|0.5}} || satellite of Eris
|- style="background: #e8e8e8;"
| style="text-align: left;" data-sort-value="78799" | {{mpl|78799|2002 XW|93}} || {{val|4.99}} || 4% || style="background: #c0e0e0;" | {{val|565|71|73}} 
|thermal|| ||?|| SDO
|}
{{notelist|group=table|refs=
<ref name=albedo>
The geometric [[Albedo#Astronomical albedo|albedo]] <math>A</math> is calculated from the measured absolute magnitude <math>H</math>
and measured diameter <math>D</math> via the formula: <math>A =\left ( \frac{1329\times10^{-H/5}}{D} \right ) ^2</math>. Ranges have been given for Triton, Pluto, and Charon, which have been observed up close and therefore have known local albedo variations.
</ref>
<ref name=system_mass>
This is the total system mass (including moons), except for Pluto, Haumea, and Orcus.
</ref>
}}

==={{vanchor|Brightest unmeasured candidates}}===
For objects without a measured size or mass, sizes can only be estimated by assuming an albedo. Most sub-dwarf objects are thought to be dark, because they haven't been resurfaced; this means that they are also relatively large for their magnitudes. Below is a table for assumed albedos between 4% (the albedo of Salacia) and 20% (a value above which suggests resurfacing), and the sizes objects of those albedos would need to be (if round) to produce the observed absolute magnitude. Backgrounds are blue for >900&nbsp;km and teal for >600&nbsp;km.

{| class="wikitable" style="text-align: center;"
|+Calculated sizes in km (based on different albedo assumptions){{efn|name=albedo|group=table2}} <br>for brightest objects without measured size or mass
!rowspan=2|H
!rowspan=2|Objects with this magnitude (H){{refn|name=mpc-tno}}{{refn|name=mpc-sdo}}
!colspan=9|Assumed albedo (''p'')
|-
! 4% !! 6% !! 8% !! 10% !! 12% !! 14% !! 16% !! 18% !! 20%
|-
!3.5
|align=left|{{mpl|2017 OF|201}} (H = 3.52 ± 0.45)
|style="background: #e0e0ff;" | {{sigfig|1326|3}}
|style="background: #e0e0ff;" | {{sigfig|1083|3}}
|style="background: #e0e0ff;" | {{sigfig|938|2}}
|style="background: #c0e0e0;" | {{sigfig|839|2}}
|style="background: #c0e0e0;" | {{sigfig|765|2}}
|style="background: #c0e0e0;" | {{sigfig|709|2}}
|style="background: #c0e0e0;" | {{sigfig|663|2}}
|style="background: #c0e0e0;" | {{sigfig|625|2}}
| {{sigfig|593|2}}
|-
!3.6
|align=left|{{mpl|2021 DR|15}} (H = 3.61 ± 0.15)<ref name="jpldata-2021-DR15"/>
|style="background: #e0e0ff;" | {{sigfig|1266|3}}
|style="background: #e0e0ff;" | {{sigfig|1034|3}}
|style="background: #e0e0ff;" | {{sigfig|895|2}}
|style="background: #c0e0e0;" | {{sigfig|801|2}}
|style="background: #c0e0e0;" | {{sigfig|731|2}}
|style="background: #c0e0e0;" | {{sigfig|677|2}}
|style="background: #c0e0e0;" | {{sigfig|633|2}}
|style="background: #c0e0e0;" | {{sigfig|597|2}}
| {{sigfig|566|2}}
|-
!3.7
|align=left| 
|style="background: #e0e0ff;" | {{sigfig|1209|3}}
|style="background: #e0e0ff;" | {{sigfig|987|2}}
|style="background: #c0e0e0;" | {{sigfig|855|2}}
|style="background: #c0e0e0;" | {{sigfig|765|2}}
|style="background: #c0e0e0;" | {{sigfig|698|2}}
|style="background: #c0e0e0;" | {{sigfig|646|2}}
|style="background: #c0e0e0;" | {{sigfig|605|2}}
| {{sigfig|570|2}}
| {{sigfig|541|2}}
|-
!3.8
|align=left|{{mpl|2014 EZ|51}}, {{mpl|2010 JO|179}}, {{mpl|2010 RF|43}}
|style="background: #e0e0ff;" | {{sigfig|1155|3}}
|style="background: #e0e0ff;" | {{sigfig|943|2}}
|style="background: #c0e0e0;" | {{sigfig|817|2}}
|style="background: #c0e0e0;" | {{sigfig|730|2}}
|style="background: #c0e0e0;" | {{sigfig|667|2}}
|style="background: #c0e0e0;" | {{sigfig|617|2}}
| {{sigfig|577|2}}
| {{sigfig|544|2}}
| {{sigfig|516|2}}
|-
!3.9
|align=left|{{mpl|2018 VG|18}} (H = 3.92 ± 0.52)<ref name="jpldata-2018-VG18"/>
|style="background: #e0e0ff;" | {{sigfig|1103|3}}
|style="background: #e0e0ff;" | {{sigfig|900|2}}
|style="background: #c0e0e0;" | {{sigfig|780|2}}
|style="background: #c0e0e0;" | {{sigfig|697|2}}
|style="background: #c0e0e0;" | {{sigfig|637|2}}
| {{sigfig|589|2}}
| {{sigfig|551|2}}
| {{sigfig|520|2}}
| {{sigfig|493|2}}
|-
!4.0
|align=left|{{mpl|2015 RR|245}}, {{mpl|2010 KZ|39}}, {{mpl|2012 VP|113}}, <br>{{mpl|2021 LL|37}} (H = 4.09 ± 0.31)<ref name="jpldata-2021-LL37"/>
|style="background: #e0e0ff;" | {{sigfig|1053|3}}
|style="background: #c0e0e0;" | {{sigfig|860|2}}
|style="background: #c0e0e0;" | {{sigfig|745|2}}
|style="background: #c0e0e0;" | {{sigfig|666|2}}
|style="background: #c0e0e0;" | {{sigfig|608|2}}
| {{sigfig|563|2}}
| {{sigfig|527|2}}
| {{sigfig|496|2}}
| {{sigfig|471|2}}
|-
!4.1
|align=left|{{mpl|2015 KH|162}}, {{mpl|2020 MK|53}} (H = 4.12 ± 0.35)<ref name="jpldata-2020-MK53"/>
|style="background: #e0e0ff;" | {{sigfig|1006|3}}
|style="background: #c0e0e0;" | {{sigfig|821|2}}
|style="background: #c0e0e0;" | {{sigfig|711|2}}
|style="background: #c0e0e0;" | {{sigfig|636|2}}
| {{sigfig|581|2}}
| {{sigfig|538|2}}
| {{sigfig|503|2}}
| {{sigfig|474|2}}
| {{sigfig|450|2}}
|-
!4.2
|align=left|{{mpl|2018 AG|37}} (H = 4.22 ± 0.1),<ref name="jpldata-2018-AG37"/> {{mpl|2013 FZ|27}}, {{mpl|2008 ST|291}}, <br>{{mpl|2010 RE|64}}
|style="background: #e0e0ff;" | {{sigfig|960|2}}
|style="background: #c0e0e0;" | {{sigfig|784|2}}
|style="background: #c0e0e0;" | {{sigfig|679|2}}
|style="background: #c0e0e0;" | {{sigfig|607|2}}
| {{sigfig|555|2}}
| {{sigfig|513|2}}
| {{sigfig|480|2}}
| {{sigfig|453|2}}
| {{sigfig|430|2}}
|-
!4.3
|align=left|{{mpl|2017 FO|161}}, {{mpl|2015 BP|519}}, <br>{{mpl|2017 OF|69}}, {{mpl|2014 AN|55}}
|style="background: #e0e0ff;" | {{sigfig|917|2}}
|style="background: #c0e0e0;" | {{sigfig|749|2}}
|style="background: #c0e0e0;" | {{sigfig|649|2}}
| {{sigfig|580|2}}
| {{sigfig|530|2}}
| {{sigfig|490|2}}
| {{sigfig|459|2}}
| {{sigfig|432|2}}
| {{sigfig|410|2}}
|-
!4.4
|align=left|{{mpl|2014 WK|509}}, {{mpl|2007 JJ|43}}, {{mpl|2014 WP|509}}
|style="background: #c0e0e0;" | {{sigfig|876|2}}
|style="background: #c0e0e0;" | {{sigfig|715|2}}
|style="background: #c0e0e0;" | {{sigfig|619|2}}
| {{sigfig|554|2}}
| {{sigfig|506|2}}
| {{sigfig|468|2}}
| {{sigfig|438|2}}
| {{sigfig|413|2}}
| {{sigfig|392|2}}
|-
!4.5
|align=left|{{mpl|2013 XC|26}}, {{mpl|2014 YA|50}}, {{mpl|2010 FX|86}}
|style="background: #c0e0e0;" | {{sigfig|837|2}}
|style="background: #c0e0e0;" | {{sigfig|683|2}}
| {{sigfig|592|2}}
| {{sigfig|529|2}}
| {{sigfig|483|2}}
| {{sigfig|447|2}}
| {{sigfig|418|2}}
| {{sigfig|394|2}}
| {{sigfig|374|2}}
|-
!4.6
|align=left|{{mpl|2020 FY|30}} (H = 4.6 ± 0.16),<ref name="jpldata-2020-FY30"/> {{mpl|2006 QH|181}} {{mpl|2007 XV|50}}, {{mpl|2014 US|277}}, <br>{{mpl|2002 WC|19}}, {{mpl|2010 OO|127}}
|style="background: #c0e0e0;" | {{sigfig|799|2}}
|style="background: #c0e0e0;" | {{sigfig|652|2}}
| {{sigfig|565|2}}
| {{sigfig|505|2}}
| {{sigfig|461|2}}
| {{sigfig|427|2}}
| {{sigfig|399|2}}
| {{sigfig|377|2}}
| {{sigfig|357|2}}
|-
!4.7
|align=left|{{mpl|2014 FC|69}}, {{mpl|2014 HA|200}}, {{mpl|2014 BV|64}}, <br>{{mpl|2014 FC|72}}, {{mpl|2014 OE|394}}, {{mpl|2010 DN|93}}, <br>{{mpl|2015 BZ|518}}
|style="background: #c0e0e0;" | {{sigfig|763|2}}
|style="background: #c0e0e0;" | {{sigfig|623|2}}
| {{sigfig|539|2}}
| {{sigfig|483|2}}
| {{sigfig|440|2}}
| {{sigfig|408|2}}
| {{sigfig|381|2}}
| {{sigfig|360|2}}
| {{sigfig|341|2}}
|-
!4.8
|align=left|{{mpl|2014 TZ|85}}, {{mpl|2007 JH|43}}, {{mpl|2015 AM|281}}, <br>{{mpl|2008 OG|19}}, {{mpl|2014 US|224}}
|style="background: #c0e0e0;" | {{sigfig|729|2}}
|style="background: #c0e0e0;" | {{sigfig|595|2}}
| {{sigfig|515|2}}
| {{sigfig|461|2}}
| {{sigfig|421|2}}
| {{sigfig|389|2}}
| {{sigfig|364|2}}
| {{sigfig|343|2}}
| {{sigfig|326|2}}
|-
!4.9
|align=left|{{mpl|2011 HP|83}}, {{mpl|2013 FS|28}}, {{mpl|2014 FT|71}}, <br>{{mpl|2013 AT|183}}, {{mpl|2011 WJ|157}}, {{mpl|2014 UM|33}}, <br>{{mpl|2014 BZ|57}}, {{mpl|2013 SF|106}}, {{mpl|2003 UA|414}}
|style="background: #c0e0e0;" | {{sigfig|696|2}}
| {{sigfig|568|2}}
| {{sigfig|492|2}}
| {{sigfig|440|2}}
| {{sigfig|402|2}}
| {{sigfig|372|2}}
| {{sigfig|348|2}}
| {{sigfig|328|2}}
| {{sigfig|311|2}}
|-
<!--too many objects to bother with here, but here are the #'s
!5.0
|style="background: #c0e0e0;" | {{sigfig|665|2}}
| {{sigfig|543|2}}
| {{sigfig|470|2}}
| {{sigfig|420|2}}
| {{sigfig|384|2}}
| {{sigfig|355|2}}
| {{sigfig|332|2}}
| {{sigfig|313|2}}
| {{sigfig|297|2}}
|-
!5.1
|style="background: #c0e0e0;" | {{sigfig|635|2}}
| {{sigfig|518|2}}
| {{sigfig|449|2}}
| {{sigfig|401|2}}
| {{sigfig|366|2}}
| {{sigfig|339|2}}
| {{sigfig|317|2}}
| {{sigfig|299|2}}
| {{sigfig|284|2}}
|-
!5.2
|style="background: #c0e0e0;" | {{sigfig|606|2}}
| {{sigfig|495|2}}
| {{sigfig|429|2}}
| {{sigfig|383|2}}
| {{sigfig|350|2}}
| {{sigfig|324|2}}
| {{sigfig|303|2}}
| {{sigfig|286|2}}
|271 -->
|}
{{notelist|group=table2|refs=
<ref name=albedo>
The diameter can be calculated from the measured absolute magnitude <math>H</math>, and for an assumed albedo <math>p</math>, via the formula: <math>D = \frac{1329\times10^{-H/5}}{\sqrt{p}} </math>
</ref>
}}

== See also ==
* [[Lists of astronomical objects]]
* [[List of trans-Neptunian objects]]
* [[List of gravitationally rounded objects of the Solar System]]
* [[List of former planets]]
* [[Planetary-mass moon]]

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

<ref name="brown-list">{{cite web
  |title      = How many dwarf planets are there in the outer solar system? 
  |publisher  = California Institute of Technology 
  |author     = Michael E. Brown 
  |author-link= Michael E. Brown 
  |url        = http://web.gps.caltech.edu/~mbrown/dps.html
  |date       = 13 September 2019
  |access-date= 24 November 2019
  |archive-url = https://web.archive.org/web/20191013130649/http://web.gps.caltech.edu/~mbrown/dps.html
  |archive-date= 13 October 2019
|url-status=live}}</ref>

<ref name="tancredi-2010">{{cite journal|date=2010|title=Physical and dynamical characteristics of icy "dwarf planets" (plutoids)|journal=Icy Bodies of the Solar System: Proceedings IAU Symposium No. 263, 2009|author=Tancredi, G.|volume=263|pages=173–185|doi=10.1017/S1743921310001717|bibcode=2010IAUS..263..173T|doi-access=free}}</ref>

<ref name="mpc-tno">{{cite web|title=List Of Trans-Neptunian Objects|url=http://www.minorplanetcenter.net/iau/lists/t_tnos.html|website=Minor Planet Center}} Retrieved 15 July 2023.</ref>

<ref name="mpc-sdo">{{cite web|title=List Of Centaurs and Scattered-Disk Objects|url=http://www.minorplanetcenter.net/iau/lists/t_centaurs.html|website=Minor Planet Center}} Retrieved 15 July 2023.</ref>

<ref name="jpldata-2021-DR15">{{cite web
  |type       = 2022-04-11 last obs.
  |title      = JPL Small-Body Database Browser: (2021 DR15)
  |url        = https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=54231255
  |publisher  = [[Jet Propulsion Laboratory]]
  |accessdate = 25 October 2022}}</ref>

<ref name="jpldata-2018-VG18">{{cite web
  |type       = 2022-03-09 last obs.
  |title      = JPL Small-Body Database Browser: (2018 VG18)
  |url        = https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=3836918
  |publisher  = [[Jet Propulsion Laboratory]]
  |access-date = 25 October 2022}}</ref>

<ref name="jpldata-2021-LL37">{{cite web
  |type       = 2022-06-16 last obs.
  |title      = JPL Small-Body Database Browser: (2021 LL37)
  |url        = https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=54281066
  |publisher  = [[Jet Propulsion Laboratory]]
  |accessdate = 25 October 2022}}</ref>

<ref name="jpldata-2020-MK53">{{cite web
  |type       = 2020-06-25 last obs.
  |title      = JPL Small-Body Database Browser: (2020 MK53)
  |url        = https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=2020%20MK53
  |publisher  = [[Jet Propulsion Laboratory]]
  |access-date = 15 July 2023}}</ref>

<ref name="jpldata-2018-AG37">{{cite web
  |type       = 2021-08-24 last obs.
  |title      = JPL Small-Body Database Browser: (2018 AG37)
  |url        = https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=54114199
  |publisher  = [[Jet Propulsion Laboratory]]
  |access-date = 25 October 2022}}</ref>

<ref name="jpldata-2020-FY30">{{cite web
  |type       = 2021-04-16 last obs.
  |title      = JPL Small-Body Database Browser: (2020 FY30)
  |url        = https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=54117580
  |publisher  = [[Jet Propulsion Laboratory]]
  |access-date = 25 October 2022}}</ref>

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

== External links ==
*[http://ssd.jpl.nasa.gov/sbdb_query.cgi NASA JPL Small-Body Database Search Engine]
*[http://public-tnosarecool.lesia.obspm.fr/Published-results.html TNOs are cool public database], incl. diameters and albedos measured by Herschel and Spitzer to date, Herschel OT KP "TNOs are Cool: A Survey of the Transneptunian Region"
* [http://web.gps.caltech.edu/~mbrown/dps.html How many dwarf planets are there in the outer solar system? (updates daily)] (Mike Brown)
* [http://www.gps.caltech.edu/~mbrown/dps_notes.html Details on the dwarf planet size calculations] (Mike Brown)
* [http://adsabs.harvard.edu/abs/2008Icar..195..851T Which are the Dwarfs in the Solar System?] Tancredi, G.; Favre, S. ''Icarus'', Volume 195, Issue 2, p.&nbsp;851–862.

{{Dwarf planets}}
{{Trans-Neptunian objects}}
{{Solar System}}
{{Portal bar|Stars|Spaceflight|Outer space|Science}}

[[Category:Possible dwarf planets| ]]
[[Category:Lists of minor planets|Possible dwarf planets]]
[[Category:Lists of trans-Neptunian objects]]
[[Category:Solar System]]