(44594) 1999 OX3, Orbit and classification
Neptune has a semi-major axis of 30 AU and 1999 OX3 has a semi-major axis of 32 AU. The Minor Planet Center (MPC) does not classify this object as a centaur because the MPC defines centaurs as having a semi-major axis of less than 30.066 AU. 1999 OX3 crosses the orbits of both Neptune and Uranus and has an inclination of only 2.62°. The Deep Ecliptic Survey (DES) defines centaurs using a dynamical classification scheme, based on the behavior of orbital integrations over 10 million years. The DES defines centaurs as nonresonant objects whose osculating perihelia are less than the osculating semimajor axis of Neptune at any time during the integration. Using the dynamical definition of a centaur, 1999 OX3 is a centaur.


(44594) 1999 OX3, Physical characteristics
In July 2009, a rotational lightcurve of 1999 OX3 was obtained from photometric observations. Lightcurve analysis gave a rotation period of 9.26 hours with a brightness amplitude of 0.11 magnitude (U=2). The period, however, is ambiguous with alternative solutions (13.4 and 15.45 hours).


(44594) 1999 OX3, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 22 August 2002. As of 2018, it has not been named.


(450894) 2008 BT18
(450894) 2008 BT18 is a sub-kilometer asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered on 31 January 2008, by the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, United States. The eccentric asteroid measures approximately 600 meters in diameter and has a composition of a basaltic achondrite.


(450894) 2008 BT18
In 2008, its minor-planet moon, designated S/2008 (450894) 1, was discovered by radar astronomers. It measures approximately 200 meters in diameter, or one third of its primary.


(450894) 2008 BT18, Orbit and classification
2008 BT18 orbits the Sun at a distance of 0.9–3.5 AU once every 3 years and 4 months (1,209 days). Its orbit has an eccentricity of 0.59 and an inclination of 8° with respect to the ecliptic. Published by the Digitized Sky Survey, a first precovery was taken at Palomar Observatory in 1955, extending the asteroid's observation arc by 53 years prior to its discovery.


(450894) 2008 BT18, Orbit and classification
The asteroid has a low Earth minimum orbit intersection distance of 0.0108 AU (1,620,000 km) which corresponds to 4.2 lunar distances (LD). On 14 July 2008, it transited Earth within 0.015 AU (5.9 LD).


(450894) 2008 BT18, Physical characteristics
2008 BT18 has been characterized as a V-type asteroid by astronomers using the SpeX spectrograph at NASA Infrared Telescope Facility, IRTF.


(450894) 2008 BT18, Physical characteristics, Rotation period
A rotational lightcurve for 2008 BT18 was obtained from photometric observations made by astronomer Alberto Silva Betzler at Salvador, Brazil, in July 2008. The lightcurve gave a rotation period of 2.726±0.007 hours with a brightness variation of 0.04 in magnitude (U=1).


(450894) 2008 BT18, Physical characteristics, Binary system
On 6 and 7 July 2008, research conducted using the Arecibo Observatory produced evidence that 2008 BT18 is a synchronous binary asteroid with a minor-planet moon in its orbit. The secondary component, provisionally designated S/2008 (450894) 1, has a diameter of at least 200 meters, about 33% the size of and up to 1.5 kilometers apart from its primary. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 650 meters, based on an absolute magnitude of 18.3.


(450894) 2008 BT18, Physical characteristics, Binary system
There are more than 60 binary near-Earth objects known to exist (2016).


(450894) 2008 BT18, Physical characteristics, Mineralogy
On 26 July 2008, observations at the IRTF using the SpeX-spectrograph showed that 2008 BT18 is a basaltic achondrite, suggesting that its parent body was subjected to sufficiently high temperatures to  produce a eutectic melt. The body's surface is thought to be dominated by iron-rich orthopyroxenes with little or no olivine.


(454101) 2013 BP73
(454101) 2013 BP73, provisional designation 2013 BP73, is a sub-kilometer asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 310 meters (1,020 ft) in diameter.


(454101) 2013 BP73, Description
From discovery until August 2013 when Sentry updated to planetary ephemeris (DE431), it had the 4th highest impact threat on the Palermo Technical Impact Hazard Scale. It was discovered on 22 January 2013 by the Mount Lemmon Survey at an apparent magnitude of 21 using a 1.5-meter (59 in) reflecting telescope. It has an estimated diameter of 310 meters (1,020 ft). Six Precovery images from April 2003 have been located. It was removed from the Sentry Risk Table on 3 January 2014.


(454101) 2013 BP73, Description
It has an observation arc of 10 years with an uncertainty parameter of 2. Perturbations by Earth, Venus, and Mercury will increase the orbital uncertainty over time. When the asteroid only had an observation arc of 52 days, virtual clones of the asteroid that fit the uncertainty region in the known trajectory showed a 1 in 588,000 chance that the asteroid could impact Earth on 11 December 2096. With a 2096


(454101) 2013 BP73, Description
Palermo Technical Scale of −3.42, the odds of impact by 2013 BP73 in 2096 were about 2630 times less than the background hazard level of Earth impacts which is defined as the average risk posed by objects of the same size or larger over the years until the date of the potential impact. Using the nominal orbit, JPL Horizons shows that the asteroid will be 0.9 AU (130,000,000 km; 84,000,000 mi) from Earth on 11 December 2096. 2013 BP73 will make a close approach to Earth on 17 December 2018 that should allow a refinement to the known trajectory.


(454101) 2013 BP73, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 December 2015 (M.P.C. 97517). As of 2018, it has not been named.


(455502) 2003 UZ413
(455502) 2003 UZ413, also written as 2003 UZ413, is a trans-Neptunian object (TNO) with an absolute magnitude of 4.38. It is in a 2:3 orbital resonance with Neptune, thus it is classified as a plutino. It is likely large enough to be a dwarf planet. It was given the minor planet number 455502 on 22 February 2016.


(455502) 2003 UZ413
It has been observed 79 times over 15 oppositions, with precovery images back to 27 July 1954.


(455502) 2003 UZ413, Orbit and rotation
2003 UZ413 is in a 2:3 resonance with Neptune, which means that when it makes two revolutions around the Sun, Neptune makes exactly three.


(455502) 2003 UZ413, Orbit and rotation
The object rotates very fast. In fact, with a period of about 4.13 hours, it is the fastest rotator known in the Kuiper belt after Haumea.


(455502) 2003 UZ413, Physical characteristics
The mean diameter of 2003 UZ413 is estimated to be 650+1−175 km, if it has a low albedo.


(455502) 2003 UZ413, Physical characteristics
Given its rapid rotation, it must have a density higher than 0.72 g/cm3. Stable Jacobi ellipsoids with an axis ratio of a/b ≥ 1.13±0.03, as implied by its light-curve amplitude of Δm = 0.13±0.03, exist for densities in the range of 2.29−3.00 g/cm3. The Johnston's Archive settles on 2.64 g/cm3, the centre of the latter range; for a 600 km equivalent spheroid body, this would equate to a mass of approximately 3.0×1020 kg.


(455502) 2003 UZ413, Physical characteristics
The relatively high estimated density (in stark contrast to many similarly sized TNOs) increases the chance that the object has no internal porosity and has collapsed into hydrostatic equilibrium (a requirement of being certified as a Dwarf Planet), but confirmation of this hypothesis requires observations to refine the size and light curve details, preferably with determination of the orbit of any satellite that may exist.


(455502) 2003 UZ413, Physical characteristics
In visible light, this object is neutral or slightly red in color and has a flat, featureless reflectance spectrum.


(456938) 2007 YV56
(456938) 2007 YV56, provisional designation 2007 YV56, is a sub-kilometer asteroid on an eccentric orbit, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 190–360 meters (620–1,200 ft) in diameter. It was discovered on 31 December 2007, by astronomers of the Catalina Sky Survey conducted at the Catalina Station in Arizona, United States.


(456938) 2007 YV56, Orbit and classification
2007 YV56 is an Apollo asteroid that crosses the orbit of Earth. Apollo's are the largest group of near-Earth objects with nearly 10 thousand known members.


(456938) 2007 YV56, Orbit and classification
It orbits the Sun at a distance of 0.60–2.55 AU once every 2 years (722 days; semi-major axis of 1.58 AU). Its orbit has a high eccentricity of 0.62 and an inclination of 6° with respect to the ecliptic. This makes it also a Mars-crossing asteroid, as it crosses the orbit of the Red Planet at 1.66 AU, as well as a Venus-crosser due to its aphelion of less than 0.71 AU. The body's observation arc begins at Catalina with its official discovery observation in December 2007.


(456938) 2007 YV56, Close approaches
2007 YV56 has a minimum orbital intersection distance (MOID) with Earth of 703,000 km; 437,000 mi (0.0047 AU), which corresponds to 1.83 lunar distances (LD). It has an absolute magnitude of 21.0. This makes it a potentially hazardous asteroid, which are defined as having a MOID of less than 0.05 AU (19 LD) and an absolute magnitude brighter than 22. Besides Earth, it also makes close approaches to Venus, Mars and the Moon.


(456938) 2007 YV56, Close approaches
On 26 December 2007, five days prior to its discovery observation, it passed Earth at a nominal distance of 0.10037 AU (39.06 LD). On 2 January 2101, it is predicted to flyby Earth at 0.00159 AU (0.62 LD) and pass the Moon at a similar distance five hours earlier as well (also see List of asteroid close approaches to Earth § Predicted encounters).


(456938) 2007 YV56, Physical characteristics
The body's spectral type is unknown. Near-Earth asteroids are often of a stony composition.


(456938) 2007 YV56, Physical characteristics, Diameter and albedo
Based on a generic magnitude-to-diameter conversion, 2007 YV56 measures 190–360 meters (620–1,180 ft) in diameter, for an absolute magnitude of 21.0, and an assumed albedo of 0.20 and 0.057, which represent typical values for stony and carbonaceous asteroids, respectively.


(456938) 2007 YV56, Physical characteristics, Rotation period
As of 2018, no rotational lightcurve of 2007 YV56 has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.


(456938) 2007 YV56, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 22 February 2016 (M.P.C. 98584). As of 2018, it has not been named.


(457175) 2008 GO98
(457175) 2008 GO98, provisional designation 2008 GO98 with cometary number 362P, is a Hildian asteroid and rare main-belt comet from the outermost regions of the asteroid belt, approximately 15 kilometers (9 miles) in diameter. It was discovered on 8 April 2008, by astronomers of the Spacewatch program at Kitt Peak National Observatory near Tucson, Arizona, in the United States. The presumably carbonaceous body has a rotation period of 10.7 hours.


(457175) 2008 GO98, Orbit and classification
2008 GO98 is classified as a member of the dynamical Hilda group, as well as a main-belt comet that shows clear cometary activity, which has also been described as a "quasi Hilda comet". Orbital backward integration suggests that it might have been a centaur or trans-Neptunian object that ended its dynamical evolution as a quasi Hilda comet.


(457175) 2008 GO98, Orbit and classification
It orbits the Sun in the outer asteroid belt at a distance of 2.9–5.1 AU once every 7 years and 11 months (2,883 days; semi-major axis of 3.96 AU). Its orbit has an eccentricity of 0.28 and an inclination of 16° with respect to the ecliptic. The body's observation arc begins with a precovery taken by the Sloan Digital Sky Survey in October 2001, more than  5 years prior to its official discovery observation by Spacewatch.


(457175) 2008 GO98, Orbit and classification
2008 GO98 has a Jupiter Tisserand's parameter (TJ) of 2.926, just below Jewitt's threshold of 3, which serves as a distinction between the main-belt asteroids (TJ larger than 3) and the Jupiter-family comets (TJ between 2 and 3).


(457175) 2008 GO98, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 16 February 2016 (M.P.C. 98587). As of 2020, it has not been named.


(457175) 2008 GO98, Physical characteristics, Rotation period
In August 2017, a rotational lightcurve of 2008 GO98 was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station (U82) in California. Lightcurve analysis gave a rotation period of 10.74±0.01 hours with a small brightness amplitude of 0.12 magnitude (U=2).


(457175) 2008 GO98, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous body of 0.057 and calculates a diameter of 14.64 kilometers based on an absolute magnitude of 12.9. Other estimates, taking into account several published magnitude measurements and a large range of albedo assumptions, estimate a diameter range of 5.5 to 24.7 kilometers.


(458732) 2011 MD5
(458732) 2011 MD5 is an Apollo near-Earth asteroid around 1.2 kilometers (0.75 miles) in diameter. It is the largest asteroid known to have passed closer than the Moon. On 17 September 1918 the asteroid passed 0.00234 AU (350 thousand km; 0.91 LD) from Earth with a peak apparent magnitude of around 8.4. The 1918 close approach distance is known with an accuracy of roughly ±200 km. The asteroid had come to opposition (opposite the Sun in the sky) on 9 August 1918 at magnitude 16.


(458732) 2011 MD5
2011 MD5 was not discovered until 30 June 2011, when the asteroid was 1.3 AU (190 million km) from Earth. The asteroid now has a 8 year observation arc and a well determined orbit.


(459883) 2014 JX55
(459883) 2014 JX55 is an asteroid from the central regions of the asteroid belt. After its first observations as 2007 EB26 in 2007, it was considered an inner heliospheric asteroid and near-Earth object with one of the closest perihelion ever observed of any body orbiting the Sun, until further observations invalidated the conclusions from early observations. The object measures approximately 2.8 kilometers (1.7 miles) in diameter.


(459883) 2014 JX55, Orbit and classification, Inner heliospheric asteroid
When the object was first observed as 2007 EB26 by the Mount Lemmon Survey in March 2007, it was considered to have the second-smallest positive semi-major axis (0.55 AU) of any known object orbiting the Sun, after Mercury. It was classified as an Apohele asteroid, which always stay inside of Earth's orbit, approaching within 0.116 AU (17,400,000 km; 10,800,000 mi) of the Sun approximately every 148 days, before leaving for a distance of 0.98 AU, making it a Mercury- and Venus-crossing asteroid. If these early orbital calculations had not turned out to be wrong, the object would still rank today among the inner heliospheric asteroids with the smallest known perihelia.


(459883) 2014 JX55, Orbit and classification, Orbital determination as main-belt asteroid
The object remained listed as an inner heliospheric asteroid for several years, until identifications with 2010 MV87 and 2014 JX55 and a subsequent improvement of the orbital uncertainty completely overturned previous calculations. 2014 JX55 is now a secured central main-belt asteroid orbiting the Sun at a distance of 2.2–3.1 AU once every 4 years and 3 months (1,555 days; semi-major axis of 2.63 AU). Its orbit has an eccentricity of 0.17 and an inclination of 32° with respect to the ecliptic.


(467336) 2002 LT38
(467336) 2002 LT38, is a sub-kilometer asteroid and suspected tumbler, classified as a near-Earth object and potentially hazardous asteroid of the Aten group, approximately 240 meters (790 ft) in diameter. It was discovered on 12 June 2002, by astronomers of the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States.


(467336) 2002 LT38, Orbit and classification
2002 LT38 orbits the Sun at a distance of 0.6–1.1 AU once every 9 months (284 days; semi-major axis of 0.85 AU). Its orbit has an eccentricity of 0.31 and an inclination of 6° with respect to the ecliptic.


(467336) 2002 LT38, Orbit and classification
The body's observation arc begins with a precovery taken at AMOS on 10 June 2002, two nights prior to its official discovery observation at Lincoln Lab's ETS.


(467336) 2002 LT38, Orbit and classification, Close approaches
2002 LT38 has an Earth minimum orbital intersection distance of 0.0344 AU (5,150,000 km) which corresponds to 13.4 lunar distances. It will pass at that distance during its close encounter with Earth on 27 June 2030.


(467336) 2002 LT38, Physical characteristics, Rotation period
In July 2016, a first rotational lightcurve of 2002 LT38 was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Station in California (U82). Lightcurve analysis gave a longer-than average rotation period of 21.80 hours with a brightness variation of 1.16 magnitude (U=2+). A high brightness amplitude typically indicates that the body has a non-spherical, elongated shape. It is also a suspected tumbler.


(467336) 2002 LT38, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 0.236 kilometers based on an absolute magnitude of 20.5.


(467336) 2002 LT38, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 21 May 2016, after its orbit determination became sufficiently secure (M.P.C. 100286). As of 2018, it has not been named.


(468861) 2013 LU28
(468861) 2013 LU28, provisional designation 2013 LU28 is a highly eccentric trans-Neptunian object, retrograde centaur and damocloid from the outer regions of the Solar System. It was discovered on 8 June 2013 by astronomers with the Mount Lemmon Survey at the Mount Lemmon Observatory in Arizona, United States. The object is unlikely a dwarf planet as it measures approximately 110 kilometers (68 miles) in diameter. It was numbered in 2016 and has not been named since.


(468861) 2013 LU28, Orbit and classification
2013 LU28 orbits the Sun at a distance of 8.7–353.1 AU once every 2434 years (888,879 days; semi-major axis of 180.92 AU). Its orbit has an exceptionally high eccentricity of 0.95 and an inclination of 125° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Mount Lemmon in June 2013.


(468861) 2013 LU28, Orbit and classification, TNO, centaur and damocloid
With a semi-major axis larger than that of Neptune, 2013 LU28 is generically classified as a trans-Neptunian object. It is also considered an (extended) centaur, due to its eccentric orbit with a low perihelion of 8.7 AU and a higher-than-90°-inclination, which gives it a retrograde orbit. There are only about a hundred known retrograde minor planets out of nearly 800,000 observed bodies, and, together with 2008 YB3 and 2011 MM4, it is among the largest such objects. 2013 LU28 also meets the orbital definition for being a damocloid, a cometary-like object without a coma or tail and a Tisserand's parameter with respect to Jupiter of less than 2 besides a retrograde orbit.


(468861) 2013 LU28, Numbering and naming
This distant minor planet was numbered by the Minor Planet Center on 20 June 2016 (M.P.C. 100585). As of 2018, it has not been named.


(468861) 2013 LU28, Physical characteristics, Diameter and albedo
According to the Johnston's archive and astronomer Michael Brown, 2013 LU28 measures 106 and 114 kilometers in diameter, based on an absolute magnitude of 8.1 and an assumed albedo for the body's surface of 0.08 and 0.09, respectively. According to Brown, 2013 LU28 is "probably not" a dwarf planet. As of 2018, no physical characteristics have been determined from photometric observations. The body's rotation period, pole and shape remain unknown.


(469306) 1999 CD158
(469306) 1999 CD158, provisional designation: 1999 CD158, is a trans-Neptunian object from the circumstellar disc of the Kuiper belt, located in the outermost region of the Solar System. The relatively bright hot classical Kuiper belt object measures approximately 310 kilometers (190 miles) in diameter. It was discovered on 10 February 1999, by American astronomers Jane Luu, David Jewitt and Chad Trujillo at Mauna Kea Observatories on the Big Island of Hawaii, United States.


(469306) 1999 CD158, Orbit and classification
1999 CD158 is candidate to the Haumea family, the only collisional group of trans-Neptunian objects currently determined. It is also sub-classified as a resonant trans-Neptunian object, as it stays in a 4:7 orbital resonance with the ice giant Neptune, which means, that for every seven orbits of Neptune around the Sun, it makes four orbits. It orbits the Sun at a distance of 37.4–50.1 AU once every 289 years and 8 months (105,787 days). Its orbit has an eccentricity of 0.15 and an inclination of 25° with respect to the ecliptic.


(469306) 1999 CD158, Orbit and classification
Its observation arc begins with its official discovery observation at Mauna Kea in 1999, as no precoveries were taken and no prior identifications were made. As of 2017 its current position is at 46.7 AU from the Sun.


(469306) 1999 CD158, Physical characteristics, Photometry
Photometric observation of 1999 CD158 in March 2015, gave a classically shaped bimodal lightcurve with a rotation period of 6.88 hours and a large brightness variation of 0.49 magnitude (U=3-).


(469306) 1999 CD158, Physical characteristics, Photometry
Observations with the New Technology Telescope at ESO's La Silla Observatory in Chile in 2008, determined the body's BVRI colors to be 0.770 (B–V), 0.630 (V–R) and 1.110 (V–I) for their respective passbands. Color indices have since been repeatedly measured.


(469306) 1999 CD158, Physical characteristics, Diameter and albedo
According to estimates by the Johnston's archive, the Collaborative Asteroid Lightcurve Link and American astronomer Michael Brown, 1999 CD158 measures between 420 and 477 kilometers in diameter. It is "probably" a dwarf planet" according to Brown's assessment (see List of possible dwarf planets § List).


(469372) 2001 QF298
(469372) 2001 QF298, provisionally known as 2001 QF298, is a resonant trans-Neptunian object that resides in the Kuiper belt in the outermost region of the Solar System. It was discovered on August 19, 2001 by Marc W. Buie. 2001 QF298 is a plutino, meaning that it is locked in a 3:2 orbital resonance with Neptune, much like Pluto.


(469372) 2001 QF298, Physical characteristics
In 2012, the size of 2001 QF298 was estimated based on thermal radiation data obtained with the Herschel Space Telescope. The result was 408.2+40.2−44.9 km.


(469372) 2001 QF298, Physical characteristics
In the visible light, the object appears to have a neutral or slightly red color.


(469372) 2001 QF298, Dwarf planet candidate
When first discovered, 2001 QF298 was calculated to have an absolute magnitude (H) of 4.7. Light-curve-amplitude analysis from 2008 showed only small deviations, which suggested that 2001 QF298 could be a spheroid about 480 kilometres (300 mi) in diameter with small albedo spots and hence a dwarf planet. It is not included in the same authors' list of dwarf-planet candidates from 2010 because, having an absolute magnitude of 5.4 and assumed albedo of 0.1, it would be less than the cut-off size of 450 kilometres (280 mi) (the same criteria as in the first paper).


(469987) 2006 HJ123
2006 HJ123  (also written 2006 HJ123) is a trans-Neptunian object (TNO). It was discovered in 2006 by Marc W. Buie. The object is a plutino (in 2:3 resonance with Neptune).


(469987) 2006 HJ123, Physical properties
The size of 2006 HJ123 was measured by the Herschel Space Telescope to be 283+142−111 km.


(470308) 2007 JH43
(470308) 2007 JH43, provisional designation 2007 JH43, is a trans-Neptunian object in the outer regions of the Solar System, approximately 500 kilometers in diameter. It was discovered on 10 May 2007, by the U.S. Palomar Observatory in California. The team of unaccredited astronomers at Palomar consisted of Megan E. Schwamb, Michael E. Brown and David L. Rabinowitz


(470308) 2007 JH43
The minor planet orbits the Sun at a distance of 38.6–40.6 AU once every 249 years and 1 month (90,983 days). Its orbit has an eccentricity of 0.02 and an inclination of 18° with respect to the ecliptic. The first precovery was taken at the Australian Siding Spring Observatory during the Digitized Sky Survey in 1984, extending the body's observation arc by 23 years prior to its discovery observation. It came to perihelion around 1888. Based on an absolute magnitude of 4.5 and assuming a generic albedo for trans-Neptunian objects of 0.09, it is about 500 kilometres (310 mi) in diameter, which makes it likely a dwarf planet.


(470308) 2007 JH43, Orbital classification
The Minor Planet Center lists 2007 JH43 as a trans-Neptunian object or a distant object in the Kuiper belt. The Deep Ecliptic Survey currently shows it as a scattered object, based on a 10-million-year integration of the orbit.


(470599) 2008 OG19
(470599) 2008 OG19 is a trans-Neptunian object and a possible dwarf planet located in the scattered disc. It was discovered on 30 July 2008 through the Palomar Observatory. It displays a large light curve amplitude of 0.437±0.011 magnitudes, implying that it is highly elongated in shape, similar to 20000 Varuna. Based on models for its light curve amplitude, they obtained an approximate density of 0.609 g/cm3 and aspect ratios of b/a = 0.513 and c/a = 0.39.


(471240) 2011 BT15
(471240) 2011 BT15, provisional designation 2011 BT15, is a stony, sub-kilometer sized asteroid and fast rotator, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group. It had been one of the objects with the highest impact threat on the Palermo Technical Impact Hazard Scale.


(471240) 2011 BT15, Discovery
It was discovered on 24 January 2011, by a team of astronomers at Pan-STARRS, the Panoramic Survey Telescope and Rapid Response System at Haleakala Observatory on Hawaii, United States. The discovery was made using a 1.8-meter Ritchey–Chrétien telescope. At the time of discovery, the object had an apparent magnitude of 22.


(471240) 2011 BT15, Orbit
Before the 2013 recovery it had an observation arc of 41 days with an uncertainty parameter of 7. Due to precovery images from 2007 it now has an observation arc of more than 5 years. It makes close approaches to Earth and Mars.


(471240) 2011 BT15, Orbit
On 28 December 2013, it passed 0.03222 AU (4,820,000 km) from Earth. The December 2013 passage was studied by the Goldstone Deep Space Network and further refined the orbit.


(471240) 2011 BT15, Orbit, Impact risk
While listed on the Sentry Risk Table, virtual clones of the asteroid that fit the uncertainty region in the known trajectory showed a 1 in 71,000 chance that the asteroid could impact Earth on 5 January 2080.


(471240) 2011 BT15, Orbit, Impact risk
In 2013 it had the 5th highest impact threat on the Palermo Technical Impact Hazard Scale. It was removed from the Sentry Risk Table on 17 June 2013.


(471240) 2011 BT15, Orbit, Impact risk
With a 2080 Palermo Technical Scale of −3.58, the odds of impact by 2011 BT15 in 2080 were about 3800 times less than the background hazard level of Earth impacts which is defined as the average risk posed by objects of the same size or larger over the years until the date of the potential impact. JPL Horizons shows that the nominal pass will be on 17 January 2080 at a distance of 0.125 AU (18,700,000 km; 11,600,000 mi) from Earth.


(471240) 2011 BT15, Physical characteristics
This near-Earth object is characterized as a common, stony S-type asteroid by the Collaborative Asteroid Lightcurve Link (CALL).


(471240) 2011 BT15, Physical characteristics, Fast rotator
In January 2014, a rotational lightcurve of 2011 BT15 was obtained from photometric observations by American astronomer Brian Warner at the CS3-Palmer Divide Station (U82) in California. Lightcurve analysis gave a well-defined rotation period of 0.109138 hours (393 seconds) with a brightness amplitude of 0.61 magnitude (U=3).


(471240) 2011 BT15, Physical characteristics, Diameter and albedo
According to the CALL and JPL's impact-risk table, this near-Earth object measures 136 and 150 meters, respectively. For its size estimate, CALL uses a standard for stony asteroids of 0.20 with an absolute magnitude of 21.7.


(471288) 2011 GM27
(471288) 2011 GM27 is a trans-Neptunian object (TNO) in the Kuiper belt, classified as a hot classical Kuiper belt object. It was discovered on 2 April 2011, at ESO's La Silla Observatory in Chile. With an absolute magnitude of 5.32, it is probably a dwarf planet, as its diameter has been roughly estimated to be about 450 kilometers (280 mi) based on an assumed geometric albedo between 0.06 to 0.09.


(471288) 2011 GM27
2011 GM27 orbits the Sun at a distance of 42.4–44.6 AU once every 286 years and 11 months (104,794 days; semi-major axis of 43.5 AU). Its orbit has an eccentricity of 0.03 and an inclination of 13° with respect to the ecliptic.


(471288) 2011 GM27
It orbits slightly outside a 3:5 resonance with Neptune, taking 16 years (5.5% of its orbit) longer to orbit the Sun than a body in 3:5 resonance. Precovery observations exist dating back to 2006 in SDSS data.


(471325) 2011 KT19
(471325) 2011 KT19 (nicknamed Niku; /niːkuː/) is a trans-Neptunian object that has an unusual 110° tilted solar orbital plane and retrograde orbit around the Sun.


(471325) 2011 KT19, Details
(471325) 2011 KT19 was discovered by the Mount Lemmon Survey on 31 May 2011. Its rediscovery was announced in August 2016 by a team of astronomers using the Pan-STARRS telescope. It was soon linked with a supposed prograde centaur (2011 KT19; inclination = 38° and semi-major axis = 28 AU) that had been lost due to a short observation arc. 2011 KT19 is in a 7:9 resonance with Neptune. Currently it is the only object with a nearly polar orbit that is in resonance with a planet. Notably, it is part of a group of objects that orbit the Sun in a highly inclined orbit; the reasons for this unusual orbit are unknown as of August 2016.


(471325) 2011 KT19, Details
The orbital characteristics of 2011 KT19 have been compared to those of 2008 KV42 (Drac). The orbits of 2011 KT19, 2008 KV42, 2002 XU93, 2010 WG9, 2007 BP102, 2011 MM4, appear to occupy a common plane, with three in prograde and three in retrograde orbits. The probability of this alignment occurring by chance is 0.016%. These orbits should leave a common plane in a few million years because the precession of prograde and retrograde orbits are in opposite directions.


(471325) 2011 KT19, Details
Simulations including the hypothetical Planet Nine did not maintain a common orbital plane and the plane does not coincide with  the plane of the predicted high-inclination large semi-major axis objects of that model. Other simulations with a few Earth-mass dwarf planet on a high-inclination orbit also failed to reproduce the alignment.


(472271) 2014 UM33
(472271) 2014 UM33, provisionally designated 2010 TQ182, is a trans-Neptunian object and possible dwarf planet residing in the outer Kuiper belt. It was discovered on October 22, 2014, by the Mount Lemmon Survey. It is listed on Mike Brown's website as a probable dwarf planet, ranked 67th most likely.


(472271) 2014 UM33
It is approximately the size of 2 Pallas in the asteroid belt. On August 18, 2015, 2014 UM33 was found to have been discovered over four years previously, with the designation 2010 TQ182. This extended its observation arc to over 4 years, and then precovery observations were found using the Sloan Digital Sky Survey from 2009.


(472651) 2015 DB216
(472651) 2015 DB216 is a centaur and Uranus co-orbital discovered on February 27, 2015, by the Mount Lemmon Survey. It is the second known centaur on a horseshoe orbit with Uranus, and the third Uranus co-orbital discovered after 2011 QF99 (a Trojan) and 83982 Crantor (a horseshoe librator). A second Uranian Trojan, 2014 YX49, was announced in 2017.


(472651) 2015 DB216, Description
An early orbital calculation of the asteroid with an observation arc of 10 days suggested an extremely close MOID to Neptune, but further observations on March 27 refined the orbit to show that the asteroid passes no less than several astronomical units away from Neptune, and show the orbit instead being that of a typical centaur, with a perihelion near that of Saturn, and traveling near to Uranus and Neptune. Later, observations suggested a distant orbit traveling extremely distant from the Sun, but now this too has been shown to be incorrect with later observations. However, it does have a semimajor axis near that of Uranus, making it a Uranus co-orbital. However it is not a Trojan, as it stays near the opposite side of the Sun from Uranus.


(472651) 2015 DB216, Description
A paper, submitted on July 27, 2015, analyzed 2015 DB216's orbital evolution, and suggested that it may be more stable than the other known Uranus co-orbitals due to its high inclination, and that many more undiscovered Uranus co-orbitals may exist.


(472651) 2015 DB216, Description
Precovery images from 2003 were located soon after 2015 DB216's discovery, giving it an 11-year observation arc.


(480808) 1994 XL1
(480808) 1994 XL1 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Aten group, approximately 200 meters (700 feet) in diameter. It was discovered on 6 December 1994, by Scottish–Australian astronomer Robert McNaught at Siding Spring Observatory in Australia. It was one of the first asteroids discovered to have a semi-major axis less than Venus.


(480808) 1994 XL1, Orbit and classification
1994 XL1 orbits the Sun at a distance of 0.3–1.0 AU once every 0 years and 7 months (201 days). Its orbit has an eccentricity of 0.53 and an inclination of 28° with respect to the ecliptic. No precoveries were taken, and no prior identifications were made. The body's observation arc begins with its official discovery observation.


(480808) 1994 XL1, Orbit and classification, Close encounter
The asteroid has an Earth minimum orbital intersection distance of 0.0365 AU (5,460,000 km), which translates into 14.2 lunar distances. It passed 0.03709 AU (5,550,000 km) from Earth on 6 December 1994. On 4 December 2044, it will pass again at 0.03637 AU (5,440,000 km) from Earth.


(480808) 1994 XL1, Physical characteristics
1994 XL1 has not been observed by any of the space-based surveys such as the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission. Based on a generic magnitude-to-diameter conversion, 1994 XL1 measures approximately 0.2 kilometers in diameter assuming an albedo of 0.20, which is a typical value for stony S-type asteroids.


(480808) 1994 XL1, Physical characteristics
As of 2017, no rotational lightcurve of this object has been obtained. The body's rotation period, shape and poles remain unknown.


(480808) 1994 XL1, Naming and numbering
After its first observation in 1994, this minor planet was numbered 23 year later by the Minor Planet Center on 12 January 2017 (M.P.C. 112958), after its last observation with the LCO–A 1-meter global telescope station at Sutherland, South Africa, on 6 December 2016 (K91). As of 2018, the asteroid has not been named .


(481394) 2006 SF6
(481394) 2006 SF6 is a sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group, approximately 300 meters (1,000 feet) in diameter. It was discovered on 17 September 2006, by the Catalina Sky Survey at Catalina Station in Arizona. On 21 November 2019, it passed Earth at a distance of 11 lunar distances (0.0288 AU), which is the object's closest flyby for centuries. The stony A/S-type asteroid is highly elongated in shape and has a rotation period of 11.5 hours.


(481394) 2006 SF6, Orbit and classification
2006 SF6 orbits the Sun at a distance of 0.7–1.2 AU once every 11 months (338 days; semi-major axis of 0.95 AU). Its orbit has an eccentricity of 0.28 and an inclination of 6° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Catalina Station in September 2006.


(481394) 2006 SF6, Orbit and classification, Close approaches
Being a potentially hazardous asteroid, 2006 SF6 has an Earth minimum orbital intersection distance (MOID) of 0.0191 AU (2,860,000 km) which corresponds to 7.4 lunar distances. In order to be classified as "potentially hazardous" an object must have an Earth-MOID of less than 0.05 AU (7,500,000 km; 4,600,000 mi) – approximately 19.5 lunar distances – and an absolute magnitude brighter than 22, approximately corresponding to a diameter above 140 meters (460 ft).


(481394) 2006 SF6, Orbit and classification, Close approaches
On 21 November 2019 at 00:01 UTC, it passed Earth at a nominal distance (measured from the center of the Earth) of 11 lunar distances (0.0288 AU) and at a relative velocity of 7.9 km/h. This is the object's closest flyby in JPL's data base, which covers 183 approaches over almost three centuries from April 1900 to November 2198.


(481394) 2006 SF6, Orbit and classification, Close approaches
On 19 November 2069, it will pass 0.0393 AU (5,880,000 km) from Earth, which will be the asteroid's second closest approach after its record flyby on 21 November 2019.


(481394) 2006 SF6, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 12 January 2017 (M.P.C. 102964). As of 2020 it has not been named.


(481394) 2006 SF6, Physical characteristics
During its apparition in November 2007, spectro-photometric data obtained of 2006 SF6 allowed for an A/S/D-type classification. This classification could be further constrained to an A/S-type, as a D-type does not agree with the object's relatively high albedo value (see below).


(481394) 2006 SF6, Physical characteristics, Rotation period
In September 2018, a rotational lightcurve of 2006 SF6 was obtained from photometric observations by Brian Warner and Robert Stephens at the Center for Solar System Studies in California. Lightcurve analysis gave a rotation period of 11.517±0.006 hours with a very high brightness amplitude of 0.97±0.04 magnitude (U=3), indicative of a highly elongated non-spherical shape. The two photometrists revisited the object in October 2019 and obtained a similar result of 11.495±0.002 hours with an even higher magnitude of 1.07±0.03 (U=3-).


(481394) 2006 SF6, Physical characteristics, Diameter and albedo
According to the NEOSurvey carried out by NASA's Spitzer Space Telescope, the asteroid's surface has an albedo of 0.21±0.15, which gives a mean-diameter of roughly 300 meters based on an absolute magnitude of 19.9. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.20 and a diameter of 0.311 kilometers using an absolute magnitude of 19.9 as well.


(481482) 2007 CA19
(481482) 2007 CA19 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It led the impact hazard list, with a Torino Scale impact risk value of 1, for one week, ending on February 19, 2007. Before and after 2007 CA19, 99942 Apophis was the object with the highest Palermo Scale rating. With an observation arc of 4.8 days, it had a Palermo Scale of −0.88.


(481482) 2007 CA19
2007 CA19 was discovered on February 11, 2007, by the Catalina Sky Survey at the University of University of Arizona. The object is estimated at 966 metres in diameter with a mass of a 1.2x1012 kg. Until February 15, it had an impact probability of 1/625000 for the day March 14, 2012. Additional observations through February 19 decreased the impact probability to ~1 in 300 million, making it of negligible concern. It was removed from the Sentry Risk Table on February 22, 2007.


(481482) 2007 CA19
2007 CA19 passed about 0.007 AU (1,000,000 km; 650,000 mi) from Venus on July 6, 1946.


(48639) 1995 TL8
(48639) 1995 TL8 is a binary trans-Neptunian object from the scattered disc in the outermost regions of the Solar System. It was discovered by Arianna Gleason in 1995 and measures approximately 176 kilometers in diameter. Its 80-kilometer minor-planet moon, provisionally designated S/2002 (48639) 1, was discovered on 9 November 2002.


(48639) 1995 TL8, Discovery
1995 TL8 was discovered on 15 October 1995, by American astronomer Arianna Gleason as part of UA's Spacewatch survey at Kitt Peak National Observatory, near Tucson, Arizona.


(48639) 1995 TL8, Discovery
It was the first of the bodies presently classified as a scattered-disc object (SDO) to be discovered, preceding the SDO prototype (15874) 1996 TL66 by almost a year.


(48639) 1995 TL8, Satellite
A companion was discovered by Denise C. Stephens and Keith S. Noll, from observations with the Hubble Space Telescope taken on 9 November 2002, and announced on 5 October 2005. The satellite, designated S/2002 (48639) 1, is relatively large, having a likely mass of about 10% of the primary. Its orbit has not been determined, but it was at a separation of only about 420 kilometres (260 mi) to the primary at the time of discovery, with a possible orbital period of about half a day and an estimated diameter of 161 kilometres (100 mi).


(48639) 1995 TL8, Scattered–extended object
1995 TL8 is classified as detached object (scattered–extended) by the Deep Ecliptic Survey, since its orbit appears to be beyond significant gravitational interactions with Neptune's current orbit. However, if Neptune migrated outward, there would have been a period when Neptune had a higher eccentricity.


(48639) 1995 TL8, Scattered–extended object
Simulations made in 2007 show that 1995 TL8 appears to have less than a 1% chance of being in a 3:7 resonance with Neptune, but it does execute circulations near this resonance.


(48639) 1995 TL8, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 20 November 2002. As of 2018, it has not been named.


(4953) 1990 MU
(4953) 1990 MU (prov. designation: 1990 MU) is a large Earth-crossing asteroid (ECA) belonging to the Apollo group of near-Earth objects which also cross the orbits of Mars and Venus. At approximately 3 km in diameter, it is one of the largest known ECAs. It has been assigned a permanent number from the Minor Planet Center (4953) indicating that its orbit has been very well determined. With an observation arc of 45 years, the asteroid's trajectory and uncertainty regions are well known through to the year 2186.


(4953) 1990 MU, Description
1990 MU was first observed over three nights in 1990. By itself, this was not enough for the asteroid to be given a permanent number since the orbit could not be calculated accurately enough for the object to be subsequently recovered. However, the object was precovered by the Anglo-Australian Near-Earth Asteroid Survey on six photographic plates from the UK Schmidt Telescope dating back to 1974. This technique has more success with the Amor group of asteroids which do not cross the orbit of the Earth and consequently have long periods of opposition when they can be observed. In this respect the Apollo asteroid 1990 MU is somewhat unusual.


(4953) 1990 MU, Description
1990 MU has an Earth minimum orbit intersection distance (MOID) of 0.0263 AU (3,930,000 km), which is close enough to classify it as a Potentially Hazardous Asteroid (PHA). It will make a close approach to Earth on 6 June 2027 at 0.0308 AU (4,610,000 km), becoming as bright as apparent magnitude 9.7 on 8 June 2027, and even closer on 5 June 2058 at 0.0231 AU (3,460,000 km). It also made a close approach to Venus on 5 October 2012 at 0.0567 AU (8,480,000 km) and will again on 3 September 2041 at 0.0581 AU (8,690,000 km).


(4953) 1990 MU, Description
1990 MU has made close approaches to Earth in the past; in June 1996 it approached within 0.25 AU and in May 1990 it approached to 0.1418 AU. The Earth MOID of 1990 MU has been decreasing (becoming more hazardous) during the 20th century, while the Venus MOID (0.0455) has been increasing.


(4953) 1990 MU, Description
Besides its original discovery at Siding Spring Observatory in Australia, 1990 MU has also been studied by radar at Goldstone Observatory in California, and Arecibo Observatory in Puerto Rico. Lightcurves have been obtained at La Silla Observatory in Chile.


(4953) 1990 MU, Description
The albedo of 1990 MU was measured by the ExploreNEOs project of the Spitzer Space Telescope in August 2009. The result obtained was 0.79 and was the second highest albedo measured by the project. However, ExploreNEO do not believe this is a plausible figure, they state that the albedo of an NEO is not likely to be much over 0.5 and their measurement uncertainty is "around a factor of 2".


(4953) 1990 MU, Description
The Gaia mission of the European Space Agency, launched in December 2013, has been tasked with measuring the Yarkovsky effect on near-Earth asteroids (NEAs). The Yarkovsky effect is a small non-gravitational force on rotating bodies that can affect their trajectories. Its effect on small bodies like asteroids can be significant and needs to be taken into account in predicting an asteroid's position. 1990 MU has been selected as one of the most promising NEAs for this measurement by Gaia.


(495603) 2015 AM281
(495603) 2015 AM281, provisional designation 2015 AM281, is a resonant trans-Neptunian object and a probable dwarf planet candidate from the outermost region of the Solar System, approximately 470 kilometers (290 miles) in diameter. It was discovered on 13 March 2010, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States.


(495603) 2015 AM281, Discovery
The body's observation arc begins with a precovery taken by the Sloan Digital Sky Survey in April 2000, nearly 10 years prior to its official discovery observation at Haleakala Observatory. The discovery was announced in a Minor Planet Electronic Circular in July 2016, after additional observations by Pan-STARRS had been found (2010–2013), preceding the team's original observation from 11 January 2015, which led to the assignment of the object's first and only provisional designation, 2015 AM281. The observations were made with Pan-STARRS 1.8-meter Ritchey–Chrétien telescope, and B. Gibson, T. Goggia, N. Primak, A. Schultz, and M. Willman were the observers.


(495603) 2015 AM281, Orbit and classification
2015 AM281 is a resonant trans-Neptunian object in a 2:5 orbital resonance with Neptune, which means that it orbits the Sun exactly twice while Neptune orbits the Sun five times. Several objects in this resonance with a period of 410 years have been found, including 2002 TC302.


(495603) 2015 AM281, Orbit and classification
It orbits the Sun at a distance of 41.4–68.9 AU once every 409 years and 5 months (149,540 days; semi-major axis of 55.14 AU). Its orbit has an eccentricity of 0.25 and an inclination of 27° with respect to the ecliptic. It still has an orbital uncertainty of 1 and 3, respectively.


(495603) 2015 AM281, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 9 June 2017 and received the number 495603 in the minor planet catalog (M.P.C. 105261). As of 2018, it has not been named.


(495603) 2015 AM281, Physical characteristics
According to the Johnston's archive and American astronomer Michael Brown, 2015 AM281 measures 468 and 479 kilometers in diameter based on an assumed albedo of 0.09 and 0.07, respectively. On his website, Michael Brown lists this object as a "probable" dwarf planet (400–500 km) which is the category with the second lowest certainty in his 5-class taxonomic system. As of 2018, no rotational lightcurve has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.


(496315) 2013 GP136
2013 GP136 is a trans-Neptunian object from the scattered disc in the outermost reaches of the Solar System, approximately 212 kilometers in diameter. It was discovered on 8 February 2013, by the Outer Solar System Origins Survey at the Mauna Kea Observatories on the island of Hawaii, United States.


(496315) 2013 GP136, Orbit and classification
2013 GP136 orbits the Sun at a distance of 41.1–268.5 AU once every 1925 years and 4 months (703,239 days). Its orbit has an eccentricity of 0.73 and an inclination of 33° with respect to the ecliptic.


(496315) 2013 GP136, Orbit and classification
It was mentioned in a 2016 paper by Malhotra of the Lunar and Planetary Laboratory, at The University of Arizona, Tucson, AZ as a detached object with a perihelion greater than 40 AUs, a 6:1 orbital period ratio with 90377 Sedna, and in a possible 9:1 mean-motion resonance with a hypothetical large Planet Nine.


(4S)-beta-phellandrene synthase (geranyl-diphosphate-cyclizing)
(4S)-beta-phellandrene synthase (geranyl-diphosphate-cyclizing) (EC , phellandrene synthase, (−)-beta-phellandrene synthase, (−)-(4S)-beta-phellandrene synthase) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing; (4S)-beta-phellandrene-forming). This enzyme catalyses the following chemical reaction


(4S)-limonene synthase
In enzymology, a (4S)-limonene synthase (EC ) is an enzyme that catalyzes the chemical reaction


(4S)-limonene synthase
Hence, this enzyme has one substrate, geranyl diphosphate, and two products, (−)-(4S)-limonene and diphosphate.


(4S)-limonene synthase
This enzyme belongs to the family of lyases, specifically those carbon-oxygen lyases acting on phosphates. The systematic name of this enzyme class is geranyl-diphosphate diphosphate-lyase [cyclizing, (−)-(4S)-limonene-forming]. Other names in common use include (−)-(4S)-limonene synthase, 4S-(−)-limonene synthase, geranyldiphosphate diphosphate lyase (limonene forming), geranyldiphosphate diphosphate lyase [cyclizing,, and (4S)-limonene-forming]. This enzyme participates in monoterpenoid biosynthesis.


(500883) 2013 JJ65
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(501214) 2013 TC146
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(501546) 2014 JJ80
(501546) 2014 JJ80, prov. designation: 2014 JJ80, is a trans-Neptunian object from the outermost region of the Solar System. It was discovered on 9 July 2013, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. It is a dwarf planet candidate, as it measures approximately 350 kilometers (220 miles) in diameter.


(501546) 2014 JJ80, Orbit and classification
2014 JJ80 orbits the Sun at a distance of 31.3–55.1 AU once every 283 years and 9 months (103,645 days; semi-major axis of 43.18 AU). Its orbit has an eccentricity of 0.28 and an inclination of 19° with respect to the ecliptic. The body's observation arc begins at Haleakalā with a precovery taken in August 2010, nearly 3 years prior to its official discovery observation.


(501546) 2014 JJ80, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 5 October 2017 and received the number 501546 in the minor planet catalog (M.P.C. 106396). As of 2021, it has not been named.


(501546) 2014 JJ80, Physical characteristics
According to American astronomer Michael Brown and the Johnston's archive, 2014 JJ80 measures 344 and 352 kilometers in diameter based on an assumed albedo of 0.08 and 0.09, respectively. On his website, Brown lists this object as a "possible" dwarf planet (200–400 km), which is the category with the lowest certainty in his 5-class taxonomic system. As of 2021, no spectral type and color indices, nor a rotational lightcurve have been obtained from spectroscopic and photometric observations. The body's color, rotation period, pole and shape remain unknown.


(501581) 2014 OB394
(501581) 2014 OB394, provisional designation 2014 OB394, is a trans-Neptunian object from the outermost region of the Solar System, approximately 260 kilometers (160 miles) in diameter. It was discovered on 25 August 2012, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. The weak dwarf planet candidate was numbered in 2017 and remains without a name.


(501581) 2014 OB394, Orbit and classification
2014 OB394 orbits the Sun at a distance of 35.0–58.2 AU once every 318 years and 5 months (116,302 days; semi-major axis of 46.63 AU). Its orbit has an eccentricity of 0.25 and an inclination of 21° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Haleakala Observatory in August 2012.


(501581) 2014 OB394, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 5 October 2017 and received the number 501581 in the minor planet catalog (M.P.C. 106397). As of 2018, it has not been named.


(501581) 2014 OB394, Physical characteristics
According to American astronomer Michael Brown and the Johnston's archive, 2014 OB394 measures 255 and 267 kilometers in diameter based on an assumed albedo of 0.08 and 0.09, respectively. On his website, Brown lists this object as a "possible" dwarf planet (200–400 km), which is the category with the lowest certainty in his 5-class taxonomic system. As of 2018, no spectral type and color indices, nor a rotational lightcurve have been obtained from spectroscopic and photometric observations. The body's color, rotation period, pole and shape remain unknown.


(501647) 2014 SD224
(501647) 2014 SD224 is an Aten near-Earth asteroid around 150 meters (490 feet) in diameter. It was discovered on 22 September 2014 when the asteroid was 0.29 AU (43 million km; 110 LD) from Earth and had a solar elongation of 123 degrees. The glare of the Sun had masked the approach of the asteroid as it passed closest approach to Earth on 11 August 2014. The asteroid now has a 6-year observation arc and a well-determined orbit. It also makes close approaches to Venus.


(501647) 2014 SD224, 2020
2014 SD224 was less than 90 degrees from the Sun until September 2020 when it still had a very faint apparent magnitude of 24. The asteroid was recovered on 22 November 2020 by Mt. Lemmon Survey. The asteroid came to opposition (opposite the Sun in the sky) on 12 December 2020 when it had a solar elongation of 149 degrees and a magnitude of 18. It reached a peak brightness on 23 December 2020 at magnitude 16.4, which is still fainter than Pluto.


(501647) 2014 SD224, 2020
The asteroid safely passed closest approach to Earth on 25 December 2020 at 20:20 UT at a distance of 0.02 AU (3.0 million km; 7.8 LD). The 2020 close approach distance is known with an accuracy of roughly ±20 km.


(5025) 1986 TS6
(5025) 1986 TS6, provisional designation 1986 TS6, is a larger Jupiter trojan from the Greek camp, approximately 50 kilometers (31 miles) in diameter. The unusual C/X-type Jovian asteroid is possibly a slow rotator with a rotation period of 250 hours. It was discovered on 5 October 1986 by Slovak astronomer Milan Antal at the Toruń Centre for Astronomy in Piwnice, Poland. It remains unnamed since its numbering in January 1992.


(5025) 1986 TS6, Orbit and classification
1986 TS6 is a Jupiter trojan which stays in a 1:1 orbital resonance with Jupiter. It is located in the leading Greek camp at its L4 Lagrangian point, 60° ahead on its orbit (see Trojans in astronomy).


(5025) 1986 TS6, Orbit and classification
It orbits the Sun at a distance of 4.8–5.6 AU once every 11 years and 10 months (4,331 days; semi-major axis of 5.2 AU). Its orbit has an eccentricity of 0.07 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Piwnice in October 1986.


(5025) 1986 TS6, Physical characteristics
1986 TS6 is an unusual C-/X-type according to Pan-STARRS survey and the SDSS-based taxonomy, and has a V–I color index of 0.830.


(5025) 1986 TS6, Physical characteristics, Rotation period
In November 2009, Stefano Mottola at the Calar Alto Observatory observed 1986 TS6 in a photometric survey of 80 Jupiter trojans. The obtained lightcurve rendered a very long rotation period of 250±25 hours with a brightness variation of 0.2 in magnitude (U=1). However, the Collaborative Asteroid Lightcurve Link (CALL) considers the result as incorrect. As of 2018, no secure period has been obtained.


(5025) 1986 TS6, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite (IRAS) and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1986 TS6 measures 39.84 and 57.83 kilometers in diameter with an albedo of 0.084 and 0.064, respectively. CALL agrees with the results obtained by IRAS, assumes an even lower albedo of 0.0404, and calculates a similar diameter of 57.56 kilometers.


(5025) 1986 TS6, Physical characteristics, Diameter and albedo
Note: missing data was completed with figures from the JPL SBDB () and from the LCDB () for the WISE/NEOWISE and SIMPS catalogs, respectively. These figures are given in italics. Also, listing is incomplete above #100.


(5025) 1986 TS6, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 19 January 1992 (M.P.C. 19489). As of 2018, it has not been named.


(505412) 2013 QO95
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(505448) 2013 SA100
(505448) 2013 SA100, provisional designation 2013 SA100 and also known as o3l79, is a trans-Neptunian object from the classical Kuiper belt in the outermost region of the Solar System. It was discovered on 5 August 2013, by astronomer with the Outer Solar System Origins Survey at the Mauna Kea Observatories, Hawaii, in the United States. The classical Kuiper belt object belongs to the hot population and is a weak dwarf planet candidate, approximately 260 kilometers (160 miles) in diameter.


(505448) 2013 SA100, Orbit and classification
It orbits the Sun at a distance of 38.6–53.8 AU once every 314 years and 1 month (114,732 days; semi-major axis of 46.21 AU). Its orbit has an eccentricity of 0.16 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Mauna Kea Observatories in August 2013.


(505448) 2013 SA100, Orbit and classification
As a cubewano, also known as classical Kuiper belt object, 2013 SA100 is located in between the resonant plutino and twotino populations and has a low-eccentricity orbit. With an inclination above 8°, it belongs to the "stirred" hot population rather than to the cold population with lower inclinations.


(505448) 2013 SA100, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 4 November 2017 and received the number 505448 in the minor planet catalog (M.P.C. 107067). As of 2018, it has not been named.


(505448) 2013 SA100, Physical characteristics
According to the American astronomer Michael Brown, 2013 SA100 measures 255 kilometers in diameter based on an assumed albedo of 0.08. On his website, Brown lists this object as a "possible" dwarf planet (200–400 km), which is the category with the lowest certainty in his 5-class taxonomic system. Similarly, Johnston's archive estimates a diameter 267 kilometers using an albedo of 0.09.


(505448) 2013 SA100, Physical characteristics
Spectroscopic measurements by the OSSOS team at the Gemini Observatory and with the Subaru Telescope gave a g–r and r–z color index of 0.61 and 0.47, respectively. As of 2018, no rotational lightcurve has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.


(505478) 2013 UT15
(505478) 2013 UT15 is an extreme trans-Neptunian object from the scattered disc, located in the outermost regions of the Solar System, approximately 260 kilometers (160 miles) in diameter. It was discovered on 2 August 2013, by astronomers of the Outer Solar System Origins Survey at Mauna Kea Observatory, Hawaii, United States.


(505478) 2013 UT15, Orbit
With a semi-major axis of 196 AU, 2013 UT15 orbits the Sun at a distance of 43.9–348 AU once every 2,742 years. Its orbit has an eccentricity of 0.78 and an inclination of 11° with respect to the ecliptic. It has a similar orbit to (148209) 2000 CR105, except for a smaller inclination.


(505478) 2013 UT15, Orbit
2013 UT15 belongs to a small number of detached objects with perihelion distances of 30 AU or more, and semi-major axes of 150 AU or more. Such objects can not reach such orbits without some perturbing object, which lead to the speculation of planet nine.


(505478) 2013 UT15, Physical characteristics, Spectral type
The object is estimated to have a bluish spectra (BB).


(505478) 2013 UT15, Physical characteristics, Diameter
2013 UT15 has been estimated to measure 243 and 340 kilometers in diameter, based on an assumed albedo of 0.09 and 0.04, respectively. A generic magnitude-to-diameter conversion gives a mean-diameter of 260 kilometers, using with a typical albedo of 0.08 and a published absolute magnitude of 6.2951.


(505478) 2013 UT15, Numbering and naming
2013 UT15 was numbered (505478) by the Minor Planet Center on 4 November 2017 (M.P.C. 107067). As of 2017, this minor planet has not received a name.


(505624) 2014 GU53
(505624) 2014 GU53, provisional designation 2014 GU53, is a trans-Neptunian object and cubewano from the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 8 April 2014, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. The classical Kuiper belt object belongs to the hot population and is a dwarf planet candidate, as it measures approximately 330 kilometers (210 miles) in diameter.


(505624) 2014 GU53, Orbit and classification
2014 GU53 orbits the Sun at a distance of 36.1–51.6 AU once every 290 years and 6 months (106,111 days; semi-major axis of 43.86 AU). Its orbit has an eccentricity of 0.18 and an inclination of 23° with respect to the ecliptic. It has an orbital uncertainty of 2–3. The object's observation arc begins with a precovery taken by Pan-STARRS in April 2012, two years prior to its official discovery observation at Haleakala Observatory in April 2014.


(505624) 2014 GU53, Orbit and classification
2014 GU53 is a cubewano, a classical, low-eccentricity object in the Kuiper belt, located in between the two prominent resonant populations of the plutinos and twotinos. Due to its relatively high inclination, this cubewano belongs to the "stirred" hot population rather than to the larger cold population.


(505624) 2014 GU53, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 4 November 2017 and received the number 505624 in the minor planet catalog (M.P.C. 107069). As of 2018, it has not been named.


(505624) 2014 GU53, Physical characteristics
According to the American astronomer Michael Brown, for an object to be considered as a "possible" dwarf planet, its diameter has to measure between 200 and 400 kilometers. With his estimated diameter of 315 kilometers, this object falls into this category, which is the one with the lowest certainty in Brown's 5-class taxonomic system used on his website. Johnston's archive estimates a diameter 336 kilometers using an albedo of 0.09. As of 2018, no spectral type and color indices, nor a rotational lightcurve have been obtained from spectroscopic and photometric observations. The body's color, rotation period, pole and shape remain unknown.


(505657) 2014 SR339
(505657) 2014 SR339, provisional designation 2014 SR339, is a dark and elongated asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 970 meters (3,200 feet) in diameter. It was discovered on 30 September 2014, by NASA's Wide-field Infrared Survey Explorer telescope (WISE) in Earth's orbit. Closely observed at Goldstone and Arecibo in February 2018, it has a rotation period of 8.7 hours.


(505657) 2014 SR339, Orbit and classification
2014 SR339 is a member of the Apollo asteroids, which cross the orbit of Earth. Apollo's are the largest group of near-Earth objects with nearly 10 thousand known objects. It orbits the Sun at a distance of 0.90–1.70 AU once every 18 months (541 days; semi-major axis of 1.30 AU). Its orbit has an eccentricity of 0.30 and an inclination of 30° with respect to the ecliptic. With an aphelion of 1.70 AU, it is also a Mars-crosser, as it crosses the orbit of the Red Planet at 1.666 AU. The body's observation arc begins with its official discovery observation by WISE in September 2014.


(505657) 2014 SR339, Orbit and classification, Close approaches
As a potentially hazardous asteroid, 2014 SR339 has a minimum orbital intersection distance (MOID) with Earth of less than 0.05 AU and a diameter of greater than 150 meters. The Earth-MOID is currently 0.0354 AU (5,300,000 km), which translates into 13.8 lunar distances (LD).


(505657) 2014 SR339, Orbit and classification, 2018 flyby
On 7 February 2018 it passed 0.054 AU (21 LD) from the Earth when its apparent magnitude brightened to 14. Goldstone observed it until the following day. While this was an 8.1-million kilometer flyby, the next close flyby of 6.3 million km will occur on 5 February 2058, and another 7.6 million km on 8 February 2095. It will also have a 3.2 million km flyby of Mars on 26 September 2048.


(505657) 2014 SR339, Physical characteristics
The asteroid's spectral type is unknown. Due to its unusually low albedo (see below) it is likely a carbonaceous C-type asteroid.


(505657) 2014 SR339, Physical characteristics, Rotation period
On 9 February, radiometric observations by the Arecibo Observatory revealed that the asteroid has an elongated, lumpy shape. The radar images also gave it a rotational period between 8 and 9 hours. A refined period of 8.7 hour agrees with (photometric) lightcurve observations by American photometrist Brian Warner at the Center for Solar System Studies (U82) during 9–11 February 2018, who obtained a period of 8.729 hours with a high brightness amplitude of 0.93 magnitude, which also indicates a non-spheroidal shape (U=3-).


(505657) 2014 SR339, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's WISE telescope, 2014 SR339 measures 0.971 kilometers in diameter and its surface has an albedo of 0.068. During its close approach in February 2018, radiometric observations by Arecibo Observatory determined that the object is at least 1.5 kilometers (0.93 miles) wide.


(505657) 2014 SR339, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 4 November 2017 (M.P.C. 107069). As of 2018, it has not been named.


(506479) 2003 HB57
(506479) 2003 HB57, is an extreme trans-Neptunian object of the extended scattered disc in the outermost region of the Solar System, approximately 180 kilometers in diameter. It was discovered by astronomers at the Mauna Kea Observatory on 26 April 2003.


(506479) 2003 HB57, Description
2003 HB57 orbits the Sun at a distance of 38.1–294.2 AU once every 2141 years and 10 months (782,317 days). Its orbit has an eccentricity of 0.77 and an inclination of 15° with respect to the ecliptic.


(506479) 2003 HB57, Description, Extended scattered disc
It is one of a small group of extreme trans-Neptunian objects with perihelion distances of 30 AU or more, and semi-major axes of 150 AU or more. Such objects can not have reached their present-day orbits without the gravitational influence of some perturbing object, which lead to the speculation of planet nine.


(506479) 2003 HB57, Description, Physical characterization
2003 HB57 has a BR-type spectrum and an estimated diameter of 147 and 200 kilometers based on an assumed albedo of 0.09 and 0.04, respectively.


(508338) 2015 SO20
(508338) 2015 SO20 is an extreme trans-Neptunian object and extended scattered disc object from the outermost region of the Solar System, approximately 220 kilometers (140 miles) in diameter.


(508338) 2015 SO20, Description
This minor planet was first observed as 2010 TF182 on 8 October 2010, by American astronomer Megan Schwamb at ESO's La Silla Observatory in northern Chile. It has also been observed as 2015 SO20 during the Calar Alto TNO Survey (Z79) at the Calar Alto Observatory, Spain, on 20 September 2015.


(508338) 2015 SO20, Description
It orbits the Sun at a distance of 33.2–290.1 AU once every 2054 years and 9 months (semi-major axis of 161 AU). Its orbit has an eccentricity of 0.79 and an inclination of 23° with respect to the ecliptic.


(508338) 2015 SO20, Description, Extended scattered disc
It is one a small number of detached objects with perihelion distances of 30 AU or more, and semi-major axes of 150 AU or more. Such objects can not reach such orbits without some perturbing object, which lead to the speculation of planet nine.


(508338) 2015 SO20, Description, Physical characteristics
Based on an absolute magnitude of 6.5 and an assumed albedo of 0.09, the Johnston's Archive calculated a mean-diameter of 222 kilometers. Michael Brown estimates an albedo of 0.08 with a diameter of 221 kilometers using an absolute magnitude of 6.7. He also considers it a dwarf-planet candidate with a low probability ("possible").


(508869) 2002 VT130
(508869) 2002 VT130, provisional designation 2002 VT130, is a trans-Neptunian object and binary system from the classical Kuiper belt, located in the outermost region of the Solar System. It was discovered by American astronomer Marc Buie at Kitt Peak Observatory on 7 November 2002. The primary measures approximately 324 kilometers (201 miles) in diameter.


(508869) 2002 VT130, Physical properties
The object belongs to the cold classical population and is a binary. The companion was discovered by Keith Noll, Will Grundy, Susan Benecchi, and Hal Levison using Hubble Space Telescope on 21 September 2008. The discovery was announced on 24 September 2009. The moon's apparent separation from the primary was 3023±93 km with an orbital period of 30.76 days. The estimated combined size of 2002 VT130 is about 324 km. The Johnston's archive estimates a mean-diameter of 251 km for the primary, and 205 km for the satellite based on a secondary-to-primary diameter ratio of 0.817.


(508869) 2002 VT130, Physical properties
2002 VT130 shows significant photometric variability with the lightcurve amplitude of 0.21. This may indicate that 2002 VT130 binary is a result of a collision.


(511002) 2013 MZ5
(511002) 2013 MZ5 , provisional designation 2013 MZ5, is a sub-kilometer asteroid, classified as a near-Earth object of the Amor group, estimated to measure approximately 300 meters (1,000 feet) in diameter. It was discovered on 18 June 2013, by astronomers with the Pan-STARRS survey at Haleakala Observatory on the island of Maui, Hawaii, in the United States. It was the 10,000th near-Earth object ever discovered.


(511002) 2013 MZ5, Orbit and classification
2013 MZ5 is an Amor asteroid – a subgroup of near-Earth asteroids that approach the orbit of Earth from beyond, but do not cross it. It orbits the Sun at a distance of 1.3–1.8 AU once every 23 months (707 days; semi-major axis of 1.55 AU). Its orbit has an eccentricity of 0.18 and an inclination of 29° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Haleakala in June 2013.


(511002) 2013 MZ5, Orbit and classification, Close approaches
The asteroid has an Earth minimum orbital intersection distance of 69,000,000 km (0.4613 AU), which translates into 180 lunar distances. It also makes close approaches to Mars. On 28 August 2125, it is projected to pass the Red Planet at a nominal distance of 13,600,000 km (0.0910 AU). With an aphelion of 1.83 AU, it is also a Mars-crossing asteroid.


(511002) 2013 MZ5, 10,000th discovered NEO
2013 MZ5 was the 10,000th near-Earth object (NEO) ever discovered in June 2013 and considered a significant milestone in exploring the NEO population.


(511002) 2013 MZ5, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 31 January 2018 and received the number 511002 in the minor planet catalog (M.P.C. 108621). As of 2019, it has not been named.


(511002) 2013 MZ5, Physical characteristics, Diameter and albedo
2013 MZ5 measures approximately 300 meters in diameter for an absolute magnitude of 20.1 and an assumed albedo 0.18, which is typical value for stony asteroids. A generic magnitude-to-diameter conversion on a wider range of possible albedos (0.30 to 0.05) gives a diameter between 230 and 570 meters. As of 2019, no rotational lightcurve of 2013 MZ5 has been obtained from photometric observations. The object's effective size, rotation period, pole and shape remain unknown.


(5119) 1988 RA1
(5119) 1988 RA1, provisional designation 1988 RA1, is a Jupiter trojan from the Trojan camp, approximately 49 kilometers (30 mi) in diameter. It was discovered on 8 September 1988 by Danish astronomer Poul Jensen at the Brorfelde Observatory near Holbæk, Denmark. The dark Jovian asteroid has a rotation period of 12.8 hours. It has not been named since its numbering in March 1992.


(5119) 1988 RA1, Discovery
On the night this minor planet was discovered at Brorfelde Observatory, Poul Jensen also discovered the Jupiter trojan (6002) 1988 RO, the 12-kilometer size main-belt asteroid (9840) 1988 RQ2, as well as (12689) 1988 RO2, (14364) 1988 RM2, (14837) 1988 RN2, and (24664) 1988 RB1, all main-belt asteroids of inner, middle and outer region of the asteroid belt, respectively.


(5119) 1988 RA1, Discovery
A first precovery was taken at Palomar Observatory in December 1954, extending the asteroid's observation arc by 34 years prior to its discovery.


(5119) 1988 RA1, Orbit and classification
1988 RA1 is a dark Jovian asteroid in a 1:1 orbital resonance with Jupiter. It is located in the trailering Trojan camp at the Gas Giant's L5 Lagrangian point, 60° behind its orbit (see Trojans in astronomy). It is also a non-family asteroid of the Jovian background population. It orbits the Sun at a distance of 4.6–5.8 AU once every 11 years and 10 months (4,333 days; semi-major axis of 5.2 AU). Its orbit has an eccentricity of 0.11 and an inclination of 16° with respect to the ecliptic.


(5119) 1988 RA1, Physical characteristics
1988 RA1 is an assumed, carbonaceous C-type asteroid, while most larger Jupiter trojans are D-types. It has a typical V–I color index of 0.97.


(5119) 1988 RA1, Physical characteristics, Lightcurve
In February 1994, 1988 RA1 was observed by Stefano Mottola and Anders Erikson at La Silla Observatory in Chile, using the ESO 1-metre telescope and its DLR MkII CCD-camera. The photometric observations were used to build a lightcurve showing a rotation period of 12.807±0.016 hours with a brightness variation of 0.31±0.01 magnitude (U=2+).


(5119) 1988 RA1, Physical characteristics, Diameter and albedo
According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the Trojan asteroid measures 49.25 kilometers in diameter and its surface has a low albedo of 0.061, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous asteroid of 0.057 and calculates a diameter of 48.48 kilometers based on an absolute magnitude of 10.3.


(5119) 1988 RA1, Numbering and naming
This minor planet was numbered on 18 March 1992 (M.P.C. 19840). As of 2018, it has not been named.


(516977) 2012 HZ84
(516977) 2012 HZ84, provisional designation 2012 HZ84, is a small trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System, approximately 74 kilometers (46 miles) in diameter. It was discovered on 17 April 2012, by a team of astronomers using one of the Magellan Telescopes in Chile during the New Horizons KBO Search in order to find a potential flyby target for the New Horizons spacecraft. In December 2017, this classical Kuiper belt object was imaged by the spacecraft from afar at a record distance from Earth.


(516977) 2012 HZ84, Orbit and classification
2012 HZ84 orbits the Sun at a distance of 37.2–55.4 AU once every 315 years and 5 months (semi-major axis of 46.33 AU). Its orbit has an eccentricity of 0.20 and an inclination of 5.4° with respect to the ecliptic.


(516977) 2012 HZ84, Orbit and classification
As a cubewano, also known as classical Kuiper belt object, 2012 HZ84 is located in between the resonant plutino and twotino populations and has a low-eccentricity orbit. It belongs to the "stirred" hot population, but only just, since the rather arbitrary threshold to the cold population is typically defined for inclinations lower than 5°.


(516977) 2012 HZ84, Orbit and classification
In the object classification of the Deep Ecliptic Survey, however, 2012 HZ84 has a secured SCATNEAR type, which is a combination of the SCAT and NEAR attributes. It means that the object does not cross the orbit of Neptune but has a higher inclination and eccentricity (SCAT) than the survey's CLASSICAL type objects, and it currently interacts with the dominant ice giant Neptune (NEAR), contrary to the much less gravitationally affected objects of the EXTD type.


(516977) 2012 HZ84, Orbit and classification
The body's observation arc begins with its first observation on 17 April 2012, made by astronomers David Osip, Paul Schechter, David Borncamp, Susan Benecchi and Scott Sheppard of the New Horizons KBO Search (268) team using the Magellan II (Clay) telescope at the Las Campanas Observatory, located in the Atacama desert in Chile.


(516977) 2012 HZ84, Milestone image
When the New Horizons spacecraft imaged 2012 HZ84 in 2017, it was the farthest from Earth ever captured by a spacecraft. The image was taken by the spacecraft's Long Range Reconnaissance Imager (LORRI) on 5 December 2017 at more than 6.12 billion kilometers (40.9 AU) away from Earth. This record was previously held by the Voyager 1 spacecraft which took the iconic Pale Blue Dot image at 6.06 billion kilometers from Earth in February 1990.


(516977) 2012 HZ84, Milestone image
In December 2017, New Horizons also imaged the trans-Neptunian object 2012 HE85, which was first observed by the same team of astronomers the night after they discovered 2012 HZ84. Both objects held this record for little more than one year, until it was superseded on New Year's Eve 2018/19, when New Horizons made its close flyby of 486958 Arrokoth at a new record distance of 6.4 billion kilometers from Earth.


(516977) 2012 HZ84, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 30 April 2018 and received the number 516977 in the minor planet catalog (M.P.C. 110093). As of 2020, it has not been named.


(516977) 2012 HZ84, Physical characteristics
According to Johnston's Archive, the object measures 74 kilometers in diameter based on an assumed albedo of 0.09 and an absolute magnitude of 8.9. As of 2019, no rotational lightcurve of 2012 HZ84 has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.


(523622) 2007 TG422
(523622) 2007 TG422, provisional designation 2007 TG422, is a trans-Neptunian object on a highly eccentric orbit in the scattered disc located in the outermost region of the Solar System, approximately 260 kilometers (160 miles) in diameter. It was discovered on 3 October 2007 by astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica during the Sloan Digital Sky Survey at Apache Point Observatory in New Mexico, United States. According to American astronomer Michael Brown, the bluish object is "possibly" a dwarf planet. It belongs to a group of objects studied in 2014, which lead to the proposition of the hypothetical Planet Nine.


(523622) 2007 TG422, Orbit and classification
2007 TG422 orbits the Sun at a distance of 35.5–910 AU once every 10279 years and 9 months (3,754,688 days; semi-major axis of 473 AU). Its orbit has an exceptionally high eccentricity of 0.92 and an inclination of 19° with respect to the ecliptic.


(523622) 2007 TG422, Orbit and classification
2007 TG422 is an extended scattered disc object, as its large aphelion distance is similar to that of the detached objects such as the sednoids (e.g. 90377 Sedna), its perihelion distance, however, is much lower and still just inside the gravitational influence of Neptune. The object came to perihelion in 2005 at a heliocentric distance of 35.5 AU, and is currently 37.9 AU from the Sun. It was in the constellation of Taurus until 2018, and came to opposition 29 November 2017. The body's observation arc begins at Apache Point in September 2007, one month prior to its official discovery observation. It has since been observed over a hundred times and has an orbital uncertainty of 1.


(523622) 2007 TG422, Orbit and classification, Unstable heliocentric solutions
Given the orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the aphelion (maximum distance from the Sun) of this object. With a 2007 epoch the object had an approximate period of about 10,611 years with aphelion at 930 AU. But using a 2012 epoch shows a period of about 13,512 years with aphelion at 1099 AU. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates.


(523622) 2007 TG422, Orbit and classification, Unstable heliocentric solutions
Using JPL Horizons with an observed orbital arc of 5 years, the barycentric orbital elements for epoch 2008-May-14 generate a semi-major axis of 503 AU and a period of 11,300 years. For comparison, Sedna has a barycentric semi-major axis of 506 AU and a period of 11,400 years. Both (308933) 2006 SQ372 and (87269) 2000 OO67 take longer than Sedna and 2007 TG422 to orbit the Sun using barycentric coordinates.


(523622) 2007 TG422, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111778). As of 2018, it has not been named.


(523622) 2007 TG422, Physical characteristics
2007 TG422 is expected to have a low albedo (see below) due to its blue (neutral) color.


(523622) 2007 TG422, Physical characteristics, Diameter and albedo
According to the Johnston's archive and to Michael Brown, 2007 TG422 measures 222 and 331 kilometers in diameter, based on an absolute magnitude of 6.5 and an assumed standard albedo of 0.09 and 0.04 for the body's surface, respectively. As of 2018, no rotational lightcurve has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. Michael Brown's website lists it as a possible dwarf planet.


(523635) 2010 DN93
(523635) 2010 DN93, provisional designation 2010 DN93, is a trans-Neptunian object from in the scattered disc located in the outermost region of the Solar System. It was discovered on 26 February 2010, by astronomers with the Pan-STARRS survey at Haleakala Observatory on the island of Maui, Hawaii, in the United States. The object is "probably" a dwarf planet as it measures approximately 490 kilometers (300 miles) in diameter. It was numbered in 2018 and remains unnamed.


(523635) 2010 DN93, Orbit and classification
2010 DN93 orbits the Sun at a distance of 45.1–65.5 AU once every 411 years (150,152 days; semi-major axis of 55.29 AU). Its orbit has an eccentricity of 0.18 and an inclination of 41° with respect to the ecliptic.


(523635) 2010 DN93, Orbit and classification
This distant minor planet is a trans-Neptunian object and a member of the scattered disc population. Scattered-disc objects are thought to have been ejected from the classical Kuiper belt into their current orbits by gravitational interactions with Neptune, and typically have highly eccentric orbits and perihelia of less than 38 AU.


(523635) 2010 DN93, Orbit and classification
2010 DN93 has also been considered a detached object, since its relatively low eccentricity of 0.18, and its perihelion distance of 45.1 AU are hard to reconcile with the celestial mechanics of a scattered-disc object.


(523635) 2010 DN93, Orbit and classification
This has led to some uncertainty as to the current theoretical understanding of the outermost Solar System. The theories include close stellar passages, unseen planet/rogue planets/planetary embryos in the early Kuiper belt, and resonance interaction with an outward-migrating Neptune. The Kozai mechanism is capable of transferring orbital eccentricity to a higher inclination. 2010 DN93 seems to belong to the same group as 2005 TB190.


(523635) 2010 DN93, Numbering and naming
The body's observation arc begins with a precovery taken by the Sloan Digital Sky Survey at Apache Point Observatory in March 2003, almost seven years prior to its official discovery observation at Haleakala. It was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111778). As of 2018, it has not been named.


(523635) 2010 DN93, Physical characteristics, Diameter and albedo
2010 DN93 has an absolute magnitude of 4.8. According to the Johnston's archive and astronomer Michael Brown, it measures 486 and 490 kilometers in diameter, based on an assumed albedo for the body's surface of 0.09 and 0.07, respectively. This is roughly a quarter the size of Pluto. According to Brown, 2010 DN93 is "probably" a dwarf planet. As of 2018, no physical characteristics have been determined from photometric observations. The body's color, rotation period, pole and shape remain unknown.


(523639) 2010 RE64
(523639) 2010 RE64, provisional designation 2010 RE64, is a trans-Neptunian object in the scattered disc located in the outermost region of the Solar System, approximately 570 kilometers (350 miles) in diameter. It was discovered on 11 July 2010 by the Pan-STARRS-1 survey at the Haleakala Observatory, Hawaii, in the United States. American astronomer Michael Brown considers it a "highly likely" dwarf planet.


(523639) 2010 RE64, Classification and orbit
2010 RE64 has an observation arc of 1774 days, and there are currently no known precovery images to help refine its orbit. It is currently 53.7 AU from the Sun. Based on JPL's best-fit solution for the orbit, it reached aphelion around 1829. It is estimated to come to perihelion around 2079. Although the discovery is credited to Pan-STARRS, the object was first announced in a Minor Planet Electronic Circular by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte observing from La Silla Observatory on 9 September 2010.


(523639) 2010 RE64, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111778). As of 2018, it has not been named.


(523639) 2010 RE64, Physical characteristics
Assuming a generic trans-Neptunian albedo of 0.09, it is about 580 kilometers in diameter. However, since the true albedo is unknown and it has an absolute magnitude of 4.4, it could easily be from about 350 to 780 km in diameter (for typical albedos of 0.05 to 0.25). Michael Brown estimates a similar diameter of 561 kilometers, also using a geometric albedo of 0.09 and a fainter 4.6 absolute magnitude.


(523643) 2010 TY53
(523643) 2010 TY53, provisional designation 2010 TY53 is a trans-Neptunian object and centaur located in the outermost region of the Solar System. With an absolute magnitude of 5.7, it approximately measures 325 kilometers (200 miles) in diameter. It was discovered on 4 August 2010 by the Pan-STARRS-1 survey at the Haleakala Observatory, Hawaii, in the United States. According to American astronomer Michael Brown, it is "possibly" a dwarf planet.


(523643) 2010 TY53, Orbit and classification
2010 TY53 orbits the Sun at a distance of 21.1–56.6 AU once every 241 years and 11 months (88,365 days; semi-major axis of 38.83 AU). Its orbit has an eccentricity of 0.46 and an inclination of 22° with respect to the ecliptic. The body's observation arc begins with a precovery at Palomar Observatory in October 2004, or almost six years prior to its official discovery observation by Pan-STARRS.


(523643) 2010 TY53, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111778). As of 2018, it has not been named.


(523643) 2010 TY53, Physical characteristics, Diameter and albedo
According to the Johnston's archive and to Michael Brown, 2010 TY53 measures 321 and 329 kilometers in diameter, based on an absolute magnitude of 5.7 and 5.8 and an assumed standard albedo of 0.09 and 0.08 for the body's surface, respectively. As of 2018, no physical characteristics have been determined from photometric observations. The body's rotation period, pole and shape remain unknown.


(523645) 2010 VK201
(523645) 2010 VK201, provisional designation 2010 VK201, is a trans-Neptunian object and member of the classical Kuiper belt, approximately 500 kilometers (310 miles) in diameter. It was discovered on 1 November 2010, by the Pan-STARRS 1 survey at Haleakala Observatory, Hawaii, United States. The "likely" dwarf planet has a rotation period of 7.6 hours. It was numbered in September 2018 and remains unnamed.


(523645) 2010 VK201, Orbit and classification
Located beyond the orbit of Neptune, 2010 VK201 is a non-resonant classical Kuiper belt object (cubewano) of the so-called hot population, which have higher inclinations than those of the cold population. According to Michael Brown it is a "likely" dwarf planet. It orbits the Sun at a distance of 38.0–48.1 AU once every 282 years and 2 months (103,060 days; semi-major axis of 43.02 AU). Its orbit has an eccentricity of 0.12 and an inclination of 29° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Haleakala in November 2010. 2010 VK201 has been identified as a member of the Haumea family in a dynamical study led by Proudfoot and Ragozzine in 2019.


(523645) 2010 VK201, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111778). As of 2018, it has not been named.


(523645) 2010 VK201, Physical characteristics
2010 VK201 is an assumed carbonaceous body with a relatively low albedo (see below).


(523645) 2010 VK201, Physical characteristics, Rotation period
In 2011, a rotational lightcurve of 2010 VK201 was obtained from photometric observations in the S- and R-band by Susan Benecchi and Scott Sheppard taken with Carnegie's 2.5-meter Irénée du Pont telescope at the Las Campanas Observatory in Chile. Lightcurve analysis gave a rotation period of 7.59±0.05 hours with a brightness amplitude of 0.30 magnitude (U=2).


(523645) 2010 VK201, Physical characteristics, Diameter and albedo
According to Michael Brown and the Collaborative Asteroid Lightcurve Link, 2010 VK201 measures 501 and 505 kilometers in diameter, based on an absolute magnitude of 4.6 and 5.0, assuming an albedo of 0.07 and 0.10 for the body's surface, respectively. The Johnston's archive estimates a smaller diameter of 443 kilometers.


(523662) 2012 MU2
(523662) 2012 MU2, provisional designation 2012 MU2, is a sub-kilometer asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered on 18 June 2012 by astronomers of the Catalina Sky Survey at an apparent magnitude of 19.9 using a 0.68-meter (27 in) Schmidt–Cassegrain telescope. It has an estimated diameter of 240 meters (790 ft). The asteroid was listed on Sentry Risk Table with a Torino Scale rating of 1 on 23 June 2012.


(523662) 2012 MU2, Orbit and classification
2012 MU2 is a member of the Apollo asteroids, a group of near-Earth objects with an Earth-crossing orbit. It orbits the Sun at a distance of 1.0–3.1 AU once every 2 years and 11 months (1,076 days; semi-major axis of 2.06 AU). Its orbit has an eccentricity of 0.51 and an inclination of 11° with respect to the ecliptic.


(523662) 2012 MU2, Orbit and classification
On 24 June 2012 with an observation arc of 6 days, 2012 MU2 showed a 1 in 7,140 chance of impacting Earth on 1 June 2015. It was removed from the Sentry Risk Table on the next day (25 June).


(523662) 2012 MU2, Orbit and classification
With an observation arc of 113 days, the JPL Small-Body Database (solution JPL 42 dated 2013-Aug-05) shows that 2012 MU2 may make a very close approach to asteroid 29 Amphitrite on 8 April 2179. The minimum approach distance is about 0.000032 AU (4,800 km; 3,000 mi), but the maximum distance is 0.14 AU (21,000,000 km; 13,000,000 mi). The nominal approach is 0.047 AU (7,000,000 km; 4,400,000 mi).


(523662) 2012 MU2, Orbit and classification
The Earth approach in 2015 occurred on 15 May 2015 at a distance of 0.11485 AU (17,181,000 km; 10,676,000 mi).


(523662) 2012 MU2, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111778). As of 2018, it has not been named.


(523671) 2013 FZ27
(523671) 2013 FZ27, provisional designation 2013 FZ27, is a trans-Neptunian object and likely dwarf planet, located in the Kuiper belt in the outermost region of the Solar System, approximately 570 kilometers (350 miles) in diameter. It was discovered on 16 March 2013, by American astronomers Scott Sheppard and Chad Trujillo at the CTIO in Chile. Numbered in 2018, this minor planet has not been named.


(523671) 2013 FZ27, Orbit and classification
2013 FZ27 is a trans-Neptunian object (TNO), located beyond the orbit of Neptune (30.1 AU). The Johnston's archive classifies it as an unspecific "other TNO", meaning that the minor planet is neither a resonant nor a classical TNO. Astronomer Michael Brown considers 2013 FZ27 to be a "likely" dwarf-planet candidate, a moderate-probability third place out of his five-level ranking system, as its estimated diameter is a little under 600 kilometers. Taking the mean of the two magnitudes, and using the standard 0.25 ~ 0.05 range for minor planets of unknown albedo, a wider 335 to 748 km spread of possibilities can be calculated for the actual diameter.


(523671) 2013 FZ27, Orbit and classification
2013 FZ27 orbits the Sun at a distance of 37.6–58.7 AU once every 334 years and 1 month (122,013 days; semi-major axis of 48.14 AU). Its orbit has an eccentricity of 0.22 and an inclination of 14° with respect to the ecliptic.


(523671) 2013 FZ27, Orbit and classification
The body's observation arc begins with a precovery taken by the Sloan Digital Sky Survey on 20 February 2001, over 10 years prior to its official discovery observation at Cerro Tololo. The object was first announced on 2 April 2014, when American astronomers Scott Sheppard and Chad Trujillo at the CTIO in Chile published their observations in a Minor Planet Electronic Circular. At the time the object was at 49 AU from the Sun and had an apparent magnitude of 21.1. The Pan-STARRS-1 survey at the Haleakala Observatory, Hawaii, in the United States also found precovery observations of 2013 FZ27 after 2013 FZ27 was announced and reported them to the Minor Planet Center at a later date.


(523671) 2013 FZ27, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111778). The body was given the wrong discovery credit in the initial MPC Circular and The Minor Planet Center issued an Errata on April 6, 2019 on MPC 112429 correcting the mistake and gives the discovery credit of 2013 FZ27 to Scott S. Sheppard and Chad Trujillo. As of August 2019, it has not been named.


(523671) 2013 FZ27, Physical characteristics, Diameter and albedo
According to Michael Brown and the Johnston's archive, 2013 FZ27 measures 561 and 584 kilometers in diameter, based on an absolute magnitude of 4.6 and 4.4 respectively. Both sources assume a standard albedo of 0.09 for the body's surface. As of 2018, no physical characteristics have been determined from photometric observations. The body's rotation period, pole and shape remain unknown.


(523674) 2013 MA12
(523674) 2013 MA12, provisional designation 2013 MA12, is a classical trans-Neptunian object and dwarf planet candidate from the Kuiper belt, located in the outermost region of the Solar System, approximately 340 kilometers (210 miles) in diameter. The cubewano belongs to the hot population. It was discovered on 26 July 2011, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States.


(523674) 2013 MA12, Orbit and classification
2013 MA12 orbits the Sun at a distance of 39.1–44.3 AU once every 269 years and 1 month (98,276 days; semi-major axis of 41.68 AU). Its orbit has an eccentricity of 0.06 and an inclination of 23° with respect to the ecliptic.


(523674) 2013 MA12, Orbit and classification
As a cubewano, also known as classical Kuiper belt object, it is located in between the resonant plutino and twotino populations and has a low-eccentricity orbit. With an inclination above 8°, it belongs to the "stirred" hot population rather than to the cold population with low inclinations. The body's observation arc begins with its official discovery observation in July 2011 at Haleakala Observatory.


(523674) 2013 MA12, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018, together with hundreds of other centaurs, trans-Neptunian and near-Earth objects (see catalog entries from 523585 to 523800). This object received the number 523674 in the minor planet catalog (M.P.C. 111779). As of 2018, it has not been named.


(523674) 2013 MA12, Physical characteristics
According to the American astronomer Michael Brown, 2013 MA12 measures 343 kilometers in diameter based on an assumed albedo of 0.08. On his website, Brown lists this object as a "possible" dwarf planet (200–400 km), which is the category with the lowest certainty in his 5-class taxonomic system. Similarly, Johnston's archive estimates a diameter 336 kilometers using an albedo of 0.09.


(523674) 2013 MA12, Physical characteristics
As of 2018, no spectroscopic or photometric observations have been made. The body's spectral type, color indices, rotation period, pole and shape remain unknown.