(523676) 2013 UL10
(523676) 2013 UL10 (prov. designation: 2013 UL10) is a reddish centaur with cometary activity orbiting the Sun between Jupiter and Uranus. It was discovered on 18 August 2010, by a team of astronomers with the Pan-STARRS survey at the Haleakalā Observatory, Hawaii. It is the first centaur known to have both comet-like activity and red surface colors. It is also one of the smallest centaurs, with a nucleus of no more than 10 kilometers (6.2 miles) in diameter. As of 2021, it has not been named.


(523676) 2013 UL10, Orbit and classification
This object belongs to the centaurs, a dynamically unstable population of small Solar System bodies with chaotic orbits between the classical asteroids and the trans-Neptunian objects. Centaurs are considered to be objects with short lifetimes of approximately one million years, transitioning from the inactive population of Kuiper belt objects to the active group of Jupiter-family comets. 2013 UL10 orbits the Sun at a distance of 6.2–13.7 AU once every 31 years and 3 months (11,404 days; semi-major axis of 9.92 AU). Its orbit has a high eccentricity of 0.38 and an inclination of 19° with respect to the ecliptic.


(523676) 2013 UL10, Orbit and classification
It has a Tisserand's parameter with respect to Jupiter (TJ) of 2.94, near the threshold of 3, typically used to distinguish asteroids from Jupiter-family comets. On 4 June 2014, the object came to perihelion at 6.2 AU and has since been moving away from the Sun. As of 2021 the object is at 10.7 AU, The body's observation arc begins with its official discovery observation at Haleakalā Observatory in August 2010.


(523676) 2013 UL10, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018, receiving the number (523676) in the minor planet catalog (M.P.C. 111778). As of 2021, it has not been named. According to the established naming conventions, it will be named after one of the many centaurs from Greek mythology, which are creatures with the upper body of a human and the lower body and legs of a horse.


(523676) 2013 UL10, Physical characteristics
As with other populations, the centaurs show a bimodal distribution of colors: red and blue-grey. Cometary-like activity is well known among the grey centaurs, prominently represented by 2060 Chiron, which is also the namesake of the Chiron-type comets. However, outgassing activity of red centaurs (e.g. 5145 Pholus) has not been observed. 2013 UL10 is the first of the group of red centaurs to display clear evidence of cometary activity.


(523676) 2013 UL10, Physical characteristics
In October 2014, 2013 UL10 was observed by astronomers using the Large Monolithic Imager of the 4.3-meter Discovery Channel Telescope in Arizona. An overall reddish color was determined with B–V, V–R and B–R color indices of 0.97±0.02, 0.67±0.02 and 1.64±0.03, respectively. It was the intrinsically faintest object observed for this study, with an absolute magnitude 13.46.


(523676) 2013 UL10, Physical characteristics
In December 2015, observations with the Galileo National Telescope on the Canary Islands revealed that 2013 UL10 exhibits comet-like activity. Apart from the object's dust coma, the astronomers also deduced a diameter of no more than 10 kilometers (6.2 miles) for this centaur's nucleus, assuming an albedo of 0.12. Further photometric observations gave a dust production rate of 10 kg/s near the object's perihelion at 6.2 AU.


(523676) 2013 UL10, Physical characteristics
The Collaborative Asteroid Lightcurve Link an estimates a diameter of kilometers 15.3 based on a albedo of 0.057 (carbonaceous) and on an absolute magnitude of 12.8. As of 2021, no rotational lightcurve of 2013 UL10 has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.


(523683) 2014 CP23
(523683) 2014 CP23, provisional designation 2014 CP23, is a trans-Neptunian object from the scattered disc located in the outermost region of the Solar System It was discovered on 29 October 2011, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. The dwarf planet candidate measures approximately 267 kilometers (170 miles) in diameter.


(523683) 2014 CP23, Orbit and classification
2014 CP23 orbits the Sun at a distance of 38.1–66.5 AU once every 378 years and 5 months (138,225 days; semi-major axis of 52.32 AU). Its orbit has an eccentricity of 0.27 and an inclination of 29° with respect to the ecliptic. It is a scattered-disc object on a moderately eccentric orbit that never comes closer than 8 AU to the orbit of Neptune.


(523683) 2014 CP23, Orbit and classification
The body's observation arc begins with a precovery taken by the Sloan Digital Sky Survey on January 2003, or more than 8 years prior to its official discovery observation at Haleakala Observatory.


(523683) 2014 CP23, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 and received the number 523683 in the minor planet catalog (M.P.C. 111779). As of 2018, it has not been named.


(523683) 2014 CP23, Physical characteristics
According to American astronomer Michael Brown and the Johnston's archive, 2014 CP23 measures 266 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.


(523684) 2014 CQ23
(523684) 2014 CQ23, provisional designation 2014 CQ23, is a trans-Neptunian object and cubewano from the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 13 March 2011, 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.


(523684) 2014 CQ23, Orbit and classification
2014 CQ23 is a cubewano, a classical, low-eccentricity object in the Kuiper belt, located in between the two resonant plutino and twotino populations, and belongs to the "stirred" hot population rather than to the cold population with low inclinations.


(523684) 2014 CQ23, Orbit and classification
It orbits the Sun at a distance of 38.7–53.7 AU once every 313 years and 8 months (114,565 days; semi-major axis of 46.16 AU). Its orbit has an eccentricity of 0.16 and an inclination of 9° with respect to the ecliptic.


(523684) 2014 CQ23, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 and received the number 523687 in the minor planet catalog (M.P.C. 111779). As of 2018, it has not been named.


(523684) 2014 CQ23, Physical characteristics
According to the American astronomer Michael Brown, 2014 CQ23 measures 343 kilometers in diameter based on an assumed albedo of 0.08. On his website, Michael 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 321 kilometers using an albedo of 0.09. As of 2018, neither a spectral type or the color indices have been determined, nor a rotational lightcurve has been obtained from spectroscopic and photometric observations. The body's color, rotation period, pole and shape remain unknown.


(523687) 2014 DF143
(523687) 2014 DF143, provisional designation 2014 DF143, is a trans-Neptunian object and cubewano from the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 12 April 2011, 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 350 kilometers (220 miles) in diameter.


(523687) 2014 DF143, Orbit and classification
2014 DF143 orbits the Sun at a distance of 40.9–44.8 AU once every 280 years and 4 months (102,379 days; semi-major axis of 42.83 AU). Its orbit has an eccentricity of 0.05 and an inclination of 24° with respect to the ecliptic. It has an orbital uncertainty of 1–2. The object's observation arc begins with a precovery taken by the Sloan Digital Sky Survey in March 2002, 9 years prior to its official discovery observation at Haleakala Observatory in March 2011.


(523687) 2014 DF143, Orbit and classification
2014 DF143 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.


(523687) 2014 DF143, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 and received the number 523687 in the minor planet catalog (M.P.C. 111779). As of 2018, it has not been named.


(523687) 2014 DF143, Physical characteristics
According to the American astronomer Michael Brown, 2014 DF143 measures 358 kilometers in diameter based on an assumed albedo of 0.08. On his website, Michael 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 352 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.


(523692) 2014 EZ51
(523692)  2014 EZ51, prov. designation: 2014 EZ51, is a trans-Neptunian object and possible dwarf planet in the scattered disc, approximately 700 kilometres (430 miles) in diameter. It was discovered on 18 April 2010, by the Pan-STARRS 1 survey at Haleakala Observatory, Hawaii, United States.


(523692) 2014 EZ51, Orbit and classification
2014 EZ51 orbits the Sun at a distance of 40.4–64.4 AU once every 379 years and 3 months (138,537 days; semi-major axis of 52.4 AU). Its orbit has an eccentricity of 0.23 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Haleakala in April 2010. According to Michael Brown it is a "highly likely" dwarf planet.


(523692) 2014 EZ51, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111779). As of 2021, it has not been named.


(523692) 2014 EZ51, Physical characteristics
According to Michael Brown and the Johnston's archive, 2014 EZ51 measures 626 and 770 kilometers in diameter, based on an absolute magnitude of 4.2 and 3.8, with an assumed albedo of 0.10 and 0.09, respectively. The MPC/JPL databases give an absolute magnitude of 3.92. On 25 February 2019, a stellar occultation by 2014 EZ51 was observed in New Zealand. From these observations, a lower limit of 575 km was placed for its mean diameter.


(523692) 2014 EZ51, Physical characteristics
As of 2021, no physical characteristics have been determined from photometric observations. The body's rotation period, pole and shape remain unknown.


(523702) 2014 HW199
(523702) 2014 HW199, provisional designation 2014 HW199, is a trans-Neptunian object from the classical Kuiper belt, located in the outermost region of the Solar System. It was discovered on 30 January 2011, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. The classical Kuiper belt object is also a dwarf planet candidate, as it measures approximately 290 kilometers (180 miles) in diameter.


(523702) 2014 HW199, Orbit and classification
2014 HW199 is a cubewano from the classical Kuiper belt. It is located in between the resonant plutino and twotino populations and has a low-eccentricity orbit. With an inclination significantly higher than 4–7°, it belongs to the "stirred" hot population rather than to the cold population with lower inclinations.


(523702) 2014 HW199, Orbit and classification
It orbits the Sun at a distance of 38.1–55.2 AU once every 318 years and 6 months (116,334 days; semi-major axis of 46.64 AU). Its orbit has an eccentricity of 0.18 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins with a precovery at Haleakala Observatory in May 2010, or eight months prior to its official discovery observation.


(523702) 2014 HW199, 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 523702 in the minor planet catalog (M.P.C. 111779). As of 2018, it has not been named.


(523702) 2014 HW199, Physical characteristics
Johnston's archive estimates a diameter of 280 kilometers based on an assumed albedo of 0.09, while American astronomer Michael Brown, calculates a diameter of 302 kilometers, using an estimated albedo of 0.08 and an absolute magnitude of 6.0.


(523702) 2014 HW199, Physical characteristics
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.


(523706) 2014 HF200
(523706) 2014 HF200, provisional designation 2014 HF200, is a trans-Neptunian object on an eccentric orbit from the scattered disc, located in the outermost region of the Solar System. It was discovered on 20 May 2012, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. The dwarf planet candidate measures approximately 300 kilometers (190 miles) in diameter.


(523706) 2014 HF200, Orbit and classification
2014 HF200 is a scattered disc object and orbits the Sun at a distance of 35.5–88.0 AU once every 485 years and 4 months (177,277 days; semi-major axis of 61.76 AU). Its orbit has an eccentricity of 0.43 and an inclination of 10° with respect to the ecliptic.


(523706) 2014 HF200, Orbit and classification
The body's observation arc begins with a precovery taken by Pan-STARRS in May 2010, two years prior to its official discovery observation. It still has a small orbital uncertainty of 1 and 2, respectively.


(523706) 2014 HF200, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 and received the number 523706 in the minor planet catalog (M.P.C. 111779). As of 2018, it has not been named.


(523706) 2014 HF200, Physical characteristics
According to the Johnston's archive and American astronomer Michael Brown, 2014 HF200 measures 293 and 302 kilometers in diameter based on an assumed albedo of 0.09 and 0.08, respectively. On his website, Michael 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.


(523719) 2014 LM28
(523719) 2014 LM28, provisional designation 2014 LM28, is a trans-Neptunian object and centaur, approximately 46 kilometers (29 miles) in diameter. It was discovered on 16 May 2013, by the Pan-STARRS 1 survey at Haleakala Observatory, Hawaii, United States. The object's orbit is highly inclined and very eccentric, with a perihelion closer to the Sun than Uranus and at an aphelion 17 times farther from the Sun than Neptune.


(523719) 2014 LM28, Orbit and classification
2014 LM28 orbits the Sun at a distance of 16.8–538.9 AU once every 4631 years and 1 month (1,691,491 days; semi-major axis of 277.83 AU). Its orbit has an eccentricity of 0.94 and an inclination of 85° with respect to the ecliptic. The body's observation arc begins with its official discovery observation by Pan-STARRS at Haleakala Observatory in May 2013.


(523719) 2014 LM28, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111779). As of 2018, it has not been named.


(523719) 2014 LM28, Features
2014 LM28 has a highly inclined orbit typical of scattered objects and orbits nearly perpendicular to the ecliptic.


(523727) 2014 NW65
(523727) 2014 NW65, provisional designation: 2014 NW65, is a large centaur from the outer Solar System, approximately 220 kilometers (140 miles) in diameter. It was discovered on 14 July 2010 by astronomers with the Pan-STARRS-1 survey at Haleakala Observatory, Hawaii, in the United States. According to American astronomer Michael Brown, it is "possibly" a dwarf planet. The minor planet was numbered in 2018 and has not been named.


(523727) 2014 NW65, Orbit and classification
2014 NW65 is a member of the centaurs, an inward-moving population of bodies transiting from the Kuiper belt to the group of Jupiter-family comets. Their eccentric orbits are often in between those of Jupiter and Neptune, that is, they have a semi-major axis of typically 5.5 to 30.1 AU. Centaurs are cometary-like bodies. They have a short dynamical lifetime due to the perturbing forces exerted on them by the Solar System's outer planets.


(523727) 2014 NW65, Orbit and classification
It orbits the Sun at a distance of 11.2–35.1 AU once every 111 years and 4 months (40,670 days; semi-major axis of 23.15 AU). Its orbit has an eccentricity of 0.52 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its official discovery observation in July 2010.


(523727) 2014 NW65, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018, receiving the number (523727) in the minor planet catalog  (M.P.C. 111779). As of 2021, it has not been named. According to the established naming conventions, it will be named after one of the many centaurs from Greek mythology, which are creatures with the upper body of a human and the lower body and legs of a horse.


(523727) 2014 NW65, Physical characteristics, Diameter and albedo
2014 NW65 has an absolute magnitude of 6.6. According to the Johnston's archive and astronomer Michael Brown, it measures 212 and 225 kilometers in diameter, based on an assumed albedo for the body's surface of 0.09 and 0.08, respectively. It is one of the largest centaurs, comparable in size with 2060 Chiron, 10199 Chariklo, and 54598 Bienor.


(523727) 2014 NW65, Physical characteristics, Diameter and albedo
According to Brown, 2014 NW65 is "possibly" a dwarf planet, which is the weakest of the 5 categories established by the astronomer. As of 2021, no physical characteristics have been determined from photometric observations. The body's color, rotation period, pole and shape remain unknown.


(523731) 2014 OK394
(523731) 2014 OK394, also known as 1995 SN55, is a trans-Neptunian object that orbits in the outer Solar System beyond the orbit of Neptune. First observed as 1995 SN55 by Spacewatch on 20 September 1995, it was a lost minor planet with an insufficiently defined orbit with only 36 days of observations. On 8 October 2010, it was rediscovered by the Pan-STARRS 1 survey and later announced as 2014 OK394 in July 2016. It was not until November 2020 when amateur astronomers S. Deen and K. Ly identified 2014 OK394 and 1995 SN55 as the same object. This identification was confirmed and announced by the Minor Planet Center in January 2021.


(523731) 2014 OK394
Once thought to be a centaur crossing the orbits of the gas giants, 1995 SN55 is now known to be a trans-Neptunian object in a 3:5 orbital resonance with Neptune. With an estimated diameter between 160–280 kilometers (99–170 miles), it was formerly considered one of the largest centaurs.


(523731) 2014 OK394, Observations, First observation and loss
1995 SN55 was near perihelion 35.4 AU from the Sun when it was first observed in 1995, by astronomers Nichole Danzl and Arianna Gleason of the Spacewatch survey at Kitt Peak Observatory in Arizona, United States. It was only observed 14 times over 36 days, from 20 September to 26 October 1995. The discovery observations of 1995 SN55 were published and announced by the Minor Planet Center on 11 June 1999. By 2020 the 3-sigma uncertainty in the heliocentric distance to the original orbit solution for 1995 SN55 was approximately ±20 AU (3.0 billion km).


(523731) 2014 OK394, Observations, Recovery
On 30 November 2020, amateur astronomers S. Deen and K. Ly identified 1995 SN55 as the 3:5 resonant trans-Neptunian object (523731) 2014 OK394, which was discovered by Pan-STARRS 1 in 2010. The identification was published by the Minor Planet Center on 27 January 2021.


(523731) 2014 OK394, Classification and orbit
2014 OK394 orbits the Sun at an average distance of 42.33 AU once every 275 years. Its orbit has an eccentricity of 0.16 and an inclination of 4° with respect to the ecliptic plane. Over the course of its orbit, its distance from the Sun ranges from 35.4 AU at perihelion to 49.3 AU at aphelion. 2014 OK394 is in a 3:5 mean-motion orbital resonance with Neptune; for every three orbits it makes, Neptune orbits five times. Its orbit has a minimum orbit intersection distance approximately 5.6 AU (840 million km; 520 million mi) from Neptune's orbital path.


(523731) 2014 OK394, Numbering and naming
2014 OK394 was numbered by the Minor Planet Center on 25 September 2018 and received the number 523731 in the minor planet catalog. The alternate provisional designation 1995 SN55 was given by the Minor Planet Center on 27 January 2021 after the two objects were linked. As of 2021, it has not been named.


(523759) 2014 WK509
(523759) 2014 WK509, provisional designation 2014 WK509 is a trans-Neptunian object and possible dwarf planet form the scattered disc, located in the outermost regions of the Solar System. It was discovered on 14 September 2010, by Pan-STARRS at Haleakala Observatory on the island of Maui, Hawaii, in the United States. The object's diameter has been estimated to measure approximately 600 kilometers.


(523759) 2014 WK509, Orbit and classification
2014 WK509 belongs to the scattered disc population. It orbits the Sun at a distance of 40.1–61.6 AU once every 362 years and 6 months (132,399 days; semi-major axis of 50.8 AU). Its orbit has an eccentricity of 0.21 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins on 14 September 2011 at Haleakala, more than 3 years prior to its official first observation. Its orbit still has a high uncertainty.


(523759) 2014 WK509, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111779). As of 2018, it has not been named.


(523759) 2014 WK509, Physical characteristics
Based on an absolute magnitude of 4.4, and an assumed albedo of 0.09, the Johnston's archive estimates a mean-diameter of approximately 584 kilometers (363 mi), while astronomer Michael Brown calculates a diameter of 574 kilometers (357 mi) using a slightly fainter magnitude of 4.5. Brown also characterizes the object as a "likely dwarf planet", an intermediate category in his classification scheme (also see list of candidates).


(523759) 2014 WK509, Physical characteristics
As of 2018, no rotational lightcurve of this object has been obtained from photometric observations. The object's rotation period, pole and shape remain unknown.


(523764) 2014 WC510
(523764) 2014 WC510, is a binary trans-Neptunian object discovered on 8 September 2011 by the Pan-STARRS survey at the Haleakalā Observatory in Hawaii. It was found by Pan-STARRS on 20 November 2014 and was announced later in July 2016 after additional observations and precovery identifications. It is in the Kuiper belt, a region of icy objects orbiting beyond Neptune in the outer Solar System. It is classified as a plutino, a dynamical class of objects in a 2:3 orbital resonance with Neptune.


(523764) 2014 WC510
On 1 December 2018, a team of astronomers observed a stellar occultation by the object, which revealed that it is a compact binary system consisting of two separate components in close orbit around each other. The primary and secondary components are estimated to have diameters of around 180 km (110 mi) and 140 km (87 mi), respectively.


(523764) 2014 WC510, Observations, Discovery
Before the announcement of its discovery, 2014 WC510 had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter Ritchey–Chrétien telescope, located at the Haleakalā Observatory atop the Hawaiian island of Maui. The accredited observers using the telescope were B. Gibson, T. Goggia, N. Primak, A. Schultz, and M. Willman.


(523764) 2014 WC510, Observations, Discovery
The object was first identified on 20 November 2014, though it was announced later in a Minor Planet Electronic Circular published on 17 July 2016, after additional observations by Pan-STARRS had been found, preceding the team's original observation from 2014. While 2014 WC510 is the object's first and only provisional designation assigned by the Minor Planet Center, the date of discovery is considered to be on 8 September 2011, which was the earliest known observation of the object before it was assigned a minor planet number.


(523764) 2014 WC510, Observations, Occultation
On 1 December 2018, 2014 WC510 occulted a 15th-magnitude double star, blocking out its starlight for a maximal duration of approximately 11 seconds. The stellar occultation was observed by astronomers and citizen scientists across the West Coast of the United States and Canada. Of the 41 participating sites, six of them reported dimmings in the star's brightness, signifying likely positive detections of the occultation. Five of these sites reported two consecutive dimmings due to the occulted star's double nature; 2014 WC510 occulted one of the two stars being observed. These observations were part of a campaign coordinated by the Research and Education Collaborative Occultation Network (RECON), a citizen science project dedicated to observing occultations by trans-Neptunian objects.


(523764) 2014 WC510, Observations, Occultation
Prior to the occultation, 2014 WC510 had only been observed by Pan-STARRS over an observation arc of 3 years. The calculated orbit from these Pan-STARRS observations had significant uncertainty, which would have been unreliable for predicting occultations. In an effort to reduce the orbital uncertainty, the RECON project collaborated with the Pan-STARRS project to do a precovery search of archival Pan-STARRS images to gather extensive astrometric positions of 2014 WC510. Follow-up observations by Pan-STARRS were also conducted through 2016–2018 and helped extend 2014 WC510's observation arc to 6.3 years. Although an observation arc of this length is generally unreliable for predicting occultations especially by distant objects, this was compensated by Pan-STARRS's highly accurate astrometric system, allowing for 2014 WC510's orbital uncertainty to be significantly reduced.


(523764) 2014 WC510, Orbit and classification
2014 WC510 is classified as a plutino, a subgroup of the resonant trans-Neptunian objects located in the inner region of Kuiper belt. Named after the group's largest member, Pluto, the plutinos are in a 2:3 mean-motion orbital resonance with Neptune. That is, they complete two orbits around the Sun for every three orbits that Neptune takes. 2014 WC510 orbits the Sun at an average distance of 39.24 astronomical units (5.87×109 km; 3.65×109 mi), taking 245.8 years to complete a full orbit. This is characteristic of all plutinos, which have orbital periods around 250 years and semi-major axes around 39 AU.


(523764) 2014 WC510, Orbit and classification
Like Pluto, 2014 WC510's orbit is elongated and inclined to the ecliptic. 2014 WC510 has an orbital eccentricity of 0.25 and an orbital inclination of 19.5 degrees with respect to the ecliptic. Over the course of its orbit, 2014 WC510's distance from the Sun varies from 29.5 AU at perihelion (closest distance) to 48.9 AU at aphelion (farthest distance). 2014 WC510 has last passed aphelion in the early 20th century, and is now moving closer to the Sun, approaching perihelion by 2032. Simulations by the Deep Ecliptic Survey show that 2014 WC510 can acquire a perihelion distance (qmin) as small as 28.7 AU over the next 10 million years.


(523764) 2014 WC510, Binary system
Observations of the December 2018 occultation revealed that 2014 WC510 is a compact binary system consisting of two separate components in close orbit around each other. Of the six sites that reported positive detections of the occultation, one site located in Bishop, California, detected a shorter dimming event separate from the main detections by the other five sites located south of it. A 2020 study led by Rodrigo Leiva and Marc Buie analyzed the occultation data and determined that the detection from Bishop was most likely an occultation by a secondary component of 2014 WC510.


(523764) 2014 WC510, Binary system
Since the two components were only observed for a short period of time during the occultation, the binary system's orbital parameters have not been determined. The projected separation distance between the primary and secondary is 349 ± 29 km (217 ± 18 mi), derived from an angular separation of 16±1 milliarcseconds. Assuming a density of 1 g/cm3 for both components, their mutual orbital period would likely be under one day. 2014 WC510 has the smallest observed component separation of all known binary TNOs as of 2020, followed by (48639) 1995 TL8 (~420 km) and 47171 Lempo (~870 km). Such close binary TNOs would be difficult to resolve in direct imaging due to their characteristic small separation distances between their components.


(523764) 2014 WC510, Binary system
Most models of the formation of the Solar System indicate that most TNOs have formed as binaries, hence they are expected to be common especially in the Kuiper belt population. While most known binary TNOs appear to have wide mutual orbits, close binary TNOs similar to 2014 WC510 are thought to have a higher chance of survival after their formation. 2014 WC510 belongs to the population of smaller TNOs, which are expected to have a primordial origin similar to the classical Kuiper belt object 486958 Arrokoth.


(523764) 2014 WC510, Physical characteristics
Assuming a circular projected shape for the components' occultation profiles, the diameters of the primary and secondary are estimated to be 181 ± 16 km (112.5 ± 9.9 mi) and 138 ± 32 km (86 ± 20 mi), respectively. The diameter ratio of the secondary to the primary is 0.76:1.00—the secondary component is approximately 75% as large as the primary. Since the mutual orbit of the components is undetermined, the mass and density of the 2014 WC510 system cannot be derived. The individual components of the 2014 WC510 system are among the smallest trans-Neptunian objects with sizes measured with stellar occultations, following the Kuiper belt object 486958 Arrokoth (~30 km).


(523764) 2014 WC510, Physical characteristics
Given the components' estimated diameters and their combined absolute magnitude of 7.2, their calculated geometric albedos indicate that they have dark surfaces, reflecting about 5% of incident visible light. However, the estimated geometric albedo may be subject to a systematic error depending on the true shapes and photometric properties of the components, resulting in a significant uncertainty of ±2%. Nonetheless, 2014 WC510 is one of the darkest objects measured with stellar occultations, being darker than 486958 Arrokoth.


(523764) 2014 WC510, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 and received the number 523764 in the minor planet catalog. As of 2020, it has not been named.


(523775) 2014 YB35
(523775) 2014 YB35, provisional designation 2014 YB35, is a stony near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 300 meters (980 feet) in diameter. It was discovered on 27 December 2014 by the Catalina Sky Survey at the Catalina Station in Arizona, United States. In March 2015, a minor-planet moon, less than half the size of its primary, was discovered by radar astronomers at Goldstone Observatory. The primary body of the binary system has a rotation period of 3.3 hours, while the secondary's orbital period remains unknown.


(523775) 2014 YB35, Orbit and classification
2014 YB35 is a member of the Apollo asteroids, a group of near-Earth object with an Earth-crossing orbit. It orbits the Sun at a distance of 1.0–2.8 AU once every 2 years and 7 months (939 days; semi-major axis of 1.88 AU). Its orbit has an eccentricity of 0.48 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins at with its official discovery observation at Catalina Station in December 2014.


(523775) 2014 YB35, Orbit and classification, Close encounters
It passed by Earth on 27 March 2015 at 06:21 UTC at a distance of 4,473,807 ± 155 km (2,779,895 ± 96 mi), or 11.7 lunar distances, and a relative speed of 10.16 km/s (6.31 mi/s). 2014 YB35's next encounter with Earth will be in 2033, at a distance of approximately 3,330,000 km (2,070,000 mi).


(523775) 2014 YB35, Satellite
The Goldstone Deep Space Communications Complex was scheduled to observe this object on 20 March 2015, at which time it was expected they could obtain coarse radar images and continuous wave spectra, which may help determine the asteroid's composition. These observations showed a small companion less than 150 meters across orbiting the asteroid, with an unknown orbit.


(523775) 2014 YB35, 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.


(523794) 2015 RR245
(523794) 2015 RR245, provisional designation 2015 RR245, is a large trans-Neptunian object of the Kuiper belt in the outermost regions of the Solar System. It was discovered on 9 September 2015, by the Outer Solar System Origins Survey at Mauna Kea Observatories on the Big island of Hawaii, in the United States. The object is in a rare 2:9 resonance with Neptune and measures approximately 600 kilometers in diameter. 2015 RR245 may have a satellite according to a study announced by Noyelles et al. in a European Planetary Science Congress meeting in 2019.


(523794) 2015 RR245, Discovery
A first precovery of 2015 RR245 was taken at the Cerro Tololo Observatory in Chile on 15 October 2004. It was first observed by a research team led by Michele Bannister while poring over images that the Canada–France–Hawaii Telescope in Hawaii took in September 2015 as part of the Outer Solar System Origins Survey (OSSOS), and later identified in images taken at Sloan Digital Sky Survey and Pan-STARRS between 2008 and 2016. The discovery was formally announced in a Minor Planet Electronic Circular on 10 July 2016.


(523794) 2015 RR245, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111779). As of 2020, it has not been named.


(523794) 2015 RR245, Orbit and classification
As of 2018, 2015 RR245 has a reasonably well defined orbit with an uncertainty of 3. It orbits the Sun at a distance of 33.8–128.6 AU once every 731 years and 6 months (for reference, Neptune's orbit is at 30 AU). Its orbit has an eccentricity of 0.58 and an inclination of 8° with respect to the ecliptic.


(523794) 2015 RR245, Orbit and classification
2015 RR245 is among the most distant known Solar System objects. As of 2018, it is 63 AU from the Sun. It will make its closest approach to the Sun in 2093, when it will reach an apparent magnitude of 21.2.


(523794) 2015 RR245, Orbit and classification, 2:9 resonance
Additional precovery astrometry from the Sloan Digital Sky Survey and the Pan-STARRS1 survey shows that 2015 RR245 is a resonant trans-Neptunian object, securely trapped in a 2:9 mean motion resonance with Neptune, meaning that this minor planet orbits the Sun twice in the same amount of time it takes Neptune to complete 9 orbits. The object is unlikely to have been trapped in the 2:9 resonance for the age of Solar System. It is much more likely that it has been hopping between various resonances and got trapped in the 2:9 resonance in the last 100 million years.


(523794) 2015 RR245, Physical characteristics, Diameter and albedo
Its exact size is uncertain, but the best estimate is around 670 km (420 mi) in diameter, assuming an albedo of 0.12 (within a wider range of 500 to 870 km, based on albedos of 0.21 to 0.07). For comparison, Pluto, the largest object in the Kuiper belt, is about 2,374 km (1,475 mi) in diameter. Astronomer Michael Brown assumes an albedo of 0.11 and calculates a diameter of 626 km, while the Johnston's Archive gives a diameter of 770 kilometers, based on an assumed albedo of 0.09. All of these estimates assume that 2015 RR245 is a single object, the discovery of a large satellite means that the size is likely to be smaller.


(523794) 2015 RR245, Satellite
2015 RR245 is suspected to be binary, though the size of the secondary body (moon) has not been determined. If the moon significantly contributes to the observed brightness of the primary, the size of 2015 RR245 may therefore be substantially smaller than estimates that assumed the system's total brightness was from a single object. Once the orbit of the satellite is determined, the mass and density of the 2015 RR245 can be determined. 2015 RR245 was be observed by the Hubble Space Telescope in 2020.


(523972) 1999 CW8
(523972) 1999 CW8, provisional designation 1999 CW8, is a bright carbonaceous asteroid and sub-kilometer near-Earth object of the Apollo group, first observed on 12 February 1999, by astronomers of the Lincoln Near Earth Asteroid Research program at Lincoln Laboratory ETS in New Mexico, United States.


(523972) 1999 CW8, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114615). As of 2019, it has not been named.


(523972) 1999 CW8, Orbit and classification
1999 CW8 is an Apollo asteroid that crosses Earth's orbit. It orbits the Sun at a distance of 0.9–3.6 AU once every 3 years and 4 months (1,221 days; semi-major axis of 2.24 AU). Its orbit has an eccentricity of 0.60 and an inclination of 34° with respect to the ecliptic. The asteroid never approaches Earth closer than 0.2 AU in the foreseeable future, but occasionally makes close approaches to Mars of 0.07 AU. It makes one such approach in 2073, at 0.067 AU, and another one in 2103, at 0.094 AU. Due to 1999 CW8's relatively high inclination, although it passes closer to the Sun than the Earth (0.9 AU), it never comes closer than 0.2 AU.


(523972) 1999 CW8, Physical characteristics
It is a carbonaceous B-type asteroid, relatively rare in the asteroid belt but common in the inner Solar System. Based on an absolute magnitude of 18.6, and an assumed albedo of 0.159 (derived from the B-type asteroid 2 Pallas), the asteroid can be estimated to have a mean-diameter of approximately 640 meters. If it impacted the Earth would cause significant damage, but not as much as the Cretaceous–Paleogene extinction event progenitor, which brought about a mass extinction, as it is only 1/20 to 1/10 the size. However, it is unlikely to come close enough to Earth to impact it, or even become a risk of impact.


(524366) 2001 XR254
(524366) 2001 XR254, provisional designation 2001 XR254, is a trans-Neptunian object and binary system from the classical Kuiper belt, located in the outermost region of the Solar System. The cubewano belongs to the cold population and measures approximately 171 kilometers (110 miles). It was first observed on 10 December 2001, by astronomers at the Mauna Kea Observatory, Hawaii. Its 140-kilometer sized companion was discovered by the Hubble Space Telescope in June 2006.


(524366) 2001 XR254, Discovery and orbit
2001 XR254 was discovered on 10 December 2001 by David C. Jewitt, Scott S. Sheppard and Jan Kleyna using 2.2-meter University of Hawaii reflector on Mauna Kea. 2001 XR254 belongs to the dynamically cold population of the classical Kuiper belt objects, which small orbital eccentricities and inclinations. Their semi-major axes reside mainly in the interval 40–45 AU.


(524366) 2001 XR254, Satellite
2001 XR254 is a binary consisting of two components of approximately equal size. Assuming that both components have the same albedo, the primary is estimated to be about 170 km in diameter. The size of the secondary (satellite) in this case is estimated at about 140 km. The total mass of the system is about 4×1018 kg. The average density of both components is about 1 g/cm3.


(524366) 2001 XR254, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114619). As of 2019, it has not been named.


(524366) 2001 XR254, Physical properties
The surfaces of both components of 2001 XR254 appear to have a neutral color.


(524435) 2002 CY248
(524435) 2002 CY248, provisional designation 2002 CY248, is a trans-Neptunian object and weak dwarf-planet candidate from the classical Kuiper belt in the outermost region of the Solar System, approximately 400–450 kilometers (250–280 mi) in diameter. It was first observed on 6 February 2002, by American astronomer Marc Buie at the Kitt Peak National Observatory in Arizona, United States.


(524435) 2002 CY248, Orbit and classification
2002 CY248 orbits the Sun at a distance of 39.4–53.1 AU once every 314 years and 6 months (114,859 days; semi-major axis of 46.2 AU). Its orbit has an eccentricity of 0.15 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins at Kitt Peak with its official first observation on 6 February 2002. A 10-million-year integration of the orbit shows that it is a Classical Kuiper belt object that does not get closer to the Sun than 38.8 AU (5.80 billion km) or further than 54 AU.


(524435) 2002 CY248, Physical characteristics
Based on an absolute magnitude of 5.2, and an assumed albedo of 0.09, the Johnston's archive estimates a mean-diameter of approximately 404 kilometers (251 mi), while astronomer Michael Brown assumes an albedo of 0.06 and calculates a diameter of 449 kilometers (279 mi) using a fainter magnitude of 5.5. Brown also characterizes the object as a "probable dwarf planet", an intermediate category in his classification scheme (also see list of candidates).


(524435) 2002 CY248, Physical characteristics
As of 2018, no rotational lightcurve of this object has been obtained from photometric observations. The object's rotation period, pole and shape remain unknown.


(524435) 2002 CY248, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114619). As of 2019, it has not been named.


(524522) 2002 VE68
(524522) 2002 VE68, provisional designation 2002 VE68, is a sub-kilometer sized asteroid and temporary quasi-satellite of Venus. It was the first such object to be discovered around a major planet in the Solar System. In a frame of reference rotating with Venus, it appears to travel around it during one Venerean year but it actually orbits the Sun, not Venus.


(524522) 2002 VE68, Discovery, orbit and physical properties
It was discovered on 11 November 2002 at Lowell Observatory. As of February 2013, 2002 VE68 has been observed telescopically 457 times with a data-arc span of 2,947 days and it was the target of Doppler observations in 5 occasions; therefore, its orbit is very well determined. Its semi-major axis of 0.7237 AU is very similar to that of Venus but its eccentricity is rather large (0.4104) and its orbital inclination is also significant (9.0060°). The spectrum of 2002 VE68 implies that it is an X-type asteroid and hence an albedo of about 0.25 should be assumed. The body is calculated to measure 236 meters in diameter. Its rotational period is 13.5 hours and its light curve has an amplitude of 0.9 mag which hints at a very elongated body, perhaps a contact binary.


(524522) 2002 VE68, Quasi-satellite dynamical state and orbital evolution
The existence of retrograde satellites or quasi-satellites was first considered by J. Jackson in 1913 but none was discovered until almost 100 years later. 2002 VE68 was the first quasi-satellite to be discovered, in 2002, although it was not immediately recognized as such. 2002 VE68 was identified as a quasi-satellite of Venus by Seppo Mikkola, Ramon Brasser, Paul A. Wiegert and Kimmo Innanen in 2004, two years after the actual discovery of the object.


(524522) 2002 VE68, Quasi-satellite dynamical state and orbital evolution
From the perspective of a hypothetical observer in a frame of reference rotating with Venus, it appears to travel around the planet during one Venusian year although it does not orbit Venus but the Sun like any other asteroid. As quasi-satellite, this minor body is trapped in a 1:1 mean-motion resonance with Venus. Besides being a Venus co-orbital, this Aten asteroid is also a Mercury grazer and an Earth crosser. 2002 VE68 exhibits resonant (or near-resonant) behavior with Mercury, Venus and Earth. It seems to have been co-orbital with Venus for only the last 7,000 years, and is destined to be ejected from this orbital arrangement about 500 years from now. During this time, its distance to Venus has been and will remain larger than about 0.2 AU (3·107 km).


(524522) 2002 VE68, Potentially hazardous asteroid
2002 VE68 is included in the Minor Planet Center list of Potentially Hazardous Asteroids (PHAs) because it comes relatively frequently to within 0.05 AU of Earth. Approaches as close as 0.04 AU occur with a periodicity of 8 years due to its near 8:13 resonance with Earth. 2002 VE68 was discovered during the close approaches of 11 November 2002. During the last close encounter on 7 November 2010, 2002 VE68 approached Earth within 0.035 AU (13.6 Lunar distances), brightening below 15th magnitude. Its next fly-by with Earth happened on 4 November 2018 at 0.038 AU (5,700,000 km; 3,500,000 mi). Numerical simulations indicate that an actual collision with Earth during the next 10,000 years is not likely, although dangerously close approaches to about 0.002 AU are possible, a distance potentially within Earth's Hill sphere.


(524522) 2002 VE68, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114620). As of 2020, it has not been named.


(52747) 1998 HM151
(52747) 1998 HM151, also written as (52747) 1998 HM151, is a cubewano. It has a perihelion (closest approach to the Sun) at 41.902 AU and an aphelion (farthest approach from the Sun) at 47.500 AU. It is 116 km in diameter. It was discovered on 29 April 1998, by astronomers at the Mauna Kea Observatory, Hawaii.


(52760) 1998 ML14
(52760) 1998 ML14, provisional designation 1998 ML14, is a stony asteroid, classified as near-Earth object of the Apollo group and potentially hazardous asteroid, approximately 1 kilometer in diameter. It was discovered on 24 June 1998, by the LINEAR survey at the Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico.


(52760) 1998 ML14, Description
1998 ML14 orbits the Sun at a distance of 0.9–3.9 AU once every 3 years and 9 months (1,366 days). Its orbit has an eccentricity of 0.62 and an inclination of 2° with respect to the ecliptic. It is also a Mars-crossing asteroid.


(52760) 1998 ML14, Description
Shortly after its discovery, 1998 ML14 was imaged by radar at Goldstone and Arecibo.


(52760) 1998 ML14, Description
The study showed that the asteroid has a rotation period of 15 hours, and a shape that is roughly spherical, with some steep protrusions and large craters.


(52760) 1998 ML14, Description
On 24 August 2013 it passed at a distance of 21.9 Lunar distances. It was hoped to be observed by Goldstone radar.


(52760) 1998 ML14, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 16 February 2003. As of 2018, it has not been named.


(527603) 2007 VJ305
(527603) 2007 VJ305, provisional designation 2007 VJ305, is an extrem trans-Neptunian object from the extended scattered disc on a highly eccentric orbit in the outermost region of the Solar System. It measures approximately 250 kilometers (160 miles) in diameter and is "possibly" a dwarf planet. The rather reddish extended scattered disc object belongs to the group of extreme trans-Neptunian objects. It was discovered on 4 November 2007 by astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica at the Apache Point Observatory in New Mexico, United States.


(527603) 2007 VJ305, Orbit and classification
2007 VJ305 orbits the Sun at a distance of 35.1–347 AU once every 2640 years and 11 months (964,601 days; semi-major axis of 191.1 AU). Its orbit has an exceptionally high eccentricity of 0.82 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins with a precovery taken during the Sloan Digital Sky Survey at Apache Point in November 2000. It has a minimum orbital intersection distance with Neptune of 5.4 AU.


(527603) 2007 VJ305, Orbit and classification
It belongs to a small group of detached objects with perihelion distances of 30 AU or more, and semi-major axes of 150 AU or more. These extreme trans-Neptunian objects (ETNOs) can not reach such orbits without some perturbing object, which lead to the speculation of Planet Nine.


(527603) 2007 VJ305, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114650). As of 2019, it has not been named.


(527603) 2007 VJ305, Physical characteristics
This ETNO's color is rather reddish with an intermediary IR spectral type and a B–R color index of 1.44.


(527603) 2007 VJ305, Physical characteristics, Diameter and albedo
According to the Johnston's archive and to American astronomer Michael Brown, 2007 VJ305 measures 202 and 279 kilometers in diameter based on an assumed albedo of 0.09 and 0.04, respectively. On his website, Michael Brown lists this object as "possibly" a dwarf planet (200–400 km) which is the least certain class in his 5-class taxonomic system.


(527603) 2007 VJ305, Physical characteristics, Rotation period and shape
As of 2019, no rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.


(527604) 2007 VL305
(527604) 2007 VL305, provisional designation 2007 VL305, is an inclined Neptune trojan that shares Neptune's orbit in the L4 Lagrangian point. It was discovered on 4 November 2007, by astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica at the Apache Point Observatory in New Mexico, United States, although images from 2005 have also been recovered. It measures approximately 160 kilometers in diameter and was the sixth Neptune trojan to be discovered. As of 2016, it is 34.1 AU from Neptune.


(527604) 2007 VL305, Orbit and classification
Neptune trojans can be considered resonant trans-Neptunian objects in a 1:1 mean-motion orbital resonance with Neptune. These trojans have a semi-major axis and an orbital period very similar to Neptune's (30.10 AU; 164.8 years).


(527604) 2007 VL305, Orbit and classification
2007 VL305 belongs to the leading L4 group, which orbits 60° ahead of Neptune's orbit. It orbits the Sun with a semi-major axis of 29.926 AU at a distance of 28.1–31.7 AU once every 163 years and 9 months (59,795 days). Its orbit has an eccentricity of 0.06 and an inclination of 28° with respect to the ecliptic. Its inclination is almost as high as that of 2011 HM102.


(527604) 2007 VL305, Physical characteristics, Diameter
The discoverers estimate that 2007 VL305 has a mean-diameter of 160 kilometers based on a magnitude of 22.2. Based on a generic magnitude-to-diameter conversion, it measures approximately 110 kilometers in diameter using an absolute magnitude of 7.9 with an assumed albedo of 0.10.


(527604) 2007 VL305, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114650). As of 2019, it has not been named. If named, it will follow the naming scheme already established with 385571 Otrera and 385695 Clete, which is to name these objects after figures related to the Amazons, an all-female warrior tribe that fought in the Trojan War on the side of the Trojans against the Greek.


(52768) 1998 OR2
(52768) 1998 OR2 (provisional designation 1998 OR2) is an asteroid on an eccentric orbit, classified as a near-Earth object and potentially hazardous asteroid of the Amor group, with a diameter of 2 kilometers (1.2 mi). It was discovered on 24 July 1998, by astronomers of the Near-Earth Asteroid Tracking (NEAT) program at the Haleakala Observatory, Hawaii. It is one of the brightest and therefore largest potentially hazardous asteroids known to exist. With an observation arc of 32 years, the asteroid has a well-determined orbit, and its trajectory is well known through the year 2197. The asteroid's orbit is only potentially hazardous on a time scale of thousands of years.


(52768) 1998 OR2, Orbit and classification
1998 OR2 is a member of the dynamical Amor group of near-Earth asteroids, and therefore does not currently cross Earth's orbit. The asteroid's closest approach to the Sun is just outside Earth's farthest distance from the Sun. When the asteroid has a perihelion point less than 1.017 AU (Earth's aphelion), it is classified an Apollo asteroid. This asteroid's category flips back and forth as time passes, due to minor perturbations of its orbit.


(52768) 1998 OR2, Orbit and classification
It orbits the Sun at a distance of 1.0–3.7 AU once every 3 years and 8 months (1,344 days; semi-major axis of 2.38 AU). Its orbit has a high eccentricity of 0.57 and an inclination of 6° with respect to the ecliptic. With its sufficiently large aphelion, this asteroid is also classified as a Mars-crosser, crossing the orbit of Mars at 1.66 AU.


(52768) 1998 OR2, Orbit and classification
The body's observation arc begins with a precovery published by the Digitized Sky Survey taken at the Siding Spring Observatory in June 1986, more than 12 years prior to its official discovery observation at Haleakala Observatory, Hawaii.


(52768) 1998 OR2, Orbit and classification, Close approaches
With an absolute magnitude of approximately 15.8, 1998 OR2 is one of the brightest and presumably largest-known potentially hazardous asteroids (see PHA-list). It currently has an Earth minimum orbital intersection distance of 0.0154 AU (2,300,000 km), which translates into 6.0 lunar distances (LD). On 16 April 2079, this asteroid will make a near-Earth encounter at a safe distance of 0.0118 AU (4.59 LD), and pass the Moon at 0.0092 AU (3.6 LD). The asteroid's orbit is only potentially hazardous on a time scale of hundreds, if not thousands, of years.


(52768) 1998 OR2, Orbit and classification, Close approaches
On 29 April 2020 at 09:56 UTC, the asteroid passed at a distance of 0.042 AU (6.3 million km; 16 LD) from Earth. With observations as recent as April 2020 and a 32-year observation arc, the 2020 close approach distance was known with an accuracy of roughly ±6 km. (For comparison, Venus will be 0.29 AU or 43 million km or 110 LD from Earth on 3 June 2020.)


(52768) 1998 OR2, Physical characteristics
According to observations by the NASA IRTF telescope during the ExploreNEOs Warm Spitzer program, 1998 OR2 is a rather rare L-type asteroid. Delay-Doppler radar observations by the Arecibo Observatory in April 2020 have shown that 1998 OR2 bears a large, crater-like concavity in its shape. These radar observations have also resolved several other topographic features on the asteroid's surface, such as hills and ridges.


(52768) 1998 OR2, Physical characteristics, Rotation period
In 2009, rotational lightcurves of 1998 OR2 were obtained from photometric observations by astronomers in Salvador, Brazil, and during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS). Lightcurve analysis gave a rotation period of 3.198 and 4.112 hours with a brightness amplitude of 0.29 and 0.16 magnitude, respectively (U=2/2+). The latter rotation period of 4.1 hours was later confirmed by radar observations of the asteroid in 2020.


(52768) 1998 OR2, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link (CALL) assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 2.15 km (1.34 mi) based on an absolute magnitude of 15.7.


(52768) 1998 OR2, Naming
As of 2020, this minor planet has not been named.


(528219) 2008 KV42
(528219) 2008 KV42 (provisionally designated: 2008 KV42, and nicknamed Drac) is a trans-Neptunian object and the first one with a retrograde orbit to be discovered. This retrograde motion with an orbital inclination of 103° suggests that it is the missing link between its source in the Hills cloud and Halley-type comets, thus providing further insight into the evolution of the outer Solar System. The object measures approximately 77 kilometers (48 miles) in diameter. With a semi-major axis of 42 AU, it takes about 269 years to complete an orbit around the Sun.


(528219) 2008 KV42
Officially discovered on 31 May 2008, the discovery was announced on 16 July 2008, by the Canada–France Ecliptic Plane Survey team led by Brett Gladman. The discovery team nicknamed 2008 KV42 "Drac" after Count Dracula.


(528219) 2008 KV42, Discovery and naming
The discovery of 2008 KV42 was announced on 16 July 2008 by the Canada–France Ecliptic Plane Survey team led by Brett Gladman from the University of British Columbia. The announcement was made during the "Asteroids, Comets, Meteors" meeting held in Baltimore, Maryland, followed by a Minor Planet Electronic Circular on the same day and an IAU Circular on 18 July. The discovery was made using images obtained on 31 May from the 3.5-meter Canada-France-Hawaii Telescope, followed by further observations until 8 July from the Whipple Observatory and Cerro Tololo.


(528219) 2008 KV42, Discovery and naming
The discovery team nicknamed 2008 KV42 Drac because of its high inclination in reference to its orbital plane resembling Count Dracula's ability to walk on walls.


(528219) 2008 KV42, Orbit
2008 KV42 is the first trans-Neptunian object (TNO) with a retrograde orbit to be discovered. With a semi-major axis of 41.7 AU, it was discovered while at a distance of 32 AU and has a perihelion at roughly the distance of Uranus.


(528219) 2008 KV42, Orbit
The object's 103° inclination makes its almost perpendicular to the ecliptic, and is, as of July 2017, one of only six objects known to have inclination and perihelion larger than 60° and 15 AU, respectively. The other six are: 2002 XU93, 2007 BP102, 2010 WG9, 2011 KT19, and 2014 LM28.


(528219) 2008 KV42, Orbit
Its unusual orbit suggests that 2008 KV42 may have been perturbed inwards from its source, most likely in the Hills cloud, by an unknown gravitational disturbance. Its discovery may reveal the source regions for Halley-type comets which also have an retrograde orbit, but their origin remains unknown. 2008 KV42 itself is believed to be in an intermediate stage towards becoming a comet, thus helping to further explain the formation and evolution of the outer Solar System.


(528219) 2008 KV42, Orbit, Planet Nine
2008 KV42 may even provide evidence of Planet Nine. The Kozai effect inside the mean-motion resonances with Planet Nine may cause a periodic exchange between its inclination and its eccentricity. When the elongated perpendicular centaurs get too close to a giant planet, orbits such as that of 2008 KV42 are created.


(528381) 2008 ST291
(528381) 2008 ST291, provisional designation 2008 ST291, is a 1:6 resonant trans-Neptunian object and dwarf planet candidate located in the outermost region of the Solar System that takes almost a thousand years to complete an orbit around the Sun. It was discovered on 24 September 2008 by American astronomers Megan Schwamb, Michael Brown and David Rabinowitz at the Palomar Observatory in California, with no known earlier precovery images.


(528381) 2008 ST291, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114657). As of 2019, it has not been named.


(528381) 2008 ST291, Orbit and classification
2008 ST291 is located at the 1:6 Neptune resonance of 99 AU meaning that it completes roughly 1 orbit for every 6 orbits Neptune makes. It orbits the Sun at a distance of 42.3–157.5 AU once every 998 years and 4 months (semi-major axis of 99.89 AU). Its orbit has an eccentricity of 0.58 and an inclination of 21° with respect to the ecliptic. Currently located at 60.9 AU from the Sun, the object came to perihelion in 1954.


(528381) 2008 ST291, Physical characteristics
Based on an absolute magnitude of 4.4, 2008 ST291 is estimated by the Johnston's Archive to be about 584 kilometres (363 mi) in diameter, assuming a typical albedo of 0.09 for trans-Neptunian objects. Astronomer Mike Brown estimates a slightly smaller 549 km from the same albedo and a fainter 4.6 magnitude. The Asteroid Dynamic Site records a brighter 4.3 magnitude, which calculates to 612 km using the same albedo (and same formula as Johnston's); using the average of these magnitudes and a standard assumed minor planet albedo range of 0.25 ~ 0.05, possible sizes of 345 to 773 km are produced.


(529366) 2009 WM1
(529366) 2009 WM1, provisional designation 2009 WM1, is a sub-kilometer asteroid and near-Earth object of the Apollo group, approximately 280 meters (920 feet) in diameter. After its discovery by the Catalina Sky Survey at the Catalina Station in Arizona, United States, this potentially hazardous asteroid was briefly listed at a Torino Scale of 1 and a cumulative Palermo Scale of −0.87. It was removed from the Sentry Risk Table on 26 June 2013.


(529366) 2009 WM1, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114667). As of 2019, it has not been named.


(529366) 2009 WM1, Orbit and classification
2009 WM1 orbits the Sun at a distance of 0.98–1.38 AU once every 15 months (468 days; semi-major axis of 1.18 AU). Its orbit has an eccentricity of 0.17 and an inclination of 26° with respect to the ecliptic.


(529366) 2009 WM1, Orbit and classification
Even though 2009 WM1 has an Earth MOID of 0.00009 AU (13,000 km; 8,400 mi), the orbit and future close approaches are well determined with an orbital uncertainty of 1.


(529366) 2009 WM1, Orbit and classification
On 23 November 2059, 2009 WM1 will pass 0.0046 AU (690,000 km; 430,000 mi) from Earth. On 23 November 2199, it will make another close approach at a distance of 0.0005 AU (75,000 km; 46,000 mi) to 0.069 AU, but since it is a close approach and the exact distance in uncertain, future close approaches after 2199 are uncertain.


(529366) 2009 WM1, 2014 passage
The 21 May 2014 Earth close approach of 0.3622 AU (54,180,000 km; 33,670,000 mi) should allow a refinement to the orbit. From 7 May 2014 until 2 June 2014 the asteroid will be brighter than apparent magnitude 20. The asteroid will come to opposition on 18 May 2014 when it will be up all night.


(532037) 2013 FY27
(532037) 2013 FY27 is a trans-Neptunian object and binary system that belongs to the scattered disc (like Eris). Its discovery was announced on 31 March 2014. It has an absolute magnitude (H) of 3.2. 2013 FY27 is a binary object, with two components approximately 740 kilometres (460 mi) and 190 kilometres (120 mi) in diameter. It is the ninth-intrinsically-brightest known trans-Neptunian object, and is approximately tied (to within measurement uncertainties) as the largest unnamed object in the Solar System.


(532037) 2013 FY27, Orbit
2013 FY27 orbits the Sun once every 449 years. It will come to perihelion around November 2202, at a distance of about 35.6 AU. It is currently near aphelion, 80 AU from the Sun, and, as a result, it has an apparent magnitude of 22. Its orbit has a significant inclination of 33°. The sednoid 2012 VP113 and the scattered-disc object 2013 FZ27 were discovered by the same survey as 2013 FY27 and were announced within about a week of one another.


(532037) 2013 FY27, Physical properties
2013 FY27 has a diameter of about 740 kilometres (460 mi), placing it at a transition zone between medium-sized and large TNOs. Using the Atacama Large Millimeter Array and Magellan Telescopes, its albedo was found to be 0.17, and its colour to be moderately red. 2013 FY27 is one of the largest moderately red TNOs. The physical processes that lead to a lack of such moderately red TNOs larger than 800 kilometres (500 mi) are not yet well understood.


(532037) 2013 FY27, Physical properties
The brightness of 2013 FY27 varies by less than 0.06 mag over hours and days, suggesting that it either has a very long rotation period, an approximately spheroidal shape, or a rotation axis pointing towards Earth.


(532037) 2013 FY27, Physical properties
Brown estimated, prior to the discovery of its satellite, that 2013 FY27 was very likely to be a dwarf planet, due to its large size. However, Grundy et al. calculate that bodies such as 2013 FY27, less than about 1000 km in diameter, with albedos less than ≈0.2 and densities of ≈1.2 g/cm3 or less, may retain a degree of porosity in their physical structure, having never collapsed into fully solid bodies.


(532037) 2013 FY27, Satellite
Using Hubble Space Telescope observations taken in January 2018, Scott Sheppard found a satellite around 2013 FY27, 0.17 arcseconds away and 3.0±0.2 mag fainter than the primary. The discovery was announced on 10 August 2018. Assuming the two components have equal albedos, they are about 740 kilometres (460 mi) and 190 kilometres (120 mi) in diameter, respectively. Follow up observations were taken between May and July 2018 in order to determine the orbit of the satellite, but the results of those observations have not yet been released. Once the orbit is known, the mass and density of the system can be determined.


(53319) 1999 JM8
(53319) 1999 JM8 is an asteroid, slow rotator and tumbler, classified as a near-Earth object and potentially hazardous asteroid (PHA) of the Apollo group, approximately 7 kilometers (4 miles) in diameter, making it the largest PHA known to exist. It was discovered on 13 May 1999, by astronomers of the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico.


(53319) 1999 JM8, Orbit and classification
1999 JM8 orbits the Sun at a distance of 1.0–4.5 AU once every 4 years and 6 months (1,644 days; semi-major axis of 2.73 AU). Its orbit has an eccentricity of 0.64 and an inclination of 14° with respect to the ecliptic. This makes it also a Mars-crossing asteroid.


(53319) 1999 JM8, Orbit and classification
The body's observation arc begins with its first identification as 1990 HD1 at Palomar Observatory in April 1990, more than 9 years prior to its official discovery observation at Socorro.


(53319) 1999 JM8, Orbit and classification, Close approaches
1999 JM8 has an Earth minimum orbital intersection distance of 0.0235 AU (3,520,000 km) which translates into 9.2 lunar distances. It passed closer than 0.20 AU to the Earth five times in the last century (0.033 AU in 1990), but its next closest approach in the 21st century will be in 2075 at 0.256 au (38,300,000 km; 23,800,000 mi) and in August 2137 at 0.0764 au (11,430,000 km; 7,100,000 mi). For comparison, the planet Venus' closest approach to Earth is about 40 million km (25 million mi).


(53319) 1999 JM8, Physical characteristics
In the SMASS and Tholen classification, 1999 JM8 is an X-type asteroid. It has also been characterized as a carbonaceous C-type asteroid, which seems more likely due to its exceptionally low albedo (see below).


(53319) 1999 JM8, Physical characteristics, Rotation period
Radar imaging by Goldstone and Arecibo observatories revealed that 1999 JM8 has an unusually slow and possibly chaotic rotation period, similar to that of asteroid 4179 Toutatis.


(53319) 1999 JM8, Physical characteristics, Rotation period
In July 1999, a rotational lightcurve of 1999 JM8 was obtained from photometric observations. It gave a period of 136±2 hours with a brightness amplitude of 0.7 magnitude (U=2), and suggested that the body is in a non-principal axis rotation, commonly known as tumbling.


(53319) 1999 JM8, Physical characteristics, Diameter and albedo
1999 JM8 measures between 5 and 7 kilometers in diameter and its surface has an exceptionally low albedo of 0.02. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.03 and adopts a diameter of 7 kilometers based on an absolute magnitude of 15.2.


(53319) 1999 JM8, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 16 February 2003. As of 2018, it has not been named.


(533560) 2014 JM80
(533560) 2014 JM80, provisional designation 2014 JM80, is a trans-Neptunian object from the scattered disc in the outermost Solar System, approximately 340 kilometers (210 miles) in diameter. It was discovered on 9 May 2010 by astronomers with 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.


(533560) 2014 JM80, Orbit and classification
2014 JM80 orbits the Sun at a distance of 46.0–80.2 AU once every 500 years and 11 months (182,969 days; semi-major axis of 63.07 AU). Its orbit has an eccentricity of 0.27 and an inclination of 20° with respect to the ecliptic.


(533560) 2014 JM80, 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.


(533560) 2014 JM80, Orbit and classification
2014 JM80 has also been considered a detached object, since its relatively low eccentricity of 0.27, and its perihelion distance of 46.0 AU are hard to reconcile with the celestial mechanics of a scattered-disc object. 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.


(533560) 2014 JM80, Orbit and classification
With an orbital period of 500 years, and similar to 2015 FJ345, it seems to be a resonant trans-Neptunian objects in a 1:3 resonance with Neptune, as several other objects, but with a lower eccentricity (0.27 instead of more than 0.60) and a higher perihelia (at 45.8 AU rather than 31–41 AU). 2014 JM80 seems to belong to the same group as 2005 TB190.


(5407) 1992 AX
(5407) 1992 AX, provisional designation 1992 AX, is a stony asteroid and a synchronous binary Mars-crosser from the innermost region of the asteroid belt, approximately 3.6 kilometers (2.2 miles) in diameter. It was discovered on 4 January 1992, by Japanese astronomers Seiji Ueda and Hiroshi Kaneda at the Kushiro Observatory on Hokkaidō, Japan. The S-type asteroid has a short rotation period of 2.5 hours. Its sub-kilometer satellite was discovered in 1997. As of 2018, the binary system has not been named.


(5407) 1992 AX, Orbit and classification
1992 AX a member of the Mars-crossing asteroids, a dynamically unstable group between the main belt and the near-Earth populations, crossing the orbit of Mars at 1.66 AU. It orbits the Sun at a distance of 1.3–2.3 AU once every 2 years and 6 months (910 days; semi-major axis of 1.84 AU). Its orbit has an eccentricity of 0.28 and an inclination of 11° with respect to the ecliptic.


(5407) 1992 AX, Orbit and classification
The asteroid makes occasional close approaches to Mars. Its next close approach, on 22 January 2027, will bring it 11,260,000 km (0.0753 AU) from Mars. The body's observation arc begins with a precovery taken at Palomar Observatory in November 1951, or more than 40 years prior to its official discovery observation at Kushiro.


(5407) 1992 AX, Naming
This minor planet was numbered by the Minor Planet Center on 9 December 1992 (M.P.C. 21249). As of 2018, it has not been named.


(5407) 1992 AX, Physical characteristics
1992 AX has been characterized as a common, stony S-type asteroid. In the SMASS taxonomy, it is an Sk-subtype, that transitions between the S and K-type asteroids. The body's color indices of 0.690 (B–V), 0.500 (V–R) and 0.840 (V–I) were also determined.


(5407) 1992 AX, Physical characteristics, Lightcurves, Rotation period
Since 1997, several rotational lightcurves of 1992 AX have been obtained from photometric observations by Petr Pravec and collaborating astronomers. Best-rated lightcurve analysis gave a rotation period of 2.5488 hours with a consolidated brightness amplitude between 0.10 and 0.12 magnitude (U=2/3). The results supersedes a tentative period determination of 3.6 hours by Marc Buie (U=1).


(5407) 1992 AX, Physical characteristics, Lightcurves, Satellite
During the observations in January 1997, it was also revealed that 1992 AX is a synchronous binary asteroid with a minor-planet moon in its orbit. The satellite measures approximately 780 meters in diameter, or about 20% of its primary, and has an orbital period of 13.52 hours with an estimated semi-major axis of 5.8 kilometers for its very circular orbit. Observations by Pravec in January and February 2012 confirmed the binary nature of this asteroid, as well as its rotational and orbital periods. The satellite's provisional designation is S/1997 (5407) 1.


(5407) 1992 AX, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Japanese Akari satellite, the Spitzer Space Telescope and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), 1992 AX measures between 2.78 and 4.18 kilometers in diameter and its surface has an albedo between 0.199 and 0.40.


(5407) 1992 AX, Physical characteristics, Diameter and albedo
In 2017, a study by WISE dedicated to Mars-crossing asteroids determined a diameter of 3.60 kilometers with a high albedo of 0.376. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.20 and derives a diameter of 3.79 kilometers based on an absolute magnitude of 14.47. The Johnston's archive gives an effective (combined) diameter of 3.98 kilometers with 3.9 and 0.78 kilometers for is primary and secondary body, respectively.


(543354) 2014 AN55
(543354) 2014 AN55 (prov. designation: 2014 AN55) is a trans-Neptunian object and a dwarf-planet candidate from the scattered disc, located in the outermost region of the Solar System, that measures approximately 600 kilometres (370 mi) in diameter. It was discovered on 25 January 2014, by astronomers with the Pan-STARRS survey at Haleakala Observatory on the island of Maui, Hawaii, in the United States.


(543354) 2014 AN55, Orbit and classification
2014 AN55 belongs to the gravitationally perturbed population of scattered disc objects, which, at their closest approaches, come close to Neptune's orbit at 30 AU, but their farthest distances reach many times of that.


(543354) 2014 AN55, Orbit and classification
It orbits the Sun at a distance of 34.3–77.6 AU once every 418 years and 2 months (152,739 days; semi-major axis of 55.92 AU). Its orbit has an eccentricity of 0.39 and an inclination of 9° with respect to the ecliptic. The body's observation arc begins with its first observation taken by the Sloan Digital Sky Survey on 12 March 2005.


(543354) 2014 AN55, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 5 February 2020 (M.P.C. 121072) and has not yet received a name.


(543354) 2014 AN55, Physical characteristics, Diameter and albedo
Using an absolute magnitude of 4.3 from the Asteroids—Dynamic Site, and assuming an albedo in the range of 0.05 to 0.25, the object's mean-diameter may be as low as 370, and as high as 820 kilometers. Johnstons's Archive assumes a similar albedo of 0.9 and calculates a diameter of 671 kilometers using an absolute magnitude of 4.1. American astronomer Michael Brown estimates a diameter of 583 kilometers, based on an absolute magnitude of 4.4 and an assumed albedo of 0.10. According to Brown, a diameter of 600 km would give 2014 AN55 a highly likely dwarf-planet status.


(5476) 1989 TO11
(5476) 1989 TO11, provisional designation 1989 TO11 is a mid-sized Jupiter trojan from the Trojan camp, approximately 35 kilometers (22 miles) in diameter. It was discovered on 2 October 1989, by American astronomer Schelte Bus at the Cerro Tololo Inter-American Observatory in Chile. The dark Jovian asteroid has a rotation period of 5.8 hours. It has not been named since its numbering in March 1993.


(5476) 1989 TO11, Classification and orbit
1989 TO11 is a Jupiter trojan which stays 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.


(5476) 1989 TO11, Classification and orbit
It orbits the Sun at a distance of 4.7–5.5 AU once every 11 years and 7 months (4,217 days; semi-major axis of 5.11 AU). Its orbit has an eccentricity of 0.07 and an inclination of 14° with respect to the ecliptic. The asteroid was first observed at Palomar Observatory in August 1952. One year later, the body's observation arc begins at Palomar in August 1953, or more than 36 years prior to its official discovery observation at Cerro Tololo.


(5476) 1989 TO11, Physical characteristics
1989 TO11 is an assumed C-type asteroid. Jovian asteroids are typically D-types, with the remainder being mostly carbonaceous C- and primitive P-type asteroids.


(5476) 1989 TO11, Physical characteristics, Rotation period
Four nights of photometric observations of this asteroid were used to build a lightcurve showing a rotation period of 5.780±0.001 hours with a brightness variation of 0.30 magnitude. The well-defined lightcurve was obtained during February 1994 by Stefano Mottola and Anders Erikson using the ESO 1-metre telescope at the La Silla Observatory in Chile (U=3).


(5476) 1989 TO11, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 35.1 kilometers in diameter and its surface has an albedo of 0.099, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a larger diameter of 42.2 kilometers.


(5476) 1989 TO11, 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.


(5476) 1989 TO11, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 8 March 1993 (M.P.C. 21774). As of 2018, it has not been named.


(5496) 1973 NA
(5496) 1973 NA, is a very eccentric and heavily tilted asteroid, classified as near-Earth object of the Apollo group, approximately 2 kilometers in diameter. It was discovered on 4 July 1973, by American astronomer Eleanor Helin at the U.S. Palomar Observatory in California. At the time of its discovery, it was the most highly inclined minor planet known to exist. It may be the parent body of the Quadrantids.


(5496) 1973 NA, Parent of the Quadrantids
1973 NA is a possible parent body of the Quadrantids, a major meteor shower that occurs every January. It may also be just a fragment of the parent or the dormant remains of the parent. Other possible parent bodies are Comet 1491 I and comet 96P/Machholz, as well as (196256) 2003 EH1.


(5496) 1973 NA, Orbit and classification
The asteroid orbits the Sun at a distance of 0.9–4.0 AU once every 3 years and 10 months (1,388 days). Its orbit has an eccentricity of 0.64 and an inclination of 68° with respect to the ecliptic. No precoveries were taken. The asteroid's observation arc even begins 2 days after its discovery.


(5496) 1973 NA, Orbit and classification
The body was also one of the first known near-Earth asteroids. Its discovery happened just two days after it had passed 0.07984 AU (11,900,000 km) from Earth on one of its closest approaches ever computed. It was then tracked for more than a month, but was not seen again until its next close approach in 1992, when it was recovered by the Siding Spring Observatory in Australia. Its minimum orbit intersection distance with Earth is now 0.0904 AU (13,500,000 km).


(5496) 1973 NA, Physical characteristics
The stony S-type asteroid is also classified as a transitional C/X-type according to observations by the NASA IRTF telescope. A rotational lightcurve for this asteroid was obtained by American astronomer Brian Skiff from photometric observations made in June 2011. Lightcurve analysis gave a well-defined rotation period of 2.855±0.001 hours with a brightness variation of 0.15 magnitude (U=3). The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 1.88 kilometers with an absolute magnitude of 16.0.


(549948) 2011 WL2
(549948) 2011 WL2 is a sub-kilometer asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered on 16 November 2011, by astronomers with the LINEAR at the Lincoln Laboratory ETS near Socorro, New Mexico, in the United States.


(549948) 2011 WL2, Orbit
2011 WL2 is a potentially hazardous asteroid (PHA), but has a well determined orbit with a 10 year observation arc. 2011 WL2 will pass at a distance of 0.0056 AU (840,000 km; 520,000 mi) from Earth on 25 October 2077. For comparison, the distance to the Moon is about 0.0026 AU (384,400 km). 2011 WL2 appears on the list of PHA close approaches issued by the Minor Planet Center (MPC), with the next close approach in the year 2038.


(549948) 2011 WL2, Orbit
The Jupiter Tisserand invariant, used to distinguish different kinds of orbits, is 5.7.


(55565) 2002 AW197
(55565) 2002 AW197 is a classical, non-resonant trans-Neptunian object from the Kuiper belt in the outermost region of the Solar System, also known as cubewano. With a likely diameter of at least 700 kilometers (430 miles), Brown considers it a highly likely dwarf planet candidate. Tancredi notes that photometric observations suggest that it is a spheroid with a high albedo and small albedo spots. However, its low albedo suggests it does not have planetary geology. It is approximately tied (to within measurement uncertainties) as the largest unnamed object in the Solar System and the largest planetoid without a moon. It was discovered at Palomar Observatory in 2002 and has a rotation period of 8.8 hours and a moderately red color.


(55565) 2002 AW197, Description, Discovery
2002 AW197 was discovered on 10 January 2002, by astronomers at the Palomar Observatory in California. Astronomers involved in the discovery were Michael Brown, Chad Trujillo, Eleanor Helin, Michael Hicks, Kenneth Lawrence and Steven H. Pravdo. It is located near the Kuiper cliff.


(55565) 2002 AW197, Description, Orbit and classification
It orbits the Sun at a distance of 40.9–53.2 AU once every 322.6 years (over 117,800 days; semi-major axis of 47 AU). Its orbit has an eccentricity of 0.13 and an inclination of 24° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Haleakala-NEAT/GEODSS (566) in December 1997, more than 4 years prior to its official discovery observation at Palomar. At 45.4 AU from the Sun, it continues to slowly approach the Sun until its perihelion passage at 41.1 AU in May 2078.


(55565) 2002 AW197, Description, Physical characteristics
Combined observations of thermal emissions by the Herschel Space Observatory and Spitzer Space Telescope give a diameter of 768+39−38 km and a geometric albedo of 0.112+0.012−0.011


(55565) 2002 AW197, Description, Physical characteristics, Surface
ESO analysis of spectra reveals a strong red slope and no presence of water ice (in contrast to Quaoar, also red) suggesting organic material (see comparison of colours and typical composition inferred from spectra of the TNOs).


(55636) 2002 TX300
(55636) 2002 TX300 is a bright Kuiper belt object in the outer Solar System estimated to be about 286 kilometres (178 mi) in diameter. It is a large member of the Haumea family that was discovered on 15 October 2002 by the Near-Earth Asteroid Tracking (NEAT) program.


(55636) 2002 TX300
2002 TX300 is a classical Kuiper belt object with an absolute magnitude between that of 50000 Quaoar and 20000 Varuna. 2002 TX300 has the most eccentric and inclined orbit of the three.


(55636) 2002 TX300
A variability of the visual brightness was also detected which could fit to 7.9 h or 15.8 h rotational period (the distinction between single or double-peaked curved could not be made with confidence). The changes in brightness are quite close to the error margin and could also be due to an irregular shape.


(55636) 2002 TX300, Orbit
The adjacent diagrams show polar and ecliptic views of the orbits of the two cubewanos. The perihelia (q) and the aphelia (Q) are marked with the dates of passage. The present positions (as of April 2006) are marked with the spheres, illustrating relative sizes and differences in albedo (both objects appear neutral in the visible spectrum).


(55636) 2002 TX300, Orbit
2002 TX300 is classified as a classical Kuiper belt object and follows an orbit very similar to that of Haumea: highly inclined (26°) and moderately eccentric (e ~0.12), far from Neptune's perturbations (perihelion at ~37 AU). Other mid-sized cubewanos follow similar orbits as well, notably 2002 UX25 and 2002 AW197.


(55636) 2002 TX300, Orbit
It has been observed 303 times, with precovery images back to 1954.


(55636) 2002 TX300, Size
In 2004, the non-detection of IR thermal emissions put an upper limit of 709 kilometres (441 mi) on its diameter and a lower limit on the albedo of 0.19. In a 2006 International Astronomical Union press release discussing the IAU 2006 draft proposal, a diagram suggested that 2002 TX300 could be as large as 50000 Quaoar. The artist's diagram was largely based on the concept that 2002 TX300, with an absolute magnitude (H) of 3.4, may have an albedo around 0.08, which resulted in an overly optimistic diameter estimate of around 1,000 kilometres (620 mi).


(55636) 2002 TX300, Size
In 2007, measurements by the Spitzer Space Telescope showed that it may be less than 641 kilometres (398 mi) in diameter. In 2008, it was considered to be a dwarf planet based on its lightcurve amplitude and the assumption that it was larger than 450 kilometres (280 mi) in diameter. Because 2002 TX300 is a member of the Haumea family, it is assumed to have an albedo of around 0.7, which would result in a diameter of about 360 kilometres (220 mi).


(55636) 2002 TX300, Size
2002 TX300 occulted a relatively bright apparent magnitude 13.1 star in the constellation of Andromeda on 9 October 2009. This event was visible from Australia, possibly New Zealand, and the southern United States and Mexico. The RA and declination for this event was about : detailed information for observers was made available. The occultation produced a diameter of 286 kilometres (178 mi), suggesting an albedo of about 0.88. Mike Brown lists it as a possible dwarf planet.


(55636) 2002 TX300, Surface
The spectrum in the visible and near-infrared rages is very similar to that of Charon, characterized by neutral to blue slope (1%/1000 Å) with deep (60%) water absorption bands at 1.5 and 2.0 μm. Mineralogical analysis indicates a substantial fraction of large ice (H2O) particles. The signal-to-noise ratio of the observations was insufficient to differentiate between amorphous or crystalline ice (crystalline ice was reported on Charon, Quaoar and Haumea). The proportion of highly processed organic materials (tholins), typically present on numerous trans-Neptunian objects, is very low. As suggested by Licandro et al. 2006, this lack of irradiated mantle suggest either a recent collision or comet activity.


(55636) 2002 TX300, Origin
Common physical characteristics with the dwarf planet Haumea together with similar orbit elements led to suggestion that 2002 TX300 was a member of the Haumean collisional family. The object, together with other members of the family ((19308) 1996 TO66, (24835) 1995 SM55, (120178) 2003 OP32 and (145453) 2005 RR43), would be created from ice mantle ejected from the proto-Haumea as result of a collision with another large (around 1,660 kilometres (1,030 mi)) body.


(55637) 2002 UX25
(55637) 2002 UX25 is a trans-Neptunian object that orbits the Sun in the Kuiper belt beyond Neptune. This TNO briefly garnered scientific attention when it was found to have an unexpectedly low density of about 0.82 g/cm3.


(55637) 2002 UX25
2002 UX25 has an absolute magnitude of about 4.0, and Spitzer Space Telescope results estimate it to be about 681 km in diameter. The low density of this and many other mid sized TNO's implies that they have likely never compressed into fully solid bodies, let alone differentiated or collapsed into hydrostatic equilibrium, and so are highly unlikely to be dwarf planets.


(55637) 2002 UX25
It was discovered on 30 October 2002, by the Spacewatch program.


(55637) 2002 UX25, Numbering and naming
This minor planet was numbered (55637) by the Minor Planet Center on 16 February 2003 (M.P.C. 47763). As of 2021, it has not been named.


(55637) 2002 UX25, Classification
2002 UX25 has a perihelion of 36.7 AU, which it will next reach in 2065. As of 2020, 2002 UX25 is 40 AU from the Sun.


(55637) 2002 UX25, Classification
The Minor Planet Center classifies 2002 UX25 as a cubewano while the Deep Ecliptic Survey (DES) classifies it as scattered-extended. The DES using a 10 My integration (last observation: 2009-10-22) shows it with a minimum perihelion (qmin) distance of 36.3 AU.


(55637) 2002 UX25, Classification
It has been observed 212 times with precovery images dating back to 1991.


(55637) 2002 UX25, Classification, Dwarf-planet status
2002 UX25 has an estimated diameter of about 660 km, and most icy objects larger than 400 km in diameter were thought to be spherical. Michael Brown's website lists it as highly likely a dwarf planet. However, light-curve analysis has questioned whether it is actually a dwarf planet. Grundy et al. suggest that the low densities common in mid sized TNOs like this one implies that they have retained significant internal porosity from their formation, in which case they would not be dwarf planets.


(55637) 2002 UX25, Physical characteristics
A variability of the visual brightness was detected which could be fit to a period of 14.38 or 16.78 h (depending on a single-peaked or double peaked curve). The light-curve amplitude is ΔM = 0.21±0.06.


(55637) 2002 UX25, Physical characteristics
The analysis of combined thermal radiometry of 2002 UX25 from measurements by the Spitzer Space Telescope and Herschel Space Telescope indicates an effective diameter of 692 ± 23 km and albedo of 0.107+0.005−0.008. Assuming equal albedos for the primary and secondary it leads to the size estimates of ~664 km and ~190 km, respectively. If the albedo of the secondary is half of that of the primary the estimates become ~640 and ~260 km, respectively. Using an improved thermophysical model slightly different sizes were obtained for UX25 and its satellite: 659 km and 230 km, respectively.


(55637) 2002 UX25, Physical characteristics
2002 UX25 has red featureless spectrum in the visible and near-infrared but has a negative slope in the K-band, which may indicate the presence of the methanol compounds on the surface. It is redder than Varuna, unlike its neutral-colored "twin" 2002 TX300, in spite of similar brightness and orbital elements.


(55637) 2002 UX25, Physical characteristics, Composition
With a density of 0.82 g/cm3, assuming that the primary and satellite have the same density, 2002 UX25 is one of the largest known solid objects in the Solar System that is less dense than water. Why this should be is not well understood, because objects of its size in the Kuiper belt often contain a fair amount of rock and are hence pretty dense. To have a similar composition to others large KBOs, it would have to be exceptionally porous, which was believed to be unlikely given the compactability of water ice; this low density thus astonished astronomers.


(55637) 2002 UX25, Physical characteristics, Composition
Studies by Grundy et al. suggest that at the low temperatures that prevail beyond Neptune, ice is brittle and can support significant porosity in objects significantly larger than 2002 UX25, particularly if rock is present; the low density could thus be a consequence of this object failing to warm sufficiently during its formation to significantly deform the ice and fill these pore spaces.


(55637) 2002 UX25, Satellite
The discovery of a minor-planet moon was reported in IAUC 8812 on 22 February 2007. The satellite was detected using the Hubble Space Telescope in August 2005. The satellite was found at 0.16 arcsec from the primary with an apparent magnitude difference of 2.5. It orbits the primary in 8.309±0.0002 days, at a distance of 4770±40 km, yielding a system mass of (1.25±0.03)×1020 kg. The eccentricity of the orbit is 0.17±0.03.


(55637) 2002 UX25, Satellite
This moon is estimated to be 210±30 km in diameter. Assuming the same albedo as the primary, it would have a diameter of 190 km, assuming an albedo of 0.05 (typical of other cold, classical KBOs of similar size) a diameter of 260 km.


(55638) 2002 VE95
(55638) 2002 VE95, prov. designation: 2002 VE95,  is a trans-Neptunian object from the outermost region of the Solar System. It was discovered on 14 November 2002, by astronomers with the Near-Earth Asteroid Tracking program at the Palomar Observatory in California, United States. This resonant trans-Neptunian object is a member of the plutino population, locked in a 2:3 resonance with Neptune. The object is likely of primordial origin with a heterogeneous surface and a notably reddish color (RR) attributed to the presence of methanol and tholins. It has a poorly defined rotation period of 6.8 hours and measures approximately 250 kilometers (160 miles) in diameter, too small to be a dwarf planet candidate. As of 2021, it has not yet been named.


(55638) 2002 VE95, Orbit and classification
2002 VE95 belongs to the plutino population, named after its largest member, Pluto. Plutinos are resonant trans-Neptunian objects, that are locked in a stable 2:3 mean-motion resonance with Neptune, orbiting the Sun twice for every three orbits Neptune does. They form a significantly large part of the inner Kuiper belt, as hundreds of these objects have already been discovered.


(55638) 2002 VE95, Orbit and classification
This minor planet orbits the Sun at a distance of 27.9–50.4 AU once every 245 years and 3 months (89,562 days; semi-major axis of 39.18 AU). Its orbit has an eccentricity of 0.29 and an inclination of 16° with respect to the ecliptic. On 29 June 2001, it came to perihelion and has since been moving away from the Sun. Due to precovery images recovered from the Digitized Sky Survey, the body's observation arc begins already in October 1990, or 12 years prior to its official discovery observation by astronomers with the Near-Earth Asteroid Tracking at Palomar.


(55638) 2002 VE95, Numbering and naming
2002 VE95 was numbered (55638) by the Minor Planet Center on 16 February 2003 (M.P.C. 47763). As of 2021, it has not been named. According to the established naming conventions for plutinos, it will be named after a mythological figure from the underworld.


(55638) 2002 VE95, Physical characteristics, Rotation period
The rotation period of 2002 VE95 is poorly defined and has ambiguous results with multiple alternative period solutions in between 4.90 and 10 hours. In December 2002, a rotational lightcurve of this object was obtained from photometric observations by astromomers from the Sierra Nevada Observatory in Spain. Lightcurve analysis gave a poorly defined period of 6.76±0.01 hours with a brightness variation of 0.08±0.04 magnitude (U=1+). Two years later in December 2004, it was revisited by the same astronomers, obtaining another poorly defined period of 9.97±0.05 hours with an amplitude of 0.05±0.01 magnitude (U=1+). Other observations by Sheppard only determined an amplitude of less than 0.06 magnitude (U=1).


(55638) 2002 VE95, Physical characteristics, Diameter and albedo
In 2010, observations with the Herschel Space Telescope, using its PACS instrument to measure the object's thermal radiation, gave a mean-diameter of 249.8+13.5−13.1 km with a relatively high albedo of 0.149+0.019−0.016 for an absolute magnitude of 5.70±0.06. In addition, an asteroid occultations on 3 December 2015, gave a best-fit ellipse dimension of (250.0 km × 250.0 km) with an poor quality rating of 1. These timed observations are taken when the asteroid passes in front of a distant star. The Collaborative Asteroid Lightcurve Link assumes a more regular albedo for a distant object of 0.10 and hence estimates a larger diameter of 297 kilometers.


(55638) 2002 VE95, Physical characteristics, Color and composition
In the visible light, 2002 VE95 has a featureless reflectance spectrum. It is very red in color (RR), with a color index of 1.080 and 0.71, in the B–V and V−R passband filters, respectively.


(55638) 2002 VE95, Physical characteristics, Color and composition
The near-infrared spectrum of 2002 VE95 is flat with two distinct absorption bands of water ice at 1.5 and 2.0 μm. There is the third feature near 2.3 μm of unclear origin. The spectral behavior of this object is similar to 5145 Pholus, a centaur. Observations with the Very Large Telescope revealed that 2002 VE95 has a heterogeneous surface—the amount of different ices and non-ice components depends on the observed area. Among the probable surface materials are water ice (4–19%), methanol ice (10–12%) and various tholins, photochemically altered organic compounds, also found on Triton and Titan. The redder areas are generally associated with the presence of methanol ice. The surface of 2002 VE95 appears to be primordial in origin.