(556416) 2014 OE394
(556416) 2014 OE394 is a large cubewano in the Kuiper belt that was discovered in July 2014 by the Pan-STARRS-1 telescope, and announced on 17 July 2016. It is one of the brighter trans-Neptunian objects, being the 34th brightest cubewano as of 23 July 2016. Its exact size is unknown, but is most likely between 240 and 730 kilometers across. Mike Brown's website lists it as a "possible" dwarf planet, with an estimated diameter of 337 kilometers.


(556416) 2014 OE394
2014 OE394 is also somewhat close to the New Horizons probe, about 8.7 AU away on 1 January 2017, and 7.5 AU on 1 January 2019. Considering its large size, it would make a possible imaging target, as 15810 Arawn was in early 2016. However, as 2014 OE394 is currently over 10 times further than the other was, it would have much lower-precision data.


(5604) 1992 FE
(5604) 1992 FE is an Aten-type near-Earth minor planet. It was discovered by Robert H. McNaught at the Siding Spring Observatory in Canberra, Australia, on March 26, 1992. The asteroid is 550 meters (1,800 ft) in diameter.


(5604) 1992 FE
The asteroid has a Venus minimum orbit intersection distance (Venus–MOID) of 0.0059 AU (880,000 km; 550,000 mi). On April 7, 2015 the asteroid passed 0.00717 AU (1,073,000 km; 666,000 mi) from Venus.


(5645) 1990 SP
(5645) 1990 SP is an eccentric and tumbling asteroid, classified as near-Earth object of the Apollo group, approximately 1.7 kilometers in diameter. It was discovered on 20 September 1990, by Scottish–Australian astronomer Robert McNaught at the Siding Spring Observatory in Canberra, Australia.


(5645) 1990 SP, Orbit and classification
The asteroid orbits the Sun at a distance of 0.8–1.9 AU once every 1 years and 7 months (576 days). Its orbit has an eccentricity of 0.39 and an inclination of 14° with respect to the ecliptic.


(5645) 1990 SP, Orbit and classification, Close approaches
This near-Earth asteroid has an Earth minimum orbit intersection distance of 0.055 AU (8,200,000 km), only slightly above the threshold minimum distance of 19.5 lunar distances (0.05 AU) to make it a potentially hazardous object. It also makes close approaches to Mars. On 14 April 1969, it passed the Red Planet at only 0.013 AU (1,900,000 km).


(5645) 1990 SP, Orbit and classification, Precovery
Published by the Digitized Sky Survey (DSS), a first precovery was taken at the discovering observatory in 1974, extending the asteroid's observation arc by 16 years prior to its discovery.


(5645) 1990 SP, Physical characteristics
The stony S-type asteroid is also characterized as a P-type, based on post-cryogenic observations by the Spitzer Space Telescope, while observations at the NASA Infrared Telescope Facility using its SpeX instrument during a follow-up campaign of the Spitzer-observed objects between 2009 and 2012, gave it a C/X/T spectral type.


(5645) 1990 SP, Physical characteristics, Rotation
In April 2002, Czech astronomer Petr Pravec obtained a rotational lightcurve from a photometric observations, which gave a relatively long period of 30.39±0.04 hours with a brightness variation of 0.7 in magnitude (U=2). The observations have also shown that the body is most likely in a tumbling motion.


(5645) 1990 SP, Physical characteristics, Diameter and albedo
Estimates for the body's diameter range from 1.6 to 2.2 kilometers with an albedo for its surface between 0.06 and 0.12, according to observations made by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and by the Spitzer Space Telescope. The Collaborative Asteroid Lightcurve Link takes the revised WISE data – an albedo of 0.0872 and a diameter of 1.65 kilometers – as the best of all available results.


(5646) 1990 TR
(5646) 1990 TR is a probable rare-type binary asteroid classified as near-Earth object of the Amor group, approximately 2.3 kilometers in diameter. It was discovered on 11 October 1990, by Japanese astronomers Seiji Ueda and Hiroshi Kaneda at Kushiro Observatory near Kushiro, in eastern Hokkaido, Japan.


(5646) 1990 TR, Orbit
The asteroid orbits the Sun at a distance of 1.2–3.1 AU once every 3 years and 2 months (1,147 days). Its orbit has an eccentricity of 0.44 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with its first observation at the Siding Spring Observatory, five months prior to its official discovery observation at Kushiro.


(5646) 1990 TR, Lightcurve
In December 2012, the so far best rated rotational lightcurve was obtained by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of 3.1999 hours with a brightness variation of 0.12 magnitude (U=3). Photometric observations also gave a period of 19.47 hours for a probable asteroid moon, with a measured diameter-ratio of 0.18±0.02, which translates into a diameter of 400 meters for its moon.


(5646) 1990 TR, Diameter and albedo
According to the surveys carried out by the Spitzer Space Telescope and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures 2.03 and 2.723 kilometers in diameter and its surface has an albedo of 0.19 and 0.66. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.18 and derives a diameter of 2.3 kilometers based on an absolute magnitude of 15.67.


(574372) 2010 JO179
(574372) 2010 JO179, provisional designation: 2010 JO179, is a large, high-order resonant trans-Neptunian object and a likely dwarf-planet candidate from the outermost regions of the Solar System, approximately 700 kilometers (430 miles) in diameter. Long-term observations suggest that the object is in a meta-stable 5:21 resonance with Neptune. Other sources classify it as a scattered disc object.


(574372) 2010 JO179, First observation and orbit
The Minor Planet Center credits the object's first official observation on 10 May 2010 to Pan-STARRS (F51) at Haleakala Observatory, Hawaii, United States. The observations were made by Pan-STARRS' Outer Solar System Survey. There are 4 February 1951 precovery images from the Palomar Observatory Sky Survey, extending the observation arc by approximately 60 years. The precovery images are from the same year the object came to perihelion (closest approach to the Sun).


(574372) 2010 JO179, First observation and orbit
2010 JO179 orbits the Sun at a distance of 39.6–118 AU once every 699 years and 5 months (semi-major axis of 78.8 AU). Its orbit has a high eccentricity of 0.50 and an inclination of 32° with respect to the ecliptic.


(574372) 2010 JO179, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 10 August 2021, receiving the number (574372) in the minor planet catalog (M.P.C. 133504). As of 2021, it has not been named.


(574372) 2010 JO179, Physical characteristics, Photometry
Photometric observations of 2010 JO179 gave a monomodal lightcurve with slow rotation period of 30.6 hours, suggesting a rather spherical shape with significant albedo patchiness. An alternative period solution of a bimodal lightcurve is considered less likely. It would double the period and imply an ellipsoidal shape with an axis-ratio of at least 1.58.


(574372) 2010 JO179, Physical characteristics, Diameter and albedo
The object's mean diameter has been estimated to measure 574 and 735 kilometers, with an assumed albedo of 0.09, by Michael Brown and the Johnston's Archive respectively, while the discoverers estimate a diameter of 600–900 kilometers with an estimated albedo of 0.21 to 0.07. In his classification scheme, astronomer Michael Brown considers this object a likely dwarf planet, rather than a "highly likely" one, as his diameter-estimate is below the 600-kilometer mark.


(5836) 1993 MF
(5836) 1993 MF is a highly eccentric, stony asteroid, classified as a near-Earth object of the Amor group of asteroids, approximately 3 kilometers in diameter. It was discovered on 22 June 1993, by American astronomers Eleanor Helin and Kenneth Lawrence at the U.S. Palomar Observatory in California.


(5836) 1993 MF, Classification and orbit
The stony S-type asteroid orbits the Sun at a distance of 1.1–3.7 AU once every 3 years and 10 months (1,392 days). Its orbit has an eccentricity of 0.54 and an inclination of 8° with respect to the ecliptic. It has an Earth minimum orbital intersection distance of nearly 0.184 AU (27,500,000 km), which corresponds to 71.8 lunar distances. As it crosses the orbit of Mars, it may also be classified as a Mars-crosser, and, on 28 November 2023, it will pass 0.02535 AU (3,792,000 km) from the Red Planet. The first precovery was taken at the Australian Siding Spring Observatory in 1981, extending the body's observation arc by 12 years prior to its discovery.


(5836) 1993 MF, Physical characteristics
Since the 1990s, and up to June 2016, four well-defined rotational lightcurves were obtained for this asteroid from photometric observations, giving a rotation period of approximately 4.95 hours with a high brightness variation between 0.53 and 0.82 in magnitude, indicating that the asteroid has a non-spheroidal shape. In the 1990s, Italian astronomer Stefano Mottola obtained a lightcurve at La Silla during the EUNEASO, a European near-Earth object search and follow-up observation program to determine additional physical parameters (U=3).


(5836) 1993 MF, Physical characteristics
Further lightcurves were obtained by Polish astronomer Wiesław Z. Wiśniewski at UA's LPL in October 1993, and by Czech astronomer Petr Pravec at Ondřejov Observatory in September 1997 (U=3/3). In June 2016, the fourth and most recent photometric observation was made by American astronomer Brian Warner at his Palmer Divide Station, Colorado, which gave a period of 4.948±0.005 hours with an amplitude of 0.82 in magnitude (U=3).


(5836) 1993 MF, Physical characteristics, Diameter
While in the 1990s, Stefano Mottola estimated the asteroid to measure 3.8 kilometers in diameter (H = 15.03), the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and derives a shorter diameter of 2.8 kilometers, based on an absolute magnitude of 15.14.


(585310) 2017 YZ1
(585310) 2017 YZ1, provisional designation: 2017 YZ1, is a sub-kilometer asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 250 meters (800 feet) in diameter. It was first observed on 20 December 2017, by astronomers with the Mount Lemmon Survey at Mount Lemmon Observatory near Tucson, Arizona, in the United States. On 29 January 2018, it passed Earth at 125 lunar distances.


(585310) 2017 YZ1, Orbit and classification
2017 YZ1 is a member of the Apollo asteroids, which cross the orbit of Earth. Apollo's are the largest group of near-Earth objects with nearly 10 thousand known objects.


(585310) 2017 YZ1, Orbit and classification
It orbits the Sun at a distance of 0.88–1.77 AU once every 18 months (558 days; semi-major axis of 1.33 AU). Its orbit has an eccentricity of 0.33 and an inclination of 21° with respect to the ecliptic.


(585310) 2017 YZ1, Risk assessment
The 9 January 2018 solution with a 15-day observation arc was listed at Torino scale 1 with a 1:21,000 chance of impacting Earth on 30 June 2047. By 9 January 2018, the geocentric 30 June 2047 uncertainty region had shrunk to ±50 million km. With a longer 20 day observation arc, it dropped to Torino scale 0 and had a 1:670,000 chance of impacting Earth on 30 June 2047. On 18 January 2018 it was removed from the Sentry Risk Table. With a 28-day observation arc, the nominal solution suggests it will be about 0.25 AU (37,000,000 km) from Earth on 30 June 2047. The 3-sigma uncertainty in the 2047 close approach distance is about ±13 million km.


(585310) 2017 YZ1, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 10 August 2021, receiving the number (585310) in the minor planet catalog (M.P.C. 133609). As of 2021, it has not been named.


(589683) 2010 RF43
(589683) 2010 RF43, provisionally designated: 2010 RF43, is a trans-Neptunian object of the scattered disc orbiting in the outermost regions of the Solar System. It measures approximately 700 kilometers (430 mi) in diameter and is a strong dwarf-planet candidate. The object was discovered on 9 September 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's La Silla Observatory in northern Chile.


(589683) 2010 RF43, Orbit and classification
2010 RF43 orbits the Sun at a distance of 37.5–61.9 AU once every 350 years and 4 months (127,948 days; semi-major axis of 49.7 AU). Its orbit has an eccentricity of 0.25 and an inclination of 31° with respect to the ecliptic. The body's observation arc begins with a precovery observation taken at Siding Spring Observatory in August 1976.


(589683) 2010 RF43, Orbit and classification
Due to its relatively high eccentricity and inclination, it is an object of the scattered disc rather than one of the regular Kuiper belt. Its perihelion of 37.5 AU is also too low to make it a detached object, which typically stay above 40 AU and never come close to the orbit of Neptune.


(589683) 2010 RF43, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 20 September 2021, receiving the number (589683) in the minor planet catalog (M.P.C. 135075). As of 2021, it has not been named.


(589683) 2010 RF43, Physical characteristics, Diameter and albedo
Based on an absolute magnitude of 3.9, and an assumed albedo of 0.09, the Johnston's archive estimates a mean-diameter of approximately 770 kilometers (480 mi), while astronomer Michael Brown assumes an albedo of 0.11 and calculates a diameter of 643 kilometers (400 mi) using a fainter magnitude of 4.0. Brown also characterizes the object as a "highly likely dwarf planet", the second-highest level in his classification scheme (also see list of candidates).


(589683) 2010 RF43, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.10 and calculates a diameter of 636 kilometers (395 mi) based on an absolute magnitude of 4.1.


(589683) 2010 RF43, Physical characteristics, Rotation period
As of 2020, no rotational lightcurve of this object has been obtained from photometric observations. The object's rotation period, pole and shape remain unknown.


(594913) 2020 AV2
(594913) 2020 AV2, provisionally designated: 2020 AV2, is a large near-Earth asteroid discovered by the Zwicky Transient Facility on 4 January 2020. It is the first asteroid discovered to have an orbit completely within Venus's orbit, and is thus the first and only known member of the inner-Venusian provisionally-named Vatira population of Atira-class asteroids. 2020 AV2 has the smallest known aphelion and third-smallest known semi-major axis among all asteroids. With an absolute magnitude approximately 16.2, the asteroid is expected to be larger than 1 km in diameter.


(594913) 2020 AV2, Discovery
2020 AV2 was discovered by the Zwicky Transient Facility (ZTF) survey at the Palomar Observatory on 4 January 2020, by astronomers Bryce Bolin, Frank Masci, and Quanzhi Ye. The discovery formed part of a campaign for detecting interior-Earth asteroids (Atiras) using the wide-field ZTF camera on the 1.22-meter Samuel Oschin telescope at the Palomar Observatory. The detection of such objects is difficult due to their close proximity to the Sun: asteroids within the orbit of Venus never reach solar elongations greater than 47 degrees, meaning that they are only observable during twilight as the Sun is below the Earth's horizon. Because of this, inner-Venusian asteroids could only be observed within a short time frame, hence why the ZTF camera was used since it can effectively detect transient objects.


(594913) 2020 AV2, Discovery
At the time of discovery, 2020 AV2 was located in the constellation Aquarius, at an apparent magnitude around 18. The discovery of 2020 AV2 was reported by astronomer Bryce Bolin, and was subsequently listed on the Minor Planet Center's near-Earth object confirmation page (NEOCP) on 4 January 2020. Follow-up observations were then conducted at various observatories in order to determine the asteroid's orbit based on its orbital motion. The discovery of the asteroid was then formally announced in a Minor Planet Electronic Circular issued by the MPC on 8 January 2020. Follow-up observations were later conducted in November 2020 by the Palomar and Xingming observatories, reducing 2020 AV2's uncertainty parameter to 5.


(594913) 2020 AV2, Discovery
Prior to the discovery of 2020 AV2, co-discoverer Quanzhi Ye and colleagues had predicted in December 2019 that the ZTF would detect its first Vatira asteroid within Venus's orbit shortly after the discoveries of several small-aphelion asteroids including 2019 AQ3 and 2019 LF6. Given the difficulty of detecting such asteroids at small solar elongations, they estimated that at least one additional Vatira asteroid will be detected by the ZTF.


(594913) 2020 AV2, Nomenclature
Upon discovery, the asteroid was given the internal designation ZTF09k5. It was then given the provisional designation 2020 AV2 by the MPC on 8 January 2020, after follow up observations have sufficiently determined its orbit. The provisional designation signifies the object's discovery date and year. The object has yet not been issued a minor planet number by the MPC since it has yet not been observed over four oppositions.


(594913) 2020 AV2, Nomenclature
As its orbit had been sufficiently determined, this minor planet was numbered by the Minor Planet Center on 20 September 2021, receiving the number (594913) in the minor planet catalog (M.P.C. 135125). and is since eligible for naming. Being the prototype of the informally named Vatira class, it will be given a name that will be used to refer to this newly confirmed population.


(594913) 2020 AV2, Orbit and classification
2020 AV2 is the only asteroid known to have an orbit completely within Venus's orbit. With an aphelion distance of approximately 0.654 astronomical units (AU), it has the smallest known aphelion of all asteroids. In comparison, Venus's average orbital distance from the Sun is 0.723 AU, with a perihelion distance of 0.718 AU. 2020 AV2 is formally classified as an Atira asteroid by the Minor Planet Center due it having an orbit within that of Earth.


(594913) 2020 AV2, Orbit and classification
However, unlike previously known Atira asteroids, 2020 AV2's orbit is contained within that of Venus, thus it falls into the proposed category of Vatira asteroids—a subclass of Atira asteroids with aphelion distances less than Venus's perihelion distance (hence the name: a portmanteau of 'Venus' and 'Atira'). 2020 AV2 is technically classified as a near-Earth object under the Atira classification, though the asteroid's minimum orbit intersection distance from Earth is 0.346 AU.


(594913) 2020 AV2, Orbit and classification
The orbit of 2020 AV2 is a well-secured with an uncertainty parameter of 2. The asteroid orbits the Sun in approximately 151 days (0.41 years), with a semi-major axis of approximately 0.5554 AU. 2020 AV2's orbit is close to a 3:2 mean-motion orbital resonance with Venus, meaning that 2020 AV2 completes approximately three orbits for every two orbits completed by Venus. The orbit of 2020 AV2 is moderately eccentric, as it approaches only 0.457 AU from the Sun at perihelion, just within Mercury's aphelion distance of 0.467 AU.


(594913) 2020 AV2, Orbit and classification
2020 AV2's orbit is also moderately inclined to the ecliptic by approximately 15.9 degrees. 2020 AV2 has a smaller orbital eccentricity and inclination compared to the generally expected values for typical Vatira asteroids, which were predicted to have an eccentricity around 0.4 and an inclination around 25 degrees. The asteroid's minimum orbit intersection distance from Mercury and Venus is about 0.066 AU (9.9×10^6 km) and 0.079 AU (11.8×10^6 km), respectively.


(594913) 2020 AV2, Orbit and classification
2020 AV2 is approximately tied with 2019 LF6 (0.5553 AU) as having the second-smallest known orbital period and semi-major axis among all asteroids, though 2019 LF6 is has a slightly smaller semi-major axis. In this case, 2020 AV2 has the third-smallest known semi-major axis among all asteroids.


(594913) 2020 AV2, Orbit and classification, Orbital dynamics
2020 AV2 had likely originated from the main asteroid belt, where its orbit was locked in a secular resonance that caused its orbital eccentricity to gradually increase over time, evolving onto an Earth-crossing orbit. Subsequent close encounters with Earth, Venus, and Mercury resulted in gravitational perturbations of the asteroid's orbit, reducing its momentum and causing it to orbit closer to the Sun. Such inward orbital migration of objects is thought to be rare. Near-Earth asteroids transitioning into the Vatira region often have unstable, short-term orbits due to frequent gravitational perturbations by Venus and Mercury.


(594913) 2020 AV2, Orbit and classification, Orbital dynamics
2020 AV2 rarely crosses the orbits of Mercury and Venus, which reduces the number of close encounters with either planet that would otherwise perturb 2020 AV2's orbit. Nevertheless its orbit is likely to be stable for less than a million years, unless it is on (or enters soon) a nearby 3:2 mean-motion resonance with Venus, which could extend its stability to a few million years.


(594913) 2020 AV2, Orbit and classification, Orbital dynamics
Dynamical modeling of 2020 AV2's orbit show that the mostly likely scenario for its orbital evolution is that 2020 AV2's orbit will oscillate for several millions of years before gravitational perturbations lead to the asteroid's eventual collision with a planet, most likely Venus. At 140 thousand years from the present, 2020 AV2's aphelion distance will exceed Venus's perihelion distance, as a result of the combined effects of the Kozai resonance and gravitational perturbations. Within the Vatira region, the Kozai resonance causes the orbital inclinations and eccentricities of asteroids to oscillate over several millions of years.


(594913) 2020 AV2, Orbit and classification, Orbital dynamics
As a result, Vatira asteroids can become Atira-class asteroids and vice versa over time, and can cross the orbits of Mercury and Venus during these orbital oscillations. The Kozai resonance often disrupts the orbits of Vatira asteroids, albeit it can also lead to orbital stability for some unperturbed Vatira asteroids. At about 1.2 million years from the present, 2020 AV2 will leave the Vatira region and will transition onto a Mercury-crossing orbit, with its perihelion oscillating around Mercury's aphelion distance before decoupling from the planet's orbit at about 2.1 million years.


(594913) 2020 AV2, Orbit and classification, Orbital dynamics
After decoupling from Mercury's orbit, 2020 AV2 was shown to oscillate between an Atira-type orbit (Q < 0.983 AU) and an Earth-crossing Aten-type orbit (Q > 0.983 AU), in which the asteroid's aphelion oscillates around Earth's perihelion distance of 0.983 AU. About 740 thousand years afterward, 2020 AV2 will likely return to its Mercury-crossing orbit, though gravitational perturbations by Mercury and Venus will scatter it onto an Earth-crossing orbit once more before colliding with either planet. At about 4.1 million years from the present, 2020 AV2 will most likely collide with Venus.


(594913) 2020 AV2, Physical characteristics
2020 AV2 is estimated to have an absolute magnitude (H) approximately 16.2. The diameter of 2020 AV2 is expected to be larger than 1 km (0.62 mi). Assuming that the albedo is between 0.25 and 0.05, its diameter should be around 1–3 km, respectively. Near-Earth asteroid population models predict that at least one asteroid of this size has an orbit within that of Venus, implying that 2020 AV2 could be one of the largest members of the Vatira population.


(594913) 2020 AV2, Physical characteristics
Visible and near-infrared spectroscopy by the Roque de los Muchachos Observatory in 2020 suggests that 2020 AV2 has a reddish surface that is olivine-rich, based on the presence of a 1 μm absorption feature characteristic of S-type asteroids. The abundance of olivine in the surface of 2020 AV2 suggests that it could be a mantle asteroid formed as a fragment from the rocky mantles of large, internally differentiated bodies. The absorption features in 2020 AV2's spectrum appear to be intermediate between the S-type and A-type spectral classes, hence it is classified as an Sa-type asteroid. Assuming an average albedo of 0.22 for S-type asteroids, 2020 AV2's diameter can be constrained to approximately 1.5 km (0.93 mi).


(6-4)DNA photolyase
(6-4)DNA photolyase (EC , DNA photolyase, H64PRH, NF-10, phr (6-4), PL-(6-4), OtCPF1, (6-4) PHR, At64PHR) is an enzyme with systematic name (6-4) photoproduct pyrimidine-lyase. This enzyme catalyses the following chemical reaction


(6002) 1988 RO
(6002) 1988 RO, provisional designation 1988 RO is a mid-sized Jupiter trojan from the Trojan camp, approximately 40 kilometers (25 miles) in diameter. It was discovered by Poul Jensen at the Brorfelde Observatory in 1988, and has not been named since its numbering in June 1994. The dark Jovian asteroid has a rotation period of 12.9 hours.


(6002) 1988 RO, Discovery
1988 RO discovered on 8 September 1988, by Danish astronomer Poul Jensen at the Brorfelde Observatory near Holbæk, Denmark, who on very same night also discovered the Jupiter trojan (5119) 1988 RA1, and several other main-belt asteroids including (9840) 1988 RQ2, (12689) 1988 RO2, (14364) 1988 RM2, (14837) 1988 RN2, and (24664) 1988 RB1.


(6002) 1988 RO, Orbit and classification
1988 RO is a dark Jovian asteroid in a 1:1 orbital resonance with Jupiter. It is located in the trailering Trojan camp at the Gas Giant's L5 Lagrangian point, 60° behind its orbit (see Trojans in astronomy). It is also a non-family asteroid of the Jovian background population.


(6002) 1988 RO, Orbit and classification
It orbits the Sun at a distance of 4.7–5.7 AU once every 11 years and 11 months (4,361 days; semi-major axis of 5.22 AU). Its orbit has an eccentricity of 0.09 and an inclination of 16° with respect to the ecliptic. A first precovery was taken at Palomar Observatory in September 1953, extending the body's observation arc by 35 years prior to its official discovery observation at Brorfelde.


(6002) 1988 RO, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 23 June 1994 (M.P.C. 23661). As of 2019, it has not been named.


(6002) 1988 RO, Physical characteristics, Rotation period
In February 1993, 1988 RO was observed by astronomers Stefano Mottola and Mario Di Martino with the ESO 1-metre telescope and its DLR MkII CCD-camera at La Silla in Chile. The photometric observations were used to build a lightcurve showing a rotation period of 12.918±0.022 hours with a brightness variation of 0.18±0.01 magnitude (U=3-). It was the body's first determined rotation period in literature.


(6002) 1988 RO, Physical characteristics, Diameter and albedo
According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, 1988 RO measures 40.4 kilometers in diameter and its surface has an albedo of 0.075, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 42.23 kilometers, based on an absolute magnitude of 10.6.


(6002) 1988 RO, 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.


(6037) 1988 EG
(6037) 1988 EG, is an eccentric, stony asteroid, classified as near-Earth object and potentially hazardous asteroid. It belongs to the group of Apollo asteroids and measures approximately half a kilometer in diameter. It was discovered by American astronomer Jeff T. Alu at the U.S. Palomar Observatory, California, on 12 March 1988.


(6037) 1988 EG, Classification and orbit
The S-type asteroid orbits the Sun at a distance of 0.6–1.9 AU once every 1 years and 5 months (523 days). Its orbit has an eccentricity of 0.50 and an inclination of 3° with respect to the ecliptic.


(6037) 1988 EG, Classification and orbit
The asteroid has an Earth minimum orbit intersection distance (MOID) of 0.0243 AU (3,600,000 km). In combination with its size, this makes it a potentially hazardous asteroid, which require an intersection distance with Earth of less than 0.05 AU, which is about 19.5 times the distance to the moon, and a diameter of at least 150 meters. On 27 February 2041, it will pass 0.02437 AU (3,646,000 km) from Earth. It also makes close approaches to Mars and Venus.


(6037) 1988 EG, Physical characteristics, Lightcurve
An ambiguous lightcurve was obtained through photometric observations by Czech astronomer Petr Pravec in 1998. The light-curve gave a rotation period of 2.760±0.002 hours with a brightness amplitude of 0.20 in magnitude. The alternative period solution is 2.919±0.22 hours with an amplitude of 0.22 in magnitude (U=2).


(6037) 1988 EG, 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 540 meters, based on an absolute magnitude of 18.7. Observations with the Spitzer Space Telescope using its Infrared Array Camera at wavelengths between 3.6 and 8.0 micrometers, gave an average diameter of 399 meters with a higher albedo of 0.37.


(60621) 2000 FE8
(60621) 2000 FE8 is a resonant and binary trans-Neptunian object, approximately 146 kilometers (91 miles) in diameter, located in the outermost region of the Solar System. It was discovered on 27 March 2000, by astronomers John Kavelaars, Brett Gladman, Jean-Marc Petit and Matthew Holman at Mauna Kea Observatory on Hawaii. This distant object resides in an eccentric orbit and is locked in a 2:5 orbital resonance with Neptune. It is known to have a 111-kilometer sized companion, which was discovered in January 2007.


(60621) 2000 FE8, Orbit
2000 FE8 has an extremely eccentric orbit which crosses the paths of many other trans-Neptunian objects, including almost all of the dwarf planets and dwarf planet candidates. As a result, its position alternates between the Kuiper belt and the scattered disc.


(60621) 2000 FE8, Orbit, Resonance with Neptune
2000 FE8 is part of a group of trans-Neptunian objects that orbit in a 2:5 resonance with Neptune. That means that for every five orbits that Neptune completes, 2000 FE8 makes only two. Several other objects are in the same orbital resonance, the largest of which is (84522) 2002 TC302.


(60621) 2000 FE8, Satellite
Like many objects of the Kuiper belt and scattered disc, 2000 FE8 has a satellite. Provisionally designated S/2007 (60621) 1, the satellite was discovered by the Hubble Space Telescope seven years after 2000 FE8 itself was found. The moon orbits at 1180 kilometres away from 2000 FE8, completing one orbit in approximately 7 days. It is thought to be 115 km in diameter, just 75.7% the diameter of 2000 FE8 itself.


(60621) 2000 FE8, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 14 June 2003. As of 2021, it has not been named.


(6178) 1986 DA
(6178) 1986 DA is a metallic asteroid, classified as near-Earth object of the Amor group, approximately 3 kilometers in diameter. It was discovered on 16 February 1986, by Japanese astronomer Minoru Kizawa at Shizuoka Observatory, Japan.


(6178) 1986 DA
1986 DA was the first near Earth asteroid thought to be of metallic composition, with high radar brightness; with that it was predicted to have 100 thousand tons of platinum group metals including gold and suggested as a resource for future space colonists.


(6178) 1986 DA, Orbit and classification
As an eccentric Amor asteroid has an Earth minimum orbit intersection distance of 0.1922 AU (28,800,000 km) and approaches the orbit of Earth from the outside but does not cross it. It crosses however the orbit of Mars and can be classified as a Mars-crosser and also approaches the orbit of Jupiter within 0.5 AU. The asteroid orbits the Sun at a distance of 1.2–4.5 AU once every 4 years and 9 months (1,732 days). Its orbit has an eccentricity of 0.58 and an inclination of 4° with respect to the ecliptic. The first precovery was taken at Siding Spring Observatory in 1977, extending the asteroid's observation arc by 9 years prior to its discovery.


(6178) 1986 DA, Physical characteristics
The metallic M-type asteroid is notable for being significantly more radar-reflective than other asteroids. Radar measurements suggest it is composed of nickel and iron and that it was derived from the center of a much larger object that experienced melting and differentiation. The observed radar albedo was 0.58 and the optical albedo was 0.14.


(6178) 1986 DA, Physical characteristics, Rotation and shape
It was most probably formed from a larger body through a catastrophic collision with another object. Radar measurements of this body indicate that the surface is relatively smooth on scales of less than a meter, but it is highly irregular on scales of 10–100 meters. Several lightcurve analysis gave it a concurring rotation period of 3.50 to 3.51 hours with a relatively high brightness amplitude between 0.03 and 0.48 in magnitude, indicating an irregular shape (U=3/3/n.a. ).


(6178) 1986 DA, Physical characteristics, Diameter and albedo
According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid has an albedo of 0.08 and 0.16, and a diameter of 3.1 to 3.2 kilometers, respectively. The Collaborative Asteroid Lightcurve Link selects 3.15 kilometers as best result, while the first estimate from 1994 gave a diameter of 2.3 kilometers.


(6178) 1986 DA, Physical characteristics, Mining considerations
The asteroid achieved its most notable recognition when scientists revealed that it contained over "10,000 tons of gold and 100,000 tons of platinum", or an approximate value at the time of its discovery of "$90 billion for the gold and a cool trillion dollars for the platinum, plus loose change for the asteroid's 10 billion tons of iron and a billion tons of nickel." In 2012 the estimated value of 100,000 tons of platinum was worth approximately five trillion US dollars. The delta-v for a spacecraft rendezvous with this asteroid from low earth orbit is 7.1 km/s.


(6265) 1985 TW3
(6265) 1985 TW3, provisional designation 1985 TW3, is a background asteroid and binary system from the inner regions of the asteroid belt. It was discovered on 11 October 1985, by astronomer by T. F. Fric and Richard Gilbrech at the Palomar Observatory in California. It is the only minor-planet discovery for these two astronomers. The stony L-type asteroid measures approximately 5 kilometers (3.1 miles) in diameter and has a rotation period of 2.7 hours. Its 1.2-kilometer sized minor-planet moon was discovered in July 2007 and announced the following month.


(6265) 1985 TW3, Orbit and classification
1985 TW3 is a non-family asteroid from the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. Based on osculating Keplerian orbital elements, the asteroid has also been classified as a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt.


(6265) 1985 TW3, Orbit and classification
It orbits the Sun in the inner asteroid belt at a distance of 1.7–2.6 AU once every 3 years and 2 months (1,164 days; semi-major axis of 2.17 AU). Its orbit has an eccentricity of 0.19 and an inclination of 4° with respect to the ecliptic. It was first observed as 1953 RK1 at the former Alma-Ata Observatory (210) in September 1953. The body's observation arc begins with its observation as 1979 YG9 at Crimea–Nauchnij in December 1979, or almost 6 years prior to its official discovery observation at Palomar Observatory.


(6265) 1985 TW3, Numbering and naming
This minor planet was permanently numbered (6265) by the Minor Planet Center on 17 March 1995 (M.P.C. 24890–24891). As of 2018, it has not been named.


(6265) 1985 TW3, Physical characteristics
In the SDSS-based taxonomy, 1985 TW3 is an unusual L-type asteroid.


(6265) 1985 TW3, Physical characteristics, Rotation period
In June 2010, a rotational lightcurve of 1985 TW3 was obtained from photometric observations by Australian astronomers David Higgins and Julian Oey at the Hunters Hill (E14) and Leura Observatory (E17). Lightcurve analysis gave a well-defined rotation period of 2.70932±0.00008 hours with a brightness variation of 0.35 magnitude (U=3). Several concurring period determinations in the range of 2.7091 to 2.710 hours with an amplitude of 0.26 to 0.36 magnitude were also made between 2007 and 2013 (U=3/3/3/3-/2).


(6265) 1985 TW3, Physical characteristics, Satellite
During a previous photometric observation by David Higgins on 15 July 2007, it was revealed that 1985 TW3 is a binary asteroid with a minor-planet moon in its orbit. The discovery was announced on 2 August 2007. The satellite, provisional designation S/2007 (6265) 1, measures approximately 1.16 kilometers. It is separated by 8 km from its primary, orbiting it once every 15 hours and 52 minutes (15.859 hours or 0.6608 days).


(6265) 1985 TW3, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), 1985 TW3 measures between 4.95 and 5.20 kilometers in diameter and its surface has an albedo between 0.285 and 0.287. The Johnston's archive derives a diameter of 4.81 km and 1.16 km for the primary and secondary, respectively, based on an effective WISE-diameter of 4.95 km and using the lower limit of 0.24 for the secondary-to-primary diameter-ratio (Ds/p) determined by David Higgins.


(6265) 1985 TW3, Physical characteristics, Diameter and albedo
Later observation by Higgins and Pravec determined a Ds/p ratio of 0.30 to 0.32, which increases the satellites size by a quarter to a third if all other factors remain unchanged. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for members of the Flora family of 0.24 and calculates a diameter of 5.17 kilometers based on an absolute magnitude of 13.6.


(6382) 1988 EL
(6382) 1988 EL, is a stony Hungaria asteroid from the inner regions of the asteroid belt, approximately 5 kilometers in diameter. It was discovered on 14 March 1988, by American astronomer Jeffrey Alu at the U.S. Palomar Observatory, California.


(6382) 1988 EL, Orbit and classification
The presumed E-type asteroid may not be a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System, but an unrelated interloper, which intruded into the Hungaria orbital space, as indicated by a lower albedos from observations by the NEOWISE mission. It orbits the Sun at a distance of 1.7–1.9 AU once every 2 years and 6 months (900 days). Its orbit has an eccentricity of 0.05 and an inclination of 19° with respect to the ecliptic. The body's first yet unused observation was made at the Chinese Purple Mountain Observatory in 1983. On 13 April 2042 and on 3 October 2113, the asteroid will pass 0.086 AU (12,900,000 km) and 0.092 AU (13,800,000 km) from Mars, respectively.


(6382) 1988 EL, Rotation period
Between February 2005 and January 2015, American astronomer Brian D. Warner obtained 5 rotational lightcurves for this asteroid from photometric observations at the CS3–Palmer Divide Station in Colorado. The lightcurves gave a well-defined rotation period of 2.892–2.898 hours with a low brightness variation between 0.06 and 0.15 magnitude (U=2/3-/3/2+/3).


(6382) 1988 EL, Diameter and albedo
According to two different data sets from space-based survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 4.9 and 5.3 kilometers in diameter and its surface has an albedo of 0.19 and 0.25, respectively, while the Collaborative Asteroid Lightcurve Link  assumes an albedo of 0.30 – a compromise value between 0.4 and 0.2, corresponding to the Hungaria asteroids as collisional family and orbital group, respectively – and calculates a smaller diameter of 4.2 kilometers, based on an absolute magnitude of 13.8.


(6491) 1991 OA
(6491) 1991 OA is a highly eccentric, stony asteroid, classified as near-Earth object and potentially hazardous asteroid, approximately half a kilometer in diameter. It was discovered on 16 July 1991, by American astronomer Henry E. Holt at the U.S. Palomar Observatory in California.


(6491) 1991 OA, Orbit and classification
The S-type body is an Amor asteroid – a subgroup of near-Earth asteroids that approach the orbit of Earth from beyond, but do not cross it. It orbits the Sun at a distance of 1.0–4.0 AU once every 3 years and 11 months (1,444 days). Its orbit has an eccentricity of 0.59 and an inclination of 6° with respect to the ecliptic. Its minimum orbit intersection distance (MOID) with Earth is 0.0420 AU, and on 1 August 2086, it will make a close approach and pass by Earth at a distance of 0.09 AU (13,000,000 km).


(6491) 1991 OA, Orbit and classification
A first precovery was taken at the Australian Siding Spring Observatory in March 1991, extending the asteroid's observation arc by 4 months prior to its discovery.


(6491) 1991 OA, Physical characteristics
In 2000, a rotational lightcurve was published from photometric observations obtained by the Near-Earth Objects Follow-up Program during the early 1990s. The lightcurve rendered a rotation period of 2.69 hours with an brightness amplitude of 0.08 in magnitude (U=2). The Collaborative Asteroid Lightcurve Link (CALL) assumes an albedo of 0.20 and derives a diameter of 0.53 kilometers, based on an absolute magnitude of 18.77.


(65407) 2002 RP120
(65407) 2002 RP120, provisional designation 2002 RP120, is a trans-Neptunian object and damocloid from the outer Solar System. Its orbit is retrograde and comet-like, and has a high eccentricity. It was discovered on 4 September 2002 by astronomers with the LONEOS survey at Anderson Mesa Station, Arizona, in the United States. The unusual object measures approximately 14.6 kilometers (9.1 miles) in diameter and is likely elongated in shape. It is a slow rotator and potentially a tumbler as well. The object was probably ejected from the ecliptic by Neptune.


(65407) 2002 RP120, Orbit and classification
2002 RP120 is a member of the damocloids, with a retrograde orbit and a negative TJupiter of −0.8340. It is also a trans-Neptunian object, as its orbit has a semi-major axis larger than that of Neptune (30.1 AU). The Minor Planet Center lists it as a critical object, centaur, and (other) unusual minor planet due to an orbital eccentricity of more than 0.5.


(65407) 2002 RP120, Orbit and classification
It orbits the Sun at a distance of 2.5–105 AU once every 396 years (semi-major axis of 53.92 AU). Its orbit has an eccentricity of 0.95 and an inclination of 119° with respect to the ecliptic. The body's observation arc begins with a precovery taken by Astrovirtel (I03) at ESO's La Silla Observatory in February 2001, or 19 months prior to its official discovery observation at Anderson Mesa.


(65407) 2002 RP120, Numbering and naming
This minor planet was permanently numbered (65407) by the Minor Planet Center on 14 June 2003 (M.P.C. 48994). As of 2018, it has not been named.


(65407) 2002 RP120, Physical characteristics
The object has a B–R magnitude of 1.37, typical for most dynamical groups in the outer Solar System.


(65407) 2002 RP120, Physical characteristics, Rotation period
In October 2010, a rotational lightcurve of 2002 RP120 was obtained from photometric observations by French amateur astronomer René Roy . Lightcurve analysis gave a rotation period of 200 hours with a brightness amplitude of 0.6 magnitude, indicative of an elongated, non-spherical shape (U=2). With a rotation period above 100 hours, it is a typical slow rotator.


(65407) 2002 RP120, Physical characteristics, Diameter and albedo
According to the survey of minor-planet albedos of bodies in a comet-like orbit, carried out by Yanga Fernández in collaboration with David Jewitt and Scott Sheppard at the Institute for Astronomy, Hawaii, 2002 RP120 measures 14.6 kilometers in diameter and its surface has an albedo of 0.098. Johnston's archive gives a rounded figure of 15 kilometers.


(6545) 1986 TR6
(6545) 1986 TR6, provisional designation 1986 TR6, is a Jupiter trojan from the Greek camp, approximately 53 kilometers (33 miles) in diameter. It was discovered on 5 October 1986, by Slovak astronomer Milan Antal at the Piwnice Astronomical Observatory in Poland. The dark D-type asteroid has a rotation period of 16.3 hours and belongs to the 90 largest Jupiter trojans. It has not been named since its numbering in September 1995.


(6545) 1986 TR6, Orbit and classification
1986 TR6 is a dark Jovian asteroid orbiting in the leading Greek camp at Jupiter's L4 Lagrangian point, 60° ahead of the Gas Giant's orbit in a 1:1 resonance (see Trojans in astronomy). It is also a non-family asteroid in the Jovian background population. It orbits the Sun at a distance of 4.9–5.4 AU once every 11 years and 8 months (4,265 days; semi-major axis of 5.15 AU). Its orbit has an eccentricity of 0.05 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Piwnice in October 1986.


(6545) 1986 TR6, Numbering and naming
This minor planet was numbered on 9 September 1995 (M.P.C. 25628). As of 2018, it has not been named.


(6545) 1986 TR6, Physical characteristics
In the SDSS-based taxonomy, 1986 TR6 is dark D-type asteroid, which agrees with the determined spectral type by Pan-STARRS. Its V–I color index of 0.91 is typical for most larger Jupiter trojans (also see table below).


(6545) 1986 TR6, Physical characteristics, Rotation period
In March 2013, a rotational lightcurve of 1986 TR6 was obtained from photometric observations by Robert Stephens at the Center for Solar System Studies in Landers, California. Lightcurve analysis gave a rotation period of 16.26±0.01 hours with a brightness amplitude of 0.31 magnitude (U=2+).


(6545) 1986 TR6, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Infrared Astronomical Satellite IRAS, 1986 TR6 measures 50.95 and 56.96 kilometers in diameter and its surface has an albedo of 0.068 and 0.0545, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 53.16 kilometers based on an absolute magnitude of 10.1.


(6545) 1986 TR6, 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.


(66063) 1998 RO1
(66063) 1998 RO1 is a stony near-Earth object of the Aten group on a highly-eccentric orbit. The synchronous binary system measures approximately 800 meters (0.50 miles) in diameter. It was discovered by astronomers of the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, on 14 September 1998.


(66063) 1998 RO1
Its minor-planet moon, provisionally designated S/2001 (66063) 1, was discovered in September 2003. It has an orbital period of 14.53 hours and measures approximately 48% of its primary, or 380 meters. It is one of seven known Aten binaries as of 2017.


(66063) 1998 RO1, Interaction with Earth
1998 RO1's orbit is very eccentric, with an aphelion beyond the orbit of Mars and a perihelion inside the orbit of Mercury. It has an orbital period of 360.29 days (0.99 years) and makes close approaches to Earth. But 1998 RO1 makes closer approaches to other inner planets, especially Mars. Its closest approach to a planet between 1950–2200 was to Mars, as it passed 0.00898 AU (1,343,000 km) from Mars on 18 March 1964, and will pass 0.0054 AU (810,000 km) from Mars on 12 October 2065.


(66063) 1998 RO1, Moon
1998 RO1 has one moon, S/2001 (66063) 1. This moon was discovered from lightcurve observations going from 13 to 28 September 2013, and was confirmed by radar observations from the Arecibo Observatory one year later. It is in a very close orbit to 1998 RO1, with a semi-major axis of 800 m (2,600 ft) and an eccentricity of 0.06, giving it a periapsis of 752 m (2,467 ft) and an apoapsis of 848 m (2,782 ft). S/2001 (66063) 1 takes 14.54 hours to complete one orbit around 1998 RO1.


(66063) 1998 RO1, Moon
From the surface of 1998 RO1, S/2001 (66063) 1 would have an apparent diameter of roughly 41°. For comparison, the Sun appears to be 0.5° from Earth. The secondary orbits its primary in a manner very similar to the adjunct image, where the red cross is the center of mass.


(66063) 1998 RO1, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 10 September 2003. As of 2018, it has not been named.


(68950) 2002 QF15
(68950) 2002 QF15 is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, that measures approximately 2 kilometers in diameter. It was discovered on 27 August 2002, by the LINEAR project at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico, United States.


(68950) 2002 QF15, Orbit and classification
2002 QF15 is a S-type asteroid that orbits the Sun at a distance of 0.7–1.4 AU once every 1 years and 1 month (397 days). Its orbit has an eccentricity of 0.34 and an inclination of 25° with respect to the ecliptic. Taken at Palomar Observatory in 1955, a first precovery from the during the Digitized Sky Survey extends the body's observation arc by 47 years prior to its official discovery observation at Socorro.


(68950) 2002 QF15, Orbit and classification
It has an Earth minimum orbital intersection distance 0.0063 AU (942,000 km), which translates into 2.6 LD.


(68950) 2002 QF15, Physical characteristics
In June 2006, a rotational lightcurve of 2002 QF15 was obtained from photometric observation taken by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of 47 hours with a brightness variation of 0.35 magnitude (U=2), superseding a lightcurve previously obtained by Czech astronomer Petr Pravec at Ondřejov Observatory in 2003, which gave a shorter period of 29 hours and an amplitude of 0.3 magnitude (U=2-).


(68950) 2002 QF15, Physical characteristics
According to the survey carried out by the Japanese Akari satellite, the asteroid measures 1.12 kilometers in diameter and its surface has an albedo of 0.428, while the Collaborative Asteroid Lightcurve Link assumes an albedo of 0.040 and calculates a diameter of 3.49 kilometers with an absolute magnitude of 16.4.


(68950) 2002 QF15, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 10 September 2003. As of 2018, it has not been named.


(6S)-6-Fluoroshikimic acid
(6S)-6-Fluoroshikimic acid is an antibacterial agent acting on the aromatic biosynthetic pathway. It may be used against Plasmodium falciparum, the causative agent of malaria. The molecule is targeting the enzymes of the shikimate pathway. This metabolic pathway is not present in mammals. The mechanism of action of the molecule is not through the inhibition of chorismate synthase but by the inhibition of 4-aminobenzoic acid synthesis.


(6S)-6-Fluoroshikimic acid
The use of the molecule led to resistances in Escherichia coli.


(7025) 1993 QA
(7025) 1993 QA is a sub-kilometer asteroid classified as near-Earth object of the Apollo and Amor group, respectively. It was discovered on 16 August 1993, by astronomers of the Spacewatch program at the Kitt Peak National Observatory near Tucson, Arizona, United States. The asteroid measures approximately half a kilometer in diameter and has a short rotation period of 2.5057 hours.


(7025) 1993 QA, Orbit and classification
1993 QA is a member of the dynamical Apollo group, which are Earth-crossing asteroids. Conversely, it is classified as a non-Earth crossing Amor asteroid by the Minor Planet Center, due to its near-threshold perihelion of 1.011 AU.


(7025) 1993 QA, Orbit and classification
It orbits the Sun at a distance of 1.01–1.94 AU once every 21 months (655 days; semi-major axis of 1.48 AU). Its orbit has an eccentricity of 0.31 and an inclination of 13° with respect to the ecliptic. The body's observation arc begins with its official discovery observation by Spacewatch on 16 August 1993.


(7025) 1993 QA, Orbit and classification, Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.0645 AU (9,650,000 km), which translates into 25.1 lunar distances. On 6 February 1996 it transited Earth at a nominal distance of 10,600,000 km; 6,580,000 mi (0.07080 AU). The body's next encounter with Earth below 0.1 AU will occur on 8 February 2048, at a distance of 9,390,000 km; 5,830,000 mi (0.06275 AU).


(7025) 1993 QA, Physical characteristics
1993 QA has been characterized as a dark D-type asteroid on images taken by the Sloan Digital Sky Survey. Conversely, Pan-STARRS' photometric survey determined a much brighter S-type.


(7025) 1993 QA, Physical characteristics, Rotation period
In the late 1990s, two rotational lightcurves of 1993 QA were obtained from photometric observations by European astronomers. Lightcurve analysis gave an identical, well-defined rotation period of 2.5057 hours with a brightness amplitude of 0.32 and 0.50 magnitude, respectively (U=3/3). Its period is near the cohesionless spin-barrier of 2.2 hours, which set the upper limit for fast-rotating asteroids.


(7025) 1993 QA, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1993 QA measures 498 meters in diameter and its surface has a high albedo of 0.340. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and derives a diameter of 770 meters based on an absolute magnitude of 17.94.


(7025) 1993 QA, Naming
As of 2018, this minor planet has not been named yet.


(7335) 1989 JA
(7335) 1989 JA, provisional designation 1989 JA, is an stony asteroid of the Apollo group, classified as near-Earth object and potentially hazardous asteroid, approximately 1 kilometer in diameter. It was discovered on 1 May 1989, by American astronomer Eleanor Helin at the U.S. Palomar Observatory in California.


(7335) 1989 JA, Orbit and classification
The S-type asteroid orbits the Sun at a distance of 0.9–2.6 AU once every 2 years and 4 months (861 days). Its orbit has an eccentricity of 0.48 and an inclination of 15° with respect to the ecliptic. The first observation was made at the discovering observatory in April 1989, extending the asteroid's observation arc by 1 month prior to its discovery observation. It has a minimum orbital intersection distance to Earth of 0.0225 AU (3,370,000 km) which corresponds to 8.8 lunar distances.


(7335) 1989 JA, Physical characteristics
During its discovery in May 1989, radiometric observations for this asteroid at Arecibo and Goldstone Observatory rendered a rotation period of 12 hours (U=n.a.). According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 0.93 kilometers in diameter and its surface has a high albedo of 0.31–0.32, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 1.18 kilometers, based on an absolute magnitude of 17.0.


(7341) 1991 VK
(7341) 1991 VK is a near-Earth minor planet in the Apollo group. It was discovered by Eleanor F. Helin and Kenneth J. Lawrence at the Palomar Observatory in California on 1 November 1991. It is listed as a potentially hazardous object. Every 5 years (from 1946 through 2091) the asteroid makes a close approach to the Earth. The most recent close approach to Earth was on Jan 25, 2017; the next close approach will be on Jan 25, 2022 at a distance of 0.064 AU (9,600,000 km; 5,900,000 mi).


(7348) 1993 FJ22
(7348) 1993 FJ22 is a carbonaceous, Themistian asteroid from the outer region of the asteroid belt, about 10 kilometers in diameter. It was discovered on 21 March 1993, by the Uppsala-ESO Survey of Asteroids and Comets (UESAC) at ESO's La Silla Observatory site in northern Chile.


(7348) 1993 FJ22, Classification and orbit
The dark C-type asteroid is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun in the outer main-belt at a distance of 2.8–3.4 AU once every 5 years and 5 months (1,987 days). Its orbit has an eccentricity of 0.11 and an inclination of 1° with respect to the ecliptic. It was first identified as 1933 FU at Heidelberg in 1933, extending the body's observation arc by 60 years prior to its official discovery observation at La Silla.


(7348) 1993 FJ22, Physical characteristics, Lightcurves
In 2014, two rotational lightcurves of this asteroid were obtained from photometric observations in the R-band at the U.S. Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 3.4735 and 3.470 hours with a brightness variation of 0.10 and 0.13 in magnitude, respectively (U=2/2).


(7348) 1993 FJ22, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link (CALL) assumes a low albedo of 0.08 for the asteroid's surface and calculates a diameter of 9.9 kilometers, based on an absolute magnitude of 13.38.


(7352) 1994 CO
(7352) 1994 CO, provisional designation 1994 CO, is a larger Jupiter trojan from the Trojan camp, approximately 48 kilometers (30 miles) in diameter. The tumbling Jovian asteroid is a slow rotator with an exceptionally long rotation period of 648 hours. It was discovered on 4 February 1994 by Japanese astronomers Seiji Ueda and Hiroshi Kaneda at the Kushiro Observatory on Hokkaidō, Japan, and has not been named since its numbering in December 1996.


(7352) 1994 CO, Classification and orbit
1994 CO is a Jupiter trojan 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.


(7352) 1994 CO, Classification and orbit
It orbits the Sun at a distance of 4.9–5.3 AU once every 11 years and 8 months (4,247 days; semi-major axis of 5.13 AU). Its orbit has an eccentricity of 0.04 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Palomar Observatory in August 1988, more than 5 years prior to its official discovery observation at Kushiro.


(7352) 1994 CO, Physical characteristics
In the SDSS-based taxonomy, 1994 CO is classified as an X/L-type. This is unusual as most Jupiter trojans are D-types, with the reminder being mostly C- and P-type asteroids. It has a V–I color index of 0.85.


(7352) 1994 CO, Physical characteristics, Rotation period
In October 2013, a rotational lightcurve was obtained for this asteroid from photometric observations by American amateur astronomer Robert Stephens at the Trojan Station (U81) of the Center for Solar System Studies in Landers, California. It gave a well-defined, outstandingly long rotation period of 648±3 hours with a brightness variation of 0.30 magnitude (U=3-). As of 2018, there are only about three dozens known slow rotators with periods longer than that of 1994 CO.


(7352) 1994 CO, Physical characteristics, Tumbler
The astronomers also detected a non-principal axis rotation seen in distinct rotational cycles in successive order. This is commonly known as tumbling. 1994 CO is the six-largest asteroid and the second-largest Jupiter trojan after 4902 Thessandrus known to be is such a state (also see list of tumblers).


(7352) 1994 CO, Physical characteristics, Diameter and albedo
According to the space-based surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1994 CO measures 47.07 and 47.73 kilometers in diameter and its surface has an albedo of 0.207 and 0.093, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a larger diameter of 55.67 kilometers, based on an absolute magnitude of 10.0.


(7352) 1994 CO, 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.


(7352) 1994 CO, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 24 December 1996 (M.P.C. 28576). As of 2018, it has not been named.


(7474) 1992 TC
(7474) 1992 TC is a large sized M-type asteroid discovered by Robert H. McNaught in 1992. It is notably one of a few similar M-type asteroids, including the named asteroids 4660 Nereus and 65803 Didymos, which can be reached easily by spacecraft from Earth. The delta-V required to reach 7474 (1992 TC) would be about 5.6 kilometres per second (3.5 mi/s), which is less than is needed to reach the moon. M-type asteroids are thought to be composed primarily of nickel and iron, which if proven to be true means that 7474 (1992 TC) may one day become an important source of raw materials in space.


(7474) 1992 TC
With an absolute magnitude of 18.0, the asteroid is about 670–1500 meters in diameter. On 2031-Aug-11 the asteroid will pass 0.085 AU (12,700,000 km; 7,900,000 mi) from Mars.


(7482) 1994 PC1
(7482) 1994 PC1 is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 kilometers in diameter. It was discovered on 9 August 1994, by astronomer Robert McNaught at the Siding Spring Observatory in Coonabarabran, Australia.


(7482) 1994 PC1, Orbit and classification
1994 PC1 orbits the Sun at a distance of 0.9–1.8 AU once every 1 years and 7 months (571 days). Its orbit has an eccentricity of 0.33 and an inclination of 33° with respect to the ecliptic.


(7482) 1994 PC1, Orbit and classification
On 17 January 1933, it passed 0.00752 AU (1,125,000 km; 699,000 mi) from Earth. On 18 January 2022, it will pass 0.01324 AU (1,981,000 km; 1,231,000 mi) from Earth.


(7482) 1994 PC1, Physical characteristics
In the SMASS classification, 1994 PC1 is a common stony S-type asteroid.


(7482) 1994 PC1, Physical characteristics, Rotation period
In 1998, a rotational lightcurve of 1994 PC1 was obtained from photometric observations by Petr Pravec. Lightcurve analysis gave a well-defined rotation period of 2.5999 hours with a brightness amplitude of 0.29 magnitude (U=3).


(7482) 1994 PC1, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1994 PC1 measures 1.052 kilometers in diameter and its surface has an albedo of 0.277. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.20 and calculates a diameter of 1.30 kilometers based on an absolute magnitude of 16.8.


(7482) 1994 PC1, 2022 flyby
On 19 January 2022, 1994 PC1 will pass just outside of 3 lunar distances of the earth, with a peak magnitude of 7-8.


(7482) 1994 PC1, Naming
As of 2018, this minor planet has not been named.


(75482) 1999 XC173
(75482) 1999 XC173  is a stony Vestian asteroid and an exceptionally slow rotating body from the inner regions of the asteroid belt, approximately 3 kilometers in diameter. It was discovered on 10 December 1999, by LINEAR at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico, United States.


(75482) 1999 XC173, Classification and orbit
The body is classified as a S-type member of the Vesta family by the Collaborative Asteroid Lightcurve Link's Light Curve Data Base (LCDB) . It orbits the Sun at a distance of 2.2–2.5 AU once every 3 years and 8 months (1,328 days). Its orbit has an eccentricity of 0.08 and an inclination of 6° with respect to the ecliptic. A first precovery was obtained at the discovering observatory in October 1999, extending the asteroid's observation arc by 2 months prior to its official discovery observation.


(75482) 1999 XC173, Physical characteristics
A rotational lightcurve was obtained for this asteroid from photometric observations at the Californian Palomar Transient Factory in September 2013. It gave a rotation period of 1234 hours with an estimated error margin of ±90 hours. As of 2016, it is the 6th slowest rotating minor planet known to exist. Its high brightness variation of 0.69 magnitude indicates that it has a non-spheroidal shape (U=2).


(75482) 1999 XC173, Physical characteristics
According to the LCDB, the body's surface has an assumed standard albedo for stony asteroids of 0.20 and a calculated diameter of 2.96 kilometers with an absolute magnitude of 15.01.


(75482) 1999 XC173, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 15 April 2004. As of 2018, it has not been named.


(7563) 1988 BC
(7563) 1988 BC, provisional designation 1988 BC, is a background asteroid from the central region of the asteroid belt, approximately 16 kilometers (10 miles) in diameter. It was discovered on 16 January 1988, by Japanese amateur astronomer Takuo Kojima at the YGCO Chiyoda Station in the Kantō region of Japan. The asteroid has a rotation period of 6.5 hours.


(7563) 1988 BC, Classification and orbit
1988 BC is non-family asteroid of the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.1–3.3 AU once every 4 years and 5 months (1,602 days; semi-major axis of 2.68 AU). Its orbit has an eccentricity of 0.23 and an inclination of 13° with respect to the ecliptic.


(7563) 1988 BC, Physical characteristics, Lightcurves
In January 2010, a rotational lightcurve of 1988 BC was obtained from photometric observations by Pierre Antonini at the Bédoin Observatory (132) in southeastern France. Lightcurve analysis gave a rotation period of 6.539±0.005 hours with a brightness variation of 0.30 in magnitude (U=3). A previous 2006-observation by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado gave a period of 6.510 hours and an amplitude of 0.24 magnitude (U=3-).


(7563) 1988 BC, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid has a low albedo of between 0.048 and 0.08, with a diameter between 12.04 and 17.27 kilometers.


(7563) 1988 BC, Physical characteristics, Diameter and albedo
Despite the results from the space-based observations, the Collaborative Asteroid Lightcurve Link assumes a higher albedo of 0.10 – a compromise between the stony and carbonaceous asteroid populations from the inner and outer main-belt, respectively – and hence calculates a smaller diameter of 12.1 kilometers with an absolute magnitude of 12.7.


(78799) 2002 XW93
(78799) 2002 XW93, provisional designation 2002 XW93, is a trans-Neptunian object and centaur from the outer Solar System, approximately 565 kilometers (351 mi) in diameter. It was discovered on 10 December 2002, by astronomers at the Palomar Observatory in California. According to American astronomer Michael Brown, the minor planet is a likely dwarf planet.


(78799) 2002 XW93, Orbit and physical characteristics
2002 XW93 orbits the Sun at a distance of 27.9–46.8 AU once every 228 years and 4 months (83,410 days; semi-major axis of 37.36 AU). Its orbit has an eccentricity of 0.25 and an inclination of 14° with respect to the ecliptic. The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken Palomar in December 1989, or 13 years prior to its official discovery observation.


(78799) 2002 XW93, Orbit and physical characteristics
As of 2016, after a total of 29 observations, its orbital uncertainty parameter is at 3. Its last observation was made by the Hubble Space Telescope in September 2008. On 10 August 1926, it most recently reached perihelion, when it was nearest to the Sun. It is a near 5:7 resonant trans-Neptunian object.


(78799) 2002 XW93, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 15 April 2004. As of 2018, it has not been named.


(7888) 1993 UC
(7888) 1993 UC is a near-Earth minor planet in the Apollo group. It was discovered by Robert H. McNaught at the Siding Spring Observatory in Coonabarabran, New South Wales, Australia, on 20 October 1993. The asteroid has an observation arc of 23 years and has a well determined orbit. Its estimated size is 2.3 to 5.2 km.


(7888) 1993 UC
On 20 March 2013, the asteroid passed 49 lunar distances or 0.12598 AU (18,846,000 km; 11,711,000 mi) from Earth at a relative velocity of 21.8 km/s (49,000 mph). The approach posed no threat to Earth. (7888) 1993 UC is not classified as a potentially hazardous asteroid (PHA) because its Earth MOID (Minimum Orbit Intersection Distance) is only 0.089 AU, and only objects with an Earth MOID less than 0.05 AU are considered PHAs.


(7888) 1993 UC
It was discovered to be a binary asteroid by Arecibo Observatory in March 2013.


(7888) 1993 UC
On 29 April 2146, the asteroid will pass 0.0346 AU (5,180,000 km; 3,220,000 mi) from asteroid 4 Vesta.


(79983) 1999 DF9
(79983) 1999 DF9 is a trans-Neptunian object of the Kuiper belt, classified as a non-resonant cubewano, that measures approximately 270 kilometers in diameter.


(79983) 1999 DF9, Discovery
It was discovered on 20 February 1999, by American and British astronomers Jane Luu, Chad Trujillo and David C. Jewitt at the U.S. Kitt Peak National Observatory in Arizona. As no precoveries were taken, the minor planet's observation arc begins with its discovery observation in 1999.


(79983) 1999 DF9, Classification and orbit
The carbonaceous minor planet is a classical Kuiper belt object or "cubewano", which are not in an orbital resonance with Neptune and do not cross the giant planet's orbit. It orbits the Sun at a distance of 39.8–53.6 AU once every 319 years and 1 month (116,560 days). Its orbit has an eccentricity of 0.15 and an inclination of 10° with respect to the ecliptic. This makes it a relatively eccentric body for a classical Kuiper belt object, which typically have low-eccentricities of 0.10 or less.


(79983) 1999 DF9, Physical characteristics
In February 2001, a rotational lightcurve was published for this minor planet from photometric observations by Portuguese astronomer Pedro Lacerda and the discovering astronomer Jane Luu. Lightcurve analysis gave a relatively short rotation period of 6.65 hours with a brightness variation of 0.40 magnitude (U=2).


(79983) 1999 DF9, Physical characteristics
The Collaborative Asteroid Lightcurve Link assumes a low albedo of 0.10 and calculates a mean-diameter of 265 kilometers, based on an absolute magnitude of 6.0, while the Johnston's archive give a diameter of 306 kilometers for an albedo of 0.09. Due to its small size, it is unlikely to be classified as a dwarf planet.


(79983) 1999 DF9, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 4 May 2004. As of 2018, it has not been named.


(8014) 1990 MF
(8014) 1990 MF is a sub-kilometer near-Earth object and potentially hazardous asteroid in the Apollo group. It was discovered by American astronomer Eleanor Helin at the Palomar Observatory in California on 26 June 1990. The asteroid measures approximately 0.7 kilometers (0.4 miles) in diameter. On 23 July 2020, it came within 0.055 AU of the Earth—about 21 times the Moon's distance.


(8035) 1992 TB
(8035) 1992 TB is an Apollo asteroid, a type of Near-Earth Object. It is also a Venus-crosser and a Mars-crosser, although it doesn't make close approaches to Mars.


(8035) 1992 TB, Encounters with Venus and Earth
1992 TB makes close approaches to Earth, but often comes many times closer to Venus. Soon after the discovery of the asteroid in 1992, a close approaches of Earth was made. Three years after it was discovered, 1992 TB came 45,720,000 km (0.3056 AU) from Earth. In 2003, (8035) 1992 TB was listed as a potentially hazardous object, but has since been removed. However, 1992 TB is not expected to come within 37,000,000 km (0.25 AU) of Earth in the near future. On the other hand, 1992 TB can come much closer to Venus. Its next Venus encounter was in 29 May 2015, where it came 11,710,000 km (0.0783 AU) from the planet. Its closest approach in the near future will be 7,380,000 km (0.0493 AU).


(8201) 1994 AH2
(8201) 1994 AH2 is a highly eccentric, rare-type asteroid, classified as near-Earth object of the Apollo group of asteroids, approximately 2 kilometers in diameter. It was discovered on 5 January 1994, by Australian amateur astronomer Gordon Garradd during the AANEAS survey at the Siding Spring Observatory, Australia. It has an Earth minimum orbit intersection distance of 0.1 AU (15 million km) and is associated with the Beta Taurids daytime meteor shower.


(8201) 1994 AH2, Orbit and classification
The asteroid orbits the Sun at a distance of 0.7–4.3 AU once every 4.04 years (1,477 days). Its orbit has an eccentricity of 0.71 and an inclination of 10° with respect to the ecliptic. It is a member of the Alinda group of asteroids with a 3:1 resonance with Jupiter that has excited the eccentricity of the orbit over the eons. As an Alinda asteroid it makes approaches to Jupiter, Earth, and Venus.


(8201) 1994 AH2, Orbit and classification
1994 AH2 has an Earth minimum orbital intersection distance of 0.1012 AU (15,100,000 km), which corresponds to 39.4 lunar distances. Due to its elongated orbit, it also approaches the orbit of Jupiter within 0.1022 AU (15,300,000 km). On 4 January 2079, it will pass 0.3595 AU (53,800,000 km) from the Earth.


(8201) 1994 AH2, Orbit and classification
A first precovery was taken at the discovering observatory in 1981, extending the asteroid's observation arc by 13 years prior to its discovery.


(8201) 1994 AH2, Physical characteristics
In the SMASS classification, 1994 AH2 is characterized as a rare O-type asteroid.


(8201) 1994 AH2, Physical characteristics, Rotation period
In the late 1990s, Czech astronomer Petr Pravec obtained two rotational lightcurves for this asteroid from photometric observations taken at the Ondřejov Observatory, Czech Republic. They gave a longer-than average rotation period of 23.949 and 24 hours with a brightness variation of 0.27 and 0.3 magnitude, respectively (U=2/n.a. ).


(8201) 1994 AH2, 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 1.86 kilometers in diameter and its surface has an albedo of 0.154. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.18 and calculates a diameter of 2.17 kilometers, based on an absolute magnitude of 15.8. American astronomer Richard Binzel gives a diameter of 2.2 kilometers.


(82075) 2000 YW134
(82075) 2000 YW134, provisional designation: 2000 YW134, is a resonant trans-Neptunian object and binary system, located in the outermost region of the Solar System. It was discovered on 26 December 2000, by astronomers with the Spacewatch survey at Kitt Peak Observatory near Tucson, Arizona. The reddish object stays in a rare 3:8 resonance with Neptune and measures approximately 216 kilometers (130 miles). Its 75-kilometer sized companion was discovered by the Hubble Space Telescope in October 2002. As of 2021, neither the primary body nor its satellite have been named.


(82075) 2000 YW134, Orbit and classification
2000 YW134 orbits the Sun at a distance of 41.0–73.8 AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its official discovery observation by Spacewatch on 26 December 2000. It last came to perihelion in 1979, and is currently at about 46.5 AU from the Sun, with an apparent magnitude of 21.54. It will reach aphelion in December 2197.


(82075) 2000 YW134, Orbit and classification
2000 YW134 is a resonant trans-Neptunian object that stays in a rare 3:8 mean-motion orbital resonance with Neptune, orbiting exactly three times the Sun for every 8 orbits Neptune does. There are currently two other objects known to have the same resonant type: 2014 UE228 and (542258) 2013 AP183. Due to its relatively large distance to Neptune, a classification as an extended-scattered or detached object was also considered earlier on (Lykawka, 2006). However, improved observations and long-term numerical integrations of the object's orbit by Emel’yanenko and Kiseleva (84% probability) and the Deep Ecliptic Survey – with all alternative integrations in agreement, showing a minimum perihelion distance of 38.2 AU – have since secured its 3:8 orbital resonance with Neptune.


(82075) 2000 YW134, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 4 May 2004, receiving the number (82075) in the minor planet catalog (M.P.C. 51853). As of 2021, it has not been named. According to the established naming conventions, it will be given a mythological name associated with the underworld.


(82075) 2000 YW134, Physical characteristics
The surface of 2000 YW134 is moderately red in the visible part of the spectrum. Its IR spectral type transitions from the very red (RR) to the intermediate blue-red (BR). Alternatively a BR-spectral type has also been assumed. The object's B−V and V–R color indices have also been measured several times, giving an averaged value of close to 1.0 and 0.5, respectively, for a combined B−R magnitude of 1.50.


(82075) 2000 YW134, Physical characteristics, Diameter and albedo
In 2010, observations with the Herschel Space Observatory constrained the object's geometric albedo to no darker than 8%, and allowed to place an upper limit to its effective mean-diameter of 500 km (310 mi), as no thermal radiation had been detected. However, according to Michael Mommert's dissertation in 2013, the object has a much higher albedo of 0.408±0.329, which greatly reduces its effective diameter to 229 km (140 mi).


(82075) 2000 YW134, Physical characteristics, Satellite
On 25 October 2002, observations in the far-infrared with the NICMOS instrument of the Hubble Space Telescope revealed, that 2000 YW134 is a binary system with a satelite in its orbit. The discovery was announced on 6 October 2005. Johnston's Archive derives a diameter of 216 km (130 mi) for the primary and a diameter of 75 km (47 mi) for the secondary, based on a secondary-to-primary diameter ratio of 0.347, for a difference of 1.3 magnitudes between the two objects. The satellite, designated S/2005 (82075) 1, orbits its primary every 10 days (estimated) at an average distance of 1,900 km (1,200 mi).


(82158) 2001 FP185
(82158) 2001 FP185, provisional designation 2001 FP185, is a highly eccentric trans-Neptunian object from the scattered disc in the outermost part of the Solar System, approximately 330 kilometers in diameter. It was discovered on 26 March 2001, by American astronomer Marc Buie at Kitt Peak National Observatory in Arizona, United States.


(82158) 2001 FP185, Orbit and classification
2001 FP185 is a scattered-disc object which belong to the most distant and coldest objects in the Solar System and are thought to be source of most periodic comets.


(82158) 2001 FP185, Orbit and classification
It orbits the Sun at a distance of 34.3–420.2 AU once every 3425 years and 4 months (1,251,096 days). Its orbit has an eccentricity of 0.85 and an inclination of 31° with respect to the ecliptic. A first precovery was taken by the Sloan Digital Sky Survey in March 1999, extending the body's observation arc by 2 years prior to its official discovery observation at Kitt Peak.


(82158) 2001 FP185, Orbit and classification, Planet Nine coorbital
If a massive trans-Neptunian object exists, like hypothetical Planet Nine, 2001 FP185 may be co-orbital with it.


(82158) 2001 FP185, Physical characteristics, Spectra and colors
2001 FP185's color has extensively been measured. The object has a determined BR and IR spectra, which are intermediate classes of the very blue BB and very red RR spectra.


(82158) 2001 FP185, Physical characteristics, Diameter and albedo
According to astronomer Michael Brown and based on radiometric observations, 2001 FP185 measures 336 kilometers in diameter and its surface has an (assumed) albedo of 0.05. Observations with the PACS-instrument of the Herschel Space Observatory during a survey of scattered-disc objects ("TNO are cool") found a similar diameter of 332 kilometer with an albedo of 0.046. The Collaborative Asteroid Lightcurve Link assumes a higher albedo of 0.10 and consequently derives a much shorter diameter of 222 kilometers based on an absolute magnitude of 6.38. Brown considers 2001 FP185 to be possibly a dwarf planet (see list).


(82158) 2001 FP185, Physical characteristics, Lightcurve
No rotational lightcurve of 2001 FP185 has been obtained from photometric observations. The body's rotation period, pole axis and brightness amplitude remains unknown.


(82158) 2001 FP185, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 4 May 2004. As of 2018, it has not been named.


(84522) 2002 TC302
(84522) 2002 TC302, prov. designation: 2002 TC302, is a large trans-Neptunian object and dwarf planet candidate, located in the outermost region of the Solar System. It was discovered on 9 October 2002, by American astronomers Mike Brown, Chad Trujillo and David Rabinowitz at the Palomar Observatory in California. The resonant trans-Neptunian object stays in a 2:5 resonance with Neptune. It has a reddish color, a rotation period of 56.1 hours and measures at least 500 kilometers (310 miles) in diameter.


(84522) 2002 TC302, Orbit and classification
2002 TC302 orbits the Sun at a distance of 39.2–71.4 AU once every 410 years and 12 months (150,105 days; semi-major axis of 55.28 AU). Its orbit has an eccentricity of 0.29 and an inclination of 35° with respect to the ecliptic. In December 2058, It will come to perihelion (minimum distance from the Sun) at 39.2 AU, which is  about the same as Pluto's semi-major axis (average distance from the Sun). Given the long orbit that TNOs have around the Sun, 2002 TC302 comes to opposition in late October of each year at an apparent magnitude of 20.5.


(84522) 2002 TC302, Orbit and classification
Both the Minor Planet Center (MPC) and the Deep Ecliptic Survey (DES) show this probable dwarf planet and resonant trans-Neptunian object to be in a 2:5 resonance with Neptune, which means it completes two orbits for every five orbits of Neptune.


(84522) 2002 TC302, Physical characteristics
2002 TC302 has an absolute magnitude of 3.78. It has an estimated diameter of 584.1+105.6−88.0 km. Using the Spitzer Space Telescope, it was previously estimated to have a diameter of 1145+337−325 km, which would have made it one of the largest possible dwarf planets. This overestimation was due to insufficient motion to allow for a good sky subtraction and because it was very close to a brighter background object. Brown noted that the Spitzer measurement involved a very large potential error and that the object would likely be smaller, making its chances of it being a dwarf planet "likely" rather than "near certainty", in his opinion.


(84522) 2002 TC302, Physical characteristics
The red spectra suggests that 2002 TC302 has very little fresh ice on its surface. Its rotation period was initially estimated by Thirouin et al. to be 5.41 h, based on a light-curve amplitude of 0.04±0.01 mag. However, this short rotation period was most likely an alias due to a bias for shorter and more easily discernable shorter periods. 2002 TC302 is highly oblate, and Ortiz et al. suggest a longer rotation period estimate of 56.1 hours.


(84522) 2002 TC302, Physical characteristics
An occultation of a 15.3 magnitude star by 2002 TC302 on 28 January 2018 over Europe suggests that it has highly oblate shape with dimensions of 543.2±18 × 459.5±11 km and a projected axial ratio of a/c=1.18. The area equivalent diameter of 2002 TC302 is 499.6 km.


(84522) 2002 TC302, Possible satellite
The mean diameter of 2002 TC302 determined from occultations in 2018 is smaller than the larger diameter estimate of 584.1+105.6−88.0 km by Spitzer in 2008. Despite the large uncertainty in the Spitzer's estimate, the difference of ~84 km between the two diameters is significant, implying that 2002 TC302 may have a large satellite with a possible size range of 100–300 km, nearly as large as 2002 TC302 itself. This possible satellite is expected to orbit 2002 TC302 at a very close distance of less than 2000 km, close enough to slow down 2002 TC302's rotation through tidal interactions.


(84522) 2002 TC302, Possible satellite
If both the primary body and satellite are doubly tidally locked, then the expected orbital period of the satellite would be approximately 54 hours, equal to 2002 TC302's rotation. Given an orbital period of 54 hours, the satellite's estimated orbital separation from the primary would be 1780 km, with an angular separation of 58 milliarcseconds, too small to be resolved with current space telescopes such as Hubble. Under the assumption the satellite's diameter is 200 km, it would cause 2002 TC302's position to oscillate by 18 milliarcseconds as it orbits around its barycenter.


(84719) 2002 VR128
(84719) 2002 VR128, also written (84719) 2002 VR128, is a trans-Neptunian object (TNO). It was discovered in 2002 by Michael Brown and Chad Trujillo. The object is a plutino, an object in 2:3 orbital resonance with Neptune.


(84719) 2002 VR128, Physical properties
The size of (84719) 2002 VR128 was measured by the Herschel Space Telescope to be 448.5+42.1−43.2 km. The surface of (84719) 2002 VR128 is red in the visible spectral range.


(84922) 2003 VS2
(84922) 2003 VS2 is a trans-Neptunian object discovered by the Near Earth Asteroid Tracking program on 14 November 2003. Like Pluto, it is in a 2:3 orbital resonance with Neptune and is thus a plutino. Mike Brown's website lists it as "likely" a dwarf planet. However, Brown assumed that 2003 VS2 was significantly larger than it really is, and analysis of its light-curve suggests that it may not be in the hydrostatic equilibrium.


(84922) 2003 VS2, Orbit and rotation
Like Pluto, (84922) 2003 VS2 is locked in the 3:2 mean-motion resonance with Neptune, although its orbit is both less inclined and significantly less eccentric than Pluto's.


(84922) 2003 VS2, Orbit and rotation
(84922) 2003 VS2 has a significant light-curve amplitude of 0.21±0.01. The most likely value of the rotation period is 7.41±0.02 h.


(84922) 2003 VS2, Physical characteristics
(84922) 2003 VS2 has a moderately red surface with a moderately red color indices B−V=0.93, V−R=0.59. Its geometrical albedo is about 0.13.


(84922) 2003 VS2, Physical characteristics
In 2007, its diameter was initially estimated by the Spitzer Space Telescope at 725±200 km. However, in 2012, this was reduced to 523.0+35.1−34.4 km after new Herschel Space Telescope observations. In 2019, 2003 VS2 was found to be ellipsoidal in shape based on stellar occultations that occurred in 2013 and 2014; the light curve derived from the occultations suggests that this plutino is not in hydrostatic equilibrium and hence not a dwarf planet. The dimensions of 2003 VS2 are estimated at 627.6 km × 531 km × 494.6 km, with a volume-equivalent diameter 548.3+29.5−44.6 km. 2003 VS2 has no known satellite that can be used to directly determine its mass, but assuming a density of 1 g/cm3, typical of mid size TNO's, gives a mass estimate of about 7.5×1019 kg.


(85182) 1991 AQ
(85182) 1991 AQ, provisional designation 1991 AQ, is a stony asteroid on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 kilometers (0.7 miles) in diameter. It was discovered on 14 January 1991, by American astronomer Eleanor Helin at the Palomar Observatory in California. Based on its brightness variation of 0.69 magnitude, this Q-type asteroid is likely elongated. It belongs to the small group of potentially hazardous asteroids larger than one kilometer.


(85182) 1991 AQ, Orbit and classification
1991 AQ is a member of the Earth-crossing class of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. It is also a Venus- and Mars-crosser due to its extreme perihelion and aphelion, respectively.


(85182) 1991 AQ, Orbit and classification
It orbits the Sun at a distance of 0.5–3.9 AU once every 3 years and 4 months (1,210 days; semi-major axis of 2.22 AU). Its orbit has a high eccentricity of 0.78 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Palomar in 1991.


(85182) 1991 AQ, Orbit and classification, Close approaches
The asteroid has currently an Earth minimum orbital intersection distance of 0.0165 AU (2,470,000 km; 1,530,000 mi), which corresponds to 6.4 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In 1991 and 1994, it approached Earth at a nominal distance of 0.054 AU (21 LD). The asteroids closest encounter with Earth is projected to occur on 27 January 2130, at a distance of 0.0106 AU (4.1 LD) only (see table). It also makes close encounters to Mercury, Venus, Mars and Jupiter.


(85182) 1991 AQ, Physical characteristics
In the Tholen classification, this object is an uncommon Q-type asteroid, that falls into the larger stony S-complex. As of 2018, no rotational lightcurve of this asteroid has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. It has a brightness variation of 0.69 magnitude, indicative for an elongated, non-spherical shape.


(85182) 1991 AQ, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, this asteroid measures 1.1 kilometers in diameter and its surface has an albedo of 0.242. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.18 and derives a diameter of 1.14 kilometers based on an absolute magnitude of 17.20.


(85182) 1991 AQ, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 30 August 2004 (M.P.C. 52517). As of 2018, it has not been named.


(85627) 1998 HP151
(85627) 1998 HP151, provisional designation 1998 HP151, is a trans-Neptunian object from the classical Kuiper belt, located in the outermost region of the Solar System. The cubewano belongs to the cold population. It has a perihelion (closest approach to the Sun) at 40.297 AU and an aphelion (farthest approach from the Sun) of 48.306 AU. It is about 146 km in diameter. It was discovered on 28 April 1998, at the Mauna Kea Observatory, Hawaii.


(85633) 1998 KR65
(85633) 1998 KR65, provisional designation 1998 KR65, is a trans-Neptunian object from the classical Kuiper belt, located in the outermost region of the Solar System. The cubewano belongs to the cold population. It has a perihelion (closest approach to the Sun) at 42.385 AU and an aphelion (farthest approach from the Sun) at 44.859 AU. It is about 192 km in diameter. It was discovered on 29 May 1998, by Gary M. Bernstein.


(85640) 1998 OX4
(85640) 1998 OX4, also written 1998 OX4, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group.


(85640) 1998 OX4, Description
It was discovered on 26 July 1998 by the Spacewatch program and subsequently lost. It was re-discovered by the Near-Earth Asteroid Tracking (NEAT) project on 31 August 2002, as 2002 PJ34. It was removed from the Sentry Risk Table on 8 August 2002. It has a well determined orbit with an observation arc of more than 10 years. It is included in the Minor Planet Center list of Potentially Hazardous Asteroids (PHAs) as it comes to within 0.05 AU of Earth periodically. It is also a Mars crossing asteroid


(85713) 1998 SS49
(85713) 1998 SS49, provisional designation 1998 SS49, is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 3 kilometers (1.9 miles) in diameter. The asteroid was discovered on 29 September 1998, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. It is one of the largest potentially hazardous asteroids and has a notably low Earth-MOID of less than the distance to the Moon.


(85713) 1998 SS49, Orbit and classification
1998 SS49 is a member of the dynamical Apollo group, which are Earth-crossing asteroids. Apollo asteroids are the largest subgroup of near-Earth objects.


(85713) 1998 SS49, Orbit and classification
It orbits the Sun at a distance of 0.7–3.2 AU once every 2 years and 8 months (975 days; semi-major axis of 1.92 AU). Its orbit has a high eccentricity of 0.64 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Socorro in September 1998.


(85713) 1998 SS49, Orbit and classification, Close approaches
At about absolute magnitude 15.6, 1998 SS49 is one of the brightest and presumably largest known potentially hazardous asteroid (see PHA-list). It has a very low Earth minimum orbital intersection distance of 0.0023 AU (340 thousand km; 0.90 LD). On 26 November 1902, this asteroid made its closest near-Earth encounter since 1900 at a nominal distance of 0.0659 AU (9.86 million km; 25.6 LD). The next notable close approach will be on 21 November 2022 passing at a nominal distance of 0.141 AU (21,100,000 km; 13,100,000 mi).


(85713) 1998 SS49, Orbit and classification, Close approaches
1998 SS49 is also a Venus- and Mars-crosser, as it crosses the orbit of Venus and the Red Planet at c. 0.72 and 1.66 AU, respectively.


(85713) 1998 SS49, Physical characteristics, Rotation period
In 2014, two rotational lightcurves of 1998 SS49 were obtained from photometric observations by American astronomer Brian Warner at the CS3–Palmer Divide Station in California (U82). Lightcurve analysis gave a rotation period of 5.370 and 5.66 hours and a brightness variation of 0.18 and 0.06 magnitude, respectively (U=2/2), one of which gave an alternative period solution of 2.686±0.002 hours. In April 2016, the EURONEAR lightcurve survey measured a period of 5.398 hours with an amplitude of 0.12 magnitude (U=2).


(85713) 1998 SS49, Physical characteristics, Diameter and albedo
Surveys contrast: of the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer. These measure the object as between 2 and 3.484 kilometers lengthways (in diameter) and to have an albedo (optical wavelength reflectivity) between 0.076 and 0.237. The Collaborative Asteroid Lightcurve Link assumes a stony typical albedo of 0.20 to calculate the diameter as 2.25 kilometers and an absolute magnitude of 15.6.


(85713) 1998 SS49, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.


(85770) 1998 UP1
(85770) 1998 UP1 is a near Earth, Aten asteroid orbiting at nearly a 1:1 resonance with Earth.


(85770) 1998 UP1, Orbit
With an orbital period of 364.3 days, 1998 UP1 is in a near 1:1 orbital resonance with Earth. Although their periods are almost identical, their orbits are very different; 1998 UP1 has a highly eccentric orbit and moves between 0.65–1.35 AU from the Sun, it is also very highly inclined at 33°. The preliminary period of 1998 UP1 was originally thought to be slightly longer than 1 year producing an error in the predicted position of about 35 degrees; it was selected as a priority for recovery and recovered by the Camarillo Observatory on 12 October 1999.


(85770) 1998 UP1, Orbit
1998 UP1 also makes close approaches to Venus and will pass 0.0255 AU (3,810,000 km; 2,370,000 mi) from Venus on 24 January 2115.


(85989) 1999 JD6
(85989) 1999 JD6 is an Aten asteroid, near-Earth object, and potentially hazardous object in the inner Solar System that makes frequent close approaches to Earth and Venus. On the Earth approach in 2015, it was observed by the Goldstone Solar System Radar and found to be a contact binary with the largest axis approximately 2 kilometers wide, and each lobe about 200–300 meters large. Although 1999 JD6 in its current orbit never passes closer than 0.047 AU to Earth, it is listed as a potentially hazardous object because it is large and might pose a threat in the future.


(85989) 1999 JD6
The asteroid is well-observed, having been observed over 2,000 times over a length of over 25 years, and was assigned a numeric designation in August 2004.


(85989) 1999 JD6, July 2015 Earth passage
On 24 July 2015 1999 JD6 came as close as 19 lunar distances to Earth. It was imaged by radar, and shown to be a contact binary, about 2 kilometers (1.2 miles) on its long axis.


(85990) 1999 JV6
(85990) 1999 JV6, provisional designation 1999 JV6, is a sub-kilometer near-Earth asteroid and a potentially hazardous object of the Apollo group. It was discovered by astronomers of the LINEAR program at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico. 1999 JV6 is a contact binary object consisting of two distinct lobes, as seen in radar images from various observatories including Arecibo and Goldstone in January 2015.


(85990) 1999 JV6, Close approaches
In January 2015, 1999 JV6 approached Earth within a distance of 32.4 lunar distances (0.0833 AU). During the encounter, 1999 JV6 was observed by radar from the Arecibo, Green Bank, and Goldstone observatories. In January 2016, 1999 JV6 has made another close approach at a distance of 12 lunar distances (0.032 AU), several times closer than the encounter in 2015.


(85990) 1999 JV6, Close approaches
The Minor Planet Center has classified 1999 JV6 as a potentially hazardous asteroid due to its large size and small Earth minimum orbit intersection distance (MOID) of 0.03 AU.