(154276) 2002 SY50
(154276) 2002 SY50, provisional designation 2002 SY50, 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 30 September 2002, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The K-type asteroid has a rotation period of 4.8 hours. It will make a close encounter with Earth on 30 October 2071.


(154276) 2002 SY50, Orbit and classification
2002 SY50 is a member of the Earth-crossing group of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members.


(154276) 2002 SY50, Orbit and classification
It orbits the Sun at a distance of 0.53–2.88 AU once every 2 years and 3 months (813 days; semi-major axis of 1.7 AU). Its orbit has an eccentricity of 0.69 and an inclination of 9° with respect to the ecliptic. Due to its large aphelion of 2.88 AU, it also crosses the orbit of Mars at 1.66 AU. The body's observation arc begins one month prior to its official discovery observation with its first observation by the NEAT program at Palomar Observatory in August 2002.


(154276) 2002 SY50, Orbit and classification, Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.0027 AU (404,000 km; 251,000 mi), which corresponds to 1.05 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size.


(154276) 2002 SY50, Orbit and classification, Close approaches
In November 1933, it approached Earth at a nominal distance of 0.098 AU (38 LD), and in November 2002 at 0.084 AU (33 LD). Its closest near-Earth encounter is predicted to occur on 30 October 2071, at a distance of 0.0088 AU (3.4 LD) only (see table).


(154276) 2002 SY50, Physical characteristics
Photometry by the Sloan Digital Sky Survey has characterized 2002 SY50 as an uncommon K-type asteroid, which is typically seen among members of the Eos family in the asteroid belt.


(154276) 2002 SY50, Physical characteristics, Rotation period
In October 2002, a rotational lightcurve of this asteroid was obtained from photometric observations by Italian astronomer Gianluca Masi at the Campo Catino Astronomical Observatory (468). Lightcurve analysis gave a well-defined rotation period of 4.823 hours with a brightness amplitude of 0.52 magnitude (U=3).


(154276) 2002 SY50, 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 1.06 kilometers in diameter and its surface has an albedo of 0.14, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 0.897 kilometers based on an absolute magnitude of 17.6.


(154276) 2002 SY50, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 2 April 2007 (M.P.C. 59337). As of 2018, it has not been named.


(15430) 1998 UR31
(15430) 1998 UR31 is a main-belt binary asteroid. It was discovered through the Beijing Schmidt CCD Asteroid Program at the Xinglong Station in the Chinese province of Hebei on October 22, 1998. A moon was discovered orbiting the asteroid in 2010. The moon has an orbital period of almost exactly a day, and is tidally locked with the asteroid.


(15502) 1999 NV27
(15502) 1999 NV27, provisional designation 1999 NV27, is a Jupiter trojan from the Trojan camp, approximately 53 kilometers (33 miles) in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The dark Jovian asteroid has a rotation period of 15.1 hours and belongs to the 90 largest Jupiter trojans. It has not been named since its numbering in June 2000.


(15502) 1999 NV27, Orbit and classification
1999 NV27 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.


(15502) 1999 NV27, Orbit and classification
It orbits the Sun at a distance of 5.0–5.2 AU once every 11 years and 7 months (4,238 days; semi-major axis of 5.12 AU). Its orbit has an eccentricity of 0.02 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins with its first observation as 1982 BX14 at Palomar Observatory in January 1982, more than 16 years prior to its official discovery observation at Socorro.


(15502) 1999 NV27, Physical characteristics
1999 NV27 is an assumed, carbonaceous C-type asteroid. It has a V–I color index of 0.875.


(15502) 1999 NV27, Physical characteristics, Rotation period
In September 2009, a first rotational lightcurve of 1999 NV27 was obtained from photometric observations by Linda French at the Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis gave a rotation period of 15.03±0.03 hours with a brightness variation of 0.10 magnitude (U=2).


(15502) 1999 NV27, Physical characteristics, Rotation period
Since then, follow-up observations by Daniel Coley and Robert Stephens at the Center for Solar System Studies during 2013–2017 gave four more refined lightcurves, with the best-rated one from January 2017 showing a rotation period of 15.129±0.002 hours and an amplitude of 0.26 magnitude (U=3).


(15502) 1999 NV27, 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, 1999 NV27 measures 50.86 and 53.10 kilometers in diameter and its surface has an albedo of 0.067 and 0.069, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 55.67 kilometers based on an absolute magnitude of 10.0.


(15502) 1999 NV27, 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.


(15502) 1999 NV27, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 21 June 2000 (M.P.C. 40827). As of 2018, it has not been named.


(155140) 2005 UD
(155140) 2005 UD (provisional designation 2005 UD) is an asteroid on an eccentric orbit, classified as a near-Earth object of the Apollo group. It was discovered on 22 October 2005, by the Catalina Sky Survey at the Catalina Station in Arizona, United States. 2005 UD is thought to be a possible fragment of 3200 Phaethon due to its similar orbit, although it is not dynamically associated with the Geminid meteor stream produced by Phaethon.


(155140) 2005 UD
Due to 2005 UD's highly eccentric orbit, it experiences extreme temperature variations up to 975 K (702 °C; 1,295 °F) at perihelion, leading to thermal fracturing of its surface regolith and ejection of dust particles. However, no activity from 2005 UD has been observed as of yet, though it has been suspected that it could be the inactive parent body of the Daytime Sextantids meteor shower. 2005 UD and Phaethon share a bluish surface color at visible wavelengths, but differ at near-infrared wavelengths where 2005 UD appears redder than Phaethon.


(15692) 1984 RA
(15692) 1984 RA, provisional designation 1984 RA, is a Hungaria asteroid from the innermost regions of the asteroid belt, approximately 2 kilometers (1.2 miles) in diameter. It was discovered on 1 September 1984, by Italian astronomer Maria Barucci at the Palomar Observatory in California, United States. The presumed E-type asteroid has a longer-than average rotation period of 37.4 hours and possibly an elongated shape.


(15692) 1984 RA, Orbit and classification
1984 RA is a bright core member of the Hungaria family (003), a large family of three thousand asteroids located within the dynamical group with the same name. Hungarias form the innermost dense concentration of asteroids in the Solar System; they are inside the asteroid belt's core region, sometimes considered a completely independent population.


(15692) 1984 RA, Orbit and classification
The asteroid orbits the Sun in the innermost asteroid belt at a distance of 1.7–2.1 AU once every 2 years and 8 months (977 days; semi-major axis of 1.93 AU). Its orbit has an eccentricity of 0.10 and an inclination of 23° with respect to the ecliptic. The body's observation arc begins with a precovery found in the Digitized Sky Survey and taken at the Siding Spring Observatory in November 1977, almost 7 years prior to its official discovery observation at Palomar.


(15692) 1984 RA, Physical characteristics
1984 RA is an assumed E-type asteroid, known for their high albedos, typically around 0.4.


(15692) 1984 RA, Physical characteristics, Rotation period
In July 2013, a rotational lightcurve of this asteroid was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station (U82) in California. Lightcurve analysis gave a long rotation period of 37.44 hours with a brightness amplitude of 0.66 magnitude, indicative of an elongated shape (U=2). While not being a slow rotator, 1984 RA has a significantly longer period than most asteroids, which rotate once every 2 to 20 hours around their axis.


(15692) 1984 RA, 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 1.728 kilometers in diameter and its surface has an exceptionally high albedo of 0.78. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.30 – a compromise value between the E- (0.40) and S-type (0.20) members of the Hungaria family and group, respectively – and calculates a diameter of 2.43 kilometers based on an absolute magnitude of 15.0.


(15692) 1984 RA, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40991). As of 2018, it has not been named.


(15700) 1987 QD
(15700) 1987 QD, provisional designation 1987 QD, is a Mars-crossing asteroid and a binary candidate from inside the innermost region of the asteroid belt, approximately 3 kilometers (1.9 miles) in diameter. It was discovered on 24 August 1987, by American astronomer Stephen Singer-Brewster at the Palomar Observatory in California. The likely spherical X-type asteroid has a rotation period of 3.1 hours. The suspected presence of a kilometer-sized minor-planet moon was announced in November 2000.


(15700) 1987 QD, Orbit and classification
1987 QD is a Mars-crossing asteroid, a member of the dynamically unstable group, located between the main belt and near-Earth populations, and crossing the orbit of Mars at 1.666 AU. It orbits the Sun inside the innermost region of the asteroid belt at a distance 1.5–2.9 AU once every 3 years and 3 months (1,199 days; semi-major axis of 2.21 AU). Its orbit has an eccentricity of 0.31 and an inclination of 27° with respect to the ecliptic.


(15700) 1987 QD, Orbit and classification
The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken at Palomar in May 1954, more than 33 years prior to its official discovery observation. It will pass 6,352,000 km (0.04246 AU) from the main-belt asteroid 7 Iris on 3 September 2173.


(15700) 1987 QD, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40991). As of 2018, it has not been named.


(15700) 1987 QD, Physical characteristics
In the SDSS-based taxonomy and according to the survey conducted by Pan-STARRS, 1987 QD is an X-type asteroid. It has also been classified as a common, stony S-type asteroid.


(15700) 1987 QD, Physical characteristics, Rotation period
In September 2010, a first rotational lightcurve of 1987 QD was obtained from photometric observations by Brian Skiff. Lightcurve analysis gave a rotation period of 3.068 hours and a brightness variation of 0.07 magnitude (U=3-). Within less than two weeks, follow-up observations by a large international collaboration of astronomers determined a refined period of 3.0586±0.0001 hours with a low amplitude of 0.07 magnitude, indicating that the body has a spherical shape (U=3). An alternative observation that gave a tentative period 9.709 hours received a poor quality rating (U=1).


(15700) 1987 QD, Physical characteristics, Strong binary candidate
The photometric observations during September and October 2010 revealed that 1987 QD is a candidate for a synchronous binary asteroid with a minor-planet moon orbiting it every 50.3±0.5 hours at an estimated average distance of 14 km. The findings were announced on 6 November 2009. The lightcurve indicated mutual occultation events, however, a conclusive solution for the orbit period was not obtained. The Johnston's archive estimates a diameter of 1.23 kilometer for the satellite, or 31% the size of its primary.


(15700) 1987 QD, Physical characteristics, Strong binary candidate
The international collaboration included Richard Durkee at the Shed of Science Observatory (H39), Petr Pravec, Kamil Hornoch and Peter Kušnirák at Ondřejov Observatory, Donald Pray at Carbuncle Hill Observatory (912), David Higgins at Canberra (E14), Jozef Világi and Štefan Gajdoš at Modra Observatory, Judit Györgyey Ries at McDonald Observatory and Julian Oey at Leura Observatory (E17), as well as astronomers at the Kharkiv Kharkov (101), Simeiz and Skalnate Pleso observatories.


(15700) 1987 QD, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1987 QD measures 2.95 kilometers in diameter and its surface has an albedo of 0.268, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and derives a diameter of 3.04 kilometers based on an absolute magnitude of 14.99.


(15788) 1993 SB
(15788) 1993 SB is a trans-Neptunian object of the plutino class. Apart from Pluto, it was one of the first such objects discovered (beaten by two days by (385185) 1993 RO and by one day by 1993 RP), and the first to have an orbit calculated well enough to receive a number. The discovery was made in 1993 at the La Palma Observatory with the Isaac Newton Telescope. Very little is known about the object. Even the diameter estimate of ~130 km is based on an assumed albedo of 0.09.


(15788) 1993 SB
KBO's found in 1993 include: (15788) 1993 SB, (15789) 1993 SC, (181708) 1993 FW, and (385185) 1993 RO.


(15788) 1993 SB
Over one thousand bodies were found in a belt between orbiting between about 30-50 AU from the Sun in the twenty years (1992-2012), after finding 1992 QB1 (named in 2018, 15760 Albion), showing a vast belt of bodies more than just Pluto and Albion. By 2018, over 2000 Kuiper belts objects were discovered.


(15789) 1993 SC
(15789) 1993 SC is a trans-Neptunian object of the plutino class. The discovery was made in 1993 at the La Palma Observatory with the Isaac Newton Telescope. It was the second plutino to receive an MPC number.


(15789) 1993 SC
KBO's found in 1993 include: (15788) 1993 SB, (15789) 1993 SC, (181708) 1993 FW, and (385185) 1993 RO.


(15807) 1994 GV9
(15807) 1994 GV9, provisional designation 1994 GV9, is a trans-Neptunian object from the classical Kuiper belt located in the outermost region of the Solar System. The cubewano belongs to the orbitally unexcited cold population. It was discovered on 15 April 1994, by astronomers David Jewitt and Jun Chen at the Mauna Kea Observatories, near Hilo, Hawaii.


(15807) 1994 GV9, Description
As of 2018, it is 43.3 AU from the Sun. Currently, the closest approach possible to Neptune (MOID) is 11.2 AU (1.68 billion km). Very little is known about the object. Based on the brightness and distance, it is estimated to be between 100 and 150 km in diameter depending on the albedo.


(15807) 1994 GV9, Description
1994 GV9 is the second cubewano to be given an official Minor Planet Center catalog number. The first cubewano is 15760 Albion.


(15820) 1994 TB
(15820) 1994 TB is a trans-Neptunian object residing in the Kuiper belt. It is in a 3:2 orbital resonance with Neptune, similar to Pluto. It was discovered on October 2, 1994, by David C. Jewitt and Jun Chen at the Mauna Kea Observatory, in Hawaii.


(15874) 1996 TL66
(15874) 1996 TL66, provisional designation 1996 TL66, is a trans-Neptunian object of the scattered disc orbiting in the outermost region of the Solar System.


(15874) 1996 TL66
The Spitzer Space Telescope has estimated this object to be about 575 kilometres (357 mi) in diameter, but 2012 estimates from the Herschel Space Observatory estimate the diameter as closer to 339 kilometres (211 mi). It is not a detached object, since its perihelion (closest approach to the Sun) is under the influence of Neptune. Light-curve-amplitude analysis suggests that it is a spheroid. Tancredi presents "in the form of a decision tree, the set of questions to be considered in order to classify an object as an icy 'dwarf planet'." They find that (15874) 1996 TL66 is very probably a dwarf planet. Mike Brown's website, using a radiometrically determined diameter of 344 kilometres (214 mi), lists it as a possible dwarf planet.


(15874) 1996 TL66, Discovery
Discovered in 1996 by David C. Jewitt et al., it was the first object to be categorized as a scattered-disk object (SDO), although (48639) 1995 TL8, discovered a year earlier, was later recognised as a scattered-disk object. It was considered one the largest known trans-Neptunian objects at the time of the discovery, being placed second after Pluto. It came to perihelion in 2001.


(15874) 1996 TL66, Orbit and size
(15874) 1996 TL66 orbits the Sun with a semi-major axis of 83.9 AU but is currently only 35 AU from the Sun with an apparent magnitude of 21. In 2007, the Spitzer Space Telescope estimated it to have a low albedo with a diameter of about 575±115 km. More-recent measurements in 2012 by the 'TNOs are Cool' research project and reanalysis of older data have resulted in a new estimate of these figures. It is now assumed that it has a higher albedo and the diameter was revised downward to 339±20 km. Light-curve-amplitude analysis shows only small deviations, suggesting (15874) 1996 TL66 is a spheroid with small albedo spots and may be a dwarf planet.


(15875) 1996 TP66
(15875) 1996 TP66, provisional designation 1996 TP66, is a resonant trans-Neptunian object of the plutino population, located in the outermost region of the Solar System, approximately 154 kilometers (96 miles) in diameter. It was discovered on 11 October 1996, by astronomers Jane Luu, David C. Jewitt and Chad Trujillo at the Mauna Kea Observatories, Hawaii, in the United States. The very reddish RR-type with a highly eccentric orbit has been near its perihelion around the time of its discovery. This minor planet was numbered in 2000 and has since not been named. It is probably not a dwarf planet candidate.


(15875) 1996 TP66, Orbit and classification
1996 TP66 belongs to the dynamical population of plutinos, named after its largest member, Pluto. Plutinos are resonant trans-Neptunian objects in a 2:3 orbital resonance with Neptune, which means that they orbit the Sun exactly twice while Neptune orbits the Sun three times.


(15875) 1996 TP66, Orbit and classification
It orbits the Sun at a distance of 26.3–52.0 AU once every 244 years and 10 months (89,435 days; semi-major axis of 39.14 AU). Its orbit has a notably high eccentricity of 0.33 and an inclination of 6° with respect to the ecliptic. Among the plutinos, 1996 TP66 has one of the most elliptical orbits, with a perihelion almost halfway between Uranus (19.2 AU) and Neptune (30.1 AU). The body's observation arc begins with its official discovery observation at Mauna Kea in October 1996. Calculations by the Minor Planet Center in 1997 showed that the eccentric orbit of 1996 TP66 comes within 6.9 AU of Uranus and stays more than 22.6 AU from Neptune over a 14,000-year period centered on the present.


(15875) 1996 TP66, Orbit and classification, Inside Neptune's orbit
In 2000, this object came closest to the Sun (perihelion) at 26.3 AU, and has since moved away to a distance of 29.2 AU by the end of 2018. This means that this small plutino is still well inside the orbit of Neptune which has a semi-major axis of 30.1 AU.


(15875) 1996 TP66, Orbit and classification, Inside Neptune's orbit
Like Pluto, this plutino spends part of its orbit closer to the Sun than Neptune. Like all resonant trans-Neptunian objects its orbit is dominated by Neptune. Simulations by the Deep Ecliptic Survey (DES) show that over the next 10 million years 1996 TP66 can acquire a perihelion distance (qmin) as small as 25.9 AU. Objects like Huya and the plutino 2004 EW95 are also currently inside the orbit of Neptune.


(15875) 1996 TP66, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 26 July 2000 and received the number 15875 in the minor planet catalog (M.P.C. 40993). As of 2018, it has not been named.


(15875) 1996 TP66, Physical properties
1996 TP66 has a RR taxonomic class, with "very red" surface in the visible (rather than a "neutral" or "grey-blue" one for objects of the BB class) and a flat featureless infrared spectrum. In 2015, Irina Belskaya published the following color indices: B–V (1.050), V–R (0.660) and V–I (1.310). The resulting B–R magnitude is 1.71.


(15875) 1996 TP66, Physical properties
These indices agree with the results obtained by the Herschel Space Observatory (Mommert): B–V (1.030), V–R (0.660) and V–I (1.320), and also agree with previous measurements by Olivier Hainaut: B–V (1.031), V–R (0.655) and V–I (1.324), as well as B–V (0.984), V–R (0.654) and V–I (11.337) from in 2012 and 2002, respectively. The numerous results are summarized at the Small Body Data Ferret.


(15875) 1996 TP66, Physical properties, Diameter and albedo
According to the survey carried out by the Herschel Space Telescope using its PACS instrument, 1996 TP66 measures 154.0+28.8−33.7 kilometers in diameter and its surface has an albedo of 0.074+0.063−0.031. The results supersedes a previous study that gave a much larger diameter of 350 kilometers with a lower albedo of 0.03. According to Michael Brown, it is "probably not" a dwarf planet candidate, due to its relatively small diameter estimated at 158 kilometers. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.10 and derives a diameter of 139.81 kilometers based on an absolute magnitude of 7.39.


(15875) 1996 TP66, Physical properties, Rotation period
1996 TP66 was part of a rotational lightcurve study which was published in the journal Nature in 1999. The photometric observations gave a brightness variation of no more than 0.12 magnitude, which is indicative of a rather spherical shape. As of 2018, the body's rotation period and pole remain unknown.


(15977) 1998 MA11
(15977) 1998 MA11, provisional designation 1998 MA11, is a Jupiter trojan from the Trojan camp, approximately 45 kilometers (28 miles) in diameter. It was discovered on 19 June 1998, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The suspected tumbler is also a slow rotator with a period of 250 hours. It has not been named since its numbering in July 2000.


(15977) 1998 MA11, Orbit and classification
1998 MA11 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).


(15977) 1998 MA11, Orbit and classification
It orbits the Sun at a distance of 4.9–5.4 AU once every 11 years and 10 months (4,309 days; semi-major axis of 5.18 AU). Its orbit has an eccentricity of 0.05 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken at Palomar Observatory in December 1953, more than 44 years prior to its official discovery observation at Socorro.


(15977) 1998 MA11, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40994). As of 2018, it has not been named.


(15977) 1998 MA11, Physical characteristics
1998 MA11 is an assumed C-type asteroid. It has a typical V–I color index of 0.906 (see table below).


(15977) 1998 MA11, Physical characteristics, Rotation period
In August 2013, Robert Stephens at the Center for Solar System Studies observed 1998 MA11 over three nights. However no meaningful rotational lightcurve could be determined, as the lightcurve's amplitude never varied more than 0.02 magnitude. A period of 11.17 hours was only derived for demonstration purpose (U=2-). In December 2015, Stephens obtained an improved lightcurve with a rotation period of 250±5 hours and a brightness variation of 0.30 magnitude (U=2-). This time the asteroid was observed on 16 nights over a period of one month. The photometric observations also revealed that this object possibly has a non-principal axis rotation, which is commonly known as tumbling.


(15977) 1998 MA11, 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 Japanese Akari satellite, 1998 MA11 measures 43.53 and 51.53 kilometers in diameter and its surface has an albedo of 0.071 and 0.046, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 46.30 kilometers based on an absolute magnitude of 10.4.


(15977) 1998 MA11, 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.


(159857) 2004 LJ1
(159857) 2004 LJ1, provisional designation 2004 LJ1, is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 3 kilometers in diameter. The asteroid was discovered on 10 June 2004, 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 known to exist.


(159857) 2004 LJ1, Orbit and classification
2004 LJ1 is a member of the dynamical Apollo group, which are Earth-crossing asteroids. Apollo asteroids are the largest subgroup of near-Earth objects.


(159857) 2004 LJ1, Orbit and classification
The body orbits the Sun at a distance of 0.9–3.6 AU once every 3 years and 5 months (1,244 days; semi-major axis of 2.26 AU). Its orbit has an eccentricity of 0.59 and an inclination of 23° with respect to the ecliptic. Its observation arc begins with a precovery from the Digitized Sky Survey taken at the Siding Spring Observatory, Australia, in February 1995, more than 9 years prior to its official discovery observation at Socorro.


(159857) 2004 LJ1, Orbit and classification, Close approaches
With an absolute magnitude of at least 15.4, 2004 LJ1 is one of the brightest and presumably largest known potentially hazardous asteroid (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0168 AU (2,510,000 km), which translates into 6.5 lunar distances (LD). On 16 November 2038, this asteroid will make its closest near-Earth encounter at a nominal distance of 0.0198 AU (7.7 LD). It is also classified as a Mars-crosser, crossing the orbit of the Red Planet at 1.66 AU.


(159857) 2004 LJ1, Physical characteristics, Rotation period
Three rotational lightcurves of 2004 LJ1 have been obtained from photometric observations by Johanna Torppa, Adrián Galád and Brian Warner since 2004. Lightcurve analysis gave a consolidated rotation period of 2.7247 hours with a brightness amplitude between 0.15 and 0.59 magnitude (U=3).


(159857) 2004 LJ1, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2004 LJ1 measures 3.07 kilometers in diameter and its surface has an albedo of 0.13. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 2.47 kilometers, based on an absolute magnitude of 15.4.


(159857) 2004 LJ1, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 30 June 2007. As of 2018, it has not been named.


(162058) 1997 AE12
(162058) 1997 AE12 is a stony, sub-kilometer asteroid and likely the slowest rotator known to exist. It is classified as near-Earth object of the Amor group and measures approximately 800 meters in diameter. The asteroid was discovered on 10 January 1997 by the Spacewatch survey at Kitt Peak National Observatory near Tucson, Arizona


(162058) 1997 AE12, Orbit and classification
1997 AE12 is an Amor asteroid, a group of near-Earth object that approach the orbit of Earth from beyond, but do not cross it. It orbits the Sun at a distance of 1.1–3.7 AU once every 3 years and 8 months (1,330 days). Its orbit has an eccentricity of 0.55 and an inclination of 5° with respect to the ecliptic.


(162058) 1997 AE12, Orbit and classification
Published by the Digitized Sky Survey, a first precovery was taken at the Australian Siding Spring Observatory in July 1992, extending the body's observation arc by more than 4 years prior to its official discovery observation at Kitt Peak.


(162058) 1997 AE12, Orbit and classification, Close approaches
1997 AE12 occasionally makes close approaches to Earth and Mars. It has an Earth minimum orbital intersection distance of 0.0881 AU (13,200,000 km), which is about 34.3 lunar distances.


(162058) 1997 AE12, Orbit and classification, Close approaches
Its closest recorded approach to Earth took place on 30 August 2003, when the asteroid came within 0.1238 AU (18,500,000 km) from Earth. It will come closer still on 8 October 2145, when it will be within 0.1042 AU (15,590,000 km) from Earth. The asteroid will make its closest approach to Mars on 29 December 2054 when it will come within 0.0376 AU (5,620,000 km) from the planet.


(162058) 1997 AE12, Physical properties, Spectral type
1997 AE12 is a rare Q-type asteroid with a very dark surface, reflecting only about 7% of the light it receives. It has also been described a common stony S-type asteroid.


(162058) 1997 AE12, Physical properties, Slow rotator
The most unusual feature of 1997 AE12, however, is its exceptionally slow rotation period of 1880±595 hours, or approximately 11 weeks (U=2). It holds the record for being the slowest-rotating asteroid discovered so far. Its precise period with a smaller error margin still needs to be determined. The lightcurve also showed a high brightness variation of at least 0.6 magnitude, which is indicative for a non-spherical shape. The asteroid may also be in a tumbling motion, but observations are not sufficient to determine any non-principal axis rotation.


(162058) 1997 AE12, Physical properties, Slow rotator
Like other slowly-rotating asteroids such as 912 Maritima, it is possible that the extremely long period of this asteroid is caused by YORP radiation pressure slowing down the asteroid's rotation. This is especially likely considering that 1997 AE12 has a very low albedo, which would allow it to absorb more radiant energy from the Sun. Furthermore, the YORP effect has also been observed on other Q-type asteroids such as 1862 Apollo.


(162058) 1997 AE12, Physical properties, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1997 AE12 measures 0.847 kilometers in diameter and its surface has an albedo of 0.186. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 0.782 kilometers based on an absolute magnitude of 17.9.


(162421) 2000 ET70
(162421) 2000 ET70 is a dark, elongated and oblate asteroid, classified as near-Earth object and potentially hazardous asteroid of the Aten group, approximately 2.2 kilometers in diameter. It was discovered on 8 March 2000, by astronomers of the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico. The body has a notably low albedo, and its shape resembles that of a "clenched fist".


(162421) 2000 ET70, Orbit and classification
2000 ET70 orbits the Sun at a distance of 0.8–1.1 AU once every 11 months (336 days; semi-major axis of 0.95 AU). Its orbit has an eccentricity of 0.12 and an inclination of 22° with respect to the ecliptic. A first precovery was found in the Digitized Sky Survey from images taken at ESO's La Silla Observatory in February 1977. The body's observation arc begins with its official discovery observation at Socorro in March 2000.


(162421) 2000 ET70, Orbit and classification, Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.0316 AU (4,730,000 km) which translates into 12.3 lunar distances. In February 2012, it was observed by radar during a close approach (0.045 AU) at the Arecibo and Goldstone observatories. The observations allowed to model the body's spin period and rotation, as well as its shape (see below).


(162421) 2000 ET70, Physical characteristics
2000 ET70 has been characterized as a Xk-subtype, which transitions between the X- and K-type asteroids.


(162421) 2000 ET70, Physical characteristics, Rotation period, pole, and shape
During its close approach in February 2012, a rotational lightcurve of 2000 ET70 was obtained from photometric observations by a collaboration of astronomers from Uruguay, Australia, and the United States. Analysis of the lightcurve gave a period of 8.947 hours with a brightness amplitude of 0.60 magnitude (U=3-).


(162421) 2000 ET70, Physical characteristics, Rotation period, pole, and shape
Radar observations at Arecibo and Goldstone showed that the asteroid spins in a retrograde manner with a rotation period of 8.96 hours. It is likely a principal axis rotator, i.e., not tumbling. Shape modelling by two independent teams gave sidereal periods of 8.96 and 8.944 hours, respectively. A spin axis of (80.0°, −50.0°) in ecliptic coordinates was determined. The observations also revealed that the asteroid has an elongated oblate shape, resembling a "clenched fist". Its surface exhibits multiple kilometer scale ridges and concavities.


(162421) 2000 ET70, Physical characteristics, Diameter and albedo
According to shape modeling of radar observations, the asteroid's overall dimensions are 2.6×2.2×2.1 kilometers. Based on an absolute magnitude of 18.2, this results in a notably low albedo of 0.018. More recent modeling combining radar, photometric, and infrared data gave and even more elongated shape of 2.9×2.2×1.5 kilometers. These authors argue that the absolute magnitude value is incorrect and report a geometric albedo of 0.09.


(162421) 2000 ET70, Physical characteristics, Diameter and albedo
2000 ET70's mean-diameter measures between 2.0 and 2.26 kilometers and its surface has an albedo between 0.018 and 0.09. The Collaborative Asteroid Lightcurve Link adopts an albedo of 0.018 and a diameter of 2.26 kilometers based on an absolute magnitude of 18.2.


(162421) 2000 ET70, Numbering and naming
This minor planet was numbered on 26 September 2007, after its orbital parameters had been sufficiently determined (M.P.C. 60670). As of 2018, it has not been named.


(163132) 2002 CU11
(163132) 2002 CU11, provisional designation 2002 CU11, is a bright, sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. Based on absolute magnitude, it is the second largest asteroid known to have passed closer than the Moon.


(163132) 2002 CU11, Description
2002 CU11 was discovered on 7 February 2002 by Lincoln Near-Earth Asteroid Research (LINEAR) at an apparent magnitude of 19 using a 1.0-meter (39 in) reflecting telescope. It has an estimated diameter of 730 meters (2,400 ft). The asteroid was listed on Sentry Risk Table with a Torino Scale rating of 1 on 20 March 2002.


(163132) 2002 CU11, Description
With an observation arc of 44 days, (163132) 2002 CU11 showed a 1 in 9,300 chance of impacting Earth in 2049. It was removed from the Sentry Risk Table on 26 April 2002. It is now known that on 3 September 2049 the asteroid will be 0.0843 AU (12,610,000 km; 7,840,000 mi) from Earth.


(163132) 2002 CU11, Description
Even though using an epoch of 27 June 2015 gives 2002 CU11 an Earth-MOID of 0.0000093 AU (1,390 km; 860 mi), the asteroid does not make any threatening approaches to Earth in the foreseeable future.


(163132) 2002 CU11, Description
The close approach of 2080 will cause an uncertainty of 4 minutes for the close approach time of 2084.


(163243) 2002 FB3
(163243) 2002 FB3, provisional designation 2002 FB3, is a stony asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Athen group, approximately 1.6 kilometers (1 mile) in diameter. It was discovered on 18 March 2002, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The Q-type asteroid has a rotation period of 6.2 hours.


(163243) 2002 FB3, Orbit and classification
2002 FB3 is a member of the Athen group of asteroids. It orbits the Sun at a distance of 0.3–1.2 AU once every 8 months (243 days; semi-major axis of 0.76 AU). Its orbit has an eccentricity of 0.60 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Socorro.


(163243) 2002 FB3, Orbit and classification, Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.0034 AU (509,000 km; 316,000 mi), which corresponds to 1.3 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size.


(163243) 2002 FB3, Physical characteristics
2003 QO104 has been characterized as an uncommon Q-type asteroid, that fall into the larger stony S-complex.


(163243) 2002 FB3, Physical characteristics, Rotation period
In March 2016, a rotational lightcurve of this asteroid was obtained from photometric observations. Lightcurve analysis gave a rotation period of 6.231 hours with a brightness amplitude of 0.19 magnitude (U=2).


(163243) 2002 FB3, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer,  measures between 1.552 and 1.682 kilometers in diameter and its surface has an albedo between 0.1426 and 0.202.


(163243) 2002 FB3, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link assumes a stony standard albedo of 0.20 and calculates a diameter of 1.49 kilometers based on an absolute magnitude of 16.5.


(163243) 2002 FB3, Naming
This minor planet was numbered by the MPC on 26 September 2007 (M.P.C. 60678). As of 2018, it has not been named.


(163249) 2002 GT
(163249) 2002 GT is an Apollo asteroid with an absolute magnitude of 18.26. It is a potentially hazardous asteroid as its orbit crosses that of Earth.


(163249) 2002 GT, Description
In 2011, NASA considered sending the unmanned spacecraft Deep Impact toward the asteroid with the aim of performing a flyby in 2020. It was uncertain whether Deep Impact carried sufficient fuel for this operation.


(163249) 2002 GT, Description
On 24 November 2011 and 4 October 2012, the space probe's thrusters were fired briefly for two trajectory correction maneuvers that targeted Deep Impact for an encounter with 2002 GT in 2020, possibly within a distance of no more than 400 kilometers. However, funding for the flyby mission was not guaranteed. In June 2013 the asteroid was observed in radar by the Arecibo Observatory.


(163249) 2002 GT, Description
However, on 8 August 2013 NASA lost communication with the spacecraft, and on 20 September 2013, NASA abandoned further attempts to contact the craft. According to A'Hearn, the most probable reason of software malfunction was a Y2K-like problem (at 11 August 2013 0:38:49 it was 232 deciseconds from 1 January 2000).


(163348) 2002 NN4
(163348) 2002 NN4 (prov. designation: 2002 NN4) is a dark, sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group that flew by Earth on 6 June 2020. The highly elongated X-type asteroid has a rotation period of 14.5 hours and measures approximately 0.7 kilometers (0.4 miles) in diameter. It was discovered by LINEAR at the Lincoln Laboratory's Experimental Test Site in New Mexico on 9 July 2002.


(163348) 2002 NN4, Orbit
2002 NN4 flew by Earth on 6 June 2020, passing 0.034 AU (5.1 million km; 13 LD) from Earth. The asteroid had been recovered two days earlier on 4 June 2020. By 11 June 2020, the asteroid had brightened to apparent magnitude 14.4, which is roughly the brightness of Pluto.


(163348) 2002 NN4, Orbit
Being a member of the Aten asteroids, 2002 NN4 orbits the Sun at a distance of 0.50–1.26 AU once every 10 months (300 days; semi-major axis of 0.88 AU). Its orbit has an eccentricity of 0.43 and an inclination of 5° with respect to the ecliptic. It was first observed by the Near-Earth Asteroid Tracking on Palomar Observatory on 2 July 2002, or seven nights prior to its official discovery observation by LINEAR. This asteroid has an Earth minimum orbit intersection distance of 0.0069 AU (1,030,000 km), which corresponds to 2.7 lunar distances (LD).


(163348) 2002 NN4, Physical characteristics
A spectroscopic survey of the small near-Earth asteroid population conducted by European astronomers determined that 2002 NN4 is an X-type asteroid. Because of the objects low albedo (see below), it would be considered a primitive P-type asteroid in the Tholen classification.


(163348) 2002 NN4, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2002 NN4 measures (735±243) meters in diameter, and its surface has a dark albedo of (0.030±0.027). (The NEOWISE publication uses the designation G3348 for this asteroid.) In 2016, astronomers using the European New Technology Telescope at La Silla Observatory found a diameter of 613 meters with an albedo of 0.047.


(163348) 2002 NN4, Physical characteristics, Rotation period
In August 2016, the first rotational lightcurve of 2002 NN4 was obtained from photometric observations over five nights by Brian Warner at the Center for Solar System Studies (U82) in California. Lightcurve analysis gave a rotation period of 14.50±0.03 hours with a high brightness variation of 0.74±0.05 magnitude, indicative of a highly elongated shape (U=3−).


(163364) 2002 OD20
(163364) 2002 OD20 is an asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, likely smaller than one kilometer in diameter.


(163364) 2002 OD20
It was scheduled to be observed by Goldstone radar in May 2013. It has a well determined orbit and made a close approach to Earth on 23 May 2013, at a distance of 0.0387 AU (5,790,000 km; 3,600,000 mi). It is due to make another close pass on 23 May 2131, coming as close as 0.0248 AU. It was discovered on 21 July 2002 by astronomers of the Near-Earth Asteroid Tracking survey at Palomar Observatory in California. With an absolute magnitude of 18.8, the diameter is estimated to between 460 and 1030 meters.


(163899) 2003 SD220
(163899) 2003 SD220 is a sub-kilometer asteroid and tumbling slow rotator, classified as near-Earth object and potentially hazardous asteroid of the Aten group, which orbit the Sun between Venus and Earth. Its orbital period of 0.75 years means that it orbits the sun about 4 times for every 3 of the Earth. It was discovered on 29 September 2003, by astronomers of the Lowell Observatory Near-Earth-Object Search at Anderson Mesa Station near Flagstaff, Arizona.


(163899) 2003 SD220, Earth flybys 2015–2027
It passed about 28 lunar distances (LD) from the Earth on 25 December 2015. It came within about 7 LD (0.0189 AU) on 22 December 2018. Its peak brightness was about 13.13 magnitude on 16 December 2018.


(163899) 2003 SD220, Earth flybys 2015–2027
Observations are planned for favorable flybys in 2021, 2024, and 2027. It will pass with 14 LD (0.0363 AU) on 17 December 2021, and 34 LD (0.0884 AU) on 2 December 2024, and 54 LD (0.1382 AU) on 12 November 2027.


(163899) 2003 SD220, Earth flybys 2015–2027
Patrick Taylor of Arecibo Observatory suggested it could be a target for a future robotic mission.


(163899) 2003 SD220, Earth flybys 2015–2027, Closest flyby 2018
2003 SD220 passed its closest distance of 7.34 LD (0.01899 AU) on 22 December 2018. It was on the list of Goldstone targets for December 2018  to gain more information for the Near-Earth Object Human Space Flight Accessible Targets Study (NHATS).


(163899) 2003 SD220, Earth flybys 2015–2027, Closest flyby 2018
Its peak brightness was about 13.1 magnitude on 16 December 2018, moving south from Ursa major and Boötes into Ophiuchus at closest approach and into Sagittarius.


(163899) 2003 SD220, Earth flybys 2015–2027, 2015
It was observed in December 2015 at a distance of 28.3 lunar distances (0.07296 AU) on December 24, and its brightest was 15.22 magnitude on December 16. It showed an elongated shape, up to 2 km wide, described as being shaped like a sweet potato.


(163899) 2003 SD220, Earth flybys 2015–2027, 2021
2003 SD220 will pass at a distance of 14.1  lunar distances (0.03628 AU) on December 17, 2021.


(164121) 2003 YT1
(164121) 2003 YT1, provisional designation 2003 YT1, is a bright asteroid and synchronous binary system on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 2 kilometers (1.2 miles) in diameter. It was discovered on 18 December 2003, by astronomers with the Catalina Sky Survey at the Catalina Station near Tucson, Arizona, in the United States. The V-type asteroid has a short rotation period of 2.3 hours. Its 210-meter sized minor-planet moon was discovered at Arecibo Observatory in May 2004.


(164121) 2003 YT1, Orbit and classification
2003 YT1 is a member of the Earth-crossing group of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members.


(164121) 2003 YT1, Orbit and classification
It orbits the Sun at a distance of 0.8–1.4 AU once every 1 years and 2 months (427 days; semi-major axis of 1.11 AU). Its orbit has an eccentricity of 0.29 and an inclination of 44° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Siding Spring Observatory in November 1989, more than 14 years prior to its official discovery observation at Catalina.


(164121) 2003 YT1, Orbit and classification, Close approaches and Torino rating
The asteroid has an Earth minimum orbital intersection distance of 0.0027 AU (404,000 km; 251,000 mi), which corresponds to 1.05 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size. On the Torino Scale, this object was rated level 1 on 27 December 2003 with an observation arc of 8.7 days. It was removed from the risk table on 29 December 2003. Over the next ten million years the asteroid has a 6% chance of impacting Earth.


(164121) 2003 YT1, Orbit and classification, Close approaches and Torino rating
On 30 April 2004 it made a close approach at a nominal distance of 0.073 AU (28 LD), and on 31 October 2016, it passed Earth at 0.034 AU (13 LD). The asteroid's closest encounter with Earth will be on 29 April 2073, when it is projected to pass at 0.0113 AU (4.4 LD) only (see table).


(164121) 2003 YT1, Orbit and classification, Close approaches and Torino rating
2003 YT1 has unique orbital characteristics among minor planets. It is the only known binary asteroid to have an Earth MOID within the Moon's Apogee.


(164121) 2003 YT1, Meteor stream
On 28 April 2017, a 2.7 cm (1 in) fragment of 2013 YT1 is suspected of having impacted Earth creating a fireball over Kyoto, Japan. The fragment would have broken off the parent body within the last ten thousand years.


(164121) 2003 YT1, Physical characteristics
This object has been characterized as a bright Vestian-like V-type asteroid.


(164121) 2003 YT1, Physical characteristics, Rotation period
Several rotational lightcurve of this asteroid have been obtained from photometric observations (U=2/n.a./3/3). Analysis of the best-rated lightcurve gave a short rotation period of 2.343 hours with a brightness amplitude between 0.16 and 0.27 magnitude.


(164121) 2003 YT1, Physical characteristics, Diameter and albedo
According to radar observations with the Arecibo Observatory and the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, this asteroid measures between 1.0 and 1.717 kilometers in diameter and its surface has an albedo between 0.198 and 0.4861.


(164121) 2003 YT1, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link derives an albedo of 0.5848 and adopts a diameter of 1.0 kilometer based on an absolute magnitude of 16.2.


(164121) 2003 YT1, Physical characteristics, Satellite
The Arecibo radar observations in May 2004 revealed that 2003 YT1 is a synchronous binary asteroid. Follow-up observations confirmed a 210-meter sized minor-planet moon orbiting its primary every 30 hours at a distance of 2.7 km.


(164121) 2003 YT1, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 26 September 2007 (M.P.C. 60686). As of 2018, it has not been named.


(164207) 2004 GU9
(164207) 2004 GU9 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It will be a quasi-satellite of Earth until around 2600.


(164207) 2004 GU9
On 14 April 2004 (with less than a 1-day observation arc), the Sentry Risk Table showed 180 virtual impactors. It was removed from the Sentry Risk Table 2 days later on 16 April 2004. (164207) 2004 GU9 now has a well determined orbit with an observation arc of 12 years.


(16882) 1998 BO13
(16882) 1998 BO13, provisional designation 1998 BO13, is a dark Zhongguo asteroid from the background population in the outermost region of the asteroid belt, approximately 10 kilometers (6 miles) in diameter. It was discovered on 24 January 1998, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States.


(16882) 1998 BO13, Orbit and classification
1998 BO13 is a non-family asteroid from the main belt's background population, and a member of the small group of Zhongguo asteroids, located in the Hecuba gap and locked in a 2:1 mean-motion resonance with the gas giant Jupiter. Contrary to the nearby Griqua group, the orbits of the Zhongguos are stable over half a billion years. According to Milani and Knežević, this asteroid is a core member of the unnamed asteroid family formed by the Zhongguo asteroid (11097) 1994 UD1.


(16882) 1998 BO13, Orbit and classification
It orbits the Sun in the outer main-belt at a distance of 2.7–3.9 AU once every 6.02 years (2,199 days; semi-major axis of 3.31 AU). Its orbit has an eccentricity of 0.19 and an inclination of 1° with respect to the ecliptic.


(16882) 1998 BO13, Orbit and classification
The body's observation arc begins with a precovery taken by Spacewatch in November 1996, or 14 months prior to its official discovery observation at Socorro.


(16882) 1998 BO13, Physical characteristics
1998 BO13 has an absolute magnitude of 13.5. As of 2018, no rotational lightcurve for this asteroid has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.


(16882) 1998 BO13, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer,  measures 9.827 kilometers in diameter and its surface has an albedo of 0.061, which is rather typical for the abundant carbonaceous C-type asteroids in the outer main-belt.


(16882) 1998 BO13, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 13 September 2000, after its orbit had sufficiently been secured (M.P.C. 41165). As of 2018, it has not been named.


(16960) 1998 QS52
(16960) 1998 QS52 (prov. designation: 1998 QS52) is a stony asteroid on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 4.1 kilometers (2.5 mi) in diameter. It was discovered on 25 August 1998, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. This asteroid is one of the largest potentially hazardous asteroid known to exist.


(16960) 1998 QS52, Orbit and classification
1998 QS52 is a member of the dynamical Apollo group, which are Earth-crossing asteroids. Apollo asteroids are the largest subgroup of near-Earth objects. It orbits the Sun at a distance of 0.31–4.1 AU once every 3 years and 3 months (1,194 days; semi-major axis of 2.20 AU). Its orbit has an exceptionally high eccentricity of 0.86 and an inclination of 18° with respect to the ecliptic.


(16960) 1998 QS52, Orbit and classification
The body's observation arc begins with a precovery taken at the Siding Spring Observatory in June 1983, more than 15 years prior to its official discovery observation at Socorro.


(16960) 1998 QS52, Orbit and classification, Close approaches
With an absolute magnitude of 14.3, 1998 QS52 is one of the brightest and largest known potentially hazardous asteroid (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0144 AU (2,150,000 km), which corresponds to 5.6 lunar distances. Its eccentric orbit leads to close approaches with Mercury and Venus and carries it beyond the asteroid belt but not as far as to the orbit of Jupiter (>4.9 AU). It is therefore also a Venus- and Mars-crossing asteroid.


(16960) 1998 QS52, Physical characteristics
In the SMASS classification, 1998 QS52 is a Sq-subtype, that transitions between the stony S- and Q-type asteroids. Observers at the NASA Infrared Telescope Facility have also characterized this body as an Sr-type, which transitions to the rare R-type asteroids.


(16960) 1998 QS52, Physical characteristics, Rotation period
In 2008, two rotational lightcurves of 1998 QS52 were obtained independently from photometric observations by Brian Warner at the Palmer Divide Observatory and by Brian Skiff during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS) . Lightcurve analysis gave a rotation period of 5.789 and 5.8 hours with a brightness amplitude of 0.24 and 1.4 magnitude, respectively (U=2/2). An alternative period solution of 2.9 hours – or half of the above period – is also possible, though considered less likely by Warner.


(16960) 1998 QS52, Physical characteristics, Diameter and albedo
1998 QS52 has not been observed by any of the space-based surveys such as IRAS, Akari or the Wide-field Infrared Survey Explorer. The Collaborative Asteroid Lightcurve Link assumes a stony standard albedo of 0.20 for its surface, and calculates a diameter of 4.10 kilometers based on an absolute magnitude of 14.3.


(16960) 1998 QS52, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 13 September 2000. As of 2018, it has not been named.


(172034) 2001 WR1
(172034) 2001 WR1, provisional designation: 2001 WR1, is a sub-kilometer near-Earth object of the Amor group, approximately 650 meters (2,100 feet) in diameter. The S-type asteroid has been identified as a potential flyby target of the Hayabusa2 mission. It was discovered on 17 November 2001, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The asteroid has a rotation period of 8.0 hours and possibly an elongated shape. It remains unnamed since its numbering in December 2007.


(172034) 2001 WR1, Orbit and classification
2001 WR1 is an Amor asteroid – a subgroup of near-Earth asteroids that approach the orbit of Earth from beyond, but do not cross it. The object orbits the Sun at a distance of 1.02–1.54 AU once every 17 months (527 days; semi-major axis of 1.28 AU). Its orbit has an eccentricity of 0.20 and an inclination of 25° with respect to the ecliptic. The body's observation arc begins with its first observation in February 1953, more than 48 years prior to its official discovery observation at Socorro. The precovery was taken at Palomar Observatory and published by the Digitized Sky Survey.


(172034) 2001 WR1, Orbit and classification, Close encounters
2001 WR1 has an Earth minimum orbital intersection distance of 0.0747 AU (11,200,000 km) which corresponds to 29.1 lunar distances. In September 1926, it approached Earth to 0.1496 AU (22,400,000 km), its closest approach of all close encounters since 1900. Only in September 2199, it will approach Earth at a similar distance of 0.1514 AU (22,600,000 km).


(172034) 2001 WR1, Hayabusa2 mission
2001 WR1 is currently the prime target of the Hayabusa2 mission for a flyby planned to occur on 27 June 2023. When the spacecraft returns to Earth and delivers the sample capsule in December 2020, it is expected to retain 30 kg of xenon propellant, which can be used to extend its service and flyby new targets to explore.


(172034) 2001 WR1, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 24 December 2007 (M.P.C. 61443). As of 2021, it has not been named.


(172034) 2001 WR1, Physical characteristics
2001 WR1 has been characterized as a common, stony S-type asteroid.


(172034) 2001 WR1, Physical characteristics, Rotation period
In March 2018, a rotational lightcurve of 2001 WR1 was obtained from photometric observations by Brian Warner at the Palmer Divide Station (U82) in California. Lightcurve analysis gave a rotation period of 8.0475±0.0003 hours with a brightness amplitude of 0.95 magnitude (U=3), indicative of a non-spherical shape.


(172034) 2001 WR1, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2001 WR1 has an albedo of 0.34 and measures 0.63 and 0.66 kilometers in diameter, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and calculates a diameter of 0.818 kilometers based on an absolute magnitude of 17.8.


(17511) 1992 QN
(17511) 1992 QN is a small, bright Apollo asteroid discovered on August 29 1992 by American astronomers Eleanor Helin and Jeff Alu at the Palomar Observatory, California, United States. It is a near-Earth asteroid whose orbit crosses that of Mars and Earth (a Mars and Earth-crossing asteroid). On January 18 1996, it passed Earth at a distance of 0.158848 AU (23.763 million km), and on July 12 2027, it will pass our planet again at a distance of 0.161858 AU (24.214 million km). (17511) 1992 QN's orbit is similar to that of Apollo asteroid 2010 JG.


(175113) 2004 PF115
(175113) 2004 PF115 (also written 2004 PF115) is a trans-Neptunian object (TNO). It was discovered in 2006 by M. Brown, C. Trujillo, D. Rabinowitz. The object is classified as a possible plutino.


(175113) 2004 PF115, Physical properties
The size of (175113) 2004 PF115 was measured by the Herschel Space Telescope to be 406.3+97.6−75.3 km.


(175706) 1996 FG3
(175706) 1996 FG3 is a carbonaceous asteroid and binary system, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.7 kilometers (1.1 miles) in diameter. The primary has a spheroidal shape. Its minor-planet moon measures approximately 490 meters (1,600 feet) in diameter.


(175706) 1996 FG3
It was discovered on 24 March 1996, by Australian astronomer Robert McNaught at Siding Spring Observatory in New South Wales, Australia. 1996 FG3 was also a target of a rejected mission-proposal for the Marco Polo spacecraft. The asteroid is a target of NASA's Janus space probe. In 2017, scientists from the Chinese Academy of Sciences' Purple Mountain Observatory revealed a plan to land a probe on this asteroid in 2029, as part of an asteroid exploration mission.


(175706) 1996 FG3, Orbit and classification
1996 FG3 orbits the Sun at a distance of 0.7–1.4 AU once every 1 years and 1 month (395 days; semi-major axis of 1.05 AU). Its orbit has an eccentricity of 0.35 and an inclination of 2° with respect to the ecliptic. It has an Earth minimum orbital intersection distance of 0.0283 AU (4,230,000 km), which corresponds to 11.0 lunar distances. In 2019 a precovery observation from Palomar Mountain was found, extending the body's observation arc into 1985.


(175706) 1996 FG3, Target of rejected Marco Polo mission
Due to its binary nature and its low delta-v heliocentric orbit (also see Hohmann transfer orbit), this asteroid was selected for MarcoPolo-R, which was the Marco Polo spacecraft's first proposed mission. MarcoPolo-R was originally selected for the assessment study phase in the M3 slot of ESA's Cosmic Vision program, but rejected in favor of PLATO by the end of 2012.


(175706) 1996 FG3, Target of planned Chinese mission
China plans to land a probe on 1996 FG3 after 2020 as part of its asteroid exploration mission. The mission includes plans for fly-by of three asteroids (one of them is 99942 Apophis), and land on 1996 FG3 to conduct in situ sampling analysis on the surface, according to Ji Jianghui, a researcher at the Purple Mountain Observatory of the Chinese Academy of Sciences and a member of the expert committee for scientific goal argumentation of deep space exploration in China. The probe is also expected to conduct a fly-by of a third asteroid to be determined at a later time. The entire mission is expected to take about six years.


(175706) 1996 FG3, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 21 February 2008. As of 2018, it has not been named.


(175706) 1996 FG3, Physical characteristics
The carbonaceous body is characterized as a rare B-type and hydrated C-type (Ch) asteroid, respectively.


(175706) 1996 FG3, Physical characteristics, Lightcurves
Several rotational lightcurves of this asteroid were obtained from photometric observations taken by astronomers Petr Pravec, Petr Scheirich and Stefano Mottola, as well as by the Very Large Telescope's VISR instrument. Lightcurve analysis gave a well-defined rotation period of 3.594 to 3.595 hours with a brightness variation of 0.08 to 0.10 magnitude (U=3/3/3/3). The asteroid is an oblate ellipsoid with a nearly spherical shape.


(175706) 1996 FG3, Physical characteristics, Diameter and albedo
According to numerous observations, including the EXPLORENEOs survey, NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission and the Spitzer Space Telescope, the asteroid measures between 1.55 and 1.90 kilometers in diameter and its surface has a low albedo of 0.03 to 0.05. The Collaborative Asteroid Lightcurve Link adopts an albedo of 0.04 and a diameter of 1.90 kilometers.


(175706) 1996 FG3, Satellite
During the photometric observations in December 1998, the binary nature of this asteroid was revealed. It was the first binary near-Earth asteroid for which eclipse events were detected in the visible spectrum. The binary system has a diameter ratio of 0.28, a density of 1.4 g/cm3, and an ecliptic latitude of -84° for its mutual spin axis. The asteroid moon has a diameter of approximately 490 meters and an orbital period of 16.1508 hours. Its orbit is nearly circular, with an eccentricity of 0.1 and a semi-major axis of approximately 3.4 primary radii. The moon's rotation period remains unknown.


(177049) 2003 EE16
(177049) 2003 EE16, provisionally known as 2003 EE16, is an Apollo near-Earth asteroid and potentially hazardous object. It was discovered on 8 March 2003 by LPL/Spacewatch II at an apparent magnitude of 20 using a 1.8-meter (71 in) reflecting telescope. It has an estimated diameter of 320 meters (1,050 ft). The asteroid was listed on Sentry Risk Table with a Torino Scale rating of 1 on 2 April 2003.


(177049) 2003 EE16, Description
Many of the virtual impactors were located near the nominal orbital solution and the asteroid has a low inclination relative to Earth's orbit. Observation by the Very Large Telescope (VLT) 8 meter facilities on 22 May and 19 June 2003 when 2003 EE16 was very dim with an apparent magnitude between 24–25 refined the orbit. It was removed from the Sentry Risk Table on 28 May 2003.


(177049) 2003 EE16, Description
2003 EE16 has the smallest Earth Minimum orbit intersection distance (MOID) of any known potentially hazardous asteroid. The Earth MOID is 0.0000475 AU (7,110 km; 4,420 mi). Asteroids with a smaller Earth MOID are less than ~100 meters in diameter such as 2013 XY8 and 2010 TD54. Earth impactors 2008 TC3 and 2014 AA had small Earth MOID values as they were on their impact approach when discovered.


(179806) 2002 TD66
(179806) 2002 TD66 (also written 2002 TD66) is a sub-kilometer asteroid, classified as near-Earth object of the Apollo group. It was discovered on 5 October 2002, by the LINEAR project at Lincoln Laboratory's ETS in Socorro, New Mexico. It was announced on 7 October 2002 and appeared later that day on the JPL current risk page.


(179806) 2002 TD66, Description
Due to the proximity of its orbit to Earth and its estimated size, this object has been classified as a potentially hazardous asteroid (PHA) by the Minor Planet Center in Cambridge, Massachusetts. In November 2006 there were 823 PHAs known. As of October 2011, there are 1261 PHAs known. 2002 TD66 was removed from the Sentry Risk Table on October 10, 2002. A Doppler observation has helped produce a well known trajectory with a condition code (Uncertainty Parameter U) of 0.


(179806) 2002 TD66, Description
Based on an absolute magnitude (H) of 20.2, the asteroid is estimated to be between 270 and 590 meters in diameter. Radar astronomy shows it is a contact binary asteroid with a diameter of 300 meters and a rotation period of 9.5 hours.


(179806) 2002 TD66, Description
On February 26, 2008, 2002 TD66 passed 0.04282 AU (6,406,000 km; 3,980,000 mi) from Earth. The asteroid also comes close to Venus, Mars, and dwarf planet Ceres.


(181708) 1993 FW
(181708) 1993 FW was the second trans-Neptunian object to be discovered after Pluto and Charon, the first having been 15760 Albion, formally known as (15760) 1992 QB1. It was discovered in 1993 by David C. Jewitt and Jane X. Luu at the Mauna Kea Observatory, Hawaii. Following its discovery it was nicknamed "Karla" after a character by John le Carré by its discoverers and was hailed as that of a new planet. Mike Brown lists it as possibly a dwarf planet on his website.


(181708) 1993 FW
Over one thousand bodies were found in a belt between orbiting between about 30-50 AU from the Sun in the twenty years (1992-2012), after finding 1992 QB1 (named in 2018, 15760 Albion), showing a vast belt of bodies more than just Pluto and Albion. By 2018, over 2000 Kuiper belts objects were discovered.


(181708) 1993 FW
The mid-1990s were time when the new region "came to life", triggering a retrospective at various predictions about various second asteroid or comet belts in the other system.


(181708) 1993 FW
Three more KBO's found in 1993 include: (15788) 1993 SB, (15789) 1993 SC, and (385185) 1993 RO


(181902) 1999 RD215
(181902) 1999 RD215 is a trans-Neptunian object of the scattered disc, approximately 148 kilometers in diameter. It was discovered on 6 September 1999, by American astronomers Chad Trujillo, Jane Luu, and David Jewitt at the Mauna Kea Observatories, Hawaii.


(181902) 1999 RD215, Orbit and classification
1999 RD215 orbits from the center of the Kuiper belt to well beyond into the scattered disc. It orbits the Sun at a distance of 37.5–204.4 AU once every 1330 years and 7 months (485,993 days; semi-major axis of 121 AU). Its orbit has an eccentricity of 0.69 and an inclination of 26° with respect to the ecliptic. The body's observation arc begins with its official discovery observation.


(181902) 1999 RD215, Diameter and albedo
According to the Johnston's Archive and Michael Brown, 1999 RD215 measures 147 and 148 kilometers in diameter, and its surface has an estimated albedo of 0.09 and 0.08, respectively.


(182294) 2001 KU76
(182294) 2001 KU76, provisionally known as 2001 KU76, is a trans-Neptunian object (TNO) that has a possible 6:11 resonance with Neptune.


(182294) 2001 KU76
Assuming a generic TNO albedo of 0.09, it is about 211 km in diameter. The assumed diameter of this object makes it a possible dwarf planet.


(182294) 2001 KU76, Resonance
Simulations by Lykawka in 2007 show that (182294) 2001 KU76 may be librating in the 11:6 resonance with Neptune. Buie classifies it as probably in resonance, although some possible orbits do not librate. (182294) 2001 KU76 has a semi-major axis of 45 AU and an orbital period of about 302 years.


(182294) 2001 KU76, Resonance
It has been observed 29 times over 6 years and has an orbit quality code of 4.


(184212) 2004 PB112
(184212) 2004 PB112, prov. designation: 2004 PB112, is a trans-Neptunian object from the scattered disc, approximately 154 kilometers (96 miles) in diameter, and in a rare high-order orbital resonance ratio (4:27) with Neptune. It was discovered on 13 August 2004, by American astronomer Marc Buie at the Cerro Tololo Inter-American Observatory in Chile.


(184212) 2004 PB112, Orbit and classification
2004 PB112 orbits the Sun at a distance of 35.3–184.6 AU once every 1153 years and 2 months (421,205 days; semi-major axis of 109.97 AU). Its orbit has a high eccentricity of 0.68 and an inclination of 15° with respect to the ecliptic. A first precovery was taken at Cerro Tololo in 2000, extending the body's observation arc by 4 years prior to its official discovery observation.


(184212) 2004 PB112, Orbit and classification
2004 PB112 reached perihelion on 5 October 2011 (JD 2455839.806). It has been classified as a highly unusual 4:27 resonant trans-Neptunian object, but also simply as a scattered disc object, or SCATNEAR, respectively, by the Deep Ecliptic Survey.


(184212) 2004 PB112, Numbering and naming
This minor planet was numbered (184212) by the Minor Planet Center on 20 April 2008 (M.P.C. 62608). As of 2021, it has not been named.


(184212) 2004 PB112, Physical characteristics
Based on a generic conversion from an absolute magnitude of 7.2, 2004 PB112 measures between 100 and 220 kilometer in diameter. Johnston's Archive estimates a mean-diameter of 154 kilometers (96 miles) assuming a typical albedo of 0.09.


(185851) 2000 DP107
(185851) 2000 DP107 is a sub-kilometer sized asteroid, classified as potentially hazardous asteroid and near-Earth object of the Apollo group that is notable because it provided evidence for binary asteroids in the near-Earth population.


(185851) 2000 DP107, Discovery
The asteroid was discovered on 29 February 2000, by the Lincoln Near-Earth Asteroid Research (LINEAR) program at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico.


(185851) 2000 DP107, Discovery
The binary nature of this asteroid was suggested from radar observations taken with the Goldstone radar antenna on September 22 and 23, 2000, based on an observing proposal by J.-L. Margot and observations by S. J. Ostro and colleagues. Confirming observations were obtained with the Arecibo telescope from September 30 to October 7, 2000.


(185851) 2000 DP107, Orbit
2000 DP107 orbits the Sun at a distance of 0.9–1.9 AU once every 19 months (583 days). Its orbit has an eccentricity of 0.38 and an inclination of 9° with respect to the ecliptic. The body's observation arc begins with its official discovery observation, as no precoveries were taken, and no prior identifications were made.


(185851) 2000 DP107, Binary system
The 800-meter-diameter primary and the 300-meter-diameter secondary orbit each other with a separation of 2.6 kilometers and a period of 1.76 days.


(185851) 2000 DP107, Binary system
The primary is spheroidal and is spinning at a rate near the breakup point for strengthless bodies. These two features were observed in multiple binary systems, suggesting that near-Earth asteroid binaries form by a mechanism involving spin-up and mass shedding. Currently the most generally accepted spin-up mechanism is the YORP effect.


(185851) 2000 DP107, Physical characteristics
The asteroid is characterized as both a carbonaceous C-type and metallic M-type asteroid.


(185851) 2000 DP107, Physical characteristics
The density of the primary was calculated using the orbital elements of the binary system, the primary-to-secondary mass ratio, and estimates of the primary size. The primary has a low density of 1.7 g/cm3, which may indicate a "rubble pile" structure containing rocks and voids.


(185851) 2000 DP107, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 20 May 2008. As of 2018, it has not been named.


(190166) 2005 UP156
(190166) 2005 UP156 is a stony asteroid and binary system, classified as near-Earth object of the Apollo group, approximately 1 kilometer in diameter. It was discovered on 31 October 2005, by astronomers of the Spacewatch survey at the Kitt Peak National Observatory in Arizona, United States. Its minor-planet moon with an orbital period of 40.25 hours was discovered in 2017.


(190166) 2005 UP156, Orbit and classification
2005 UP156 is an Amor asteroid that approaches the orbit of Earth from beyond but does not cross it. It orbits the Sun at a distance of 1.1–3.1 AU once every 3 years and 1 month (1,124 days). Its orbit has an eccentricity of 0.47 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins with a precovery image taken by NEAT at Palomar Observatory in November 2002, almost four years prior to its official discovery observation. Due to its high eccentricity, the asteroid is also a Mars-crosser, which means that it also crosses the orbit of Mars (at 1.666 AU).


(190166) 2005 UP156, Orbit and classification, Close approaches
This near-Earth object has an Earth minimum orbital intersection distance of 0.1316 AU (19,700,000 km) which corresponds to 51.3 lunar distances. On 10 July 2017, it approached Earth to a distance of 0.133 AU and will make its next close approach at 0.128 AU in July 2057.


(190166) 2005 UP156, Physical characteristics, Rotation period
Since 2004, several rotational lightcurves of 2005 UP156 were obtained from photometric observations by French amateur astronomers David Romeuf, René Roy, as well as by American astronomer Brian Warner. Analysis of the best-rated lightcurve gave a rotation period of 40.542 hours with a brightness variation of 1.1 magnitude (U=2/3/3/2).


(190166) 2005 UP156, Physical characteristics, Rotation period
While not being a slow rotator, 2005 UP156 has a much longer rotation period than most asteroids, especially for it nearly sub-kilometer size. The lightcurve's high brightness amplitude also indicates that the body has a non-spheroidal shape.


(190166) 2005 UP156, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2005 UP156 measures 1.045 kilometers in diameter and its surface has an albedo of 0.234, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 1.08 kilometers based on an absolute magnitude of 17.2. The asteroid has an estimated density of 1.8 g/cm3.


(190166) 2005 UP156, Binary system
In May 2017, photometric observations by Brian Warner and Alan Harris revealed that 2005 UP156 is a synchronous binary system with a secondary component orbiting around the system barycenter every 40.572 hours. The secondary has been confirmed by radar observations. Its provisional designation is S/2017 (190166) 1.


(190166) 2005 UP156, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 19 August 2008. As of 2018, it has not been named.


(19255) 1994 VK8
(19255) 1994 VK8 is a trans-Neptunian object (TNO) of the "cold" cubewano class orbiting the Sun in the Kuiper belt of the outer Solar System. It was discovered on November 8, 1994, by Alan Fitzsimmons, Donal O'Ceallaigh, and Iwan P. Williams at Roque de los Muchachos Observatory on the island of La Palma, Spain.


(19255) 1994 VK8
(19255) 1994 VK8 is the fourth cubewano to be given an official Minor Planet Center catalog number. The first three official cubewanos are 15760 Albion, (15807) 1994 GV9, and (16684) 1994 JQ1.


(192642) 1999 RD32
(192642) 1999 RD32, provisional designation 1999 RD32, is an eccentric asteroid and suspected contact binary, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 5 kilometers in diameter. It was discovered on 8 September 1999, at a magnitude of 18, by astronomers of the LINEAR program using its 1-meter telescope at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, United States. The asteroid is likely of carbonaceous composition and has a rotation period of 17.08 hours.


(192642) 1999 RD32, Description
1999 RD32 orbits the Sun at a distance of 0.6–4.7 AU once every 4 years and 4 months (1,571 days; semi-major axis of 2.64 AU). Its orbit has a high eccentricity of 0.77 and an inclination of 7° with respect to the ecliptic.


(192642) 1999 RD32, Description
The asteroid's observation arc begins with a precovery taken at Palomar Observatory in January 1995. It is known that 1999 RD32 passed 0.0093 AU (1,390,000 km; 860,000 mi) from Earth on 27 August 1969. During the 1969 close approach the asteroid reached about apparent magnitude 8.8. The similarly-sized 4179 Toutatis also reached that brightness in September 2004. It passed less than 0.007 AU (1,000,000 km; 650,000 mi) from asteroid 29 Amphitrite on 17 January 1939.


(192642) 1999 RD32, Description
Arecibo radar observations on 5–6 March 2012 showed that 1999 RD32 is approximately 5 kilometers (3 mi) in diameter and has an estimated albedo of only 0.04. Other sources calculate a smaller diameter of 1.63 kilometers based on a dated assumption, that the object is a stony rather than a carbonaceous asteroid. The two visible lobes suggest that 1999 RD32 is a tight binary asteroid or contact binary. About 10–15% of near-Earth asteroids larger than 200 meters are expected to be contact binary asteroids with two lobes in mutual contact.


(192642) 1999 RD32, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 13 November 2008. As of 2018, it has not been named.


(19308) 1996 TO66
(19308) 1996 TO66 (also written (19308) 1996 TO66) is a trans-Neptunian object that was discovered in 1996 by Chadwick Trujillo, David Jewitt and Jane Luu. Until 20000 Varuna was discovered, it was the second-largest known object in the Kuiper belt, after Pluto.


(19308) 1996 TO66, Origin
Based on their common pattern of IR water-ice absorptions, neutral visible spectrum and the clustering of their orbital elements, the other KBOs (24835) 1995 SM55, (55636) 2002 TX300, (120178) 2003 OP32 and (145453) 2005 RR43 all appear to be collisional fragments broken off of the dwarf planet Haumea.


(19308) 1996 TO66, Orbit
The eccentricity of 1996 TO66 varies between ca. 0.110 and 0.125 every 2 million years, with additional variations on the order of ± 0.01 on much shorter time scales. It is in an intermittent 19:11 resonance with Neptune. The resonance breaks every 2 million years when the eccentricity is highest and the orbit is closest to Neptune.


(1952–19??)
(1952–19??) is the seventh 12" vinyl record album by DIY home recording pioneer and one-man band R. Stevie Moore. It was released on Alan Jenkins' Cordelia Records label in the UK.


(1952–19??)
"You and Me" was included on Moore's 2012 best-of, Lo Fi High Fives.


(196256) 2003 EH1
(196256) 2003 EH1 is an asteroid, classified as near-Earth object of the Amor group. It was discovered on 6 March 2003, by astronomers of the LONEOS program at Anderson Mesa Station near Flagstaff, Arizona, in the United States. Peter Jenniskens (2003–2004) proposed that it is the parent body of the Quadrantid meteor shower. 2003 EH1 is likely an extinct comet and may even be related to the comet C/1490 Y1. 2003 EH1 came to perihelion on 12 March 2014.


(196256) 2003 EH1, Notes
†Assuming an albedo between 0.04 (typical of extinct comet nuclei) and 0.09.


(2+1)-dimensional topological gravity
In two spatial and one time dimensions, general relativity turns out to have no propagating gravitational degrees of freedom. In fact, it can be shown that in a vacuum, spacetime will always be locally flat (or de Sitter or anti-de Sitter depending upon the cosmological constant). This makes (2+1)-dimensional topological gravity (2+1D topological gravity) a topological theory with no gravitational local degrees of freedom.


(2+1)-dimensional topological gravity
Physicists became interested in the relation between Chern–Simons theory and gravity during the 1980s. During this period, Edward Witten argued that 2+1D topological gravity is equivalent to a Chern–Simons theory with the gauge group SO(2,2){\displaystyle SO(2,2)} for a negative cosmological constant, and SO(3,1){\displaystyle SO(3,1)} for a positive one. This theory can be exactly solved, making it a toy model for quantum gravity. The Killing form involves the Hodge dual.


(2+1)-dimensional topological gravity
Witten later changed his mind, and argued that nonperturbatively 2+1D topological gravity differs from Chern–Simons because the functional measure is only over nonsingular vielbeins. He suggested the CFT dual is a Monster conformal field theory, and computed the entropy of BTZ black holes.


(2,1)-Pascal triangle
In mathematics, the (2,1)-Pascal triangle (mirrored Lucas triangle)is a triangular array.


(2,1)-Pascal triangle
The rows of the (2,1)-Pascal triangle (sequence  in the OEIS) are conventionally enumerated starting with row n = 0 at the top (the 0th row). The entries in each row are numbered from the left beginning with k = 0 and are usually staggered relative to the numbers in the adjacent rows.


(2,1)-Pascal triangle
The triangle is based on the Pascal's Triangle with the second line being (2,1) and the first cell of each row set to 2.


(2,1)-Pascal triangle
This construction is related to the binomial coefficients by Pascal's rule, with one of the terms being 2x+y{\displaystyle 2x+y}.


(2,1)-Pascal triangle, Patterns and properties
(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.


(2,1)-Pascal triangle, Patterns and properties, Diagonals
The diagonals of Pascal's triangle contain the figurate numbers of simplices:


(2,2,3-Trimethyl-5-oxocyclopent-3-enyl)acetyl-CoA 1,5-monooxygenase
(2,2,3-Trimethyl-5-oxocyclopent-3-enyl)acetyl-CoA 1,5-monooxygenase (EC , 2-oxo-Delta3-4,5,5-trimethylcyclopentenylacetyl-CoA monooxygenase, 2-oxo-Delta3-4,5,5-trimethylcyclopentenylacetyl-CoA 1,2-monooxygenase, OTEMO) is an enzyme with systematic name ((1R)-2,2,3-trimethyl-5-oxocyclopent-3-enyl)acetyl-CoA,NADPH:oxygen oxidoreductase (1,5-lactonizing). This enzyme catalyses the following chemical reaction


(2,2,3-Trimethyl-5-oxocyclopent-3-enyl)acetyl-CoA 1,5-monooxygenase
(2,2,3-trimethyl-5-oxocyclopent-3-enyl)acetyl-CoA 1,5-monooxygenase is FAD dependent enzyme isolated from Pseudomonas putida.


(2,2,3-trimethyl-5-oxocyclopent-3-enyl)acetyl-CoA synthase
(2,2,3-trimethyl-5-oxocyclopent-3-enyl)acetyl-CoA synthase (EC , 2-oxo-Delta3-4,5,5-trimethylcyclopentenylacetyl-CoA synthetase) is an enzyme with systematic name ((1R)-2,2,3-trimethyl-5-oxocyclopent-3-enyl)acetate:CoA ligase (AMP-forming). This enzyme catalyses the following chemical reaction


(2,3,7) triangle group
In the theory of Riemann surfaces and hyperbolic geometry, the triangle group (2,3,7) is particularly important. This importance stems from its connection to Hurwitz surfaces, namely Riemann surfaces of genus g with the largest possible order, 84(g − 1), of its automorphism group.


(2,3,7) triangle group
A note on terminology – the "(2,3,7) triangle group" most often refers, not to the full triangle group Δ(2,3,7) (the Coxeter group with Schwarz triangle (2,3,7) or a realization as a hyperbolic reflection group), but rather to the ordinary triangle group (the von Dyck group) D(2,3,7) of orientation-preserving maps (the rotation group), which is index 2.


(2,3,7) triangle group
Torsion-free normal subgroups of the (2,3,7) triangle group are Fuchsian groups associated with Hurwitz surfaces, such as the Klein quartic, Macbeath surface and First Hurwitz triplet.


(2,3,7) triangle group, Constructions, Hyperbolic construction
To construct the triangle group, start with a hyperbolic triangle with angles π/2, π/3, π/7. This triangle, the smallest hyperbolic Schwarz triangle, tiles the plane by reflections in its sides. Consider then the group generated by reflections in the sides of the triangle, which (since the triangle tiles) is a non-Euclidean crystallographic group (discrete subgroup of hyperbolic isometries) with this triangle for fundamental domain; the associated tiling is the order-3 bisected heptagonal tiling. The (2,3,7) triangle group is defined as the index 2 subgroup consisting of the orientation-preserving isometries, which is a Fuchsian group (orientation-preserving NEC group).


(2,3,7) triangle group, Constructions, Group presentation
It has a presentation in terms of a pair of generators, g2, g3, modulo the following relations:


(2,3,7) triangle group, Constructions, Group presentation
Geometrically, these correspond to rotations by 2π2,2π3{\displaystyle {\frac {2\pi }{2}},{\frac {2\pi }{3}}}, and 2π7{\displaystyle {\frac {2\pi }{7}}} about the vertices of the Schwarz triangle.


(2,3,7) triangle group, Constructions, Quaternion algebra
The (2,3,7) triangle group admits a presentation in terms of the group of quaternions of norm 1 in a suitable order in a quaternion algebra. More specifically, the triangle group is the quotient of the group of quaternions by its center ±1.


(2,3,7) triangle group, Constructions, Quaternion algebra
we see that Q(η) is a totally real cubic extension of Q. The (2,3,7) hyperbolic triangle group is a subgroup of the group of norm 1 elements in the quaternion algebra generated as an associative algebra by the pair of generators i,j and relations i2 = j2 = η, ij = −ji. One chooses a suitable Hurwitz quaternion order QHur{\displaystyle {\mathcal {Q}}_{\mathrm {Hur} }} in the quaternion algebra. Here the order QHur{\displaystyle Q_{\mathrm {Hur} }} is generated by elements


(2,3,7) triangle group, Constructions, Quaternion algebra
In fact, the order is a free Z[η]-module over the basis 1,g2,g3,g2g3{\displaystyle 1,g_{2},g_{3},g_{2}g_{3}}. Here the generators satisfy the relations


(2,3,7) triangle group, Constructions, Quaternion algebra
which descend to the appropriate relations in the triangle group, after quotienting by the center.


(2,3,7) triangle group, Relation to SL(2,R)
Extending the scalars from Q(η) to R (via the standard imbedding), one obtains an isomorphism between the quaternion algebra and the algebra M(2,R) of real 2 by 2 matrices. Choosing a concrete isomorphism allows one to exhibit the (2,3,7) triangle group as a specific Fuchsian group in SL(2,R), specifically as a quotient of the modular group. This can be visualized by the associated tilings, as depicted at right: the (2,3,7) tiling on the Poincaré disc is a quotient of the modular tiling on the upper half-plane.


(2,3,7) triangle group, Relation to SL(2,R)
However, for many purposes, explicit isomorphisms are unnecessary. Thus, traces of group elements (and hence also translation lengths of hyperbolic elements acting in the upper half-plane, as well as systoles of Fuchsian subgroups) can be calculated by means of the reduced trace in the quaternion algebra, and the formula


(2,3-dihydroxybenzoyl)adenylate synthase
In enzymology, a (2,3-dihydroxybenzoyl)adenylate synthase (EC ) is an enzyme that catalyzes the chemical reaction


(2,3-dihydroxybenzoyl)adenylate synthase
Thus, the two substrates of this enzyme are ATP and 2,3-dihydroxybenzoate, whereas its two products are diphosphate and (2,3-dihydroxybenzoyl)adenylate.


(2,3-dihydroxybenzoyl)adenylate synthase
This enzyme belongs to the family of transferases, specifically those transferring phosphorus-containing nucleotide groups (nucleotidyltransferases). The systematic name of this enzyme class is ATP:2,3-dihydroxybenzoate adenylyltransferase. This enzyme is also called 2,3-dihydroxybenzoate-AMP ligase. This enzyme participates in biosynthesis of siderophore group nonribosomal.


(2,4,6-Trimethylphenyl)gold
(2,4,6-Trimethylphenyl)gold is a member of a special group of compounds where an aryl carbon atom acts as a bridge between two gold atoms. This compound is formed in a reaction between Au(CO)Cl and the Grignard reagent mesitylmagnesium bromide. It crystallizes as a cyclical pentamer.


(2-Bromophenyl)diphenylphosphine
(2-Bromophenyl)diphenylphosphine is an organophosphorus compound with the formula (C6H4Br)P(C6H5)2. It is a white crystalline solid that is soluble in nonpolar organic solvents. The compound is used as a precursor to the 2-lithiated derivative of triphenylphosphine, which in turn is a precursor to other phosphine ligands.


(2-Bromophenyl)diphenylphosphine, Preparation
The compound has been prepared by several methods. An efficient route is the coupling reaction of diphenylphosphine and 2-bromoiodobenzne, which is catalyzed by palladium complexes (Ph = C6H5):


(2-Chlorophenyl)thiourea
(2-Chlorophenyl)thiourea is a chemical compound used as an herbicide. As of 1998, the Environmental Protection Agency did not have it registered as a pesticide in the United States.


(20161) 1996 TR66
(20161) 1996 TR66 is a trans-Neptunian object orbiting beyond Pluto in the Kuiper belt of the outermost Solar System, approximately 139 kilometers (86 miles) in diameter. It was discovered on 8 October 1996, by astronomers David Jewitt, Chad Trujillo, Jane Luu, and Jun Chen at the Mauna Kea Observatory, Hawaii, in the United States. It was the first discovery of a twotino.


(20161) 1996 TR66, Orbit and classification
It orbits the Sun at a distance of 28.6–66.6 AU once every 328 years and 8 months (120,032 days). Its orbit has an eccentricity of 0.40 and an inclination of 12° with respect to the ecliptic. Near perihelion, it comes closer to the Sun than Neptune does (29.7 AU). It has a semi-major axis (average distance from the Sun) near the edge of the classical belt.


(20161) 1996 TR66, Orbit and classification, Twotino
1996 TR66 was the first twotino discovered. Twotinos stay in a 1:2 orbital resonance with Neptune, which means that for every one orbit a twotino makes, Neptune orbits two times. Both the Minor Planet Center and the Deep Ecliptic Survey list this trans-Neptunian object as a twotino.


(20161) 1996 TR66, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 9 January 2001. As of 2018, it has not been named.


(202421) 2005 UQ513
(202421) 2005 UQ513, also written as 2005 UQ513, is a cubewano with an absolute magnitude of 3.4. Mike Brown's website lists it as a highly likely dwarf planet. (202421) 2005 UQ513's spectrum has a weak signature of absorption by water ice. Like Quaoar, it has a very red spectrum, which indicates that its surface probably contains many complex, processed organic molecules. Its light curve shows variations of Δm=0.3 mag, but no period has been determined.


(202421) 2005 UQ513, Classification
(202421) 2005 UQ513 has a perihelion of 37.3 AU. The Minor Planet Center (MPC) classifies it as a cubewano while the Deep Ecliptic Survey (DES) classifies it as ScatExt (scattered-extended). Although dynamically it would have been a good candidate to be a member of the Haumea collisional family, given its red spectrum, it is not.


(202421) 2005 UQ513, Distance
As of December 2018, it is currently 48.0 AU from the Sun. It will come to perihelion in 2123.


(202421) 2005 UQ513, Distance
It has been observed 194 times over 14 oppositions with precovery images back to 1990.


(20729) 1999 XS143
(20729) 1999 XS143, provisional designation 1999 XS143, is a Jupiter trojan from the Greek camp, approximately 51 kilometers (32 miles) in diameter. It was discovered on 15 December 1999, by American astronomer Charles Juels at the Fountain Hills Observatory in Arizona. The dark Jovian asteroid has a short rotation period of 5.72 hours and belongs to the 90 largest Jupiter trojans. It has not been named since its numbering in January 2001.


(20729) 1999 XS143, Orbit and classification
1999 XS143 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.


(20729) 1999 XS143, Orbit and classification
It orbits the Sun at a distance of 4.9–5.5 AU once every 11 years and 11 months (4,352 days; semi-major axis of 5.22 AU). Its orbit has an eccentricity of 0.06 and an inclination of 22° with respect to the ecliptic.


(20729) 1999 XS143, Orbit and classification
The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken at the Palomar Observatory in February 1953, almost 47 years prior to its official discovery observation at Fountain Hills.


(20729) 1999 XS143, Numbering and naming
This minor planet was numbered on 9 January 2001 (M.P.C. 41908). As of 2018, it has not been named.


(20729) 1999 XS143, Physical characteristics
1999 XS143 is an assumed, carbonaceous C-type asteroid. It has a high V–I color index of 1.00 (see table below).


(20729) 1999 XS143, Physical characteristics, Rotation period
In September 2008, a rotational lightcurve of 1999 XS143 was obtained from photometric observations. Lightcurve analysis gave a rotation period of 5.72±0.02 hours with a brightness variation of 0.33 magnitude (U=2).


(20729) 1999 XS143, Physical characteristics, Rotation period
Observations by Stefano Mottola at the Calar Alto Observatory in October 2009 showed a divergent period of 7.631 hours with an amplitude of 0.20 magnitude (U=2).


(20729) 1999 XS143, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1999 XS143 between 50.96 kilometers in diameter and its surface has an albedo of 0.052, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 46.30 kilometers based on an absolute magnitude of 10.4. The object was neither observed by IRAS nor the Akari satellite.


(20729) 1999 XS143, 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.


(208996) 2003 AZ84
(208996) 2003 AZ84 is a trans-Neptunian object with a possible moon from the outer regions of the Solar System. It is approximately 940 kilometers across its longest axis, as it has an elongated shape. It belongs to the plutinos – a group of minor planets named after its largest member Pluto – as it orbits in a 2:3 resonance with Neptune in the Kuiper belt. It was discovered on 13 January 2003, by American astronomers Chad Trujillo and Michael Brown during the NEAT survey using the Samuel Oschin telescope at Palomar Observatory.


(208996) 2003 AZ84
Its lightcurve amplitude deviates little from that of a Jacobi ellipsoid, which suggests that it is likely one with small albedo spots.


(208996) 2003 AZ84
It is considered a very likely dwarf planet by astronomers Gonzalo Tancredi and Michael Brown. However, Grundy et al. conclude that objects such as this, in the size range of 400–1000 km, with albedos less than ≈0.2 and densities of ≈1.2 g/cm3 or less, have likely never compressed into fully solid bodies, let alone differentiated or collapsed into hydrostatic equilibrium, and so are highly unlikely to be dwarf planets. It is possibly the largest unnamed object in the Solar System, given the large measurement uncertainties of all unnamed objects with greater best-estimate diameters.


(208996) 2003 AZ84, Physical characteristics
The Spitzer Space Telescope has estimated its size at 686±96 km, while an analysis of a combination of Spitzer and Hershel data yielded a slightly higher estimate of 727.0+61.9−66.5 km. These results are in agreement with each other. Its large size of 2003 AZ84 makes it a probable dwarf planet. Its mass is unknown since the satellite has not been recovered.


(208996) 2003 AZ84, Physical characteristics
A stellar occultation in 2010 measured a single chord of 573±21 km. But this is only a lower limit for the diameter of 2003 AZ84 because the chord may not have passed through the center of the body.


(208996) 2003 AZ84, Physical characteristics
In 2017, stellar occultations and data from its rotational lightcurve suggested that 2003 AZ84 had an elongated shape, presumably due to its rapid rotation rate of 6.71 hours, similar to Haumea and Varuna. That would give 2003 AZ84 approximate dimensions of 940×766×490 km, with its longest axis nearly twice as long as its polar axis.


(208996) 2003 AZ84, Physical characteristics
The spectra and colors of 2003 AZ84 are very similar to those of Orcus, another large object in 2:3 resonance with Neptune. Both bodies have a flat featureless spectrum in the visible and moderately strong water ice absorption bands in the near-infrared, although 2003 AZ84 has a lower albedo. Both bodies also have a weak absorption band near 2.3 μm, which may be caused by ammonia hydrate or methane ice.