(208996) 2003 AZ84, Orbit and rotation
2003 AZ84 orbits the Sun at an average distance of 39.4 astronomical units (AU) and completes a full orbit in 247 years. It is in a 2:3 orbital resonance with Neptune; 2003 AZ84 completes two orbits around the Sun for every three orbits completed by Neptune. Since it is in a 2:3 resonance with Neptune, 2003 AZ84 is classified as a plutino. Its orbit is inclined to the ecliptic by 13.6 degrees. The orbit of 2003 AZ84 is moderately eccentric, with an orbital eccentricity of 0.183.


(208996) 2003 AZ84, Orbit and rotation
As of July 2019, 2003 AZ84 is currently located 44.43 AU (6.647×109 km) from the Sun. It had approached its aphelion (furthest distance from the Sun) in 1982 and will come to its perihelion (closest distance to the Sun) in 2107. Simulations by the Deep Ecliptic Survey show that over the next 10 million years 2003 AZ84 will not come closer (qmin) than 31.6 AU from the Sun (it will stay farther away than Neptune).


(208996) 2003 AZ84, Orbit and rotation
The rotation period of this minor planet was first measured by Scott Sheppard in 2003. Light curves obtained by Sheppard at the University of Hawai'i's 2.2-meter telescope gave an ambiguous rotation period of either 6.71 or 13.42 hours, with a brightness variation of 0.14 magnitudes (U=2). The shorter rotation period refers to the single-peaked solution, expected if the brightness variations resulted from albedo spots. The longer rotation period is for a double-peaked solution, more consistent with an elongated shape.


(208996) 2003 AZ84, Satellite
Using observations with the Hubble Space Telescope, the discovery of a satellite of 2003 AZ84 was reported in IAUC 8812 on 22 February 2007. The object was measured with a separation of 0.22 arcsec and an apparent magnitude difference of 5.0. As of 2012, attempts to recover the satellite have failed. The unrecovered satellite is estimated to be about 72±12 km in diameter.


(214869) 2007 PA8
(214869) 2007 PA8 is an asteroid and slow rotator, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.4 kilometers in diameter.


(214869) 2007 PA8
It came within 6.5 million km (4 million miles, 17 lunar distances) of Earth on 5 November 2012.


(214869) 2007 PA8
It was discovered on 9 August 2007, by the Lincoln Near-Earth Asteroid Research team (LINEAR) at the U.S. Lincoln Laboratory Experimental Test Site in Socorro, New Mexico.


(214869) 2007 PA8
It was studied by the 70-meter (230 ft) Goldstone Deep Space Network antenna as it came near Earth, which resulted in radar images and other data about the asteroid, such as its very long rotation period of approximately 100 hours.


(214869) 2007 PA8
2007 PA8 may be a dormant comet related to the November γ Pegasids meteor shower.


(214869) 2007 PA8, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 9 May 2009. As of 2018, it has not been named.


(21601) 1998 XO89
(21601) 1998 XO89, provisional designation 1998 XO89, is a Jupiter trojan from the Greek camp, approximately 55 kilometers (34 miles) in diameter. It was discovered on 15 December 1998, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico. The dark Jovian asteroid has a rotation period of 12.7 hours and belongs to the 80 largest Jupiter trojans. It has not been named since its numbering in February 2001.


(21601) 1998 XO89, Orbit and classification
1998 XO89  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.


(21601) 1998 XO89, Orbit and classification
It orbits the Sun at a distance of 5.0–5.4 AU once every 11 years and 11 months (4,356 days; semi-major axis of 5.22 AU). Its orbit has an eccentricity of 0.04 and an inclination of 19° with respect to the ecliptic. The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken at the Siding Spring Observatory in March 1991, more than 7 years prior to its official discovery observation at Socorro.


(21601) 1998 XO89, Physical characteristics
1998 XO89 is an assumed C-type asteroid. Its V–I color index of 0.97 is typical for that of D-type asteroids, the dominant spectral type among the Jupiter trojans.


(21601) 1998 XO89, Physical characteristics, Rotation period
In April 2013, a rotational lightcurve of 1998 XO89 was obtained from photometric observations by Robert Stephens at the Center for Solar System Studies (CS3) in California. Lightcurve analysis gave a rotation period of 12.65±0.01 hours and a brightness variation of 0.30 magnitude (U=2+). Observations by his college Brian Warner at CS3 in July 2017, gave a similar period of 12.530 hours with an amplitude of 0.25 magnitude (U=2+).


(21601) 1998 XO89, 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, 1998 XO89 measures 54.91 and 56.08 kilometers in diameter and its surface has an albedo of 0.064 and 0.100, 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.


(21601) 1998 XO89, 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.


(21601) 1998 XO89, Numbering and naming
This minor planet was numbered on 8 February 2001 (M.P.C. 22480). As of 2018, it has not been named.


(219774) 2001 YY145
(219774) 2001 YY145, provisional designation 2001 YY145 is a stony background asteroid and exceptionally slow rotator from the central region of the asteroid belt, approximately 1.5 kilometers (0.9 miles) in diameter. It was discovered on 18 December 2001, by astronomers with the Lowell Observatory Near-Earth-Object Search at Anderson Mesa Station near Flagstaff, Arizona, in the United States. The assumed S-type asteroid is likely elongated and has a rarely seen rotation period of 1007 hours, making it the 13th slowest rotator.


(219774) 2001 YY145, Orbit and classification
2001 YY145 is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main-belt at a distance of 2.2–2.9 AU once every 4 years and 2 months (1,515 days; semi-major axis of 2.58 AU). Its orbit has an eccentricity of 0.13 and an inclination of 10° with respect to the ecliptic. A first precovery was taken at Lincoln Lab's ETS in October 2001, extending the asteroid's observation arc by 2 months prior to its official discovery observation at Anderson Mesa.


(219774) 2001 YY145, Physical characteristics, Slow rotator
In October 2013, a rotational lightcurve was obtained of this asteroid from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. It gave a rotation period of 1007.7 hours – or nearly 42 days – with an assigned error margin of ±86 hours. According to the Light Curve Data Base, it is the 13th slowest rotating minor planet known to exist among more than 15,000 observed small Solar System bodies. Due to its high brightness variation of 0.86 magnitude, the body is likely to have a non-spheroidal shape (U=2). As of 2018, no follow-up observation have been published.


(219774) 2001 YY145, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 1.54 kilometers, based on an absolute magnitude of 16.43.


(219774) 2001 YY145, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 4 October 2009. As of 2018, it has not been named.


(22149) 2000 WD49
(22149) 2000 WD49, provisional designation 2000 WD49, is a Jupiter trojan from the Greek camp, approximately 50 kilometers (31 miles) in diameter. It was discovered on 21 November 2000, 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 belongs to the largest Jupiter trojans and has a rotation period of 7.84 hours. It has not been named since its numbering in February 2001.


(22149) 2000 WD49, Orbit and classification
2000 WD49 is a dark Jovian asteroid in a 1:1 orbital resonance with Jupiter. It is located in the leading Greek camp at the Gas Giant's L4 Lagrangian point, 60° ahead of its orbit (see Trojans in astronomy). It is also a non-family asteroid in the Jovian background population. It orbits the Sun at a distance of 4.9–5.4 AU once every 11 years and 9 months (4,280 days; semi-major axis of 5.16 AU). Its orbit has an eccentricity of 0.05 and an inclination of 21° with respect to the ecliptic. The body's observation arc begins with its first observation as 1994 NE6 at the La Silla Observatory in July 1994, more than 6 years prior to its official discovery observation at Socorro.


(22149) 2000 WD49, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 8 February 2001 (M.P.C. 42121). As of 2018, it has not been named.


(22149) 2000 WD49, Physical characteristics
2000 WD49 is an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a high V–I color index of 1.090.


(22149) 2000 WD49, Physical characteristics, Rotation period
In July 2006, a first rotational lightcurve of 2000 WD49 was obtained from photometric observations by Italian amateur astronomer Silvano Casulli. Lightcurve analysis gave a rotation period of 7.84±0.03 hours with a brightness amplitude of 0.20 magnitude (U=2).


(22149) 2000 WD49, Physical characteristics, Diameter and albedo
According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, 2000 WD49 measures 48.19 and 50.37 kilometers in diameter and its surface has an albedo of 0.063 and 0.076, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 50.77 kilometers based on an absolute magnitude of 10.2.


(22149) 2000 WD49, 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.


(225312) 1996 XB27
(225312) 1996 XB27, provisional designation 1996 XB27, is a bright mini-asteroid, classified as near-Earth object of the Amor group, approximately 84 meters in diameter. It was discovered on 12 December 1996, by astronomers of the Spacewatch program at the Kitt Peak National Observatory near of Tucson, Arizona, United States.


(225312) 1996 XB27, Description
1996 XB27 is classified as an Amor asteroid because its perihelion is less than 1.3 AU and does not cross Earth's orbit. The asteroid is on a low-eccentricity and low-inclination orbit between the orbits of Earth and Mars. This is within a region of stability where bodies may survive for the age of the Solar System, and hence it may have formed near its current orbit.


(225312) 1996 XB27, Description
It orbits the Sun at a distance of 1.1–1.3 AU once every 1 years and 4 months (474 days; semi-major axis of 1.19 AU). Its orbit has an eccentricity of 0.06 and an inclination of 2° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Kitt Peak in December 1996.


(225312) 1996 XB27, Description
Between 1900 and 2200 its closest approach with Earth is more than 0.11 AU.


(230965) 2004 XA192
(230965) 2004 XA192 is a Kuiper-belt object with a diameter of 339+120−95 km. It has an absolute magnitude of approximately 4.42, and albedo around 26%. It was discovered on 12 December 2004 at Palomar Observatory.


(230965) 2004 XA192
It is currently at 35.8 AU from the Sun, near its perihelion.


(231937) 2001 FO32
(231937) 2001 FO32 is a near-Earth asteroid classified as a potentially hazardous asteroid of the Apollo group. With an estimated diameter around 550 m (1,800 ft), it was discovered by the Lincoln Near-Earth Asteroid Research at Socorro, New Mexico on 23 March 2001. The asteroid safely passed by Earth on 21 March 2021 16:03 UTC from a closest approach distance of 0.0135 AU (2.02 million km; 1.25 million mi), or 5.25 lunar distances (LD).


(231937) 2001 FO32
During the day before closest approach, 2001 FO32 reached a peak apparent magnitude of 11.7 and was visible to ground-based observers with telescope apertures of at least 20 cm (8 in). It is the largest and one of the fastest asteroids to approach Earth within 10 LD (3.8 million km; 2.4 million mi) in 2021.


(231937) 2001 FO32
With an observation arc of 20 years, 2001 FO32 has a well-determined orbit, and its trajectory is well known through the year 2196. The asteroid's orbit is only potentially hazardous on a time scale of thousands of years.


(231937) 2001 FO32, Discovery
2001 FO32 was discovered on 23 March 2001 by the Lincoln Near-Earth Asteroid Research (LINEAR) at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico. The asteroid was first observed in the constellation Hydra at an apparent magnitude of 15.6. Shortly after discovery, follow-up observations were carried out by four other observatories until the asteroid's subsequent confirmation by the Minor Planet Center on 24 March 2003. The asteroid was given the provisional designation 2001 FO32 and was recognized as a potentially hazardous asteroid. The accredited LINEAR observers are M. Blythe, F. Shelly, M. Bezpalko, R. Huber, L. Manguso, and S. Adams.


(231937) 2001 FO32, Orbit and classification
2001 FO32 is a member of the dynamical Apollo group of Earth-crossing near-Earth asteroids with orbital semi-major axes greater than 1 astronomical unit (AU). It follows a highly elongated orbit around the Sun at a distance of 0.3–3.1 AU once every 2.22 years (810 days; semi-major axis of 1.7 AU). Its orbit has a high eccentricity of 0.83 and an inclination of 39° with respect to the ecliptic. With its highly eccentric orbit, it crosses the orbits of all four inner planets of the Solar System.


(231937) 2001 FO32, Orbit and classification
Having a long observation arc nearly 20 years, the orbit of 2001 FO32 is well-defined with a condition code of 0. Although it is classified as a potentially hazardous asteroid due to its large size combined with its small minimum orbit intersection distance (MOID) of 0.00375 AU (1.46 lunar distances) from Earth's orbital path, the asteroid will not make any close approaches within 0.01 AU (3.9 LD) over the next 200 years. The asteroid's orbit is only potentially hazardous on a time scale of thousands of years.


(231937) 2001 FO32, Orbit and classification, Close approaches
Over the course of its highly eccentric orbit, 2001 FO32 makes numerous close encounters with the inner planets—most often Mercury, Venus, and Earth. Its MOIDs from Mercury and Venus are 0.036 AU (5.4 million km; 3.3 million mi) and 0.075 AU (11.2 million km; 7.0 million mi), respectively. 2001 FO32's most recent close encounter with either one of those planets was on 16 January 2008, when it passed by Mercury from a distance of 0.094 AU (14.1 million km; 8.7 million mi).


(231937) 2001 FO32, Orbit and classification, Close approaches
On 21 March 2021, 2001 FO32 passed by Earth from a distance of 0.0135 AU (2.02 million km; 1.25 million mi) or 5.25 LD and made its closest approach at 16:03 UTC. During the few days leading up to closest approach, 2001 FO32 steadily became brighter and peaked at apparent magnitude 11.7 on 21 March 2021 2:00 UTC. Although its maximum brightness was too faint to be seen with the naked eye, it was visible to observers using telescopes with apertures of at least 20 cm (8 in).


(231937) 2001 FO32, Orbit and classification, Close approaches
Due to its highly inclined and eccentric orbit, its relative velocity to Earth during the close approach is 34.4 km/s (21.4 mi/s), making it one of the fastest asteroids to pass by Earth in 2021. By the time 2001 FO32 makes its closest approach to Earth, its solar elongation (angular separation from the Sun) would be 64°, too small to be observable from Earth.


(231937) 2001 FO32, Orbit and classification, Close approaches
In the next 100 years, 2001 FO32 will not make any close approaches to Earth closer than the 21 March 2021 encounter. It will make a similarly close approach to Earth on 22 March 2052 18:57±00:03 UTC, from a slightly farther nominal distance of 0.0189 AU (2.83 million km; 1.76 million mi) or 7.37 LD.


(231937) 2001 FO32, Observations
Preliminary observations by NEOWISE show that 2001 FO32 appears to be faint in infrared wavelengths of light, indicating that the asteroid is likely less than 1 kilometer in diameter. Based on this, the diameter is estimated around 550 ± 110 m (1,800 ± 360 ft). Near-infrared spectral data obtained by NASA's Infrared Telescope Facility in 2018 suggests that 2001 FO32 is a stony asteroid classified under the Sr spectral class.


(231937) 2001 FO32, Observations
2001 FO32 was first observed with radar on 21 March 2021 at Canberra, Australia and Narrabri, New South Wales, which provided refinement of its orbit. One day after its closest approach, bistatic radar observations were carried out by NASA's Goldstone Deep Space Communications Complex in California and Green Bank Telescope in West Viriginia. The radar images revealed that the asteroid has a bilobate shape.


(231937) 2001 FO32, Observations
February 2021 observations of 2001 FO32 by the La Silla Observatory show that it displays a light curve amplitude of 0.9 magnitudes. The preliminary photometry indicates that the body is tumbling with a long main rotation period of 39.89±0.05 hours.


(237442) 1999 TA10
(237442) 1999 TA10, provisionally known as 1999 TA10, is a near-Earth object (NEO) from the Amor asteroid group. It is suspected of being an inner fragment of the differentiated asteroid 4 Vesta.


(237442) 1999 TA10
Given an absolute magnitude (H) of 17.9, and that the albedo is unknown, this NEO could vary from 500 to 1500 meters in diameter.


(237442) 1999 TA10
1999 TA10 was discovered by LINEAR at Lincoln Laboratory ETS on 5 October 1999 at apparent magnitude 17.7, when it was only 0.39 AU from Earth. In 2010, it came within 0.3 AU of Earth. During the 2010 close approach, NASA Infrared Telescope Facility (NASA IRTF) studies suggested that 1999 TA10 originated from the interior of Vesta. The next close approach will be in 2023. In 2086, it will come within 0.017 AU (2,500,000 km; 1,600,000 mi) of Mars.


(23958) 1998 VD30
(23958) 1998 VD30, provisional designation 1998 VD30, is a Jupiter trojan from the Greek camp, approximately 47 kilometers (29 miles) in diameter. It was discovered on 10 November 1998, by astronomers with the LINEAR survey at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The dark Jovian asteroid belongs to the 110 largest Jupiter trojans and shows an exceptionally slow rotation of 562 hours. It has not been named since its numbering in April 2001.


(23958) 1998 VD30, Orbit and classification
1998 VD30 is a dark Jupiter trojan in a 1:1 orbital resonance with Jupiter. It is located in the leading Greek camp at the Gas Giant's L4 Lagrangian point, 60° ahead of its orbit (see Trojans in astronomy). It is also a non-family asteroid in the Jovian background population. It orbits the Sun at a distance of 4.7–5.7 AU once every 12 years (4,370 days; semi-major axis of 5.23 AU). Its orbit has an eccentricity of 0.10 and an inclination of 25° with respect to the ecliptic. The body's observation arc begins with its first observation as 1986 WG9 at the Kiso Observatory in November 1986, or 12 years prior to its official discovery observation at Socorro.


(23958) 1998 VD30, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 8 April 2001 (M.P.C. 42554). As of 2018, it has not been named.


(23958) 1998 VD30, Physical characteristics
1998 VD30 is an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical V–I color index of 0.99 and a BR-color of 1.15.


(23958) 1998 VD30, Physical characteristics, Rotation period
With a rotation period of 562 hours, this slow rotator belongs to the Top 100 slowest rotators known to exist. It is also the third-slowest rotator among the larger Jupiter trojans after 4902 Thessandrus (738 hours) and (7352) 1994 CO (648 hours).


(23958) 1998 VD30, Physical characteristics, Rotation period
In August 2015, a rotational lightcurve of 1998 VD30 was obtained from photometric observations by the Kepler space observatory during its K2 mission. Lightcurve analysis gave an exceptionally long period of 562±4 hours with a brightness amplitude of 0.45 magnitude, somewhat indicative of a non-spherical shape (U=2). A second, lower-rated lightcurve from Kepler gave an alternative, even longer period of 1143±155 hours (U=2).


(23958) 1998 VD30, Physical characteristics, Rotation period
These results supersede a poor period determination made at the Sierra Nevada Observatory in 2007, which gave a period 12.080 hours (U=1).


(23958) 1998 VD30, 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 VD30 measures 46.00 and 47.91 kilometers in diameter and its surface has an albedo between 0.076 and 0.084, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a larger diameter of 50.77 kilometers based on an absolute magnitude of 10.2.


(23958) 1998 VD30, 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.


(24)7.ai
[ 24]7.ai (full company name [24]7.ai, Inc.) is a customer experience software and services company based in California that uses artificial intelligence and machine learning to understand consumer intent. It helps companies create a personalized experience across channels.


(24)7.ai, History
[ 24]7.ai was founded in April 2000 by P. V. Kannan and Shanmugam Nagarajan. Kannan previously founded Business Evolution, a software company, which was acquired by Kana Software in 1999. The company is headquartered in San Jose, California. Other offices are located in Toronto, London, and Sydney. [ 24]7.ai has customers in many industries, including agencies, education, financial services, healthcare, insurance, retail & e-commerce, telecom, travel & hospitality, and utilities.


(24)7.ai, History
In 2003, [24]7.ai was privately funded in part by Michael Moritz and his venture capital firm Sequoia Capital. The total venture funding was estimated at about $22 million. The company was profitable by the end of 2003.


(24)7.ai, History
In February 2012 a deal was announced in which [24]7.ai and Microsoft would combine technologies for natural user interfaces (NUIs) and data analytics at cloud scale. Microsoft made an equity investor and transferred approximately 400 employees of the former Tellme Networks to [24]7.ai. At the same time, [24]7.ai acquired the call center automation developer Voxify, which had been based in Alameda, California, and was funded by investors such as Intel. In 2012, the company rebranded its business, adopting a new logo dropping the word "Customer" and putting square brackets around the "24". In January 2013 it announced it would market some internally developed software products for combining chat with analytics.


(24)7.ai, History
In May 2013 the company announced the acquisition of social commerce firm Shopalize for an undisclosed amount of money. [ 24]7.ai was also listed on Forbes list of America's Most Promising Companies in 2013.


(24)7.ai, History
In November 2014, [24]7.ai acquired IntelliResponse, a provider of digital self-service technology, including virtual agent solutions.


(24)7.ai, History
In August 2015, [24]7.ai acquired Campanja, a leading Search Engine bidding platform with offices in Stockholm, London, Palo Alto, Chicago and New York, adding realtime marketing capability to the [24]7.ai offering.


(24)7.ai, History
In July 2015, the company announced it had become the world's largest provider of chat agents, with more than 5,000 dedicated chat agents operating in its contact centers.


(24)7.ai, History
In October 2017, the company announced a name change, adding .ai to promote artificial intelligence.


(24)7.ai, Products
The product is sales and service-oriented software that encompasses big data, predictive analytics, virtual agents and real-time decisioning. It integrates different channels of communication, including web chat, mobile devices and interactive voice response, which incorporates the company's proprietary natural language technology. The company operates contact centers that outsource voice and chat agent services, for sales and support. Its largest customers are in telecommunications, financial services, retail, insurance, and travel industries. Its early offerings were contact center services with voice contact center agents. Contact centers were originally located in Bangalore and Hyderabad, India, and in the Philippines, but by 2007 (with about 7,000 total employees) expanded to Guatemala, Nicaragua, and Colombia to support Spanish-language customers.


(242450) 2004 QY2
(242450) 2004 QY2 (prov. designation: 2004 QY2) is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 3 kilometers (2 miles) in diameter. It was discovered on 20 August 2004 by the Siding Spring Survey at an apparent magnitude of 16.5 using the 0.5-metre (20 in) Uppsala Southern Schmidt Telescope. It is one of the largest potentially hazardous asteroids known to exist.


(242450) 2004 QY2, Orbit and classification
2004 QY2 orbits the Sun at a distance of 0.6–1.6 AU once every 14 months (412 days; semi-major axis of 1.08 AU). Its orbit has an eccentricity of 0.48 and an inclination of 37° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Siding Spring.


(242450) 2004 QY2, Orbit and classification
The object is a member of the Apollo asteroids, the largest subgroup of near-Earth asteroids which cross the orbit of Earth. Unlike many other members of this dynamical group, 2004 QY2 is not a Mars-crosser, as its aphelion is too small to cross the orbit of the Red Planet at 1.66 AU.


(242450) 2004 QY2, Orbit and classification, Close approaches
With an absolute magnitude of 14.7, 2004 QY2 is one of the brightest potentially hazardous asteroids ever discovered (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0469 AU (7,020,000 km), which translates into 18.3 lunar distances. On 29 July 2012, it passed Earth at a distance of 0.4314 AU (64,540,000 km; 40,100,000 mi).


(242450) 2004 QY2, Orbit and classification, Sentry Risk Table
Due to its originally estimated size of 5.5 kilometers, 2004 QY2 was one of the largest objects to appear on the Sentry Risk Table. It was removed from the Sentry Risk Table on 25 August 2004.


(242450) 2004 QY2, Physical characteristics
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2004 QY2 has an albedo of 0.274, and it measures 2.914 and 3.320 kilometers in diameter, respectively.


(242450) 2004 QY2, Physical characteristics
As of 2018, no rotational lightcurve of 2004 QY2 has been obtained from photometric observations. The body's rotation period, shape and spin axis remain unknown. In addition, the body's spectral type has never been assessed.


(242450) 2004 QY2, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 26 June 2006. As of 2018, it has not been named.


(24835) 1995 SM55
(24835) 1995 SM55, provisional designation 1995 SM55, is a trans-Neptunian object and member of the Haumea family that resides in the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 19 September 1995, by American astronomer Nichole Danzl of the Spacewatch program at Kitt Peak National Observatory near Tucson, Arizona, in the United States. It measures approximately 200 kilometers in diameter and was the second-brightest known object in the Kuiper belt, after Pluto, until 1996 TO66 was discovered.


(24835) 1995 SM55, Origin
1995 SM55 is a member of the Haumea family. It has the highest collisional velocity, a δv of 123.3 m/s, of all confirmed members. Based on their common pattern of IR water-ice absorptions, neutral visible spectrum and the clustering of their orbital elements, the other KBOs 1996 TO66, 2002 TX300, 2003 OP32 and 2005 RR43 all appear to be collisional fragments broken off of the dwarf planet Haumea.


(24835) 1995 SM55, Naming
As of 2018, this minor planet has not been named by the Minor Planet Center.


(248835) 2006 SX368
(248835) 2006 SX368, provisional designation: 2006 SX368, is a centaur, approximately 75 kilometers (47 miles) in diameter, orbiting in the outer Solar System between Saturn and Neptune. It was discovered on 16 September 2006, by American astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica at Apache Point Observatory in Sunspot, New Mexico.


(248835) 2006 SX368, Orbit and classification
Centaurs have short dynamical lives due to strong interactions with the giant planets. The orbit of 2006 SX368 is unusually eccentric — near the perihelion it comes under influence of Uranus, while at the aphelion it travels slightly beyond the orbit of Neptune.


(248835) 2006 SX368, Orbit and classification
It orbits the Sun at a distance of 11.9–32.0 AU once every 103 years and 2 months (37,683 days; semi-major axis of 22.0 AU). Its orbit has an eccentricity of 0.46 and an inclination of 36° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Apache Point in September 2006.


(248835) 2006 SX368, Physical characteristics
In 2010, thermal flux from 2006 SX368 in the far-infrared was measured by the Herschel Space Telescope. As a result, its equivalent size was estimated to lie within a range from 70 kilometres (43 mi) to 80 kilometres (50 mi).


(24952) 1997 QJ4
(24952) 1997 QJ4, also written as 1997 QJ4, is a plutino and as such, it is trapped in a 2:3 mean-motion resonance with Neptune. It was discovered on 28 August, 1997, by Jane X. Luu, Chad Trujillo, David C. Jewitt and K. Berney. This object has a perihelion (closest approach to the Sun) at 30.463 AU and an aphelion (farthest approach from the Sun) at 48.038 AU, so it moves in a relatively eccentric orbit (0.224). It has an estimated diameter of 139 km; therefore, it is unlikely to be classified as a dwarf planet.


(24978) 1998 HJ151
(24978) 1998 HJ151, also written as (24978) 1998 HJ151, is a cubewano. It has a perihelion (closest approach to the Sun) of 41.339 AU and an aphelion (farthest approach to the Sun) of 45.889 AU. It has a diameter of about 139 km. It was discovered on 28 April 1998, by Jane X. Luu, Chadwick A. Trujillo, David J. Tholen and David C. Jewitt.


(251732) 1998 HG49
(251732) 1998 HG49, provisional designation 1998 HG49, is a sub-kilometer asteroid and near-Earth object of the Amor group, approximately 200 meters in diameter. It was discovered on 27 April 1998 by astronomers of the Spacewatch program at the Kitt Peak National Observatory near Tucson, Arizona, United States.


(251732) 1998 HG49, Description
1998 HG49 is an Amor asteroid because its perihelion is less than 1.3 AU and does not cross Earth's orbit. It is on a low-eccentricity and low-inclination orbit between the orbits of Earth and Mars. This is within a region of stability where bodies may survive for the age of the Solar System, and hence it may have formed near its current orbit.


(251732) 1998 HG49, Description
The asteroid orbits the Sun at a distance of 1.1–1.3 AU once every 1 year and 4 months (480 days; semi-major axis of 1.20 AU). Its orbit has an eccentricity of 0.11 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Kitt Peak in April 1998.


(251732) 1998 HG49, Description
Between 1900 and 2200 its closest approach to Earth is more than 0.14 AU.


(251732) 1998 HG49, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 28 November 2010. As of 2018, it has not been named.


(26308) 1998 SM165
(26308) 1998 SM165 is a resonant trans-Neptunian object and binary system from the Kuiper belt in the outermost regions of the Solar System. It was discovered on 16 September 1998, by American astronomer Nichole Danzl at the Kitt Peak National Observatory in Arizona. It is classified as a twotino and measures approximately 280 kilometers in diameter. Its minor-planet moon was discovered in 2001.


(26308) 1998 SM165, Twotino
1998 SM165 has a semi-major axis (average distance from the Sun) near the edge of the classical belt. The Deep Ecliptic Survey (DES) list this trans-Neptunian object as a twotino that stays in a 1:2 orbital resonance with the planet Neptune (for every one orbit that a twotino makes, Neptune orbits twice).


(26308) 1998 SM165, Physical characteristics
The observations with the infrared Spitzer Space Telescope combined with the orbits established using the Hubble Telescope allow the estimation of the density, assuming the components of equal albedo.


(26308) 1998 SM165, Physical characteristics
The resulting estimate of 0.51+0.29−0.14 g/cm3is similar to the density of the binary plutino 47171 Lempo (0.3–0.8 g/cm3) and Saturn's moon Hyperion (0.567±0.102 g/cm3)Such a low density is indicative of a highly porous composition dominated by ice.


(26308) 1998 SM165, Physical characteristics
1998 SM165 is fairly red, with a color comparable to 79360 Sila–Nunam.


(26308) 1998 SM165, Satellite
On 22 December 2001, a minor-planet moon, provisionally designated S/2001 (26308) 1, was discovered by American astronomer Michael Brown and Chad Trujillo using the Hubble Space Telescope. The discovery was announced in January 2002. The satellite measures approximately 96 ± 12 km (59.7 ± 7.5 mi) in diameter and orbits its primary at a distance of 11,310 ± 110 km (7,028 ± 68 mi). Assuming a circular orbit, this takes 130.1±1 days to complete one orbit.


(26308) 1998 SM165, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 5 July 2001. As of 2018, it has not been named.


(26375) 1999 DE9
(26375) 1999 DE9 (also written (26375) 1999 DE9) is a trans-Neptunian object. Light-curve-amplitude analysis shows only small deviations, suggesting (26375) 1999 DE9 is a spheroid with small albedo spots. Measurements by the Spitzer Space Telescope estimate that it is 461 ± 45 km in diameter. It was discovered in 1999 by Chad Trujillo and Jane X. Luu. It is possibly a dwarf planet.


(26375) 1999 DE9
(26375) 1999 DE9 orbit is in 2:5 resonance with Neptune's. Spectral analysis has shown traces of ice.


(275809) 2001 QY297
(275809) 2001 QY297 is a trans-Neptunian object from the classical Kuiper belt, located in the outermost region of the Solar System. The binary classical Kuiper belt object belongs to the cold population.


(275809) 2001 QY297, Discovery and orbit
2001 QY297 was discovered on 21 August 2001 by Marc William Buie from Cerro Tololo Observatory, La Serena, Chile. 2001 QY297 belongs to the dynamically cold population of the classical Kuiper belt objects, which have small orbital eccentricities and inclinations. Their semi-major axes reside mainly in the interval 40–45 AU.


(275809) 2001 QY297, Satellite
2001 QY297 is a binary system consisting of two components of approximately equal size. The satellite was discovered on 18 April 2006. Assuming that both components have the same albedo, the primary is estimated to be about 169 km in diameter. The size of the secondary (satellite) in this case is estimated at around 154 km. The total mass of the system is approximately 4×1018 kg. The average density of both components is about 1 g/cm3.


(275809) 2001 QY297, Physical properties
The surfaces of both components of 2001 QY297 appear to have a red color. The object shows significant photometric variability with lightcurve amplitude of 0.49±0.03. The rotational period is either 5.84 or 11.68 hours.


(276033) 2002 AJ129
(276033) 2002 AJ129, provisional designation 2002 AJ129, is a Mercury-crossing asteroid. It has the ninth-smallest perihelion of all numbered asteroids, after asteroids such as 2000 BD19, 2004 UL, and 2008 XM. It makes close approaches to all of the inner planets and asteroid 4 Vesta. The asteroid is estimated to be between 0.5–1.2 kilometers (0.3–0.7 mi) across. In January 2018 there was much media hype about this asteroid being classified as a potentially hazardous asteroid, although there is no known threat of an impact for hundreds if not thousands of years. The media has compared the size of the asteroid to the Burj Khalifa in Dubai.


(276033) 2002 AJ129, Description
2002 AJ129 was discovered on 15 January 2002 by astronomers of the NEAT team at Haleakala Observatory, Hawaii, United States. It was removed from the Sentry Risk Table on 3 February 2002.


(276033) 2002 AJ129, Description
It is a Mercury-, Venus-, Earth- and Mars-crossing asteroid. With an observation arc of 14 years, it has a well determined orbit and was last observed in 2016. It is classified as an Apollo asteroid because it is a near-Earth asteroid with a semi-major axis larger than Earth's. It is also categorized as a potentially hazardous asteroid, but that does not mean there is a near-term threat of an impact. It is a potentially hazardous asteroid merely as a result of its size (absolute magnitude H ≤ 22) and Earth minimum orbit intersection distance (Earth MOID ≤ 0.05 AU).


(276033) 2002 AJ129, Description, 2018 approach
On 4 February 2018 at 21:31 UT, the asteroid passed about 0.028126 AU (4,207,600 km; 2,614,500 mi) from Earth. The 2018 Earth approach distance was known with a 3-sigma accuracy of ±200 km. Goldstone is scheduled to observe the asteroid from 3 to 6 February. By 4 February 2018 11:00 UT, the asteroid brightened to apparent magnitude 14 and had a solar elongation of more than 100°.


(276033) 2002 AJ129, Description, 2172 approach
On 8 February 2172, the asteroid will pass about 0.00458 AU (685,000 km; 426,000 mi) from Earth. The 2172 Earth approach distance is known with a 3-sigma accuracy of ±4000 km.


(276033) 2002 AJ129, Description, 2172 approach
As we look even further into the future the known trajectory becomes more divergent. By the Earth approach of 0.24 AU (36,000,000 km; 22,000,000 mi) on 19 February 2196 the uncertainty increases to ±2.4 million km.


(277475) 2005 WK4
(277475) 2005 WK4, provisional designation 2005 WK4, is a stony, sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group that passed Earth within 8.2 lunar distances on 8 August 2013. It was discovered on 27 November 2005, by astronomers of the Siding Spring Survey at Siding Spring Observatory, Australia.


(277475) 2005 WK4, Description
In August 2013, 2005 WK4 was radar-imaged by the Deep Space Network dish at Goldstone Observatory, United States, and had been observed previously at Arecibo Observatory in July 2012 (this was not a close approach though).


(277475) 2005 WK4, Description, Physical characteristics
2005 WK4 measures approximately 250 meters in diameter, and has a rotation period of 2.595 hours. Its spectral type is that of an Sk-subtype, which transitions from the stony S-type to the uncommon K-type asteroids.


(277810) 2006 FV35
(277810) 2006 FV35, provisional designation 2006 FV35, is a sub-kilometer near-Earth asteroid in the dynamical Apollo asteroid group, discovered by Spacewatch at Kitt Peak National Observatory, Arizona, on 29 March 2006. It is a quasi-satellite of Earth. It is also notable for having a low delta-v requirement for rendezvous. Although its orbital period is almost exactly 1 year, the orbit of 2006 FV35 has a high eccentricity which causes it to cross the paths of both Venus and Mars.


(277810) 2006 FV35, Transfer energy
With a semi-major axis of almost exactly 1 astronomical unit, 2006 FV35 has a relatively low transfer energy from Earth. The delta-v required to transfer to the asteroid varies between 11 and 13 km/s; this change in delta-v oscillates over an approximately 200-year period with the current transfer cost near its maximum of 13 km/s.


(278361) 2007 JJ43
(268361) 2007 JJ43 is a large trans-Neptunian object (TNO) orbiting the Sun near the outer edge of the Kuiper belt. If size estimates based on its absolute magnitude are correct, it is a possible dwarf planet.


(278361) 2007 JJ43
Its discovery images were taken in 2007, and its absolute magnitude of 4.5 is one of the twenty brightest exhibited by TNOs. Assuming it has a typical albedo, this would make it roughly the same size as Ixion (about 530–620 km diameter). Michael Brown's website lists it as a "likely" dwarf planet. In a paper in the Astrophysical Journal Letters András Pál and colleagues estimate a diameter for (278361) 2007 JJ43 of 610+170−140 km.


(278361) 2007 JJ43
Observations by Brown in 2012, using the W. M. Keck Observatory, suggest that (278361) 2007 JJ43 does not have a companion.


(278361) 2007 JJ43
As of 2014, it is about 41.3 AU from the Sun.


(285263) 1998 QE2
(285263) 1998 QE2, provisional designation 1998 QE2, is a dark asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3 kilometers in diameter. It was discovered on 19 August 1998, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. Its sub-kilometer minor-planet moon was discovered by radar on 30 May 2013.


(285263) 1998 QE2, Classification and orbital characteristics
As an Amor asteroid the orbit of 1998 QE2 is entirely beyond Earth's orbit. The asteroid orbits the Sun at a distance of 1.0–3.8 AU once every 3 years and 9 months (1,378 days; semi-major axis of 2.42 AU). Its orbit has an eccentricity of 0.57 and an inclination of 13° with respect to the ecliptic. The Earth minimum orbit intersection distance with the orbit of the asteroid is 0.035 AU (5,200,000 km; 3,300,000 mi), which translates into 13.4 lunar distances. As with many members of the Amor group, this asteroid has an aphelion beyond the orbit of Mars (at 1.66 AU) which also makes it a Mars-crosser.


(285263) 1998 QE2, Classification and orbital characteristics
The sooty surface of 1998 QE2 suggested that it might have previously been a comet that experienced a close encounter with the Sun. However, the Tisserand parameter with respect to Jupiter (TJ=3.2) does not make it obvious whether 1998 QE2 was ever a comet, since cometary TJ values are typically below 3.


(285263) 1998 QE2, Classification and orbital characteristics, Earth approach
On 31 May 2013, 1998 QE2 approached within 0.039 AU (5,800,000 km; 3,600,000 mi) (15 lunar distances) of Earth at 20:59 UT (4:59 pm EDT). This was the closest approach the asteroid will make to Earth for at least the next two centuries. It is a very strong radar target for Goldstone from May 30 to June 9 and will be one for Arecibo from June 6 to June 12. At its closest approach the asteroid had an apparent magnitude of 11 and therefore required a small telescope to be seen.


(285263) 1998 QE2, Classification and orbital characteristics, Earth approach
Integrating the orbital solution shows the asteroid passed 0.08 AU (12,000,000 km; 7,400,000 mi) from Earth on 8 June 1975 with an apparent magnitude of about 13.9. The next notable close approach will be 27 May 2221, when the asteroid will pass Earth at a distance of 0.038 AU (5,700,000 km; 3,500,000 mi).


(285263) 1998 QE2, Satellite
Goldstone radar observations on 29 May 2013 discovered that 1998 QE2 is orbited by a minor-planet moon approximately 600–800 meters in diameter. In radar images, the satellite appears brighter than 1998 QE2 because it is rotating significantly more slowly, which compresses the radar return of the satellite along the Doppler axis. This makes the satellite appear narrow and bright compared to 1998 QE2. The satellite orbits the primary every 32 hours with a maximum separation of 6.4 kilometers (4.0 mi). Once the satellite's orbit is well determined, astronomers and astrophysicists will be able to determine the mass and density of 1998 QE2.


(285263) 1998 QE2, Physical characteristics, Surface, albedo and composition
The surface of 1998 QE2 is covered with a sooty substance, making it optically dark with a geometric albedo of 0.06, meaning it absorbs 94% of the light that hits it, which is indicative for a carbonaceous surface of a C-type asteroid. The asteroid is covered with craters and is dark, red, and primitive.


(285263) 1998 QE2, Physical characteristics, Diameter
With a diameter between 2.7 and 3.2 kilometers, 1998 QE2 is one of largest known potentially hazardous asteroid (see PHA-list). Conversely, 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.


(29075) 1950 DA
(29075) 1950 DA, provisional designation 1950 DA, is a risk–listed asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 kilometers (0.68 miles) in diameter. It once had the highest known probability of impacting Earth. In 2002, it had the highest Palermo rating with a value of 0.17 for a possible collision in 2880. Since that time, the estimated risk has been updated several times. In December 2015, the odds of an Earth impact were revised to 1 in 8,300 (0.012%) with a Palermo rating of −1.42. As of 2021, It is tied on the Sentry Risk Table for having the highest cumulative Palermo rating. 1950 DA is not assigned a Torino scale rating, because the 2880 date is over 100 years in the future.


(29075) 1950 DA, Discovery and nomenclature
1950 DA was first discovered on 23 February 1950 by Carl A. Wirtanen at Lick Observatory. It was observed for seventeen days and then lost because this short observation arc resulted in large uncertainties in Wirtanen's orbital solution. On 31 December 2000, it was recovered at Lowell Observatory and was announced as 2000 YK66 on 4 January 2001. Just two hours later it was recognized as 1950 DA.


(29075) 1950 DA, Observations
On 5 March 2001, 1950 DA made a close approach to Earth at a distance of 0.05207 AU (7.790 million km; 4.840 million mi; 20.26 LD). It was studied by radar at the Goldstone and Arecibo observatories from March 3 to 7, 2001.


(29075) 1950 DA, Observations
The studies showed that the asteroid has a mean diameter of 1.1 km, assuming that 1950 DA is a retrograde rotator. Optical lightcurve analysis by Lenka Sarounova and Petr Pravec shows that its rotation period is 2.1216±0.0001 hours. Due to its short rotation period and high radar albedo, 1950 DA is thought to be fairly dense (more than 3.5 g/cm3, assuming that it has no internal strength) and likely composed of nickel–iron. In August 2014, scientists from the University of Tennessee determined that 1950 DA is a rubble pile rotating faster than the breakup limit for its density, implying the asteroid is held together by van der Waals forces rather than gravity.


(29075) 1950 DA, Observations
1950 DA made a distant approach to Earth on 5 February 2021. However, at that time it was half an AU away from Earth, preventing more useful astrometrics and timing that occurs when an object is closer to Earth. The next close approach that presents a good opportunity to observe the asteroid will be on 2 March 2032, when it will be 0.075 AU (11.2 million km) from Earth. The following table lists next five approaches closer than 0.10 AU. By 2136 the close approach solutions are becoming notably more divergent.


(29075) 1950 DA, Possible Earth impact
That 1950 DA has one of the best-determined asteroid orbital solutions is due to a combination of:


(29075) 1950 DA, Possible Earth impact
Main-belt asteroid 78 Diana (~125 km in diameter) will pass about 0.003 AU (450,000 km; 280,000 mi) from 1950 DA on 5 August 2150. At that distance and size, Diana will perturb 1950 DA enough so that the change in trajectory is notable by 2880 (730 years later). In addition, over the intervening time, 1950 DA's rotation will cause its orbit to slightly change as a result of the Yarkovsky effect.


(29075) 1950 DA, Possible Earth impact
If 1950 DA continues on its present orbit, it may approach Earth on 16 March 2880, though the mean trajectory passes many millions of kilometres from Earth, so 1950 DA does not have a significant chance of impacting Earth. As of the 7 December 2015 solution, the probability of an impact in 2880 is 1 in 8,300 (0.012%).


(29075) 1950 DA, Possible Earth impact
The energy released by a collision with an object the size of 1950 DA would cause major effects on the climate and biosphere, which would be devastating to human civilization. The discovery of the potential impact heightened interest in asteroid deflection strategies.


(292220) 2006 SU49
(292220) 2006 SU49, provisional designation 2006 SU49, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group that had a small chance of impacting Earth in 2029.


(292220) 2006 SU49
It was discovered on 20 September 2006, by the Spacewatch project at the University of Arizona using the dedicated 0.9-meter telescope at Kitt Peak National Observatory. The asteroid was calculated to measure 377 meters in diameter with a mass of 7.3×1010 kg.


(292220) 2006 SU49, Description
2006 SU49 had a 1 in 42,000 chance of impacting Earth on 22 January 2029. By 29 October 2006, it was listed with a Torino Scale impact risk value of 0. It was removed from the Sentry Risk Table on 23 November 2006. It is now known that on 28 January 2029, the asteroid will be 0.00818 AU (1,224,000 km; 760,000 mi) from Earth.


(292220) 2006 SU49, Description
It is a near-Earth asteroid that received minor attention in late September and early October 2006 because initial observations indicated a higher than usual probability that it would strike the Earth in 2029. However, the Near-Earth Object (NEO) Office at NASA's Jet Propulsion Laboratory (JPL) removed 2006 SU49 from its risk list as additional observations provided improved predictions that eliminated the possibility of an impact on Earth or the Moon through 2106. Similarly, NEODyS estimates show a zero impact probability through 2080.


(292220) 2006 SU49, Description
2006 SU49 briefly led the Earth-impact hazard list from 27 September 2006 through 4 October 2006, temporarily displacing (144898) 2004 VD17 from the number one position. At the time, both held a Torino scale of level 1 and were the only asteroids to hold a Torino value greater than 0.


(292220) 2006 SU49, Description
Even though 2006 SU49 has an Earth MOID of 0.0003 AU (45,000 km; 28,000 mi), the orbit and future close approaches are well determined with an orbital uncertainty of 0. It is also an Earth-crosser and Mars-crosser asteroid.


(2R)-2-Methylpent-4-enoic acid
(2R)-2-Methylpent-4-enoic acid is an organic acid with the chemical formula C6H10O2. Other names for this molecule include (R)-2-methyl-4-pentenoic acid, (R)-(−)-2-methyl-4-pentenoic acid, and methylallylacetic acid.


(2R)-2-Methylpent-4-enoic acid, Synthesis
(R)-2-Methylpent-4-enoic acid can be synthesized using a chiral auxiliary such an oxazolidinone derivative, popularized by David Evans. One route of synthesis consists of three steps:


(2R)-2-Methylpent-4-enoic acid, Uses
(R)-2-Methylpent-4-enoic acid can also be used in synthesis of other chiral compounds. For example, it has been used in the process of synthesizing the drug Sacubitril as a reagent for adding a chircal center to the molecule


(2R)-3-sulfolactate dehydrogenase (NADP+)
(2R)-3-sulfolactate dehydrogenase (NADP+) (EC , (R)-sulfolactate:NADP+ oxidoreductase, L-sulfolactate dehydrogenase, (R)-sulfolactate dehydrogenase, ComC) is an enzyme with systematic name (2R)-3-sulfolactate:NADP+ oxidoreductase. This enzyme catalyses the following chemical reaction


(2R)-3-sulfolactate dehydrogenase (NADP+)
The enzyme from the bacterium Chromohalobacter salexigens can only utilize NADP+.


(2Z,4Z,6Z,8Z)-Thionine
(2Z,4Z,6Z,8Z)-Thionine or Thionine is an unsaturated heterocycle of nine atoms, with a sulfur replacing a carbon at one position. Thionine is a partially aromatic compound.


(2Z,6Z)-farnesyl diphosphate synthase
(2Z,6Z)-farnesyl diphosphate synthase (EC , cis,cis-farnesyl diphosphate synthase, Z,Z-FPP synthase, zFPS, Z,Z-farnesyl pyrophosphate synthase) is an enzyme with systematic name dimethylallyl-diphosphate:isopentenyl-diphosphate cistransferase (adding 2 isopentenyl units). This enzyme catalyses the following chemical reaction


(3,5-dihydroxyphenyl)acetyl-CoA 1,2-dioxygenase
(3,5-dihydroxyphenyl)acetyl-CoA 1,2-dioxygenase (EC , DpgC) is an enzyme catalyses the following chemical reaction


(3,5-dihydroxyphenyl)acetyl-CoA 1,2-dioxygenase
This enzyme is involved in the biosynthesis of the nonproteinogenic amino acid (S)-3,5-dihydroxyphenylglycine (Dpg) responsible of the production of vancomycin and teicoplanin antibiotics. It catalyzes the unusual conversion 3,5-dihydroxyphenylacetyl-CoA (DPA-CoA) to 3,5-dihydroxyphenylglyoxylate.


(3-Aminopropyl)triethoxysilane
(3-Aminopropyl)triethoxysilane (APTES) is an aminosilane frequently used in the process of silanization, the functionalization of surfaces with alkoxysilane molecules. It can also be used for covalent attaching of organic films to metal oxides such as silica and titania.


(3-Aminopropyl)triethoxysilane, Use with PDMS
APTES can be used to covalently bond thermoplastics to poly(dimethylsiloxane) (PDMS). Thermoplastics are treated with oxygen plasma to functionalize surface molecules, and subsequently coated with an aqueous 1% by volume APTES solution. PDMS is treated with oxygen plasma and placed in contact with the functionalized thermoplastic surface. A stable, covalent bond forms within 2 minutes.


(3-Aminopropyl)triethoxysilane, Silsesquioxane synthesis
Octa(3-aminopropyl)silsesquioxane can be obtained in a one step hydrolytic condensation using APTES and hydrochloric or trifluoromethanesulfonic acid (CF3SO3H).


(3-Aminopropyl)triethoxysilane, Use with cell cultures
APTES-functionalized surfaces have been shown to be nontoxic to embryonic rat cardiomyocytes in vitro. Further experimentation is needed to evaluate toxicity to other cell types in extended culture.


(3-Aminopropyl)triethoxysilane, Toxicity
APTES is a toxic compound with an MSDS health hazard score of 3. APTES fumes are destructive to the mucous membranes and the upper respiratory tract, and should be used in a fume hood with gloves. If a fume hood is not available, a face shield and full face respirator must be implemented. The target organs of APTES are nerves, liver and kidney.


(3-methyl-2-oxobutanoate dehydrogenase (2-methylpropanoyl-transferring))-phosphatase
(3-methyl-2-oxobutanoate dehydrogenase (2-methylpropanoyl-transferring))-phosphatase (EC , branched-chain oxo-acid dehydrogenase phosphatase, branched-chain 2-keto acid dehydrogenase phosphatase, branched-chain alpha-keto acid dehydrogenase phosphatase, BCKDH, [3-methyl-2-oxobutanoate dehydrogenase (lipoamide)]-phosphatase, [3-methyl-2-oxobutanoate dehydrogenase (lipoamide)]-phosphate phosphohydrolase) is an enzyme with systematic name (3-methyl-2-oxobutanoate dehydrogenase (2-methylpropanoyl-transferring))-phosphate phosphohydrolase. This enzyme catalyses the following chemical reaction


(3-methyl-2-oxobutanoate dehydrogenase (2-methylpropanoyl-transferring))-phosphatase
This mitochondrial enzyme is associated with the 3-methyl-2-oxobutanoate dehydrogenase complex.


(300163) 2006 VW139
(300163) 2006 VW139, provisional designations 2006 VW139 and P/2006 VW139, as well as periodic cometary number 288P, is a kilometer-sized asteroid from the outer regions of the asteroid belt and the first "binary main-belt comet" ever discovered.


(300163) 2006 VW139
2006 VW139 belongs to the exclusive class of main-belt comets, which display properties of both comets and asteroids. It is also a synchronous binary system and potentially the slowest rotator known to exist. The object was discovered by Spacewatch in 2006. Its binary nature was confirmed by the Hubble Space Telescope in September 2016. Both primary and its minor-planet moon are similar in mass and size, making it a true binary system. The components are estimated to measure 1.8 kilometers in diameter, orbiting each other at a wide separation of 104 kilometers every 135 days.


(300163) 2006 VW139, Discovery
2006 VW139 was discovered on 15 November 2006, by the Spacewatch survey at Kitt Peak National Observatory near Tucson, Arizona. The possible cometary activity was seen in November 2011 by Pan-STARRS. Both Spacewatch and Pan-STARRS are asteroid survey projects of NASA's Near Earth Object Observations Program. After the Pan-STARRS observations it was also given a comet designation of 288P.


(300163) 2006 VW139, Orbit and classification
2006 VW139 is a non-family asteroid of the main-belt's background population. It is both a binary asteroid and a main-belt comet, also known as "active asteroid". It orbits the Sun in the outer main-belt at a distance of 2.4–3.7 AU once every 5 years and 4 months (1,944 days; semi-major axis of 3.05 AU). Its orbit has an eccentricity of 0.20 and an inclination of 3° with respect to the ecliptic.


(300163) 2006 VW139, Orbit and classification
The body's observation arc begins on September 2000, with a precovery taken by the Sloan Digital Sky Survey at Apache Point Observatory, New Mexico, more than six years prior to its official discovery observation by Spacewatch at Kitt Peak.


(300163) 2006 VW139, Orbit and classification, First binary main-belt comet
2006 VW139 was first observed by the Hubble Space Telescope (HST) in December 2011. It was imaged by HST in September 2016, just before it made its closest approach to the Sun and confirmed its binary nature with two asteroids orbiting each other, and revealed ongoing cometary activity. This makes the object the first known binary asteroid that is also classified as a main-belt comet. The binary is thought to be the result of fission of the precursor caused by YORP-driven spinup.


(300163) 2006 VW139, Orbit and classification, First binary main-belt comet
Observations of the HST revealed ongoing activity in this binary system. The combined features of this binary asteroid - wide separation, near-equal component size, high eccentricity orbit, and comet-like activity also make it unique among the few known binary asteroids that have a wide separation.


(300163) 2006 VW139, Physical characteristics, Diameter albedo and mass
2006 VW139 has a derived diameter of 1.8±0.2 kilometer. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.057 and calculates a diameter of 3.20 kilometers based on an absolute magnitude of 16.2. The binary system has an estimated mass between 1.3×1012 kg and 1.1×1013 kg. A single component has a derived mass of (6.15±4.85)×1012 kg.


(300163) 2006 VW139, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 12 October 2011 (M.P.C. 76600). As of 2020, it has not been named.


(303775) 2005 QU182
(303775) 2005 QU182, also written as (303775) 2005 QU182, is a trans-Neptunian object with a bright absolute magnitude of ca. 3.6. Mike Brown lists it as probably a dwarf planet.


(303775) 2005 QU182, Distance
It came to perihelion in 1971 and is currently 51.8 AU from the Sun. In April 2013, it moved beyond 50 AU from the Sun.


(303775) 2005 QU182, Distance
It has been observed 81 times over 10 oppositions with precovery images back to 1974.


(307261) 2002 MS4
(307261) 2002 MS4 is a large classical Kuiper belt object and a possible dwarf planet in the Kuiper belt, a region of icy planetesimals beyond Neptune. It was discovered in 2002 by Chad Trujillo and Michael Brown. 2002 MS4 has been observed 77 times, with precovery images back to 8 April 1954.


(307261) 2002 MS4
As of 2021, 2002 MS4 is 46.4 AU from the Sun. It will reach perihelion, its closest point to the Sun, in 2123. At approximately 800 km (500 mi) in diameter, it is approximately tied with three other trans-Neptunian objects (to within measurement uncertainties) as the largest unnamed object in the Solar System.


(307261) 2002 MS4, Discovery
2002 MS4 was discovered on 18 June 2002 by Chad Trujillo and Michael Brown in their Caltech Wide Area Sky Survey conducted at Palomar Observatory. The discovery was announced by the Minor Planet Center on 21 November 2002.


(307261) 2002 MS4, Discovery
In 2007, an archive search revealed the existence of several precovery observations of 2002 MS4, the earliest of which was taken on 8 April 1954, as part of the Digitized Sky Survey at Palomar Mountain.


(307261) 2002 MS4, Orbit and classification
2002 MS4 is similar in orbit and current position to Quaoar, although with higher eccentricity and inclination, orbiting every 272.5 years. 2002 MS4 belongs to the class of dynamically hot Kuiper belt objects. It is in an intermittent 18:11 orbital resonance with Neptune.


(307261) 2002 MS4, Observations
As of November 2019, 2002 MS4 has been observed 77 times. With precovery images, it has an observation arc of 66 years.


(307261) 2002 MS4, Observations
In 2008, the Spitzer Space Telescope estimated it to have a diameter of 726±123 km, while the Herschel Space Telescope estimated it to be 934±47 km. If the latter case is true, 2002 MS4 would be comparable in size to the dwarf planet Ceres, and would also be the largest Solar System object without a name as of 2020. 2002 MS4 is one of the 10 largest TNOs currently known and large enough to be considered a dwarf planet under the 2006 draft proposal of the IAU.


(307261) 2002 MS4, Observations
2002 MS4 has measured color indices of B−V=0.69±0.02 and V−R=0.38±0.02, which indicates that it has a neutral (gray) surface color. Per Barucci et al. 's classification scheme for TNO color indices, 2002 MS4 falls under the BB group of TNOs with neutral colors.


(307261) 2002 MS4, Observations, New Horizons
In July 2016, 2002 MS4 was observed by the New Horizons spacecraft, as part of its extended Kuiper belt mission. The observations significantly improved the knowledge of 2002 MS4's orbit and phase curve.


(307261) 2002 MS4, Observations, Occultations
2002 MS4 passes through the Milky Way sky of the constellation Scutum with 7 stellar occultations predicted between 2019 and 2021.


(307261) 2002 MS4, Observations, Occultations
Two stellar occultations by 2002 MS4 were observed from South America and Canada on 9 July and 26 July 2019, both yielding at least two positive detections from participating observers. A negative chord grazing the projected shape of 2002 MS4 on the 9 July event allowed for constraints on its diameter, yielding a best-fit equivalent spherical radius of 770±2 km. In the following month, two observers from Canada recorded another stellar occultation by 2002 MS4 on 19 August 2019. The two positive chords from the event suggested that 2002 MS4 may have an oblate shape, with projected dimensions of 842 × 688 km.


(307261) 2002 MS4, Observations, Occultations
On 8 August 2020, a campaign organized by Lucky Star project successfully observed the occultation of a magnitude 14.6 star with 22 positive detections. The resulting projected dimensions of 2002 MS4 were 808 × 748 km, consistent with the results from the previous year. Topographic features 20 km (12 mi) in depth and height were observed on 2002 MS4's surface.


(307261) 2002 MS4, Observations, Rotation
As of 2019, the rotation period of 2002 MS4 is unknown. Observations in 2005 and 2011 showed possible periods of either 7.33 hours or its alias 10.44 hours (single-peaked), or twice those values for the double-peaked solution, with a small light curve amplitude of 0.05±0.01 mag. Light curve observations of 2002 MS4 are difficult because of the dense field of background stars it is crossing. Observations made in June and July 2011 took advantage of 2002 MS4 moving in front of a dark nebula.


(307261) 2002 MS4, Observations, No known moons
2002 MS4 does not have any known moons orbiting it, thus an accurate mass estimate cannot be made. Based on its size, Brown lists it as nearly certain to be a dwarf planet, however, its low albedo may imply the opposite: dark, mid-sized bodies such as this, less than about 1000 km in diameter and with albedos less than about 0.2, have likely never collapsed into solid bodies, much less differentiated or relaxed into hydrostatic equilibrium, and thus are unlikely to be dwarf planets.


(307463) 2002 VU130
(307463) 2002 VU130, prov. designation: 2002 VU130, is a trans-Neptunian object, located in the circumstellar disc of the Kuiper belt in the outermost region of the Solar System. The resonant trans-Neptunian object belongs to the population of plutinos and measures approximately 253 kilometers (160 miles) in diameter. It was discovered on 7 November 2002, by American astronomer Marc Buie at the Kitt Peak Observatory near Tucson, Arizona. The object has not been named yet.


(307463) 2002 VU130, Orbit and classification
2002 VU130 is a plutino, a population of objects in the Kuiper belt that stay in a 2:3 resonance with Neptune. A large part of the inner Kuiper belt is formed by objects belonging to this population which is named after its largest member, Pluto. 2002 VU130 orbits the Sun at a distance of 30.9–47.1 AU once every 243 years and 9 months (89,021 days; semi-major axis of 39.02 AU). Its orbit has an eccentricity of 0.21 and an inclination of 1° with respect to the ecliptic. The body's observation arc begins with its official discovery observation on 7 November 2002. It is currently approaching the Sun at 39.428 AU, with its perihelion-passage projected to occur in June 2076.


(307463) 2002 VU130, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 10 December 2011 (M.P.C. 77418). As of 2021, it has not been named. If named, it will follow the already established scheme of naming these objects after mythological entities associated with the underworld.


(307463) 2002 VU130, Physical characteristics, Diameter and albedo
Observations with Herschel's PACS instrument were published in 2011. For 2002 VU130, the measurements gave a mean-diameter of 252.9+33.6−31.3 km with an unusually high albedo of 0.179+0.202−0.103 and an absolute magnitude of 5.47±0.83. This result has been adopted in Johnston's Archive, giving a rounded diameter of 253 kilometers (160 miles), while Mike Brown estimates as similar one of 260 km with an albedo of 0.18 and an absolute magnitude of 5.5.


(308193) 2005 CB79
(308193) 2005 CB79 is a trans-Neptunian object that is a member of the Haumea family.


(308193) 2005 CB79, Haumea family
As a member of the Haumea family, (308193) 2005 CB79 is suspected of being an icy mantle collisional fragment from dwarf planet Haumea. With an absolute magnitude (H) of 4.7, and a Haumea-family albedo of 0.7, this object would have a diameter of 158 km.


(308193) 2005 CB79, Haumea family
Observations by Mike Brown in 2012 using the W. M. Keck Observatory suggest that (308193) 2005 CB79 does not have a companion.


(308242) 2005 GO21
(308242) 2005 GO21 is a large Aten near-Earth asteroid and potentially hazardous object. It has a well determined orbit with an observation arc of 7 years and an uncertainty parameter of 0. It was discovered on 1 April 2005 by the Siding Spring Survey at an apparent magnitude of 18.1 using the 0.5-metre (20 in) Uppsala Southern Schmidt Telescope.


(308242) 2005 GO21
Based on an absolute magnitude of 16.4, the asteroid has an estimated diameter of 1.6 km (within a factor of two). (308242) 2005 GO21 is the largest potentially hazardous asteroid (PHA) discovered in 2005. On 21 June 2012 it passed Earth at a distance of 0.043963 AU (6,576,800 km; 4,086,600 mi). The 2012 passage was studied with radar using Goldstone and Arecibo.


(308635) 2005 YU55
(308635) 2005 YU55, provisionally named 2005 YU55,  is a potentially hazardous asteroid 360±40 meters in diameter, as measured after its Earth flyby. Previously it was estimated to be 310 meters or about 400 m (1,300 feet) in diameter. It was discovered on 28 December 2005 by Robert S. McMillan at Steward Observatory, Kitt Peak. On 8 November 2011 it passed 0.85 lunar distances (324,900 kilometers; 201,900 miles) from Earth.


(308635) 2005 YU55, 8 November 2011 flyby
In February 2010, (308635) 2005 YU55 was rated 1 on the Torino Scale for a potential pass near Earth on 10 November 2103, that posed no unusual level of danger. On 19 April 2010, radar ranging by the Arecibo radio telescope reduced uncertainties about the orbit by 50%. This improvement eliminated any possibility of an impact with Earth within the next 100 years. It was removed from the Sentry Risk Table on 22 April 2010 and as such it now has a rating of 0 on the Torino Scale. It is now known that on 10 November 2103 (308635) 2005 YU55 will be roughly 2 AU from Earth.


(308635) 2005 YU55, 8 November 2011 flyby
On 8 November 2011 at 23:28 UT the asteroid passed 0.85 LD (330,000 km; 200,000 mi) from Earth. On 9 November 2011 at 07:13 UT the asteroid passed 0.6231 LD (239,500 km; 148,800 mi) from the Moon. During the close approach the asteroid reached about apparent magnitude 11, and would have been visible to experienced observers using high-end binoculars with an objective lens of 80+ mm if it were not for bright moonlight preventing a true dark sky. Since the gibbous moon did interfere with the viewing, observers trying to visually locate the asteroid required a telescope with an aperture of 6 inches (15 centimeters) or larger.


(308635) 2005 YU55, 8 November 2011 flyby
The next few times a known asteroid this large will come this close to Earth will be in 2028 when (153814) 2001 WN5 passes 0.65 LD from Earth, and in 2029 when the 325-meter 99942 Apophis comes even closer at just 0.10 LD.


(308635) 2005 YU55, 8 November 2011 flyby
According to Jay Melosh, if an asteroid the size of (308635) 2005 YU55 (~400 m across) were to hit land, it would create a crater 6.3 km (3.9 mi) across, 518 m (1,699 ft) deep and generate a seven-magnitude-equivalent-earthquake. The chances of an actual collision with an asteroid like (308635) 2005 YU55 is about 1 percent in the next thousand years.


(308635) 2005 YU55, Study
During the 2011 passage (308635) 2005 YU55 was studied with radar using Goldstone, Arecibo, the Very Long Baseline Array, and the Green Bank Telescope. The Herschel Space Observatory has made far-infrared measurements of (308635) 2005 YU55 on 10 November, helping determine its temperature and composition.


(308635) 2005 YU55, Study
Radar analysis has also helped to pin down the asteroid's albedo, or diffuse reflectivity. Although radar measurements do not detect visible light they can determine the distance and size of an object with a high degree of accuracy. This information, coupled with visible light measurements, provides a more accurate measure of an object's absolute magnitude, and therefore its albedo.


(308635) 2005 YU55, Study
On 8 November 2011, NASA released a statement mentioning a number of structures on the surface of the asteroid, which were detected as it passed near Earth. On 11 November 2011, higher-resolution images showed concavities, a ridge near the asteroid's equator, and numerous features interpreted as decameter-scale boulders. Shape modeling based on the radar images shows that YU55's shape is close to spheroidal, with maximum dimensions of 360±40 m, and an equator-aligned ridge. A 150–200 meter-long, ~20 meter-high rise forms a portion of the ridge-line, and the number of boulders on the surface is comparable to that seen on the asteroid 25143 Itokawa by the Hayabusa spacecraft.


(308635) 2005 YU55, Study
Optical lightcurve measurements during the flyby provided a more accurate estimate of the asteroid's spin period –  about 19.3 hours. Because (308635) 2005 YU55 is so nearly spheroidal, it was not significantly torqued by Earth's tides during the flyby, and there is no evidence of non-principal-axis rotation. Optical, near-infrared, and ultraviolet spectroscopy confirmed that 2005 YU55 is a C-type asteroid.


(308635) 2005 YU55, Future trajectory
On 19 January 2029, (308635) 2005 YU55 will pass 0.0023 AU (340,000 km; 210,000 mi) from Venus. The close approach distance to Venus in 2029 will determine how close the asteroid will pass to Earth in 2041. Before the November 2011 observations, the uncertainties in the post-2029 trajectory showed that the asteroid would pass somewhere between 0.002 AU (300,000 km; 190,000 mi) and 0.3 AU (45,000,000 km; 28,000,000 mi) of Earth in 2041. Radar astrometry in November 2011 clarified the Earth passage in 2041 and beyond.


(308635) 2005 YU55, Future trajectory
As a result of the November 2011 radar observations, it is now known that (308635) 2005 YU55 will pass between 0.1017 AU (15,210,000 km; 9,450,000 mi) and 0.1020 AU of Earth on 12 November 2041. Using the current uncertainty region integrated until the future, the 2075 approach will be between 0.0013 AU (190,000 km; 120,000 mi) and 0.0021 AU (310,000 km; 200,000 mi).


(308933) 2006 SQ372
(308933) 2006 SQ372 is a trans-Neptunian object and highly eccentric centaur on a cometary-like orbit in the outer region of the Solar System, approximately 123 kilometers (76 miles) in diameter. It was discovered through the Sloan Digital Sky Survey by astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica on images first taken on 27 September 2006 (with precovery images dated to 13 September 2005).


(308933) 2006 SQ372, Characteristics
It has a highly eccentric orbit, crossing that of Neptune near perihelion but bringing it more than 1,500 AU from the Sun at aphelion. It takes about 22,500 years to orbit the barycenter of the Solar System. The large semi-major axis makes it similar to 2000 OO67 and Sedna. With an absolute magnitude (H) of 8.1, it is estimated to be about 60 to 140 km in diameter. Michael Brown estimates that it has an albedo of 0.08 which would give a diameter of around 110 km.


(308933) 2006 SQ372, Characteristics
The object could possibly be a comet. The discoverers hypothesize that the object could come from the Hills cloud, but other scientists like California Institute of Technology's Michael Brown also consider other possibilities, including the theory "it may have formed from debris just beyond Neptune [in the Kuiper belt] and been 'kicked' into its distant orbit by a planet like Neptune or Uranus".


(308933) 2006 SQ372, Perturbation
The orbit of 2006 SQ372 currently comes closer to Neptune than any of the other giant planets. More than half of the simulations of this object show that it gets too close to either Uranus or Neptune within the next 180 million years, sending it in a currently unknown direction. This makes it difficult to classify this object as only a centaur or a scattered disc object. The Minor Planet Center, which officially catalogues all trans-Neptunian objects, lists centaurs and SDOs together. (29981) 1999 TD10 is another such object that blurs the two categories.


(308933) 2006 SQ372, Perturbation
Given the extreme orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the aphelion distance (maximum distance) of this object. With a 2005 epoch the object had an approximate period of about 22,000 years with aphelion at 1557 AU. But using a 2011 epoch shows a period of about 32,000 years with aphelion at 2006 AU. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates. Using JPL Horizons with an observed orbital arc of only 2.9 years, the barycentric orbital elements for epoch 2008-May-14 generate a semi-major axis of 796 AU and a period of 22,466 years.


(309239) 2007 RW10
(309239) 2007 RW10, provisionally known as 2007 RW10, is a temporary quasi-satellite of Neptune. Observed from Neptune, it would appear to go around it during one Neptunian year but it actually orbits the Sun, not Neptune.


(309239) 2007 RW10, Discovery, orbit and physical properties
(309239) 2007 RW10 was discovered by the Palomar Distant Solar System Survey on September 9, 2007, with precovery images from 1988 (also taken at Palomar). At the time of discovery, this minor body was believed to be a Neptune trojan, but it is no longer listed as such. The Jet Propulsion Laboratory classifies (309239) 2007 RW10 as trans-Neptunian object butthe Minor Planet Center includes the object among centaurs. It movesin an orbit with an inclination of 36.2°, a semi-major axis of 30.18 AU, and an eccentricity of 0.3020. Herschel-PACS observations indicate that it has a diameter of 247 km.


(309239) 2007 RW10, Quasi-satellite dynamical state and orbital evolution
(309239) 2007 RW10 is currently following a quasi-satellite loop around Neptune. It has been a quasi-satellite of Neptune for about 12,500 years and it will remain in that dynamical state for another 12,500 years. Prior to the quasi-satellite dynamical state, (309239) 2007 RW10 was an L5 trojan and it will go back to that state soon after leaving its current quasi-satellite orbit. Its orbital inclination is the largest among known Neptune co-orbitals. It is also possibly the largest known object trapped in the 1:1 mean-motion resonance with any major planet.


(309239) 2007 RW10, Origin
(309239) 2007 RW10 is a dynamically hot (both, high eccentricity and inclination) object that isunlikely to be a primordial Neptune co-orbital. It probably originated well beyond Neptune and waslater temporarily captured in the 1:1 commensurability with Neptune.


(310071) 2010 KR59
(310071) 2010 KR59, provisional designation 2010 KR59, is a trans-Neptunian object, approximately 110 kilometers in diameter. The object is trapped in a 1:1 mean motion resonance with Neptune, and rotates nearly every 9 hours around its axis.


(310071) 2010 KR59, Discovery
(310071) 2010 KR59 was discovered on May 18, 2010 at 7:45 UT by the WISE spacecraft. The WISE telescope scanned the entire sky in infrared light from January 2010 to February 2011.


(310071) 2010 KR59, Orbit
(310071) 2010 KR59 follows a very eccentric orbit (eccentricity of 0.57) with a semi-major axis of 29.97 AU and an inclination of 19.76º. Its aphelion goes into the trans-neptunian belt but its perihelion is relatively close to Saturn's orbit.


(310071) 2010 KR59, Physical properties
(310071) 2010 KR59 is a rather large minor body with an absolute magnitude of7.7 that translates into a diameter close to 100 kilometers. The discovering WISE/NEOWISE mission estimates a diameter of 110.060 kilometers with a large error margin of 30.820 km.


(310071) 2010 KR59, Co-orbital with Neptune
(310071) 2010 KR59 follows a complicated and short-lived horseshoe orbit around Neptune. Classical horseshoe orbits include the Lagrangian points L3, L4 and L5, this object horseshoe path goes from the L4 point towards Neptune reaching the L5 point and back. It will become a quasi-satellite of Neptune in about 5,000 years.


(311999) 2007 NS2
(311999) 2007 NS2 is an asteroid and Mars trojan orbiting near the L5 point of Mars.


(311999) 2007 NS2, Discovery, orbit and physical properties
(311999) 2007 NS2 was discovered on 14 July 2007, by the Observatorio Astronómico de La Sagra. Its orbit is characterized by low eccentricity (0.054), moderate inclination (18.6°) and a semi-major axis of 1.52 AU. Upon discovery, it was classified as Mars-crosser by the Minor Planet Center. Its orbit is well determined as it is currently (March 2013) based on 87 observations with a data-arc span of 4,800 days. 2007 NS2 has an absolute magnitude of 17.8, which gives a characteristic diameter of 870 m.


(311999) 2007 NS2, Mars trojan and orbital evolution
Jean Meeus suspected that (311999) 2007 NS2 was a Mars Trojan, and this was confirmed by Reiner Stoss's analysis of two sets of observations dating from 1998 on the MPC database. It was confirmed to be a Mars Trojan numerically in 2012. Recent calculations confirm that it is a stable L5 Mars Trojan asteroid with a libration period of 1310 years and an amplitude of 14°. These values as well as its short-term orbital evolution are similar to those of 5261 Eureka. Out of all known Mars Trojans, it currently has the smallest relative (to Mars) semimajor axis, 0.000059 AU.


(311999) 2007 NS2, Origin
Long-term numerical integrations show that its orbit is very stable on Gyr time-scales (1 Gyr = 1 billion years). As in the case of Eureka, calculations in both directions of time (4.5 Gyr into the past and 4.5 Gyr into the future) indicate that (311999) 2007 NS2 may be a primordial object, perhaps a survivor of the planetesimal population that formed in the terrestrial planets region early in the history of the Solar System.


(31345) 1998 PG
(31345) 1998 PG is an eccentric, stony asteroid and binary system, classified as near-Earth object of the Amor group of asteroids, approximately 900 meters in diameter. It minor-planet moon, S/2001 (31345) 1, has an estimated diameter of 270 meters.


(31345) 1998 PG
This asteroid was discovered on 3 August 1998, by the Lowell Observatory Near-Earth-Object Search (LONEOS) at Anderson Mesa Station, near Flagstaff, Arizona, United States.


(31345) 1998 PG, Orbit
1998 PG orbits the Sun at a distance of 1.2–2.8 AU once every 2 years and 10 months (1,046 days). Its orbit has an eccentricity of 0.39 and an inclination of 7° with respect to the ecliptic. A first precovery was taken at Palomar Observatory in 1978, extending the body's observation arc by 20 years prior to its official discovery observation at Anderson Mesa.


(31345) 1998 PG, Orbit, Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.2354 AU (35,200,000 km), which translates into approximately 92 lunar distances. It has made multiple close approaches to Earth, with the closest being 35,648,680 kilometers on 15 October 1978. With an aphelion of more than 2.8 AU, 1998 PG is also a Mars-crosser.


(31345) 1998 PG, Physical characteristics, Spectral type
In the SMASS taxonomy, 1998 PG is classified as a transitional Sq-type, which is an intermediary between the common stony S-type and the less frequent Q-type asteroids.


(31345) 1998 PG, Physical characteristics, Diameter and albedo
According to the 2006-published Photometric survey of binary near-Earth asteroids by Petr Pravec and derived data from the Collaborative Asteroid Lightcurve Link and the "Johnston's archive", 1998 PG measures between 880 and 940 meters in diameter and its surface has an albedo of 0.18 and 0.20, respectively.


(31345) 1998 PG, Physical characteristics, Rotation
In the late 1990s, a rotational lightcurve of 1998 PG was obtained from photometric observations by Hungarian astronomers László Kiss, Gyula Szabó and Krisztián Sárneczky. Lightcurve analysis gave a rotation period of 2.5 hours with a brightness variation of 0.1 magnitude (U=n.a. ).


(31345) 1998 PG, Physical characteristics, Rotation
A second lightcurve obtained and published in 2000, by an international collaboration of astronomers gave a rotation period of 2.51620±0.00003 hours with a brightness amplitude of 0.11 magnitude (U=2).


(31345) 1998 PG, Moon
During the second photometric observation, it was discovered that 1998 PG is a probable/possible asynchronous binary system with a minor-planet moon orbiting it every 7.0035	hours, or twice this period solution.


(31345) 1998 PG, Moon
The moon's provisional designation is S/2001 (31345) 1. The system has an estimated secondary-to-primary mean-diameter ratio of more than 0.3, which translates into a diameter of 270 meter for the satellite. The "Johnston's archive" also estimates that the moon's orbit has a semi-major axis of 1.4 kilometers.


(31345) 1998 PG, Moon
From the surface of 1998 PG, the moon would have an angular diameter of about 16.3°. For comparison, the Sun appears to be 0.5° from Earth.


(31345) 1998 PG, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 30 November 2001. As of 2018, it has not been named.


(315530) 2008 AP129
(315530) 2008 AP129 is a trans-Neptunian object and possibly a cubewano from the outermost regions of the Solar System, approximately 480 kilometers in diameter. It was discovered on 11 January 2008, by American Michael E. Brown and Megan Schwamb at Palomar Observatory in California.


(315530) 2008 AP129, Description
2008 AP129 orbits the Sun at a distance of 36.1–47.6 AU once every 270 years and 5 months (98,778 days; semi-major axis of 41.8 AU). Its orbit has an eccentricity of 0.14 and an inclination of 27° with respect to the ecliptic. It has 3 precovery observations back to 1989. Lightcurve analysis gave an ambiguous rotation period of 9.04 hours with a brightness amplitude of 0.12 magnitude (U=2). Michael Brown considers it a probable dwarf planet with an estimated diameter of 496 kilometers and albedo of 0.07. 2008 AP129 has been identified as a member of the Haumea family in a dynamical study led by Proudfoot and Ragozzine in 2019.


(315530) 2008 AP129, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 7 February 2012. As of 2018, it has not been named.


(315898) 2008 QD4
(315898) 2008 QD4, prov. designation: 2008 QD4, is a centaur orbiting in the outer Solar System with a perihelion greater than Jupiter and a semi-major axis less than Saturn.


(315898) 2008 QD4, Perihelion
2008 QD4 is listed as a centaur by the Minor Planet Center, Jet Propulsion Laboratory, and the Deep Ecliptic Survey (DES). Of numbered objects listed as a centaur by all 3 major institutions, (315898) 2008 QD4 has the smallest perihelion distance.


(316179) 2010 EN65
(316179) 2010 EN65 is a trans-Neptunian object orbiting the Sun. However, with a semi-major axis of 30.8 AU, the object is actually a jumping Neptune trojan, co-orbital with Neptune, as the giant planet has a similar semi-major axis of 30.1 AU. The body is jumping from the Lagrangian point L4 into L5 via L3. As of 2016, it is 54 AU from Neptune. By 2070, it will be 69 AU from Neptune.


(316179) 2010 EN65, Discovery
(316179) 2010 EN65 was discovered on 7 March 2010, by David L. Rabinowitz and Suzanne W. Tourtellotte using the 1.3-meter Small and Medium Research Telescope System (SMARTS) at Cerro Tololo Observatory in Chile.


(316179) 2010 EN65, Orbit
2010 EN65 follows a rather eccentric orbit (0.31) with a semi-major axis of 30.72 AU and an inclination of 19.3º. Its orbit is well determined with images dating back to 1989.


(316179) 2010 EN65, Physical properties
2010 EN65 is a quite large minor body with an absolute magnitude of 7.17 and an estimated diameter of 176 kilometers (109 miles) based on an assumed albedo of 0.08.


(316179) 2010 EN65, Jumping trojan
2010 EN65 is another co-orbital of Neptune, the second brightest after the quasi-satellite (309239) 2007 RW10. 2010 EN65 is currently transitioning from librating around Lagrangian point L4 to librating around L5. This unusual trojan-like behavior is termed "jumping trojan".


(316179) 2010 EN65, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 7 February 2012 (M.P.C. 78220). As of 2021, it has not been named. If named, it will follow the naming scheme already established with 385571 Otrera and 385695 Clete, which is to name these objects after figures related to the Amazons, an all-female warrior tribe that fought in the Trojan War on the side of the Trojans against the Greek.


(31669) 1999 JT6
(31669) 1999 JT6 is an Earth-crossing asteroid belonging to the Apollo family of asteroids which also crosses the orbit of Mars. 1999 JT6 is the asteroid's temporary discovery name. It has now been assigned a permanent number from the Minor Planet Center (31669) indicating that its orbit has been confirmed, but has not (at least so far) been assigned a name. Only a small fraction of asteroids have been named.


(31669) 1999 JT6
It has an Earth minimum orbit intersection distance of 0.00354 AU (328,978 miles), which is close enough to classify it as a Potentially Hazardous Asteroid (PHA). It will make a close approach to Earth on 14 December 2076 at 0.0260 AU (2,506,321 miles) and an even closer approach to the minor planet Ceres on 16 Feb 2084 at 0.0171 AU (1,587,064 miles).


(322756) 2001 CK32
(322756) 2001 CK32 is a sub-kilometer asteroid and near-Earth object of the Aten group. It is also a transient Venus co-orbital, and a Mercury grazer as well as an Earth crosser. It was once designated as a potentially hazardous asteroid.


(323137) 2003 BM80
(323137) 2003 BM80, provisional designation 2003 BM80 and cometary designation 282P, is an asteroid and main-belt comet from the outer regions of the asteroid belt, approximately 4 kilometers in diameter. It was discovered on 31 January 2003, by astronomers of the LONEOS program conducted at Anderson Mesa Station near Flagstaff, Arizona, in the United States.


(323137) 2003 BM80, Orbit and classification
2003 BM80 is a main-belt comet with a Jupiter Tisserand's parameter of 2.99. It orbits the Sun in the outer asteroid belt at a distance of 3.4–5.1 AU once every 8 years and 9 months (3,199 days; semi-major axis of 4.25 AU). Its orbit has an eccentricity of 0.19 and an inclination of 6° with respect to the ecliptic.


(323137) 2003 BM80, Orbit and classification
The body's observation arc begins with its first precovery observation by the NEAT program in December 2001, more than a year prior to its official discovery observation at Anderson Mesa.


(323137) 2003 BM80, Physical characteristics
Based on a generic magnitude-to-diameter conversion, 2003 BM80 measures approximately 4.4 kilometers in diameter using an absolute magnitude of 15.3 and an estimated albedo 0.07, typical for rather dark cometary-like bodies.


(323137) 2003 BM80, Physical characteristics
As of 2018, no rotational lightcurve of 2003 BM80 has been obtained from photometric observations. The body's rotation period, shape and spin axis remain unknown.


(323137) 2003 BM80, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 6 April 2012. As of 2018, it has not been named.


(32496) 2000 WX182
(32496) 2000 WX182, provisional designation 2000 WX182, is a Jupiter trojan from the Trojan camp, approximately 50 kilometers (31 miles) in diameter. It was discovered on 18 November 2000, by astronomers with the LINEAR program at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The dark Jovian asteroid belongs the 100 largest Jupiter trojans and has a rotation period of 23.3 hours. It has not been named since its numbering in November 2001.


(32496) 2000 WX182, Orbit and classification
2000 WX182 is a Jupiter trojan in a 1:1 orbital resonance with Jupiter. It is located in the trailering Trojan camp at the Gas Giant's L5 Lagrangian point, 60° behind its orbit (see Trojans in astronomy). It is also a non-family asteroid of the Jovian background population. It orbits the Sun at a distance of 4.9–5.7 AU once every 12 years and 1 month (4,419 days; semi-major axis of 5.27 AU). Its orbit has an eccentricity of 0.08 and an inclination of 30° with respect to the ecliptic.


(32496) 2000 WX182, Orbit and classification
The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken at Palomar Observatory in January 1955, more than 45 years prior to its official discovery observation at Socorro.


(32496) 2000 WX182, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 30 November 2001 (M.P.C. 44050). As of 2018, it has not been named.


(32496) 2000 WX182, Physical characteristics
2000 WX182 is an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical V–I color index of 0.95 and a BR color of 1.23 (also see table below).


(32496) 2000 WX182, Physical characteristics, Rotation period
In November 2013, a rotational lightcurve of 2000 WX182 was obtained from eleven nights of photometric observations by Robert Stephens at the Center for Solar System Studies in Landers, California. Lightcurve analysis gave a rotation period of 23.34±0.01 hours with a brightness amplitude of 0.19 magnitude (U=3-).


(32496) 2000 WX182, 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, 2000 WX182 measures 48.02 and 51.63 kilometers in diameter and its surface has an albedo of 0.070 and 0.080, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 50.77 kilometers based on an absolute magnitude of 10.2.


(32496) 2000 WX182, 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.


(33001) 1997 CU29
(33001) 1997 CU29, also written as (33001) 1997 CU29 is a cold classical Kuiper belt object, or cubewano. It has a perihelion (closest approach to the Sun) at 41.6 AU and an aphelion (farthest approach from the Sun) of 45.1 AU. 1997 CU29 is about 280 km in diameter. It was discovered on February 6, 1997, by David C. Jewitt, Jane X. Luu, Chad Trujillo, and Jun Chen at the Mauna Kea Observatory, Hawaii.


(332446) 2008 AF4
(332446) 2008 AF4 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, which was listed on the Sentry Risk Table in January 2008 with a Torino Scale rating of 1. The asteroid showed a 1 in 71,000 chance of impact on 9 January 2089. It was briefly downgraded to Torino Scale 0 in February 2008, but still showed a cumulative 1 in 53,000 chance of an impact. In March it was back at Torino Scale 1 with a 1 in 28,000 chance of impact on 9 January 2089. By mid April 2008, it was back to Torino Scale 0. It was removed from the Sentry Risk Table on 19 December 2009.


(332446) 2008 AF4, 2183 passage
2008 AF4 may pass as close as 0.002 AU (300,000 km; 190,000 mi) from Earth on 12 January 2183. But the nominal solution shows the asteroid passing 0.009 AU (1,300,000 km; 840,000 mi) from Earth.


(33340) 1998 VG44
(33340) 1998 VG44, also written as (33340) 1998 VG44, is a trans-Neptunian object. It has a 2:3 orbital resonance with the planet Neptune, similar to Pluto, classifying it as a plutino. Its average distance from the Sun is 39.083 AU with a perihelion of 29.354 AU and an aphelion at 48.813 AU. Its orbit has an eccentricity of 0.249, and is inclined by 3°. It is about 221 km in diameter, so it is unlikely to be classified as a dwarf planet. It was discovered on November 14, 1998, by J. A. Larsen, Nicole M. Danzl and A. Gleason at the Steward Observatory.


(33342) 1998 WT24
(33342) 1998 WT24 is a bright, sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid (PHA) of the Aten group, located in Venus's zone of influence that has frequent close encounters with Mercury, Venus, and Earth. It made a close approach to Earth on 11 December 2015, passing at a distance of about 4.2 million kilometers (2.6 million miles, 11 lunar distances) and reaching about apparent magnitude 11.


(33342) 1998 WT24
The asteroid was discovered on 25 November 1998 by LINEAR about four months after a close encounter with the planet Mercury (about 0.047 AU). It measures approximately 400 meters in diameter. It is also one of the best studied PHAs and was the 10th Aten asteroid to be numbered.


(33342) 1998 WT24, Classification and orbit
1998 WT24 orbits the Sun at a distance of 0.42–1.02 AU once every 7 months (222 days; semi-major axis of 0.72 AU). Its orbit has an eccentricity of 0.42 and an inclination of 7° with respect to the ecliptic.


(33342) 1998 WT24, Classification and orbit, Low aphelion
At the time of its discovery, astronomers were trying to find the first Apohele asteroid (one that is always closer to the Sun than Earth). All asteroids known at the time that got closer to the Sun than Earth also crossed Earth's orbit. Earlier that year, David J. Tholen claimed to have spotted the first Apohele asteroid, which was dubbed 1998 DK36. However, the object was lost without being confirmed. Thus, 1993 DA remained the asteroid with the lowest known aphelion at 1.023 AU.


(33342) 1998 WT24, Classification and orbit, Low aphelion
When 1998 WT24 was discovered, it was found to have a slightly smaller aphelion (1.019 AU) than 1993 DA, and was thus the closest thing to an Apohele asteroid known at the time. It lost its smallest aphelion title almost immediately when (415713) 1998 XX2 was discovered only a few weeks later (aphelion = 1.014 AU). Asteroids with even smaller aphelions were discovered until February 2003, when finally, an asteroid with an aphelion smaller than 1.000 AU was discovered. This was 163693 Atira, the first confirmed Apohele asteroid.


(33342) 1998 WT24, Classification and orbit, Venus zone of influence
1998 WT24 was the second asteroid discovered to be close enough to Venus as to be within the major planet's zone of influence. It is located at about the inner edge of the zone, while (99907) 1989 VA, the first asteroid discovered there, is at about the outer edge. It is possible for planets to capture asteroids located in their sphere of influences into co-orbital relationships such as Trojan and horseshoe asteroids. Because of its frequent close encounters with Mercury and Earth, however, it may prove difficult for Venus to keep 1998 WT24 in a co-orbital relationship for any length of time. Of the six objects in Venus's zone of influence, only one (2002 VE68) is currently a co-orbital.