(+)-Naloxone, Relation of TLR4 to opioid drugs
Both "normal" and "unnatural" enantiomers of various opioid analgesic drugs including morphine, meperidine, fentanyl, methadone and buprenorphine, as well as some otherwise inactive metabolites like morphine-3-glucuronide, have been found to act as agonists of TLR4, and chronic use of these drugs consequently causes constant low-level release of TNF-α and IL-1β as well as other downstream effects.


(+)-Naloxone, Relation of TLR4 to opioid drugs
This is thought to be involved in various adverse properties of opioid analgesic drugs, such as loss of efficacy with extended use and the associated development of tolerance and dependence, as well as the development of side effects such as hyperalgesia and allodynia, which can cause long-term use of opioid analgesics to not only fail to treat neuropathic pain, but ultimately exacerbate it.


(+)-Naloxone, Applications of (+)-naloxone and related drugs
Several opioid antagonist drugs were found to act as antagonists for TLR4, including naloxone and naltrexone. However it was found that not only the "normal" (-) enantiomers, but also the "unnatural" (+) enantiomers of these drugs acted as TLR4 antagonists (though (+)-nalmefene was inactive). Since (+)-naloxone and (+)-naltrexone lack affinity for opioid receptors, they do not block the effects of opioid analgesic drugs, and so can be used to counteract the TLR4-mediated side effects of opioid agonists without affecting analgesia, though (+)-naloxone does reduce the reinforcing effects of opioid drugs.


(+)-Naloxone, Applications of (+)-naloxone and related drugs
(+)-Naloxone was also found to be neuroprotective, and both (+)-naloxone and (+)-naltrexone are effective in their own right at treating symptoms of neuropathic pain in animal models. However (+)-naloxone was also found to reduce the effects of stimulant drugs, suggesting additional actions beyond TLR4 antagonism (possibly as a sigma receptor antagonist), that might potentially result in unwanted side effects or drug interactions.


(+)-Pulegone reductase
(+)-pulegone reductase (EC ) is an enzyme with systematic name (-)-menthone:NADP+ oxidoreductase. This enzyme catalises the following chemical reaction


(+)-Sabinene 3-hydroxylase
(+)-Sabinene 3-hydroxylase (EC ) is an enzyme with systematic name (+)-sabinene,NADPH:oxygen oxidoreductase (3-hydroxylating). This enzyme catalyses the following chemical reaction


(+)-T-muurolol synthase
(+)-T-muurolol synthase (EC ) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase (cyclizing, (+)-T-muurolol-forming). This enzyme catalyses the following chemical reaction


(+)-Thujan-3-ol dehydrogenase
(+)-Thujan-3-ol dehydrogenase (EC , d-3-thujanol dehydrogenase, TDH) is an enzyme with systematic name (+)-thujan-3-ol:NAD(P)+ oxidoreductase. This enzyme catalyses the following chemical reaction


(+)-abscisic acid 8'-hydroxylase
In enzymology, a (+)-abscisic acid 8'-hydroxylase (EC ) is an enzyme that catalyzes the chemical reaction


(+)-abscisic acid 8'-hydroxylase
The four substrates of this enzyme are (+)-abscisate, NADPH, H+, and O2, whereas its three products are 8'-hydroxy-abscisate, NADP+, and H2O.


(+)-abscisic acid 8'-hydroxylase
This enzyme belongs to the family of oxidoreductases, to be specific those acting on paired donors, with O2 as oxidant and incorporation or reduction of oxygen. The oxygen incorporated need not be derived from O2 with NADH or NADPH as one donor, and incorporation of one atom of oxygen into the other donor. This enzyme participates in carotenoid biosynthesis.


(+)-abscisic acid 8'-hydroxylase, Nomenclature
The systematic name of this enzyme class is abscisate,NADPH:oxygen oxidoreductase (8'-hydroxylating). Other names in common use include


(+)-alpha-barbatene synthase
(+)-alpha-barbatene synthase (EC , AtBS) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase ((+)-alpha-barbatene-forming). This enzyme catalyses the following chemical reaction


(+)-alpha-barbatene synthase
The recombinant enzyme from the plant Arabidopsis thaliana produces alpha-barbatene, thujopsene and beta-chamigrene.


(+)-alpha-pinene synthase
(+)-alpha-pinene synthase (EC , (+)-alpha-pinene cyclase, cyclase I) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (+)-alpha-pinene-forming). This enzyme catalyses the following chemical reaction


(+)-alpha-pinene synthase
Cyclase I of Salvia officinalis (sage) gives about equal parts (+)-alpha-pinene and (+)-camphene.


(+)-alpha-santalene synthase ((2Z,6Z)-farnesyl diphosphate cyclizing)
(+)-alpha-santalene synthase ((2Z,6Z)-farnesyl diphosphate cyclizing) (EC , SBS) is an enzyme with systematic name (2Z,6Z)-farnesyl diphosphate lyase (cyclizing; (+)-alpha-santalene-forming). This enzyme catalyses the following chemical reaction


(+)-alpha-santalene synthase ((2Z,6Z)-farnesyl diphosphate cyclizing)
The enzyme synthesizes a mixture of sesquiterpenoids from (2Z,6Z)-farnesyl diphosphate.


(+)-alpha-terpineol synthase
(+)-alpha-terpineol synthase (EC ) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (+)-alpha-terpineol-forming). This enzyme catalyses the following chemical reaction


(+)-beta-caryophyllene synthase
(+)-beta-caryophyllene synthase (EC , GcoA) is an enzyme with systematic name (2Z,6E)-farnesyl-diphosphate diphosphate-lyase (cyclizing, (+)-beta-caryophyllene-forming). This enzyme catalyses the following chemical reaction:


(+)-beta-pinene synthase
(+)-beta-pinene synthase (EC , (+)-pinene cyclase, cyclase III) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase ((+)-beta-pinene-forming). This enzyme catalyses the following chemical reaction


(+)-beta-pinene synthase
Cyclase III from Salvia officinalis (sage) gives roughly equal parts of (+)-beta-pinene and (+)-alpha-pinene.


(+)-borneol dehydrogenase
In enzymology, a (+)-borneol dehydrogenase (EC ) is an enzyme that increases the rate of, or catalyzes, the chemical reaction


(+)-borneol dehydrogenase
Thus, the two substrates of this enzyme are (+)-borneol and NAD+, whereas its 3 products are (+)-camphor, NADH, and H+.


(+)-borneol dehydrogenase
This enzyme belongs to the family of oxidoreductases, specifically those acting on the CH-OH group of donor with NAD+ or NADP+ as acceptor. The systematic name of this enzyme class is (+)-borneol:NAD+ oxidoreductase. This enzyme is also called bicyclic monoterpenol dehydrogenase.


(+)-camphene synthase
(+)-camphene synthase (EC ) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (+)-camphene-forming). This enzyme catalyses the following chemical reaction


(+)-camphene synthase
Cyclase I of Salvia officinalis (sage) gives about equal parts (+)-camphene and (+)-alpha-pinene.


(+)-car-3-ene synthase
(+)-car-3-ene synthase (EC , 3-carene cyclase, 3-carene synthase, 3CAR, (+)-3-carene synthase) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (+)-car-3-ene-forming). This enzyme catalyses the following chemical reaction


(+)-car-3-ene synthase
The enzyme reacts with (3S)-linalyl diphosphate twice as rapidly as geranyl diphosphate.


(+)-cis-2-Aminomethylcyclopropane carboxylic acid
(+)-cis-2-Aminomethylcyclopropane carboxylic acid ((+)-CAMP) is an agonist for the GABAA-rho receptor.


(+)-cubenene synthase
(+)-cubenene synthase (EC ) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase ((+)-cubenene-forming). This enzyme catalyses the following chemical reaction


(+)-delta-selinene synthase
(+)-delta-selinene synthase (EC ) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase ((+)-delta-selinene-forming). This enzyme catalyses the following chemical reaction


(+)-delta-selinene synthase
Initial cyclization gives germacrene C in an enzyme bound form.


(+)-endo-beta-bergamotene synthase ((2Z,6Z)-farnesyl diphosphate cyclizing)
(+)-endo-beta-bergamotene synthase ((2Z,6Z)-farnesyl diphosphate cyclizing) (EC , SBS) is an enzyme with systematic name (2Z,6Z)-farnesyl diphosphate lyase (cyclizing; (+)-endo-beta-bergamotene-forming). This enzyme catalyses the following chemical reaction


(+)-endo-beta-bergamotene synthase ((2Z,6Z)-farnesyl diphosphate cyclizing)
The enzyme synthesizes a mixture of sesquiterpenoids from (2Z,6Z)-farnesyl diphosphate.


(+)-epi-alpha-bisabolol synthase
(+)-epi-alpha-bisabolol synthase (EC ) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase (cyclizing, (+)-epi-alpha-bisabolol-forming). This enzyme catalyses the following chemical reaction


(+)-epi-alpha-bisabolol synthase
This enzyme is isolated from the plant Phyla dulcis (Aztec sweet herb).


(+)-epicubenol synthase
(+)-epicubenol synthase (EC , farnesyl pyrophosphate cyclase) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase ((+)-epicubenol-forming). This enzyme catalyses the following chemical reaction


(+)-gamma-cadinene synthase
(+)-gamma-cadinene synthase (EC ) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase ((+)-gamma-cadinene-forming). This enzyme catalyses the following chemical reaction


(+)-gamma-cadinene synthase
The enzyme from the melon, Cucumis melo, forms mainly delta- and gamma-cadinene.


(+)-germacrene D synthase
(+)-germacrene D synthase (EC ) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase ((+)-germacrene-D-forming). This enzyme catalyses the following chemical reaction


(+)-neomenthol dehydrogenase
In enzymology, a (+)-neomenthol dehydrogenase (EC ) is an enzyme that catalyzes the chemical reaction


(+)-neomenthol dehydrogenase
Thus, the two substrates of this enzyme are (+)-neomenthol and NADP+, whereas its 3 products are (−)-menthone, NADPH, and H+.


(+)-neomenthol dehydrogenase
This enzyme belongs to the family of oxidoreductases, specifically those acting on the CH-OH group of donor with NAD+ or NADP+ as acceptor. The systematic name of this enzyme class is (+)-neomenthol:NADP+ oxidoreductase. This enzyme is also called monoterpenoid dehydrogenase. This enzyme participates in monoterpenoid biosynthesis.


(+)-sabinene synthase
(+)-sabinene synthase (EC , SS) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (+)-sabinene-forming). This enzyme catalyses the following chemical reaction


(+)-sabinol dehydrogenase
In enzymology, a (+)-sabinol dehydrogenase (EC ) is an enzyme that catalyzes the chemical reaction


(+)-sabinol dehydrogenase
Thus, the two substrates of this enzyme are (+)-cis-sabinol and NAD+, whereas its 3 products are (+)-sabinone, NADH, and H+.


(+)-sabinol dehydrogenase
This enzyme belongs to the family of oxidoreductases, specifically those acting on the CH-OH group of donor with NAD+ or NADP+ as acceptor. The systematic name of this enzyme class is (+)-cis-sabinol:NAD+ oxidoreductase. This enzyme is also called (+)-cis-sabinol dehydrogenase.


(+)-sativene synthase
(+)-sativene synthase (EC , cop4) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase (cyclizing, (+)-sativene-forming). This enzyme catalyses the following chemical reaction


(+)-trans-carveol dehydrogenase
In enzymology, a (+)-trans-carveol dehydrogenase (EC ) is an enzyme that catalyzes the chemical reaction


(+)-trans-carveol dehydrogenase
Thus, the two substrates of this enzyme are (+)-trans-carveol and NAD+, whereas its 3 products are (+)-(S)-carvone, NADH, and H+.


(+)-trans-carveol dehydrogenase
This enzyme belongs to the family of oxidoreductases, specifically those acting on the CH-OH group of donor with NAD+ or NADP+ as acceptor. The systematic name of this enzyme class is (+)-trans-carveol:NAD+ oxidoreductase. This enzyme is also called carveol dehydrogenase. This enzyme participates in monoterpenoid biosynthesis and the degradation of the terpenes limonene and pinene.


(-)-Endo-fenchol dehydrogenase
(−)-endo-fenchol dehydrogenase (EC , l-endo-fenchol dehydrogenase, FDH) is an enzyme with systematic name (−)-endo-fenchol:NAD(P)+ oxidoreductase. This enzyme catalyses the following chemical reaction


(-)-Isopiperitenone reductase
(-)-Isopiperitenone reductase (EC ) is an enzyme with systematic name (+)-cis-isopulegone:NADP+ oxidoreductase. It catalyses the following chemical reaction:


(-)-alpha-cuprenene synthase
(-)-alpha-cuprenene synthase (EC , Cop6) is an enzyme with systematic name (-)-alpha-cuprenene hydrolase (cyclizing, (-)-alpha-cuprenene-forming). This enzyme catalyses the following chemical reaction


(-)-alpha-cuprenene synthase
The enzyme from the fungus Coprinopsis cinerea produces (-)-alpha-cuprenene with high selectivity.


(-)-alpha-pinene synthase
(-)-alpha-pinene synthase (EC , (-)-alpha-pinene/(-)-camphene synthase, (-)-alpha-pinene cyclase) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (-)-alpha-pinene-forming). This enzyme catalyses the following chemical reaction


(-)-alpha-pinene synthase
Cyclase II of Salvia officinalis (sage) gives about equal parts (-)-alpha-pinene, (-)-beta-pinene and (-)-camphene.


(-)-alpha-terpineol synthase
(-)-alpha-terpineol synthase (EC ) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (-)-alpha-terpineol-forming). This enzyme catalyses the following chemical reaction


(-)-beta-caryophyllene synthase
(-)-beta-caryophyllene synthase (EC , beta-caryophyllene synthase) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase ((-)-beta-caryophyllene-forming). This enzyme catalyses the following chemical reaction


(-)-beta-pinene synthase
(-)-beta-pinene synthase (EC , beta-geraniolene synthase, (-)-(1S,5S)-pinene synthase, geranyldiphosphate diphosphate lyase (pinene forming)) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (-)-beta-pinene-forming). This enzyme catalyses the following chemical reaction


(-)-beta-pinene synthase
Cyclase II of Salvia officinalis (sage) produces about equal parts (-)-alpha-pinene, (-)-beta-pinene and (-)-camphene.


(-)-borneol dehydrogenase
In enzymology, a (−)-borneol dehydrogenase (EC ) is an enzyme that catalyzes the chemical reaction


(-)-borneol dehydrogenase
Thus, the two substrates of this enzyme are (−)-borneol and NAD+, whereas its 3 products are (−)-camphor, NADH, and H+.


(-)-borneol dehydrogenase
This enzyme belongs to the family of oxidoreductases, specifically those acting on the CH-OH group of donor with NAD+ or NADP+ as acceptor. The systematic name of this enzyme class is (−)-borneol:NAD+ oxidoreductase.


(-)-camphene synthase
(-)-camphene synthase (EC , CS) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (-)-camphene-forming). This enzyme catalyses the following chemical reaction


(-)-camphene synthase
(-)-Camphene is the major product in Abies grandis (grand fir) with traces of other monoterpenoids.


(-)-delta-cadinene synthase
(-)-delta-cadinene synthase (EC ) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase (cyclizing, (-)-delta-cadinene-forming). This enzyme catalyses the following chemical reaction


(-)-endo-alpha-bergamotene synthase ((2Z,6Z)-farnesyl diphosphate cyclizing)
(-)-endo-alpha-bergamotene synthase ((2Z,6Z)-farnesyl diphosphate cyclizing) (EC , SBS) is an enzyme with systematic name (2Z,6Z)-farnesyl diphosphate lyase (cyclizing; (-)-endo-alpha-bergamotene-forming). This enzyme catalyses the following chemical reaction


(-)-endo-alpha-bergamotene synthase ((2Z,6Z)-farnesyl diphosphate cyclizing)
The enzyme synthesizes a mixture of sesquiterpenoids from (2Z,6Z)-farnesyl diphosphate.


(-)-endo-fenchol synthase
In enzymology, a (−)-endo-fenchol synthase (EC ) is an enzyme that catalyzes the chemical reaction


(-)-endo-fenchol synthase
Thus, the two substrates of this enzyme are geranyl diphosphate and H2O, whereas its two products are (−)-endo-fenchol and diphosphate.


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


(-)-gamma-cadinene synthase ((2Z,6E)-farnesyl diphosphate cyclizing)
(-)-gamma-cadinene synthase ((2Z,6E)-farnesyl diphosphate cyclizing) (EC , (-)-gamma-cadinene cyclase) is an enzyme with the systematic name (2Z,6E)-farnesyl-diphosphate diphosphate-lyase ((-)-gamma-cadinene-forming). This enzyme catalyses the following chemical reaction:


(-)-germacrene D synthase
(-)-germacrene D synthase (EC ) is an enzyme with systematic name (2E,6E)-farnesyl-diphosphate diphosphate-lyase ((-)-germacrene-D-forming). This enzyme catalyses the following chemical reaction


(-)-germacrene D synthase
In Solidago canadensis the biosynthesis results in the pro-R hydrogen at C-1 of the farnesyl diphosphate.


(-)-menthol dehydrogenase
A (−)-menthol dehydrogenase (EC ) is an enzyme that catalyzes the chemical reaction


(-)-menthol dehydrogenase
i.e., catalyses the breakdown of menthol. Thus, the two substrates of this enzyme are (−)-menthol and NADP+, whereas its 3 products are (−)-menthone, NADPH, and H+.


(-)-menthol dehydrogenase
This enzyme belongs to the family of oxidoreductases, specifically those acting on the CH-OH group of donor with NAD+ or NADP+ as acceptor. The systematic name of this enzyme class is (−)-menthol:NADP+ oxidoreductase. This enzyme is also called monoterpenoid dehydrogenase. This enzyme participates in monoterpenoid biosynthesis.


(-)-menthol monooxygenase
In enzymology, a (−)-menthol monooxygenase (EC ) is an enzyme that catalyzes the chemical reaction


(-)-menthol monooxygenase
The 4 substrates of this enzyme are (−)-menthol, NADPH, H+, and O2, whereas its 3 products are p-menthane-3,8-diol, NADP+, and H2O.


(-)-menthol monooxygenase
This enzyme belongs to the family of oxidoreductases, specifically those acting on paired donors, with O2 as oxidant and incorporation or reduction of oxygen. The oxygen incorporated need not be derived from O2 with NADH or NADPH as one donor, and incorporation of one atom o oxygen into the other donor. The systematic name of this enzyme class is (−)-menthol,NADPH:oxygen oxidoreductase (8-hydroxylating). This enzyme is also called l-menthol monooxygenase.


(-)-menthol monooxygenase, Uses
Use of (−)-menthol monooxygenase has been explored by several companies including Procter & Gamble for cleaning products.


(-)-sabinene synthase
(-)-sabinene synthase (EC ) is an enzyme with systematic name geranyl-diphosphate diphosphate-lyase (cyclizing, (-)-sabinene-forming). This enzyme catalyses the following chemical reaction


(..)ibra
(..)ibra was a king of Meluhha according to an inscription attributed to the reign of Naram-Sin of Akkad (2254–2218 BC), the third successor and grandson of Sargon of Akkad (2334–2279 BC).


(..)ibra, Inscription
In an earlier inscription, Sargon of Akkad referred to ships coming from Meluhha, Magan and Dilmun. His grandson Naram-Sin (2254–2218 BC) listing the rebel kings to his rule, mentioned "(..)ibra, man of Melukha". In an inscription, Gudea of Lagash (21st century BC) referred to the Meluhhans who came to Sumer to sell gold dust, carnelian etc... In the Gudea cylinders (inscription of cylinder A, IX:19), Gudea mentions that "I will spread in the world respect for my Temple, under my name the whole universe will gather in it, and Magan and Meluhha will come down from their mountains to attend". In cylinder B, XIV, he mentions his procurement of "blocks of lapis lazuli and bright carnelian from Meluhha." There are no known mentions of Meluhha after 1760 BC.


(04:30) Idler
(4:30) Idler is the second album by London-based singer and producer Jamie Isaac. It was released on June 1, 2018 via Marathon Artists.


(1+ε)-approximate nearest neighbor search
(1+ε)-approximate nearest neighbor search is a special case of the nearest neighbor search problem. The solution to the (1+ε)-approximate nearest neighbor search is a point or multiple points within distance (1+ε) R from a query point, where R is the distance between the query point and its true nearest neighbor.


(1+ε)-approximate nearest neighbor search
Reasons to approximate nearest neighbor search include the space and time costs of exact solutions in high-dimensional spaces (see curse of dimensionality) and that in some domains, finding an approximate nearest neighbor is an acceptable solution.


(1+ε)-approximate nearest neighbor search
Approaches for solving (1+ε)-approximate nearest neighbor search include kd-trees, Locality Sensitive Hashing and brute force search.


(1,1'-Bis(diphenylphosphino)ferrocene)palladium(II) dichloride
[1,1'‑Bis(diphenylphosphino)ferrocene]palladium(II) dichloride is a palladium complex containing the bidentate ligand 1,1'-bis(diphenylphosphino)ferrocene (dppf), abbreviated as [(dppf)PdCl2]. This commercially available material can be prepared by reacting dppf with a suitable nitrile complex of palladium dichloride:


(1,1'-Bis(diphenylphosphino)ferrocene)palladium(II) dichloride
The compound is popularly used for palladium-catalyzed coupling reactions, such as the Buchwald–Hartwig amination and the reductive homocoupling of aryl halides.


(1,2,5,6-Tetrahydropyridin-4-yl)methylphosphinic acid
(1,2,5,6-Tetrahydropyridin-4-yl)methylphosphinic acid (TPMPA) is a GABA antagonist selective for the GABAA-ρ (previously known as GABAC) subtype.


(1-4)-a-D-glucan 1-a-D-glucosylmutase
(1->4)-alpha-D-glucan 1-alpha-D-glucosylmutase (EC , malto-oligosyltrehalose synthase, maltodextrin alpha-D-glucosyltransferase) is an enzyme with systematic name (1->4)-alpha-D-glucan 1-alpha-D-glucosylmutase. This enzyme catalyses the following chemical reaction


(1-4)-a-D-glucan 1-a-D-glucosylmutase
The enzyme from Arthrobacter sp., Sulfolobus acidocaldarius acts on (1->4)-alpha-D-glucans containing three or more (1->4)-alpha-linked D-glucose units.


(1-hydroxycyclohexan-1-yl)acetyl-CoA lyase
In enzymology, a (1-hydroxycyclohexan-1-yl)acetyl-CoA lyase (EC ) is an enzyme that catalyzes the chemical reaction


(1-hydroxycyclohexan-1-yl)acetyl-CoA lyase
Hence, this enzyme has one substrate, (1-hydroxycyclohexan-1-yl)acetyl-CoA, and two products, acetyl-CoA and cyclohexanone.


(1-hydroxycyclohexan-1-yl)acetyl-CoA lyase
This enzyme belongs to the family of lyases, specifically the oxo-acid-lyases, which cleave carbon-carbon bonds. The systematic name of this enzyme class is (1-hydroxycyclohexan-1-yl)acetyl-CoA cyclohexanone-lyase (acetyl-CoA-forming). This enzyme is also called (1-hydroxycyclohexan-1-yl)acetyl-CoA cyclohexanone-lyase.


(10115) 1992 SK
(10115) 1992 SK, is a stony near-Earth object and potentially hazardous asteroid on an eccentric orbit. It belongs to the group of Apollo asteroids and measures approximately 1 kilometer (0.6 miles) in diameter. It was discovered by American astronomers Eleanor Helin and Jeff Alu at the Palomar Observatory in California on 24 September 1992.


(10115) 1992 SK, Classification and orbit
The asteroid orbits the Sun at a distance of 0.8–1.7 AU once every 17 months (509 days). Its orbit has an eccentricity of 0.32 and an inclination of 15° with respect to the ecliptic. Its Earth minimum orbit intersection distance is 0.0449 AU (6,720,000 km). This makes the body a potentially hazardous asteroid, because its MOID is less than 0.05 AU and its diameter is greater than 150 meters. The first precovery was obtained at Palomar Observatory in 1953, extending the asteroid's observation arc by 39 years prior to its discovery.


(10115) 1992 SK, Physical characteristics
In the SMASS classification, 1992 SK is characterized as a common stony S-type asteroid.


(10115) 1992 SK, Physical characteristics, Rotation period
Several rotational lightcurves form photometric observations have been obtained for this body. In 1999, Czech astronomer Petr Pravec constructed a lightcurve, that rendered a rotation period of 7.328 hours and a brightness variation of 0.72 in magnitude (U=n/a).


(10115) 1992 SK, Physical characteristics, Rotation period
In March 2006, observations by astronomer David Polishook from the ground-based Wise Observatory, Israel, gave a rotation period of 7.31 and amplitude of 0.70 mag (U=2), and in November 2011, American astronomer Brian Warner at the Palmer Divide Observatory, Colorado, obtained the first well-defined period of 7.323 hours with an amplitude of 0.50 mag (U=3).


(10115) 1992 SK, Physical characteristics, Diameter and albedo
According to the surveys carried out by NASA's space-based Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures 1.0 and 0.94 kilometers in diameter and its surface has an albedo of 0.28 ot 0.32, respectively. The ExploreNEOs project finds an albedo of 0.34, with an diameter of 0.9 kilometers, and the Collaborative Asteroid Lightcurve Link calculates a diameter of 1.18 kilometers based on an assumed standard albedo for stony asteroids of 0.20 and an absolute magnitude of 17.0.


(10115) 1992 SK, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 2 March 1999. As of 2019, it has not been named.


(101429) 1998 VF31
(101429) 1998 VF31 is a sub-kilometer asteroid that orbits near Mars's L5 Lagrangian point, on average trailing 60° behind it. Its orbit is highly stable, and was originally thought to be spectroscopically similar to 5261 Eureka, suggesting they may both be primordial Martian asteroids.


(101429) 1998 VF31
Spectroscopic observations through 2007 indicate that it has a large proportion of metal and achondrites on its surface (either with or without a mesosiderite contribution); which could also indicate that the surface regolith has undergone space weathering. These observations also reveal differences in the spectra with 5261 Eureka, suggesting they may not be related to each other after all.


(101869) 1999 MM
(101869) 1999 MM, provisional designation 1999 MM is a sub-kilometer asteroid on an eccentric orbit, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered on 20 June 1999, by the Lowell Observatory Near-Earth-Object Search (LONEOS) at its U.S. Anderson Mesa Station in Flagstaff, Arizona. The first observation was made by Catalina Sky Survey just 8 days before its official discovery.


(101869) 1999 MM, Orbit and classification
The asteroid orbits the Sun at a distance of 0.6–2.6 AU once every 2 years and 1 month (756 days). Its orbit has an eccentricity of 0.61 and an inclination of 5° with respect to the ecliptic. It has a notably low Earth minimum orbit intersection distance of 0.0016 AU (240,000 km), which is less than one lunar distance, and also approaches Mars and Venus to within 15 million kilometers.


(101869) 1999 MM, Orbit and classification
1999 MM's orbit is very similar to that of 69230 Hermes, which in 1937 made what was for decades the closest observed approach to Earth by an asteroid. Its nearest pass to Earth within at least a century of present was the 930,000 kilometers one in 1875. In 2090 it passes Venus at 788,000 kilometers.


(101869) 1999 MM, Physical characteristics
Based on its absolute magnitude of 19.3, its mean-diameter is between 370 and 830 meters, assuming an albedo in the range of 0.05 to 0.25.


(101869) 1999 MM, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 19 October 2005. As of 2018, it has not been named.


(10302) 1989 ML
(10302) 1989 ML is an as yet unnamed near-Earth asteroid. It is approximately 0.6 km in diameter. An Amor asteroid, it orbits between Earth and Mars. It is an X-type asteroid, so its surface composition is yet unknown. It was discovered by Eleanor F. Helin and Jeff T. Alu at Palomar Observatory on 29 June 1989.


(10302) 1989 ML, Targeting by spacecraft
The delta-v ('effort') required to reach 1989 ML from a low-Earth orbit is only 4.8 km/s, ranking fifth (as of March 2007) amongst the near-Earth asteroids with well-established orbits. 1989 ML is thus particularly 'easy' (and 'cheap') to reach by spacecraft.


(10302) 1989 ML, Targeting by spacecraft
1989 ML was considered as a target of the Japanese spacecraft Hayabusa (then Muses-C) but had to be given up due to technical reasons. It was also considered by the European Space Agency as a candidate target for the Don Quijote mission to study the effects of impacting a spacecraft into an asteroid; however, they too changed to other targets.


(111253) 2001 XU10
(111253) 2001 XU10, provisional designation 2001 XU10, is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 3 kilometers in diameter. It was discovered on 9 December 2001, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The asteroid is one of the largest potentially hazardous asteroids.


(111253) 2001 XU10, Orbit and classification
2001 XU10 orbits the Sun at a distance of 0.98–2.52 AU once every 2 years and 4 months (848 days; semi-major axis of 1.75 AU). Its orbit has an eccentricity of 0.44 and an inclination of 42° with respect to the ecliptic. The body's observation arc begins with a precovery taken by the Sloan Digital Sky Survey in February 2000.


(111253) 2001 XU10, Orbit and classification
2001 XU10 is a member of the Apollo asteroids, the largest subgroup of near-Earth asteroids which cross the orbit of Earth. It is also a Mars-crosser, as it crosses the orbit of the Red Planet at 1.66 AU.


(111253) 2001 XU10, Orbit and classification, Close approaches
With an absolute magnitude of 15.2, 2001 XU10 is one of the brightest and presumably largest known potentially hazardous asteroid (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0293 AU (4,380,000 km), which translates into 11.4 lunar distances (LD). On 29 July 2054, this asteroid will make its closest near-Earth encounter of the 21st century at a nominal distance of 0.079 AU (31.1 LD).


(111253) 2001 XU10, Physical characteristics
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2001 XU10 measures 3.006 kilometers in diameter and its surface has an albedo of 0.178.


(111253) 2001 XU10, Physical characteristics
As of 2018, no rotational lightcurve of 2001 XU10 has been obtained from photometric observations. The asteroid's rotation period, spin axis and shape remain unknown. In addition, the body's spectral type has never been assessed.


(111253) 2001 XU10, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 19 October 2005. As of 2018, it has not been named.


(11436) 1969 QR
(11436) 1969 QR, is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 3.7 kilometers in diameter. It was discovered on 22 August 1969, by Czech astronomer Luboš Kohoutek at Bergedorf Observatory in Hamburg, Germany.


(11436) 1969 QR, Description
The S-type asteroid is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun at a distance of 1.9–2.5 AU once every 3 years and 4 months (1,212 days). Its orbit has an eccentricity of 0.14 and an inclination of 7° with respect to the ecliptic. As no precoveries were taken, the asteroid's observation arc starts with its discovery observation in 1969.


(11436) 1969 QR, Description
A rotational lightcurve for this asteroid was published by several Hungarian astronomers in August 2005. The photometric observations gave a rotation period of 2.65 hours with a brightness variation of 0.27 magnitude (U=2).


(11436) 1969 QR, Description
The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – derived from 8 Flora, the largest member and namesake of its orbital family – and calculates a diameter of 3.7 kilometers.


(11436) 1969 QR, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 28 September 1999. As of 2018, it has not been named.


(11474) 1982 SM2
(11474) 1982 SM2 is a carbonaceous Baptistina asteroid and potentially slow rotator from the inner regions of the asteroid belt, approximately 6 kilometers in diameter. It was discovered on 18 September 1982, by Belgian astronomer Henri Debehogne at ESO' La Silla Observatory in northern Chile.


(11474) 1982 SM2, Orbit and classification
The C-type asteroid belongs to the small Baptistina family. It orbits the Sun at a distance of 1.8–2.7 AU once every 3 years and 5 months (1,254 days). Its orbit has an eccentricity of 0.20 and an inclination of 5° with respect to the ecliptic. As no precoveries were taken, and no prior identifications were made, the asteroid's observation arc begins with its official discovery observation.


(11474) 1982 SM2, Physical characteristics
In September 2013, a rotational lightcurve of this asteroid was obtained from photometric observations in the R-band at the Palomar Transient Factory in California. It gave an exceptionally long rotation period of 1917 hours with a brightness amplitude of 0.04 magnitude (U=1). However, the fragmentary light-curve has received a low quality rating by the Collaborative Asteroid Lightcurve Link (CALL) which means that the result could be completely wrong (also see potentially slow rotator).


(11474) 1982 SM2, Physical characteristics
CALL assumes a standard albedo for carbonaceous asteroids of 0.057 and calculates a diameter of 5.71 kilometers, based on an absolute magnitude of 14.49.


(11474) 1982 SM2, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 28 September 1999. As of 2018, it has not been named.


(118228) 1996 TQ66
(118228) 1996 TQ66 , prov. designation: 1996 TQ66, is a resonant trans-Neptunian object of the plutino population in the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 8 October 1996, by American astronomers Jun Chen, David Jewitt, Chad Trujillo and Jane Luu, using the UH88 telescope at the Mauna Kea Observatories, Hawaii. The very red object measures approximately 185 kilometers (110 miles) in diameter. As of 2021, it has not been named.


(118228) 1996 TQ66, Orbit and classification
1996 TQ66 orbits the Sun at a distance of 34.5–44.2 AU once every 247 years and 1 month (90,254 days; semi-major axis of 39.38 AU). Its orbit has an eccentricity of 0.12 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at the Mauna Kea Observatories on 8 October 1996. It came to perihelion in 1998. As of 2021, it is at 35.6 AU from the Sun and has an apparent magnitude of 22.85.


(118228) 1996 TQ66, Orbit and classification
1996 TQ66 is a trans-Neptunian object and belongs to the plutino population, a large group of objects named after their largest member, Pluto. These resonant trans-Neptunian objects stay in a 2:3 mean-motion orbital resonance with Neptune, orbiting exactly two times the Sun for every three orbits Neptune does and are therefore protected from the planets scattering effect. Plutinos form in inner rim of the Kuiper belt, a circumstellar disc of mostly non-resonant classical Kuiper belt objects.


(118228) 1996 TQ66, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 16 November 2005, receiving the number (118228) in the minor planet catalog (M.P.C. 55524). As of 2021, it has not been named. According to the established naming conventions, it will be given a mythological name associated with the underworld.


(118228) 1996 TQ66, Physical characteristics
1996 TQ66 has a very red surface color (RR) in the visible part of the spectrum, with B−V and V–R color indices of 1.190±0.020 and 0.660±0.030, respectively, for a combined B−R magnitude of 1.85. A red surface color is typically associated with the presence of tholins, polymer-like organic compounds, formed by long exposures to solar and cosmic radiation.


(118228) 1996 TQ66, Physical characteristics, Rotation period
In 1999, results of a photometric survey of Kuiper belt objects by Romanishin and Tegler were published in the Journal Nature. For 1996 TQ66, a brightness variation of no more than 0.22 in magnitude could be determined, which is indicative of a modestly irregular shape. As of 2021, no rotational lightcurve for this object has been obtained from photometry. The body's rotation period, pole and actual shape remain unknown.


(118228) 1996 TQ66, Physical characteristics, Diameter and albedo
Based on a generic magnitude-to-diameter conversion, 1996 TQ66 measures approximately 185 kilometers (110 miles) in diameter, for an assumed albedo of 0.9 and an magnitude of 7. According to Mike Brown, who estimates a mean-diameter of 186 km (120 mi), the object is too small for being considered a dwarf planet candidate ("probably not").


(118378) 1999 HT11
(118378) 1999 HT11, provisional designation: 1999 HT11, is a trans-Neptunian object from the outermost region of the Solar System, locked in a 4:7 orbital resonance with Neptune. It was discovered on 17 April 1999, by astronomers at the Kitt Peak Observatory, Arizona, in the United States. The very red object measures approximately 134 kilometers (83 miles) in diameter. As of 2021, it has not been named.


(118378) 1999 HT11, Discovery
1999 HT11 was first observed on the night of 17 April 1999, by astronomers using the 4-meter Nicholas U. Mayall Telescope at Kitt Peak National Observatory in Arizona. Five additional objects were discovered on the same weekend: 1999 HR11, 1999 HS11, 1999 HU11 (Deucalion), 1999 HV11 and 1999 HW11. The observing astronomers were Robert Millis, James Elliot, Matthew Holman, Mark Wagner as well as Kim Falinski. Follow-up observations with the Nordic Optical Telescope at the Roque de los Muchachos Observatory, La Palma, Spain, were made three weeks later. The body's observation arc begins with its official discovery observation at Kitt Peak on 17 April 1999.


(118378) 1999 HT11, Orbit and classification
This minor planet orbits the Sun at a distance of 38.7–49.0 AU once every 290 years and 7 months (106,124 days; semi-major axis of 43.87 AU). Its orbit has an eccentricity of 0.12 and an inclination of 5° with respect to the ecliptic. As of 2021, it is at 39.7 AU from the Sun with an apparent magnitude of 23.42, and will come to perihelion in 2047.


(118378) 1999 HT11, Orbit and classification
1999 HT11 is a resonant trans-Neptunian object that stays in a 4:7 mean-motion orbital resonance with Neptune, orbiting exactly four times the Sun for every seven orbits Neptune does and are therefore protected from the planets scattering effect. The classification is deemed secure. The 4:7 resonance is located in the midst of the classical objects of the Kuiper belt, a circumstellar disc of otherwise non-resonant bodies, contrary to the more prominent resonant plutinos (2:3) and twotinos (1:2) which form the inner and outer rim of the Kuiper belt, respectively.


(118378) 1999 HT11, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 16 November 2005, receiving the number (118378) in the minor planet catalog (M.P.C. 55526). As of 2021, it has not been named. According to the established naming conventions, it will be given a mythological name associated with the underworld or with creation.


(118378) 1999 HT11, Physical characteristics
1999 HT11 has a very red surface color (RR) in the visible part of the spectrum, with B−V and V–R color indices of 1.150±0.064 and 0.670±0.040, respectively, for a combined B−R magnitude of 1.820±0.050. A red surface color is typically associated with the presence of tholins, polymer-like organic compounds, formed by long exposures to solar and cosmic radiation.


(118378) 1999 HT11, Physical characteristics
Based on a generic magnitude-to-diameter conversion, 1999 HT11 measures approximately 134 kilometers (83 miles) in diameter, for an assumed albedo of 0.9 and an magnitude of 7.6. According to Mike Brown, who estimates a mean-diameter of 137 km (85 mi), the object is too small for being considered a dwarf planet candidate ("probably not"). As of 2021, no rotational lightcurve for this body has been obtained from photometric observations. Its rotation period, pole and shape remain unknown.


(119070) 2001 KP77
(119070) 2001 KP77, provisional designation: 2001 KP77, is a resonant trans-Neptunian object in the Kuiper belt, a circumstellar disc located in the outermost region of the Solar System. It was discovered on 23 May 2001, by American astronomer Marc Buie at the Cerro Tololo Observatory in Chile. The object is locked in a 4:7 orbital resonance with Neptune. It has a red surface color and measures approximately 176 kilometers (110 miles) in diameter. As of 2021, it has not been named.


(119070) 2001 KP77, Discovery
2001 KP77 was first observed near its perihelion on 23 May 2001, using the 4-meter Blanco Telescope at Cerro Tololo Inter-American Observatory in Chile. During the same night, 2001 KN77, 2001 KO77, 2001 KQ77 were also discovered. Besides Marc Buie, who is solely credited with the discovery of this object, the Minor Planet Electronic Circular also mentions James Elliot, Lawrence Wasserman, Robert Millis and Susan Kern as observers and measurers, respectively. Follow-up observations with the 6.5-meter Baade Telescope (Magellan) at the Las Campanas Observatory were made three weeks later. The body's observation arc begins with its official discovery observation at Cerro Tololo on 23 May 2001.


(119070) 2001 KP77, Orbit and classification
This minor planet orbits the Sun at a distance of 36.1–51.9 AU once every 291 years and 7 months (106,514 days; semi-major axis of 43.98 AU). Its orbit has an eccentricity of 0.18 and an inclination of 3° with respect to the ecliptic. The object came to perihelion in 2002. As of 2021, it is 37.0 AU from the Sun and has an apparent magnitude of 22.8.


(119070) 2001 KP77, Orbit and classification
2001 KP77 is a resonant trans-Neptunian object that stays in a 4:7 mean-motion orbital resonance with Neptune, orbiting exactly four times the Sun for every seven orbits Neptune does. The classification is deemed secure. The 4:7 resonance is located at 43.7 AU in the midst of the classical objects of the Kuiper belt, a circumstellar disc of typically non-resonant bodies, contrary to the more prominent resonant plutinos (2:3) and twotinos (1:2) which form the inner and outer rim of the Kuiper belt, respectively.


(119070) 2001 KP77, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 16 November 2005, receiving the number (119070) in the minor planet catalog (M.P.C. 55533). As of 2021, it has not been named. According to the established naming conventions, it will be given a mythological name associated with the underworld or with creation.


(119070) 2001 KP77, Physical characteristics
This object has a red surface color, with a high B−R color index of 1.720±0.319 in the visible part of the spectrum. A red surface color is typically associated with the presence of tholins, polymer-like organic compounds, formed by long exposures to solar and cosmic radiation. A higher B−R magnitude of 1.980±0.229 including B−V and V−R color indices of 1.544 and 0.574, respectively, were previously published in 2004.


(119070) 2001 KP77, Physical characteristics
Based on a generic magnitude-to-diameter conversion, 2001 KP77 measures approximately 176 kilometers (110 miles) in diameter, for an assumed albedo of 0.9 and an magnitude of 7.0. According to Mike Brown, who estimates a mean-diameter of 113 km (70 mi), the object is too small for being considered a dwarf planet candidate ("probably not"). As of 2021, no rotational lightcurve for this body has been obtained from photometric observations. Its rotation period, pole and shape, as well as its composition remain unknown.


(119951) 2002 KX14
(119951) 2002 KX14, also written as 2002 KX14, is a medium sized trans-Neptunian object (TNO) residing within the Kuiper belt. It was discovered on 17 May 2002 by Michael E. Brown and Chad Trujillo.


(119951) 2002 KX14
It has a semi-major axis, orbital period and orbital eccentricity close to that of a plutino. The orbital periods of plutinos cluster around 247.2 years (1.5 times Neptune's orbital period), close to 2002 KX14's orbital period. However, 2002 KX14 is not a plutino, as it is not actually in a resonance with Neptune, and it may have formed near its present nearly circular orbit lying almost perfectly on the ecliptic.


(119951) 2002 KX14
This TNO may have remained dynamically cold since its formation, and thus its orbit may not have been a direct result of significant perturbations from Neptune during its migration to the outer solar system. The Deep Ecliptic Survey (DES) currently classifies it as a cubewano (classical) based on a 10-million-year integration of the orbit.


(119951) 2002 KX14
2002 KX14 comes to opposition in late May at an apparent magnitude of 20.4. This makes it about 360 times fainter than Pluto.


(119979) 2002 WC19
(119979) 2002 WC19 is a twotino, that is, a planetoid in a 1:2 orbital resonance with Neptune. It was discovered on November 16, 2002 at the Palomar Observatory. It is probably a dwarf planet in Brown's estimation,but is likely much too small to be a solid body.


(119979) 2002 WC19
Knowing how many twotinos there are may reveal whether Neptune took roughly 1 million or 10 million years to migrate about 7 AU from its birth location.


(119979) 2002 WC19, Satellite
A natural satellite was reported to be orbiting (119979) 2002 WC19 on February 27, 2007. It is estimated to be 4092±94 km from the primary, with an orbital period of 8.403±0.001 days, an eccentricity of 0.21±0.05 and an inclination of 24.0°±0.7°. Assuming similar albedos, it is a quarter the diameter of its primary, or around 81 kilometres (50 mi) in diameter.


(120132) 2003 FY128
(120132) 2003 FY128, also written as (120132) 2003 FY128, is a trans-Neptunian object with a diameter of about 460 km. It orbits the Sun at a distance of about 49.81 astronomical units. It was discovered on 26 March 2003 by the NEAT program at the Palomar Observatory, California.


(120132) 2003 FY128, Classification
It is classified as a detached object by the Deep Ecliptic Survey (DES), since its orbit appears to be beyond the current control of Neptune. Though, if Neptune migrated outward, there would have been a period when Neptune had a higher eccentricity.


(120178) 2003 OP32
(120178) 2003 OP32, also written as (120178) 2003 OP32, is a trans-Neptunian object (TNO) that resides in the Kuiper belt. It was discovered on July 26, 2003 by Michael E. Brown, Chad Trujillo and David L. Rabinowitz at Palomar Mountain in California.


(120178) 2003 OP32, Origin
Based on their common pattern of infrared water-ice absorption and the clustering of their orbital elements, the other KBOs 1995 SM55, (19308) 1996 TO66, (55636) 2002 TX300 and (145453) 2005 RR43, among others, appear to be collisional fragments broken off the dwarf planet Haumea. The neutral color of the spectrum of these objects in the visible range evidences a lack of complex organics on the surface of these bodies that has been studied in detail for the surface of Haumea.


(120216) 2004 EW95
(120216) 2004 EW95, provisionally known as 2004 EW95, is a resonant trans-Neptunian object in the Kuiper belt located in the outermost regions of the Solar System. It measures approximately 291 kilometers in diameter. It has more carbon than typical of KBOs, and the first to be confirmed as having this composition in this region of space. It is thought that it had originated closer to the Sun, maybe even the main asteroid belt.


(120216) 2004 EW95, Orbit
Like Pluto, 2004 EW95 is classified as a plutino. It stays in a 2:3 resonance with Neptune. For every 2 orbits that a plutino makes, Neptune orbits 3 times.


(120216) 2004 EW95, Orbit
2004 EW95 is currently 27.0 AU from the Sun, and came to perihelion (q=26.98 AU) in April 2018. This means that this object is currently inside the orbit of the planet Neptune. Like Pluto, this plutino spends part of its orbit closer to the Sun than Neptune is even though their orbits are controlled by Neptune. (Probable dwarf planet Huya and plutino (15875) 1996 TP66 are also currently inside the orbit of Neptune.) Simulations by the Deep Ecliptic Survey (DES) show that over the next 10 million years 2004 EW95 can acquire a perihelion distance (qmin) as small as 24.6 AU.


(120216) 2004 EW95, Orbit
It comes within 9 AU (1.3 billion km) of Uranus and stays more than 21 AU from Neptune over a 14,000 year period. 2004 EW95 has been observed 158 times with an observation arc of 13 years and has an orbit quality of 2.


(120216) 2004 EW95, Physical characteristics
2004 EW95 has a dark albedo of 0.04, giving it a diameter of about 291 km. Its reflectance spectrum bears striking resemblance to those of some hydrated C-type asteroids, indicating that this object possibly formed in the same environment as the C-type asteroids found today in the outer asteroid belt.


(120216) 2004 EW95, Physical characteristics
Unlike the majority of small objects in the Kuiper belt observed so far, the visible spectrum of 2004 EW95 has two features, each respectively associated with ferric oxides and phyllosilicates. The presence of a phyllosilicate feature in the spectrum of a minor planet indicates that the rocky component of its composition has been altered by the presence of liquid water at some point since its formation. For this to have occurred on 2004 EW95 in its current orbit and at temperatures of ~35K, significant quantities of thermal energy would have been required.


(120216) 2004 EW95, Physical characteristics
While this energy could have been delivered by a very large chance collision, the strong overall similarity between the modern C-type asteroids in the outer asteroid belt and 2004 EW95 suggests that these objects formed in the same region of the early Sun's protoplanetary disk, much closer to the Sun and at higher temperatures.


(120216) 2004 EW95, Physical characteristics
The Grand tack hypothesis predicts that the primitive C-type asteroids were dispersed from their formation location by the migrations of Jupiter and Saturn and many were injected into the outer asteroid belt where we find them today. By the same mechanism (and others that result from planetary formation), simulations show that C-types can also be thrown outward to the trans-Neptunian region, where later they may become captured into the mean-motion resonances of Neptune.


(120348) 2004 TY364
(120348) 2004 TY364, provisionally known as 2004 TY364, is a trans-Neptunian object. It is an inner classical Kuiper belt object in the definition by Gladman, Marsden, and Van Laerhoven (e<0.24). Its inclination of almost 25 degrees disqualifies it as such in Marc Buie's definition. It is also not listed as a scattered disc object by the Minor Planet Center. It was discovered  by Michael E. Brown, Chad Trujillo and David L. Rabinowitz on October 3, 2004 at the Palomar Observatory.


(120348) 2004 TY364
With an absolute magnitude of 4.5, it is likely a dwarf planet. However, light-curve analysis has questioned whether it really is one.


(120348) 2004 TY364
As of 2014, it is 39.2 AU from the Sun.


(121514) 1999 UJ7
(121514) 1999 UJ7 is a small asteroid orbiting near the L4 point of Mars (60 degrees ahead Mars on its orbit). As of September 2011, it is the only known asteroid to orbit the leading L4 point of Mars, although at least three other asteroids orbit Mars's trailing L5 point: 5261 Eureka, (101429) 1998 VF31, and 2007 NS2. Not only does (121514) 1999 UJ7 orbit on the other side of Mars from other similar asteroids, its spectrum is different as well, which is puzzling because all of the Martian trojans seem to be in very stable orbits.


(121514) 1999 UJ7, Orbit
(121514) 1999 UJ7 orbits around the L4 point of Mars in a very stable orbit and is large enough that the Yarkovsky effect will not affect its orbit.


(121514) 1999 UJ7, Physical characteristics
Due to similarity in the measured brightness of (121514) 1999 UJ7 with other Martian trojans, it is thought to be a small asteroid with an effective diameter on the order of 1 kilometer (0.62 mi). Its spectrum suggests that it is an X-type asteroid, which is different from 5261 Eureka and 1998 VF31, and is somewhat puzzling since different mineral compositions suggest different origins for the two groups of asteroids. The long lifetime of the orbits for these asteroids makes the possibility of one or more of them being interlopers unlikely, however.


(121514) 1999 UJ7, Physical characteristics
This suggests that either one or more of the Martian trojans was captured in such a way as to give it a long-term stable orbit (and it is therefore not a primordial Martian asteroid), or that some fusion or combination of previous asteroids resulted in the presently observed ones. The Yarkovsky effect may provide a potential capture mechanism but not enough is known about the shapes of these objects to provide a useful Yarkovsky model.


(12538) 1998 OH
(12538) 1998 OH is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.8 kilometers (1.1 miles) in diameter. It was discovered on 19 July 1998, by astronomers of the Near-Earth Asteroid Tracking program at the Haleakala Observatory in Hawaii, United States. In 2019, the asteroid came within about 73 lunar distances of Earth.


(12538) 1998 OH, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 23 November 1999. As of 2018, it has not been named.


(12538) 1998 OH, Orbit and classification
1998 OH is a member of the Apollo group of asteroids, which are Earth-crossing asteroids. They are the largest group of near-Earth objects with approximately 10 thousand known members.


(12538) 1998 OH, Orbit and classification
It orbits the Sun at a distance of 0.9–2.2 AU in 1 year and 11 months (699 days). Its orbit has an eccentricity of 0.41 and an inclination of 25° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in October 1991, more than 7 years prior to its official discovery observation at Haleakala.


(12538) 1998 OH, Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.0280 AU (4,190,000 km; 2,600,000 mi), which corresponds to 10.9 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size. It will pass close to Earth in 2042 and 2132, at a distance of 0.0292 AU and 0.0317 AU, respectively.


(12538) 1998 OH, Physical characteristics
In the SMASS classification, 1998 OH is a common stony S-type asteroid.


(12538) 1998 OH, Physical characteristics, Rotation period
In 2014, several rotational lightcurves of 1998 OH were obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station in California, by the Spanish amateur astronomer group OBAS, and by astronomers of the EURONEAR lightcurve NEO survey. Lightcurve analysis gave a rotation period of 5.154 hours with an alternative period solution of 2.58 hours, or half the period. The asteroid's brightness amplitude is rather low with a maximum between 0.11 and 0.20 magnitude, which is indicative for a spherical rather than elongated shape (U=3/3/2-/3/2/2).


(12538) 1998 OH, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1998 OH measures 1.663 kilometers in diameter and its surface has an albedo of 0.232. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 2.06 kilometers based on an absolute magnitude of 15.8.


(126154) 2001 YH140
(126154) 2001 YH140, also written as (126154) 2001 YH140, is a resonant trans-Neptunian object discovered on 18 December 2001, by American astronomers Chad Trujillo and Michael Brown at the Palomar Observatory in California. It measures approximately 345 kilometers in diameter.


(126154) 2001 YH140, Orbit and rotation
2001 YH140 is locked in 3:5 mean-motion resonance with Neptune. When it makes three revolutions around the Sun, Neptune makes exactly five. The rotation period of (126154) 2001 YH140 is estimated to be 13.25 ± 0.2 hours.


(126154) 2001 YH140, Physical characteristics
In 2010 thermal flux from (126154) 2001 YH140 in the far-infrared was measured by the Herschel Space Telescope. As a result, its size has been estimated to be 300–390 km (190–240 mi).


(126155) 2001 YJ140
(126155) 2001 YJ140, provisionally known as 2001 YJ140, is a resonant trans-Neptunian object from the outermost regions of the Solar System, approximately 154 kilometers in diameter. It discovered on 20 December 2001, by American astronomers Chad Trujillo, Glenn Smith and Michael E. Brown at the Palomar Observatory in California.


(126155) 2001 YJ140, Orbit and rotation
2001 YJ140 is classified as a plutino. Its orbit has a semi-major axis of 42.396 AU and an orbital period of about 249 years. Perihelion leads to 27.881 AU from the Sun and its aphelion in the distance of 51.348 AU.


(127546) 2002 XU93
(127546) 2002 XU93, provisional designation 2002 XU93, is a trans-Neptunian object and centaur on highly inclined and eccentric orbit in the outer region of the Solar System. It measures approximately 170 kilometers (110 mi) in diameter and is one of few objects with such an unusual orbit. It was discovered on 4 December 2002, by American astronomer Marc Buie at the Kitt Peak National Observatory in Arizona, United States.


(127546) 2002 XU93, Orbit and classification
2002 XU93 orbits the Sun at a distance of 21–114 AU once every 552 years and 1 month (201,654 days; semi-major axis of 67.3 AU). Its orbit has an eccentricity of 0.69 and an inclination of 78° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Kitt Peak in December 2002.


(127546) 2002 XU93, Orbit and classification
This object belongs to the short-lived population of centaurs. Generically, it is also classified as a trans-Neptunian object as its semi-major axis is larger than Neptune's 30.1 AU. Due to this highly inclined and eccentric orbit, and with a Tisserand's parameter of only 1.167, its cometary-like orbit resembles that of the damocloid and extended-centaur population. It is one of few objects with and inclination above 60° and a perihelion below 15 AU, along with the first discovered 2008 KV42.


(127546) 2002 XU93, Physical characteristics
2002 XU93 has a BB–BR taxonomy type. It shows only a moderately red surface with a spectral gradient similar to the known comets, extinct comets, Jupiter trojans, Neptune trojans, irregular satellites and damocloids.


(127546) 2002 XU93, Physical characteristics
With a B–R magnitude of 1.2, the difference between the blue and red filter magnitude, it is still redder than the spectrum of the Sun (which is 1.02 mag). It has an absolute magnitude of 8.0.


(127546) 2002 XU93, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2002 XU93 measures 170 kilometers in diameter and its surface has an low albedo of 0.04. The Johnston's archive gives a mean-diameter of 164 kilometers (102 mi) and albedo  of 0.038 from various measurement, while astronomer Michael Brown gives an albedo of 0.04 and a diameter of 180 kilometers (110 mi) from radiometric observations, listing an absolute magnitude of 7.9. Due to its small size, Brown does not consider it to be dwarf-planet candidate, grouping it into the "probably not"-category of his classification scheme (also see list of candidates).


(127546) 2002 XU93, Physical characteristics, Rotation period
As of 2018, no rotational lightcurve of this object has been obtained from photometric observations. The object's rotation period, pole and shape remain unknown.


(127546) 2002 XU93, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 14 March 2006 (M.P.C. 56238). It has not yet received an official name.


(131696) 2001 XT254
(131696) 2001 XT254, provisionally known as 2001 XT254,  is a Kuiper belt object (KBO) that has a 3:7 resonance with Neptune.


(131696) 2001 XT254
Assuming a generic TNO albedo of 0.09, it is about 146 km in diameter.


(131696) 2001 XT254, Resonance
Simulations by Emel’yanenko and Kiseleva in 2007 show that (131696) 2001 XT254 is librating in a 3:7 resonance with Neptune. This libration can be stable for less than 100 million to billions of years.


(131697) 2001 XH255
(131697) 2001 XH255, provisionally known as 2001 XH255,  is a trans-Neptunian object (TNO) that has a 4:5 resonance with Neptune.


(131697) 2001 XH255
Assuming a generic TNO albedo of 0.09, it is about 100 km in diameter.


(131697) 2001 XH255, Resonance
According to the Deep Ecliptic Survey and Minor Planet Center, (131697) 2001 XH255 has a 4:5 resonance with Neptune. It comes as close as 32.2 AU from the Sun and has a fairly low orbital eccentricity of 0.07 with an inclination of only 2.86 degrees.


(131697) 2001 XH255, Resonance
The Neptune 4:5 resonance keeps it more than 7 AU from Neptune over a 14000-year period.


(131697) 2001 XH255, Resonance
It has been observed 21 times over 5 oppositions and has an orbit quality code of 3.


(131697) 2001 XH255, Potential for Exploration
A NASA study in 2019 that confirmed the viability of using small radioisotope or nuclear fission power systems combined with xenon electric propulsion for deep space exploration, used 2001 XH255 as a representative Kuiper Belt Object as the mission's destination to orbit.


(13366) 1998 US24
(13366) 1998 US24, provisional designation 1998 US24, is a Jupiter trojan from the Greek camp, approximately 33 kilometers (21 miles) in diameter. It was discovered on 18 October 1998, by astronomers with the Lowell Observatory Near-Earth-Object Search at the Anderson Mesa Station near Flagstaff, Arizona, in the United States. The dark Jovian asteroid is a slow rotator with a long rotation period of potentially 400 hours. It has not been named since its numbering in January 2000.


(13366) 1998 US24, Orbit and classification
1998 US24 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 4.7–5.8 AU once every 11 years and 12 months (4,367 days; semi-major axis of 5.23 AU). Its orbit has an eccentricity of 0.10 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in February 1954, more than 44 years prior to its official discovery observation at Anderson Mesa.


(13366) 1998 US24, Numbering and naming
This minor planet was numbered by the MPC on 24 January 2000 (M.P.C. 37586). As of 2018, it has not been named.


(13366) 1998 US24, Physical characteristics
1998 US24 is an assumed C-type asteroid, while most larger Jupiter trojans are D-types.


(13366) 1998 US24, Physical characteristics, Rotation period
In August 2015, a first rotational lightcurve of 1998 US24 was obtained from photometric observations by the Kepler space telescope during its K2 mission. Lightcurve analysis gave a rotation period of 400±105 hours with a brightness variation of 0.23 magnitude (U=2-). One month later, a second, lower-rated lightcurve by Kepler determined an alternative period of 522±36 hours with an amplitude of 0.20 (U=1+). As of 2018, no secure period of this slow rotator has yet been obtained.


(13366) 1998 US24, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1998 US24 measures 33.30 kilometers in diameter and its surface has an albedo of 0.058, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 32.03 kilometers based on an absolute magnitude of 11.2.


(13366) 1998 US24, 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.


(136617) 1994 CC
(136617) 1994 CC is a sub-kilometer trinary asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group.


(136617) 1994 CC, Discovery
1994 CC was discovered by Spacewatch's Jim Scotti at Kitt Peak National Observatory on 3 February 1994. In June 2009 it was shown to be a triple system, i.e. the largest body is orbited by two satellites; only about one percent (1%) of near-Earth asteroids observed by a radar are found to be triple systems such as this one. The only other unambiguously identified triple asteroids in the near-Earth population are (153591) 2001 SN263, which was discovered to be a triple system in 2008, and 3122 Florence, which was found to be a triple system in 2017.


(136617) 1994 CC, Observations
A team of NASA's Jet Propulsion Laboratory (JPL) (Pasadena, California) scientists led by Marina Brozovic and Lance Benner, made the discovery using radar imaging at NASA's Goldstone Solar System Radar on June 12 and June 14, 2009. They showed that the near-Earth asteroid 1994 CC is a triple system, which encountered Earth within 2.52 million kilometers on June 10, 2009. This relatively close approach to Earth made the discovery possible, as before the approach, scientists knew very little about this asteroid. In fact, 1994 CC is only the second triple system known in the near-Earth objects population.


(136617) 1994 CC, Observations
1994 CC consists of a central object about 700 meters in diameter that has two moons revolving around it. Scientists' preliminary analysis of the system suggests that the moons are at least 50 meters in diameter. In a similar study, the radar observations at Arecibo Observatory in Puerto Rico, led by the Mike Nolan, also confirmed the detection of all three objects. The scientists plan to use the combined observations from the Goldstone and Arecibo observatories to study 1994 CC's orbital and physical properties further.


(136617) 1994 CC, Observations
The next similar Earth flyby for the asteroid 1994 CC will happen in 2074 when the triple system is projected to fly past Earth at a distance of 2.5 million kilometers.


(136617) 1994 CC, Orbital characteristics of satellites
The orbital properties of the satellites are listed in this table. The orbital planes of both satellites are inclined relative to each other, by approximately 16°. Such a large inclination is suggestive of past evolutionary events (e.g. close encounter with a terrestrial planet, mean-motion resonance crossing) that may have excited their orbits from a coplanar configuration to an inclined state.


(136617) 1994 CC, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 5 December 2006. As of 2019, it has not been named.


(137108) 1999 AN10
(137108) 1999 AN10 is a kilometer-length near-Earth asteroid and potentially hazardous asteroid of the Apollo group. It was discovered by LINEAR on 13 January 1999.


(137108) 1999 AN10
On 7 August 2027, this asteroid will pass at about 0.0026 AU (390,000 km; 240,000 mi; 1.0 LD) of the Earth center. During the close approach, it should peak at about apparent magnitude 7.3, and will be visible in binoculars.


(137108) 1999 AN10
1999 AN10 has a well-determined orbit with an observation arc of 65 years. It was found by Andreas Doppler and Arno Gnädig in precovery images from 1955. When astronomers had an observation arc of the object of 123 days, computations gave a 1 in 10 million chance it would return on an impact trajectory in 2039.


(137108) 1999 AN10
On 7 August 1946, the asteroid passed 0.00625 AU (935,000 km; 581,000 mi) from Earth and then 0.00404 AU (604,000 km; 376,000 mi) from the Moon.


(137924) 2000 BD19
(137924) 2000 BD19, provisional designation 2000 BD19, is a 970-meter asteroid and near-Earth object with the second smallest perihelion of any numbered asteroid (0.092 AU—38% of Mercury's orbital radius). With its high eccentricity, not only does 2000 BD19 get very close to the Sun, but it also travels relatively far away from it. It has the third largest aphelion of any numbered Aten asteroid and is one of a small group of Aten asteroids that is also a Mars grazer. Its orbital elements indicate that it may be an extinct comet, but it hasn't been seen displaying cometary activity so far.


(137924) 2000 BD19
2000 BD19 was discovered by LINEAR in January 2000 and was soon after located by DANEOPS on Palomar plates from 10 February 1997. This allowed a reasonably precise orbit determination, and as a result it was spotted again on 27 February 2001 and 21 January 2002. When it was discovered, it beat 1995 CR's record for both asteroid with the smallest perihelion and for Aten asteroid with the highest eccentricity.


(137924) 2000 BD19
It is estimated that 2000 BD19's surface temperature reaches ~920 K at perihelion, enough to melt lead and zinc, and nearly enough to melt aluminium. 2000 BD19 is considered a good candidate for measuring the effects of Albert Einstein's general theory of relativity because of how close it comes to the Sun.


(137924) 2000 BD19
2000 BD19 shares noticeable orbit similarities with two other low-perihelion asteroids: (425755) 2011 CP4 and 1995 CR, their longitude of perihelion differing by only 9.9 and 7.1 degrees, respectively. Combined with their similar semimajor axis (average distance from the Sun) of 0.877, 0.911, and 0.907 astronomical units respectively, they could possibly be fragments of 2000 BD19 that separated from it in the past.


(139775) 2001 QG298
(139775) 2001 QG298 is a trans-Neptunian object (TNO) that resides in the Kuiper belt and was discovered on 19 August 2001 by Marc William Buie at Cerro Tololo Observatory. It is classified as a plutino, which means that it is in the 3:2 mean motion resonance with Neptune.


(139775) 2001 QG298, Physical properties
2001 QG298 is a small plutino occupying the 3:2 mean motion resonance with Neptune. Its size is estimated at 122 km assuming a comet-like albedo of about 4%.


(139775) 2001 QG298, Physical properties
2001 QG298 has a double peaked light curve with a large amplitude, which has changed from 1.14 in 2003 to 0.7 in 2010. This large amplitude implies that it is actually a contact binary consisting of two elongated components of approximately equal size viewed from almost the equatorial perspective. The size of the components separated by the distance of approximately 300 km will be then about 95 km each. The density of 2001 QG298 should be at least 0.6–0.7 g/cm3 for it to remain bound.


(13E)-labda-7,13-dien-15-ol synthase
(13E)-labda-7,13-dien-15-ol synthase (EC , labda-7,13E-dien-15-ol synthase) is an enzyme with systematic name geranylgeranyl-diphosphate diphosphohydrolase ((13E)-labda-7,13-dien-15-ol-forming). This enzyme catalyses the following chemical reaction


(143649) 2003 QQ47
(143649) 2003 QQ47, provisionally designated: 2003 QQ47, is a kilometer-sized asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It  became briefly notable upon its discovery in late August 2003, when media outlets played up a very preliminary report that it had a 1 in 250,000 chance of impacting into Earth on 21 March 2014. The discovery of a companion, approximately 310 meters (1,000 ft) in diameter, was announced in September 2021.


(143649) 2003 QQ47, Description
2003 QQ47 was discovered on 24 August 2003. It was added to the Sentry Risk Table on 30 August 2003. By 31 August 2003 (with an observation arc of 7 days) the odds of an impact on 21 March 2014 were already reduced to 1 in 1.7 million. The asteroid was removed from the Sentry Risk Table on 14 September 2003, indicating there is no risk of an impact by it in the next 100 years.


(143649) 2003 QQ47, Description
2003 QQ47 safely passed within 0.1283 AU (19,190,000 km; 11,930,000 mi) of Earth on 26 March 2014. With an observation arc of 10 years and an orbital uncertainty of 0, its orbit and future close approaches are well-determined.


(143649) 2003 QQ47, Preliminary reports
Newly discovered asteroid 2003 QQ47 has received considerable media attention over the last few days because it had a small chance of colliding with the Earth in the year 2014 and was rated a "1" on the Torino Impact Hazard Scale, which goes from 0 to 10. The odds of collision in 2014, as estimated by JPL's Sentry impact monitoring system, peaked at 1 chance in 250,000, a result which was posted on our Impact Risk Page on Saturday, August 30, 2003. Impact events at the Torino Scale 1 level certainly merit careful monitoring by astronomers, but these events do not warrant public concern. In fact, each year several newly discovered asteroids reach Torino Scale 1 for a brief period after discovery; 2003 QQ47 is the fourth such case this year.


(143649) 2003 QQ47, Preliminary reports
On September 2, 2003, new measurements of 2003 QQ47's position allowed us to narrow our prediction of its path in 2014, and thus we could rule out any Earth impact possibilities for 2014.


(143649) 2003 QQ47, Preliminary reports
2003 QQ47 has a diameter of approximately 1.24 km, and a mass of approximately 2.0×1012 kg. If it were to hit the Earth, it would be a major event, with an energy of approximately 350,000 megatons of TNT (1.5 ZJ), enough to cause global damage.


(143649) 2003 QQ47, Preliminary reports
Sara Russell, a meteorite researcher at London's Natural History Museum, told the BBC on 2 September 2003 that she was not worried that 2003 QQ47 would be a danger; "The odds are very, very low ... We have to keep some kind of perspective", she said.


(143649) 2003 QQ47, Preliminary reports
As a result of the press coverage of asteroids such as 2003 QQ47, astronomers are now planning to re-word the Torino scale, or to phase it out completely in favour of a scale that is less likely to generate false alarms that may reduce public confidence in genuine alerts.


(143649) 2003 QQ47, Binary system
A minor-planet moon, provisionally designated S/2021 (143649) 1, was first detected on 29 August 2021, by Petr Pravec, Peter Kušnirák, Kamil Hornoch, and others using photometric data from ESO's La Silla Observatory in Chile. The discovery was announced on 17 September 2021. The secondary measures a third the size of its primary (Ds/Dp-ratio of 0.33), resulting in a mean-diameter of approximately 310 meters. It is estimated to be tidally locked, orbiting 1.4 kilometers (4,600 ft) from the primary every 13.065 hours. The primary has a rotation period of 2.6446±0.0007 hours and a derived diameter of 0.94±0.40 kilometers, for a resulting effective diameter (system) of 0.995±0.42 kilometers.


(143651) 2003 QO104
(143651) 2003 QO104, provisional designation 2003 QO104, is a stony asteroid, slow rotator and suspected tumbler on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Amor and Apollo group, respectively. It was discovered on 31 August 2003, by astronomers of the Near-Earth Asteroid Tracking program at the Haleakala Observatory in Hawaii, United States. The Q-type asteroid has a rotation period of 114.4 hours and possibly an elongated shape. It measures approximately 2.3 kilometers (1.4 miles) in diameter and belongs the largest potentially hazardous asteroids known to exist.


(143651) 2003 QO104, Orbit and classification
2003 QO104 is a member of the Apollo group of asteroids, which are Earth-crossing asteroids. They are the largest group of near-Earth objects with approximately 10 thousand known members. As it just grazes the orbit of Earth, the Minor Planet Center (MPC), groups it to the non-Earth crossing Amor asteroids.


(143651) 2003 QO104, Orbit and classification
It orbits the Sun at a distance of 1.015–3.3 AU once every 3 years and 1 month (1,140 days; semi-major axis of 2.14 AU). Its orbit has an eccentricity of 0.52 and an inclination of 12° with respect to the ecliptic. The body's observation arc begins with a precovery taken at the Siding Spring Observatory on in July 1981, more than 18 years prior to its official discovery observation at Haleakala.


(143651) 2003 QO104, Orbit and classification, Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.0042 AU (628,000 km; 390,000 mi), which corresponds to 1.6 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size. On the Torino Scale, this object was rated level 1 in early October 2003, and removed on 13 October 2003.


(143651) 2003 QO104, Orbit and classification, Close approaches
On 18 May 1985, it passed Earth at a nominal distance of 0.00709 AU (2.76 LD) which translates into 1,060,648 km (659,000 mi) and made another approach in June 2009 at a much larger distance of 37 LD. In 2034, 2037 and 2062, it will pass Earth at a distance of 0.18 AU, 0.44 AU and 0.045 AU, respectively. It frequently approaches Jupiter at 1.7–2.0 AU as well.


(143651) 2003 QO104, Physical characteristics
2003 QO104 has been characterized as an uncommon Q-type asteroid, that falls into the larger stony S-complex.


(143651) 2003 QO104, Physical characteristics, Slow rotator and tumbler
Several rotational lightcurve of this asteroid were obtained from photometric observations during its close approach to the Earth in 2009. Analysis of the best-rated lightcurve – obtained by Brian Warner at his Palmer Divide Observatory in collaboration with Robert Stephens and Albino Carbognani – gave a well-defined rotation period of 114.4 hours with a high brightness amplitude of 1.60 magnitude (U=3), which is indicative of an elongated shape. With a period of more than 100 hours, 2003 QO104 is a slow rotator as most asteroids typically rotate every 2 to 20 hours once around their axis. The asteroid also shows several characteristics of a non-principal axis-rotation, which is commonly known as tumbling.


(143651) 2003 QO104, Physical characteristics, Slow rotator and tumbler
This asteroid has also been studied by radar at the Goldstone and Arecibo observatories by Lance Benner and Mike Nolan.


(143651) 2003 QO104, Physical characteristics, Diameter and albedo
According to post-cryogenic observations made by the Spitzer Telescope during the ExploreNEOs survey, this asteroid measures 2.29 and 2.31 kilometers in diameter and its surface has an albedo between 0.13 and 0.14, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 1.88 kilometers based on an absolute magnitude of 16.0.


(143651) 2003 QO104, Naming
This minor planet was numbered by the MPC on 5 December 2006 (M.P.C. 58189). As of 2018, it has not been named.


(144897) 2004 UX10
(144897) 2004 UX10 is a Kuiper-belt object. It has a diameter of about 360 kilometres (220 mi) and was discovered by Andrew Becker, Andrew Puckett and Jeremy Kubica on 20 October 2004 at Apache Point Observatory in Sunspot, New Mexico. The object is classified as a cubewano. It is near a 2:3 resonance with Neptune.


(144897) 2004 UX10
Brown estimates it is likely a dwarf planet based on its presumed size, calculated from its absolute magnitude (H) and assumed albedo.


(144897) 2004 UX10, Orbit and rotation
Based on an integration of its motion over 10 million years, (144897) 2004 UX10 has been classified as a classical Kuiper belt object (cubewano). It is near a 2:3 resonance with Neptune. The object is currently at 39 AU from the Sun.


(144897) 2004 UX10, Orbit and rotation
The rotational period of (144897) 2004 UX10 is 5.68 h.


(144897) 2004 UX10, Physical properties
The size of (144897) 2004 UX10 was measured by the Herschel Space Telescope to be 361+124−94 km. The mass of the object is currently unknown but should be greater than about 3×1019 kg.


(144897) 2004 UX10, Physical properties
(144897) 2004 UX10 has a moderately red slope in the visible spectral range. Its visible spectrum does not show any features, although there is a small departure from the linearity near 0.8 μm.


(144898) 2004 VD17
(144898) 2004 VD17, provisional designation 2004 VD17, is a sub-kilometer asteroid, classified as near-Earth object of the Apollo group once thought to have a low probability of impacting Earth on 4 May 2102.


(144898) 2004 VD17, Description
From February to May 2006, 2004 VD17 was listed with a Torino Scale impact risk value of 2, only the second asteroid in risk-monitoring history to be rated above value 1. The Torino rating was lowered to 1 after additional observations on 20 May 2006, and finally dropped to 0 on 17 October 2006. It was removed from the Sentry Risk Table on 14 February 2008.


(144898) 2004 VD17, Description
As of 4 January 2008, the Sentry Risk Table assigned 2004 VD17 a Torino value of 0 and an impact probability of 1 in 58.8 million for 4 May 2102. This value was far below the background impact rate of objects this size.


(144898) 2004 VD17, Description
2004 VD17 was discovered on 7 November 2004, by the NASA-funded LINEAR asteroid survey. The object is estimated by NASA's Near Earth Object Program Office to be 580 meters in diameter with an approximate mass of 2.6×1011 kg.


(144898) 2004 VD17, Description
It will pass 0.02 AU (3,000,000 km; 1,900,000 mi) from the Earth on 1 May 2032, allowing a refinement to the orbit.


(144898) 2004 VD17, Description
Being approximately 580 meters in diameter, if 2004 VD17 were to impact land, it would create an impact crater about 10 kilometres wide and generate an earthquake of magnitude 7.4.


(144908) 2004 YH32
(144908) 2004 YH32, provisional designation 2004 YH32, is a centaur and damocloid orbiting the Sun with a very high inclination of almost 80°. It was discovered on 18 December 2004 by the Siding Spring Survey at the Siding Spring Observatory in Australia. The critical and unusual object measures approximately 12 kilometers (7.5 miles) in diameter.


(144908) 2004 YH32, Orbit and classification
It orbits the Sun at a distance of 3.6–12.8 AU once every 23 years and 4 months (8,520 days; semi-major axis of 8.16 AU). Its orbit has an eccentricity of 0.57 and an inclination of 79° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at the Siding Spring Observatory in December 2004.


(144908) 2004 YH32, Physical characteristics
Johnston's Archive assumes a standard albedo of 0.09 and calculates a diameter of 12 kilometers based on an absolute magnitude of 12.9.


(145451) 2005 RM43
(145451) 2005 RM43, provisionally known as 2005 RM43, is a trans-Neptunian object that resides in the scattered disc region beyond the Kuiper belt. It was discovered on 9 September 2005, by American astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica at Apache Point Observatory in Sunspot, New Mexico. It measures approximately 500-600 kilometers in diameter.


(145451) 2005 RM43, Description
2005 RM43 is considered likely to be a dwarf planet by both Brown and Tancredi. Based on an absolute magnitude of 4.4, the body's diameter could be anywhere in the range of 350 to 800 kilometres (km), depending on its albedo, the surface reflectivity of the object. Johnston's Archive gives an estimate of 584 km, based on an assumed albedo of 0.09. Brown estimates a diameter of 524 km, based on an absolute magnitude of 4.8 and an assumed albedo of 0.08. A stellar occultation by 2005 RM43 in December 2018 gave a minimum diameter of 458 km.


(145451) 2005 RM43, Description
In 2018, two stellar occultations by 2005 RM43 were observed on 3 February and 24 December. Observations of the February occultation yielded a single chord length of 456 km (283 mi). Observations of the December occultation yielded two positive chords, which suggest an approximate diameter of 644 km (400 mi) for 2005 RM43.


(145451) 2005 RM43, Description
It has been observed 303 times over 17 oppositions, with precovery images dating back to 1976. The orbit is well determined with an uncertainty parameter of 2.


(145452) 2005 RN43
(145452) 2005 RN43, also written as (145452) 2005 RN43, is a classical Kuiper belt object. It has an estimated diameter of 679+55−73 km. It was discovered by Andrew Becker, Andrew Puckett and Jeremy Kubica on 10 September 2005 at Apache Point Observatory in Sunspot, New Mexico. Brown estimates that it is possibly a dwarf planet.


(145452) 2005 RN43, Classification
The Minor Planet Center (MPC) classifies it as a cubewano. But since this object has an inclination of 19.3°, the Deep Ecliptic Survey (DES) classifies it as scattered-extended.


(145452) 2005 RN43, Classification
It has been observed 119 times over thirteen oppositions, with precovery images back to 1954.


(145453) 2005 RR43
(145453) 2005 RR43, also written as (145453) 2005 RR43, is a trans-Neptunian object (TNO) estimated to be about 250 km in diameter. It was discovered on 9 September 2005 by Andrew Becker, Andrew Puckett and Jeremy Kubica at Apache Point Observatory in Sunspot, New Mexico.


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


(145453) 2005 RR43, Surface
The surface is covered by water ice as attested by deep absorption at 1.5 and 2 μm in the infrared spectrum and neutral (i.e. non-red) colour. Scattering models reveal that the observed water ice is, at least in a significant fraction, crystalline and organics, detected on the surface of many TNOs, are completely absent. These physical and orbital characteristics common with Haumea led to suggestion that 2005 RR43 is a member of the Haumea collisional family. The object, together with other members of the family ((19308) 1996 TO66, (24835) 1995 SM55, (55636) 2002 TX300 and (120178) 2003 OP32), would be created from ice mantle ejected from the proto-Haumea as result of a collision with another large (around 1,660 kilometres (1,030 mi)) body.


(145480) 2005 TB190
(145480) 2005 TB190, provisionally known as 2005 TB190, is a trans-Neptunian object (TNO) with an absolute magnitude of 4.4, making it a likely dwarf planet.


(145480) 2005 TB190, Orbit
(145480) 2005 TB190 is classified as scattered-extended by the Deep Ecliptic Survey (DES), because its orbit appears to be beyond significant gravitational interactions with Neptune's current orbit. However, if Neptune migrated outward, there would have been a period when Neptune had a higher eccentricity. The aphelion of (145480) 2005 TB190 lies at 104 AU.


(145480) 2005 TB190, Orbit
Simulations by Emel’yanenko and Kiseleva in 2007 showed that (145480) 2005 TB190 appears to have less than a 1% chance of being in a 4:1 resonance with Neptune.


(145480) 2005 TB190, Orbit
It has been observed 202 times over seven oppositions. It will come to perihelion in January 2017. There are precovery observations dating back to November 2001.


(145480) 2005 TB190, Physical properties
In 2010, thermal flux from (145480) 2005 TB190 in the far-infrared was measured by the Herschel Space Telescope. As a result, its size was estimated to lie within a range from 335 to 410 km.


(145480) 2005 TB190, Physical properties
In the visible light, (145480) 2005 TB190 has a moderately red spectral slope.


(145480) 2005 TB190, Physical properties
The TNO was found in 2009 to have a rotation period of 12.68 ±3 hours, a common value for trans-Neptunian objects of its size. Similarly-sized (120348) 2004 TY364 has a rotation period of 11.7 ± 3 hours.


(148209) 2000 CR105
(148209) 2000 CR105 is a trans-Neptunian object and the tenth-most-distant known object in the Solar System as of 2015. Considered a detached object, it orbits the Sun in a highly eccentric orbit every 3305 years at an average distance of 222 astronomical units (AU).


(148209) 2000 CR105, Description
Mike Brown's website lists it as a possible dwarf planet with a diameter of 328 kilometres (204 mi) based on an assumed albedo of 0.04 . The albedo is expected to be low because the object has a blue (neutral) color. However, if the albedo is higher, the object could easily be half that size.


(148209) 2000 CR105, Description
(148209) 2000 CR105 and Sedna differ from scattered-disc objects in that they are not within the gravitational influence of the planet Neptune even at their perihelion distances (closest approaches to the Sun). It is something of a mystery as to how these objects came to be in their current, far-flung orbits. Several hypotheses have been put forward:


(148209) 2000 CR105, Description
(148209) 2000 CR105 is the first object discovered in the Solar System to have a semi-major axis exceeding 150 AU, a perihelion beyond Neptune, and an argument of perihelion of 340°±55°. It is one of eleven objects known with a semi-major axis greater than 100 AU and perihelion beyond 42 AU. It may be influenced by Planet Nine.


(148975) 2001 XA255
(148975) 2001 XA255, provisional designation: 2001 XA255, is a dark minor planet in the outer Solar System, classified as centaur, approximately 38 kilometers (24 miles) in diameter. It was discovered on 9 December 2001, by David C. Jewitt, Scott S. Sheppard, and Jan Kleyna observing from the Mauna Kea Observatory. The object is currently trapped in a 1:1 mean-motion resonance with Neptune following a path of the horseshoe type.


(148975) 2001 XA255, Orbit and classification
2001 XA255 follows a very eccentric orbit (0.68) with perihelion just inside the orbit of Saturn, aphelion in the trans-Neptunian belt and a semi-major axis of 28.9 AU. The orbital inclination of this object is moderate at 12.6º.


(148975) 2001 XA255, Orbit and classification, Resonance with Neptune
2001 XA255 was identified as trapped in a 1:1 mean-motion resonance with Neptune and 1:2 with Uranus by T. Gallardo in 2006. The object is dynamically unstable and it entered the region of the giant planets relatively recently, perhaps 50,000 years ago, from the scattered disk. It follows a short-lived horseshoe orbit around Neptune.


(148975) 2001 XA255, Physical characteristics
The object has an estimated diameter of 12.5 km and it was classified as an inactive centaur by David Jewitt. Observations by the NEOWISE mission gave a larger diameter of 37.7 kilometers and an albedo of 0.041. It has an absolute magnitude is 11.1.


(152680) 1998 KJ9
(152680) 1998 KJ9 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. Based on absolute magnitude, it is the third largest asteroid known to have passed closer than the Moon.


(152680) 1998 KJ9, Description
It was discovered on 27 May 1998, by astronomers of the Lincoln Near-Earth Asteroid Research (LINEAR) at Lincoln Laboratory's ETS near Socorro, New Mexico, at an apparent magnitude of 17.6 using a 1.0-meter (39 in) reflector. It was tracked through 9 June 1998. It was recovered on 28 December 2003 which extended the observation arc by 5 years. Two precovery images from January 1990 extended the observation arc by 8 years.


(152680) 1998 KJ9, Description
Based on an absolute magnitude of 19.4, the asteroid has an estimated diameter of about 500 metres (1,600 ft). (152680) 1998 KJ9 is noted for a close approach to the Earth on 31 December 1914 at a distance of 0.00155 AU (232,000 km; 144,000 mi). It is one of the largest objects known to have come inside the orbit of the moon. During the 1914 close approach the asteroid reached about apparent magnitude 7.7.


(153201) 2000 WO107
(153201) 2000 WO107 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Aten group with a very well determined orbit. It was discovered on 29 November 2000, by astronomers of the Lincoln Near-Earth Asteroid Research (LINEAR) at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. It is a contact binary.


(153201) 2000 WO107, Orbit
The orbit of this potentially hazardous asteroid (PHA) has been well-established with 20 years of observations. It orbits from inside the orbit of Mercury out to the orbit of Mars. It makes close approaches to all of the inner planets.


(153201) 2000 WO107, Orbit, 2020
The asteroid came to perihelion on 13 October 2020 when it passed the Sun going 88 kilometers per second (320,000 kilometers per hour). The asteroid was not more than 60 degrees from the Sun until 26 November 2020 and was observed by Goldstone radar on 27 November 2020. On 29 November 2020 the asteroid passed 0.02876 AU (4.302 million km; 11.19 LD) from Earth. Even the 2018 orbit solution had a known accuracy of roughly ±150 km for the close approach. With the radar observations the close approach distance is known with an accuracy of roughly ±5 km.


(153201) 2000 WO107, Orbit, 2140
This asteroid will pass 0.00162 AU (242 thousand km; 0.63 LD) from Earth on 1 December 2140. The 2140 close approach distance is known with an accuracy of roughly ±1000 km. For comparison, the distance to the Moon is about 0.0026 AU (384,400 km).


(153201) 2000 WO107, Orbit, 2140
The Jupiter Tisserand invariant, used to distinguish different kinds of orbits, is 6.228.


(153201) 2000 WO107, Physical characteristics
In the SMASS classification, the object's spectral type is that of an X-type. According to the space-based survey by NASA's NEOWISE mission, the asteroid measures 510 meters in diameter and its surface has an albedo of 0.129.


(153201) 2000 WO107, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 2 April 2007. As of 2018, it has not been named.


(153591) 2001 SN263
(153591) 2001 SN263 is a carbonaceous trinary asteroid, classified as near-Earth object and former potentially hazardous asteroid of the Amor group, approximately 2.6 kilometers (1.6 miles) in diameter. It was discovered by the Lincoln Near-Earth Asteroid Research project at Lincoln Lab's Experimental Test Site in Socorro, New Mexico, on 20 September 2001. The two synchronous minor-planet moons measure approximately 770 and 430 meters and have an orbital period of 16.46 and 150 hours, respectively.


(153591) 2001 SN263, Numbering and naming
This minor planet was numbered by the Minor Planet Center on 2 April 2007. As of 2018, the primary and its moons have not been named. In the scientific literature, the components of the trinary system are generically referred to as Alpha, Beta and Gamma, but these labels are not recognized by the IAU.


(153591) 2001 SN263, Primary
2001 SN263, the primary object of this trinary system, is an unusual carbonaceous near-Earth asteroid of a C- or somewhat brighter B-type. It orbits the Sun at a distance of 1.0–2.9 AU once every 2 years and 10 months (1,023 days). Its orbit has an eccentricity of 0.48 and an inclination of 7° with respect to the ecliptic. A first precovery was taken at Palomar Observatory during the Digitized Sky Survey in 1990, extending the body's observation arc by 11 years prior to its official discovery observation at Socorro.


(153591) 2001 SN263, Primary
It has an Earth minimum orbital intersection distance (MOID) of 0.0520 AU (7,780,000 km), which translates into 20.3 lunar distances. With an Earth MOID above 0.05 AU, 2001 SN263 is no longer a potentially hazardous asteroid, but it was classified as such by the MPC until early 2017.


(153591) 2001 SN263, Primary
Radar observations show that it measures 2.5 kilometers in diameter. Its surface has a low albedo of 0.048. Rotational lightcurves obtained from photometric observations gave a rotation period of 3.423 hours (best result) with a brightness variation between 0.13 and 0.27 magnitude (U=2/3/3). Radar observations gave a concurring period of 3.4256 hours, and subsequent modeling of both radiometric and photometric observations gave a spin axis of (309.0°, −80.0°) in ecliptic coordinates (λ, β).


(153591) 2001 SN263, Trinary system
In 2008, scientists using the planetary radar at Arecibo Observatory discovered that the object is orbited by two satellites, when the triple asteroid made a close approach to Earth of 0.066 AU (nearly 10 million kilometers). The largest body (preliminarily called Alpha) is spheroid in shape, with principal axes of 2.8±0.1 km, 2.7±0.1 km, and 2.9±0.3 km, with an effective diameter of 2.5±0.3 km and a density of 1.1±0.2 g/cm3. The satellites, named Beta and Gamma, are several times smaller in size. Beta is 0.77±0.12 km in diameter and Gamma 0.43±0.14 km.


(153591) 2001 SN263, Trinary system
The only other unambiguously identified triple asteroids in the near-Earth population are (136617) 1994 CC, which was discovered to be a triple system in 2009, and 3122 Florence, which was found to be a triple system in September 2017.


(153591) 2001 SN263, Trinary system, Orbital characteristics of satellites
The orbital properties of the satellites are listed in this table. The orbital planes of both satellites are inclined relative to each other; the relative inclination is about 14 degrees. Such a large inclination is suggestive of past evolutionary events (e.g. close encounter with a terrestrial planet, mean-motion-resonance crossing) that may have excited their orbits from a coplanar configuration to an inclined state.


(153591) 2001 SN263, Exploration
This triple asteroid system is the target for the planned ASTER mission scheduled for launch in 2021 by the Brazilian Space Agency.


(153814) 2001 WN5
(153814) 2001 WN5 is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group.


(153814) 2001 WN5, Description
It was discovered by the Lowell Observatory Near-Earth-Object Search at Anderson Mesa Station on 20 November 2001, The potentially hazardous asteroid was removed from the Sentry Risk Table on 30 January 2002.


(153814) 2001 WN5, Description
There are precovery images dating back to 10 February 1996. The orbit is well determined with an observation arc of 14.9 years which includes two radar delay observations. It has an Uncertainty Parameter of 0.


(153814) 2001 WN5, Description
The asteroid will pass within 250,000 km (0.65 lunar distances) from the Earth on 26 June 2028. During the close approach, the asteroid should peak at about apparent magnitude 6.7, and will be visible in binoculars. It has an absolute magnitude (H) of 18.2.


(153814) 2001 WN5, Description
According to observations by the NEOWISE mission, the asteroid measures approximately 0.9 km in diameter and its surface has a rather low albedo of 0.097.