id string | question string | answer string | documents list |
|---|---|---|---|
(184212)_2004_PB112_8505668 | What information does the article about '(184212) 2004 PB112' provide on 'Physical characteristics'? | Based on a generic conversion from an absolute magnitude of 7.2, measures between 100 and 220 kilometer in diameter. Johnston's Archive estimates a mean-diameter of 154 km assuming a typical albedo of 0.09. | [
"(184212) 2004 PB112 β Physical characteristics\n\nBased on a generic conversion from an absolute magnitude of 7.2, measures between 100 and 220 kilometer in diameter. Johnston's Archive estimates a mean-diameter of 154 km assuming a typical albedo of 0.09.",
"(184212) 2004 PB112 β Numbering and naming\n\nThis m... |
(184212)_2004_PB112_8505667 | What information does the article about '(184212) 2004 PB112' provide on 'Numbering and naming'? | This minor planet was numbered (184212) by the Minor Planet Center on 20 April 2008 (M.P.C. 62608). , it has not been named. | [
"(184212) 2004 PB112 β Physical characteristics\n\nBased on a generic conversion from an absolute magnitude of 7.2, measures between 100 and 220 kilometer in diameter. Johnston's Archive estimates a mean-diameter of 154 km assuming a typical albedo of 0.09.",
"(184212) 2004 PB112 β Numbering and naming\n\nThis m... |
(184212)_2004_PB112_8505666 | Explain what '(184212) 2004 PB112' covers in the 'Orbit and classification' section. | orbits the Sun at a distance of 35.3β184.6 AU once every 1153 years and 2 months (421,205 days; semi-major axis of 109.97 AU). Its orbit has a high eccentricity of 0.68 and an inclination of 15Β° with respect to the ecliptic. A first precovery was taken at Cerro Tololo in 2000, extending the body's observation arc by 4 ... | [
"(184212) 2004 PB112 β Physical characteristics\n\nBased on a generic conversion from an absolute magnitude of 7.2, measures between 100 and 220 kilometer in diameter. Johnston's Archive estimates a mean-diameter of 154 km assuming a typical albedo of 0.09.",
"(184212) 2004 PB112 β Numbering and naming\n\nThis m... |
(184212)_2004_PB112_8505665 | Summarize the following section from the article on '(184212) 2004 PB112'. | , prov. designation:, is a trans-Neptunian object from the scattered disc, approximately 154 km in diameter, and in a rare high-order orbital resonance ratio (4:27) with Neptune. It was discovered on 13 August 2004, by American astronomer Marc Buie at the Cerro Tololo Inter-American Observatory in Chile. | [
"(184212) 2004 PB112 β Physical characteristics\n\nBased on a generic conversion from an absolute magnitude of 7.2, measures between 100 and 220 kilometer in diameter. Johnston's Archive estimates a mean-diameter of 154 km assuming a typical albedo of 0.09.",
"(184212) 2004 PB112 β Numbering and naming\n\nThis m... |
(185851)_2000_DP107_1476667 | Based on the article about '(185851) 2000 DP107', describe the 'Binary system' section. | The 800-meter-diameter primary and the 300-meter-diameter secondary orbit each other with a separation of 2.6 kilometers and a period of 1.76 days. The primary is spheroidal and is spinning at a rate near the breakup point for strengthless bodies. These two features were observed in multiple binary systems, suggesting ... | [
"(185851) 2000 DP107 β Binary system\n\nThe 800-meter-diameter primary and the 300-meter-diameter secondary orbit each other with a separation of 2.6 kilometers and a period of 1.76 days. The primary is spheroidal and is spinning at a rate near the breakup point for strengthless bodies. These two features were obse... |
(185851)_2000_DP107_1476669 | Reconstruct the content about 'Numbering and naming' from the article on '(185851) 2000 DP107'. | This minor planet was numbered by the Minor Planet Center on 20 May 2008. As of 2018, it has not been named. | [
"(185851) 2000 DP107 β Binary system\n\nThe 800-meter-diameter primary and the 300-meter-diameter secondary orbit each other with a separation of 2.6 kilometers and a period of 1.76 days. The primary is spheroidal and is spinning at a rate near the breakup point for strengthless bodies. These two features were obse... |
(185851)_2000_DP107_1476666 | Summarize the 'Orbit' part of '(185851) 2000 DP107'. | orbits the Sun at a distance of 0.9β1.9 AU once every 19 months (583 days). Its orbit has an eccentricity of 0.38 and an inclination of 9Β° with respect to the ecliptic. The body's observation arc begins with its official discovery observation, as no precoveries were taken, and no prior identifications were made. | [
"(185851) 2000 DP107 β Binary system\n\nThe 800-meter-diameter primary and the 300-meter-diameter secondary orbit each other with a separation of 2.6 kilometers and a period of 1.76 days. The primary is spheroidal and is spinning at a rate near the breakup point for strengthless bodies. These two features were obse... |
(185851)_2000_DP107_1476665 | What does the article about '(185851) 2000 DP107' say regarding 'Discovery'? | The asteroid was discovered on 29 February 2000, by the Lincoln Near-Earth Asteroid Research (LINEAR) program at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico. The binary nature of this asteroid was suggested from radar observations taken with the Goldstone radar antenna on September 22 and 23, ... | [
"(185851) 2000 DP107 β Binary system\n\nThe 800-meter-diameter primary and the 300-meter-diameter secondary orbit each other with a separation of 2.6 kilometers and a period of 1.76 days. The primary is spheroidal and is spinning at a rate near the breakup point for strengthless bodies. These two features were obse... |
(185851)_2000_DP107_1476668 | Describe the 'Physical characteristics' section of the article about '(185851) 2000 DP107'. | The asteroid is characterized as both a carbonaceous C-type and metallic M-type asteroid. The density of the primary was calculated using the orbital elements of the binary system, the primary-to-secondary mass ratio, and estimates of the primary size. The primary has a low density of 1.7 g/cm3, which may indicate a "r... | [
"(185851) 2000 DP107 β Binary system\n\nThe 800-meter-diameter primary and the 300-meter-diameter secondary orbit each other with a separation of 2.6 kilometers and a period of 1.76 days. The primary is spheroidal and is spinning at a rate near the breakup point for strengthless bodies. These two features were obse... |
(190166)_2005_UP156_30962240 | Reconstruct the content about 'Diameter and albedo' from the article on '(190166) 2005 UP156'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.045 kilometers in diameter and its surface has an albedo of 0.234, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 1.08... | [
"(190166) 2005 UP156 β Physical characteristics\n\nis an assumed S-type asteroid.",
"(190166) 2005 UP156 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.045 kilometers in diameter and its surface has an albedo of 0.234, ... |
(190166)_2005_UP156_30962239 | From the article on '(190166) 2005 UP156', restate the 'Rotation period' content. | Since 2004, several rotational lightcurves of were obtained from photometric observations by French amateur astronomers David Romeuf, RenΓ© Roy, as well as by American astronomer Brian Warner. Analysis of the best-rated lightcurve gave a rotation period of 40.542 hours with a brightness variation of 1.1 magnitude (U=2/3... | [
"(190166) 2005 UP156 β Physical characteristics\n\nis an assumed S-type asteroid.",
"(190166) 2005 UP156 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.045 kilometers in diameter and its surface has an albedo of 0.234, ... |
(190166)_2005_UP156_30962235 | Summarize the following section from the article on '(190166) 2005 UP156'. | is a stony asteroid and binary system, classified as near-Earth object of the Apollo group, approximately 1 kilometer in diameter. It was discovered on 31 October 2005, by astronomers of the Spacewatch survey at the Kitt Peak National Observatory in Arizona, United States. Its minor-planet moon with an orbital period o... | [
"(190166) 2005 UP156 β Physical characteristics\n\nis an assumed S-type asteroid.",
"(190166) 2005 UP156 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.045 kilometers in diameter and its surface has an albedo of 0.234, ... |
(190166)_2005_UP156_30962242 | Based on the article about '(190166) 2005 UP156', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 19 August 2008. As of 2018, it has not been named. | [
"(190166) 2005 UP156 β Physical characteristics\n\nis an assumed S-type asteroid.",
"(190166) 2005 UP156 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.045 kilometers in diameter and its surface has an albedo of 0.234, ... |
(190166)_2005_UP156_30962241 | Summarize the 'Binary system' part of '(190166) 2005 UP156'. | In May 2017, photometric observations by Brian Warner and Alan Harris revealed that is a synchronous binary system with a secondary component orbiting around the system barycenter every 40.572 hours. The secondary has been confirmed by radar observations. Its provisional designation is. | [
"(190166) 2005 UP156 β Physical characteristics\n\nis an assumed S-type asteroid.",
"(190166) 2005 UP156 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.045 kilometers in diameter and its surface has an albedo of 0.234, ... |
(190166)_2005_UP156_30962236 | Explain what '(190166) 2005 UP156' covers in the 'Orbit and classification' section. | is an Amor asteroid that approaches the orbit of Earth from beyond but does not cross it. It orbits the Sun at a distance of 1.1β3.1 AU once every 3 years and 1 month (1,124 days). Its orbit has an eccentricity of 0.47 and an inclination of 4Β° with respect to the ecliptic. The body's observation arc begins with a preco... | [
"(190166) 2005 UP156 β Physical characteristics\n\nis an assumed S-type asteroid.",
"(190166) 2005 UP156 β Diameter and albedo\n\nAccording to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 1.045 kilometers in diameter and its surface has an albedo of 0.234, ... |
(1952β19??)_12536763 | Reconstruct the content from the article about '(1952β19??)'. | (1952β19??) is the seventh 12" vinyl record album by DIY home recording pioneer and one-man band R. Stevie Moore. It was released on Alan Jenkins' Cordelia Records label in the UK. "You and Me" was included on Moore's 2012 best-of, Lo Fi High Fives. | [
"(1952β19??)\n\n(1952β19??) is the seventh 12\" vinyl record album by DIY home recording pioneer and one-man band R. Stevie Moore. It was released on Alan Jenkins' Cordelia Records label in the UK. \"You and Me\" was included on Moore's 2012 best-of, Lo Fi High Fives.",
"(1952β19??) β Track listing\n\n1) \"Signal... |
(1952β19??)_12536764 | Explain what '(1952β19??)' covers in the 'Track listing' section. | 1) "Signal" β 2:50 ; 2) "Studio Animal" β :34 ; 3) "Jesus Rocks" β 2:56 ; 4) "Records" β 1:25 ; 5) "The Flavour Is Mine" β 4:33 ; 6) "Sox" β 1:08 ; 7) "Back in Time" β 4:39 ; 8) "Without Cause" β 1:14 ; 9) "Treat Me" β 2:43 ; 10) "Satisfaction" β 2:59 ; 11) "Technical Difficulty" β 2:43 1) "Genus Lupus" β 0:53 ; 2) "Wh... | [
"(1952β19??)\n\n(1952β19??) is the seventh 12\" vinyl record album by DIY home recording pioneer and one-man band R. Stevie Moore. It was released on Alan Jenkins' Cordelia Records label in the UK. \"You and Me\" was included on Moore's 2012 best-of, Lo Fi High Fives.",
"(1952β19??) β Track listing\n\n1) \"Signal... |
(1R,3R)-1,2,3-trimethylcyclopentane_31752283 | Summarize the 'Occurrences' part of '(1R,3R)-1,2,3-trimethylcyclopentane'. | (1R,3R)-1,2,3-trimethylcyclopentane has been identified by the United States Environmental Protection Agency in their Master List of Compounds Emitted by Mobile Sources as a component of mobile source air toxics that can be found in gasoline exhaust and liquefied petroleum gas (LPG) exhaust. Mobile source air toxics ar... | [
"(1R,3R)-1,2,3-trimethylcyclopentane β Occurrences\n\n(1R,3R)-1,2,3-trimethylcyclopentane has been identified by the United States Environmental Protection Agency in their Master List of Compounds Emitted by Mobile Sources as a component of mobile source air toxics that can be found in gasoline exhaust and liquefie... |
(1R,3R)-1,2,3-trimethylcyclopentane_31752280 | Reconstruct the content from the article about '(1R,3R)-1,2,3-trimethylcyclopentane'. | (1R,3R)-1,2,3-trimethylcyclopentane is an organic hydrocarbon alicyclic cycloalkane compound with the molecular formula C8H16. It is a saturated cyclopentane with three methyl substituents branching off carbons 1,2, and 3. The methyl groups off carbons 1 and 3 are trans with respect to each other, while the methyl grou... | [
"(1R,3R)-1,2,3-trimethylcyclopentane β Occurrences\n\n(1R,3R)-1,2,3-trimethylcyclopentane has been identified by the United States Environmental Protection Agency in their Master List of Compounds Emitted by Mobile Sources as a component of mobile source air toxics that can be found in gasoline exhaust and liquefie... |
(1R,3R)-1,2,3-trimethylcyclopentane_31752281 | Describe the content of the article about '(1R,3R)-1,2,3-trimethylcyclopentane'. | angle, 109.5 degrees. However, in a planar molecule such as (1R,3R)-1,2,3-trimethylcyclopentane eclipsing interactions of adjacent C-H, adjacent methyl groups, and adjacent methyl groups & C-H bonds can contribute considerable strain. Therefore, the ring distorts slightly to adopt a minimum energy conformation that red... | [
"(1R,3R)-1,2,3-trimethylcyclopentane β Occurrences\n\n(1R,3R)-1,2,3-trimethylcyclopentane has been identified by the United States Environmental Protection Agency in their Master List of Compounds Emitted by Mobile Sources as a component of mobile source air toxics that can be found in gasoline exhaust and liquefie... |
(1R,3R)-1,2,3-trimethylcyclopentane_31752282 | What information does the article about '(1R,3R)-1,2,3-trimethylcyclopentane' provide on 'Isomers'? | Various stereoisomers exist for (1R,3R)-1,2,3-trimethylcyclopentane. Because (1R,3R)-1,2,3-trimethylcyclopentane is a cycloalkane, its three methyl substituents are capable of exhibiting cis/trans isomerism. This implies that the methyl groups in positions 1,2, and 3 may occupy different spacial arrangements (i.e.they ... | [
"(1R,3R)-1,2,3-trimethylcyclopentane β Occurrences\n\n(1R,3R)-1,2,3-trimethylcyclopentane has been identified by the United States Environmental Protection Agency in their Master List of Compounds Emitted by Mobile Sources as a component of mobile source air toxics that can be found in gasoline exhaust and liquefie... |
(2,1)-Pascal_triangle_27652546 | Summarize the 'Patterns and properties' part of '(2,1)-Pascal triangle'. | (2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence. | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652555 | What information does the article about '(2,1)-Pascal triangle' provide on 'Overall patterns and properties'? | ; style="background:aqua; width:50px;"|35 ; style="background:lime; width:50px;"|9 ; style="background:yellow; width:50px;"|1 ; } bgcolor=lime|9 ; style="background:yellow;"|16 ; style="background:orange;"|14 ; bgcolor=red|6 ; bgcolor=violet|1 ; - align=center ; bgcolor=red|2 ; style="background:violet;"|11 ; style="ba... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652545 | Describe the content of the article about '(2,1)-Pascal triangle'. | In mathematics, the (2,1)-Pascal triangle (mirrored Lucas triangle )is a triangular array. The rows of the (2,1)-Pascal triangle are conventionally enumerated starting with row n = 0 at the top (the 0th row). The entries in each row are numbered from the left beginning with k = 0 and are usually staggered relative to t... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652553 | Summarize the 'Overall patterns and properties' part of '(2,1)-Pascal triangle'. | ; style="background:violet;"|7 ; bgcolor=red|9 ; style="background:orange;"|5 ; style="background:yellow;"|1 ; - align=center ; style="background:violet;"|2 ; bgcolor=red|9 ; style="background:orange;"|16 ; style="background:yellow;"|14 ; bgcolor=lime|6 ; bgcolor=aqua|1 ; - align=center ; bgcolor=red|2 ; style="backgro... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652552 | What does the article about '(2,1)-Pascal triangle' say regarding 'Overall patterns and properties'? | in the grid, count the number of paths there are in the grid (without backtracking) which connect this node to the top node (1) of the triangle. The answer is the Pascal number associated to that node. ; One property of the triangle is revealed if the rows are left-justified. In the triangle below, the diagonal coloure... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652547 | Explain what '(2,1)-Pascal triangle' covers in the 'Rows' section. | Except the row n = 0, 1, The sum of the elements of a single row is twice the sum of the row preceding it. For example, row 1 has a value of 3, row 2 has a value of 6, row 3 has a value of 12, and so forth. This is because every item in a row produces two items in the next row: one left and one right. The sum of the el... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652554 | Describe the 'Overall patterns and properties' section of the article about '(2,1)-Pascal triangle'. | ; - align=center ; style="background:aqua;"|2 ; bgcolor=lime|3 ; bgcolor=yellow|1 ; - align=center ; bgcolor=red|2 ; bgcolor=violet|5 ; style="background:aqua;"|4 ; bgcolor=lime|1 ; - align=center ; bgcolor=yellow|2 ; style="background:orange;"|7 ; bgcolor=red|9 ; style="background:violet;"|5 ; style="background:aqua;"... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652550 | Based on the article about '(2,1)-Pascal triangle', describe the 'Diagonals' section. | The diagonals going along the right edges contain only 1's while the diagonals going along the right edges contain only 2s except the first cell. ; The diagonals next to the left edge diagonal contain the odd numbers in order. ; The diagonals next to the right edge diagonal contain the natural numbers in order. ; Movin... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652549 | Reconstruct the content about 'Rows' from the article on '(2,1)-Pascal triangle'. | term, then add the third term, then subtract, so on and so forth until you reach the end of the row, the result is always equal to 0. ; row 3: 2 β 3 + 1 = 0 ; row 4: 2 β 5 + 4 β 1 = 0 ; row 5: 2 β 7 + 9 β 5 + 1 = 0 ; row 6: 2 β 9 + 16 β 14 + 6 β 1 = 0 ; row 7: 2 β 11 + 25 β 30 + 20 β 7 + 1 = 0 ; row 8: 2 β 13 + 36 β 55... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652548 | Describe the 'Rows' section of the article about '(2,1)-Pascal triangle'. | Example, row 4 is 2 7 9 5 1, so the formula would be 9 β (7 + 5) + (2 + 1) = 0, row 6 is 2 11 25 30 20 7 1, so the formula would be 30 β (25 + 20) + (11 + 7) β (2 + 1) = 0. So every even row of the Pascal triangle equals 0 when you take the middle number, then subtract the integers directly next to the cent... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,1)-Pascal_triangle_27652551 | Describe the 'Overall patterns and properties' section of the article about '(2,1)-Pascal triangle'. | The pattern obtained by coloring only the odd numbers in Pascal's triangle closely resembles the fractal called the Sierpinski triangle. This resemblance becomes more and more accurate as more rows are considered; in the limit, as the number of rows approaches infinity, the resulting pattern is the Sierpinski triangle,... | [
"(2,1)-Pascal triangle β Patterns and properties\n\n(2,1)-Pascal triangle has many properties and contains many patterns of numbers. It can be seen as a sister of the Pascal's triangle, in the same way that a Lucas sequence is a sister sequence of the Fibonacci sequence.",
"(2,1)-Pascal triangle β Overall pattern... |
(2,3,7)_triangle_group_5128109 | Describe the content of the article about '(2,3,7) triangle group'. | In the theory of Riemann surfaces and hyperbolic geometry, the triangle group (2,3,7) is particularly important. This importance stems from its connection to Hurwitz surfaces, namely Riemann surfaces of genus g with the largest possible order, 84(g β 1), of its automorphism group. A note on terminology β the "(2,3,7) t... | [
"(2,3,7) triangle group\n\nIn the theory of Riemann surfaces and hyperbolic geometry, the triangle group (2,3,7) is particularly important. This importance stems from its connection to Hurwitz surfaces, namely Riemann surfaces of genus g with the largest possible order, 84(g β 1), of its automorphism group. A note ... |
(2,3,7)_triangle_group_5128113 | Describe the 'Relation to SL(2,R)' section of the article about '(2,3,7) triangle group'. | Extending the scalars from Q(Ξ·) to R (via the standard imbedding), one obtains an isomorphism between the quaternion algebra and the algebra M(2,R) of real 2 by 2 matrices. Choosing a concrete isomorphism allows one to exhibit the (2,3,7) triangle group as a specific Fuchsian group in SL(2,R), specifically as a quotien... | [
"(2,3,7) triangle group\n\nIn the theory of Riemann surfaces and hyperbolic geometry, the triangle group (2,3,7) is particularly important. This importance stems from its connection to Hurwitz surfaces, namely Riemann surfaces of genus g with the largest possible order, 84(g β 1), of its automorphism group. A note ... |
(2,3,7)_triangle_group_5128112 | What does the article about '(2,3,7) triangle group' say regarding 'Quaternion algebra'? | The (2,3,7) triangle group admits a presentation in terms of the group of quaternions of norm 1 in a suitable order in a quaternion algebra. More specifically, the triangle group is the quotient of the group of quaternions by its center Β±1. Let Ξ· = 2cos(2Ο/7). Then from the identity which descend to the appropriate re... | [
"(2,3,7) triangle group\n\nIn the theory of Riemann surfaces and hyperbolic geometry, the triangle group (2,3,7) is particularly important. This importance stems from its connection to Hurwitz surfaces, namely Riemann surfaces of genus g with the largest possible order, 84(g β 1), of its automorphism group. A note ... |
(2,3,7)_triangle_group_5128111 | Based on the article about '(2,3,7) triangle group', describe the 'Group presentation' section. | about the vertices of the Schwarz triangle. It has a presentation in terms of a pair of generators, g2, g3, modulo the following relations: | [
"(2,3,7) triangle group\n\nIn the theory of Riemann surfaces and hyperbolic geometry, the triangle group (2,3,7) is particularly important. This importance stems from its connection to Hurwitz surfaces, namely Riemann surfaces of genus g with the largest possible order, 84(g β 1), of its automorphism group. A note ... |
(2-Hydroxyethyl)_dimethylsulfoxonium_chloride_15615767 | What does the article about '(2-Hydroxyethyl) dimethylsulfoxonium chloride' say regarding 'Properties'? | (2-Hydroxyethyl) dimethylsulfoxonium chloride is colourless. It dissolves in dioxane, methanol, chloroform or water. (2-Hydroxyethyl) dimethylsulfoxonium chloride is a sulfoxonium compound, with a sulfur atom having a positive charge. Attached to the sulfur are two methyl groups, and oxygen atom, and an ethoxy group at... | [
"(2-Hydroxyethyl) dimethylsulfoxonium chloride β Properties\n\n(2-Hydroxyethyl) dimethylsulfoxonium chloride is colourless. It dissolves in dioxane, methanol, chloroform or water. (2-Hydroxyethyl) dimethylsulfoxonium chloride is a sulfoxonium compound, with a sulfur atom having a positive charge. Attached to the su... |
(20161)_1996_TR66_29066225 | From the article on '(20161) 1996 TR66', restate the 'Orbit and classification' content. | It orbits the Sun at a distance of 28.6β66.6 AU once every 328 years and 8 months (120,032 days). Its orbit has an eccentricity of 0.40 and an inclination of 12Β° with respect to the ecliptic. Near perihelion, it comes closer to the Sun than Neptune does (29.7 AU). It has a semi-major axis (average distance from the Sun... | [
"(20161) 1996 TR66 β Orbit and classification\n\nIt orbits the Sun at a distance of 28.6β66.6 AU once every 328 years and 8 months (120,032 days). Its orbit has an eccentricity of 0.40 and an inclination of 12Β° with respect to the ecliptic. Near perihelion, it comes closer to the Sun than Neptune does (29.7 AU). It... |
(20161)_1996_TR66_29066227 | Summarize the 'Numbering and naming' part of '(20161) 1996 TR66'. | This minor planet was numbered by the Minor Planet Center on 9 January 2001. As of 2018, it has not been named. | [
"(20161) 1996 TR66 β Orbit and classification\n\nIt orbits the Sun at a distance of 28.6β66.6 AU once every 328 years and 8 months (120,032 days). Its orbit has an eccentricity of 0.40 and an inclination of 12Β° with respect to the ecliptic. Near perihelion, it comes closer to the Sun than Neptune does (29.7 AU). It... |
(20161)_1996_TR66_29066224 | What information does the article about '(20161) 1996 TR66' provide? | is a trans-Neptunian object orbiting beyond Pluto in the Kuiper belt of the outermost Solar System, approximately 139 km in diameter. It was discovered on 8 October 1996, by astronomers David Jewitt, Chad Trujillo, Jane Luu, and Jun Chen at the Mauna Kea Observatory, Hawaii, in the United States. It was the first disco... | [
"(20161) 1996 TR66 β Orbit and classification\n\nIt orbits the Sun at a distance of 28.6β66.6 AU once every 328 years and 8 months (120,032 days). Its orbit has an eccentricity of 0.40 and an inclination of 12Β° with respect to the ecliptic. Near perihelion, it comes closer to the Sun than Neptune does (29.7 AU). It... |
(20161)_1996_TR66_29066226 | Describe the 'Twotino' section of the article about '(20161) 1996 TR66'. | was the first twotino discovered. Twotinos stay in a 1:2 orbital resonance with Neptune, which means that for every one orbit a twotino makes, Neptune orbits two times. Both the Minor Planet Center and the Deep Ecliptic Survey list this trans-Neptunian object as a twotino. | [
"(20161) 1996 TR66 β Orbit and classification\n\nIt orbits the Sun at a distance of 28.6β66.6 AU once every 328 years and 8 months (120,032 days). Its orbit has an eccentricity of 0.40 and an inclination of 12Β° with respect to the ecliptic. Near perihelion, it comes closer to the Sun than Neptune does (29.7 AU). It... |
(202421)_2005_UQ513_31936819 | What does the article about '(202421) 2005 UQ513' say regarding 'Classification'? | has a perihelion of 37.3 AU. The Minor Planet Center (MPC) classifies it as a cubewano while the Deep Ecliptic Survey (DES) classifies it as ScatExt (scattered-extended). Although dynamically it would have been a good candidate to be a member of the Haumea collisional family, given its red spectrum, it is not. | [
"(202421) 2005 UQ513 β Classification\n\nhas a perihelion of 37.3 AU. The Minor Planet Center (MPC) classifies it as a cubewano while the Deep Ecliptic Survey (DES) classifies it as ScatExt (scattered-extended). Although dynamically it would have been a good candidate to be a member of the Haumea collisional family... |
(202421)_2005_UQ513_31936818 | Summarize the following section from the article on '(202421) 2005 UQ513'. | , also written as 2005 UQ513, is a cubewano with an absolute magnitude of 3.4. Its spectrum has a weak signature of absorption by water ice. Like Quaoar, it has a very red spectrum, which indicates that its surface probably contains many complex, processed organic molecules. Its light curve shows variations of Ξm=0.3 m... | [
"(202421) 2005 UQ513 β Classification\n\nhas a perihelion of 37.3 AU. The Minor Planet Center (MPC) classifies it as a cubewano while the Deep Ecliptic Survey (DES) classifies it as ScatExt (scattered-extended). Although dynamically it would have been a good candidate to be a member of the Haumea collisional family... |
(202421)_2005_UQ513_31936820 | Summarize the 'Distance' part of '(202421) 2005 UQ513'. | As of December 2018, it is currently 48.0 AU from the Sun. It will come to perihelion in 2123. It has been observed 194 times over 14 oppositions with precovery images back to 1990. | [
"(202421) 2005 UQ513 β Classification\n\nhas a perihelion of 37.3 AU. The Minor Planet Center (MPC) classifies it as a cubewano while the Deep Ecliptic Survey (DES) classifies it as ScatExt (scattered-extended). Although dynamically it would have been a good candidate to be a member of the Haumea collisional family... |
(20729)_1999_XS143_11686103 | Describe the content of the article about '(20729) 1999 XS143'. | , provisional designation:, is a Jupiter trojan from the Greek camp, approximately 51 km in diameter. It was discovered on 15 December 1999, by American astronomer Charles Juels at the Fountain Hills Observatory in Arizona. The dark Jovian asteroid has a short rotation period of 5.72 hours and belongs to the 90 largest... | [
"(20729) 1999 XS143\n\n, provisional designation:, is a Jupiter trojan from the Greek camp, approximately 51 km in diameter. It was discovered on 15 December 1999, by American astronomer Charles Juels at the Fountain Hills Observatory in Arizona. The dark Jovian asteroid has a short rotation period of 5.72 hours an... |
(20729)_1999_XS143_11686108 | What does the article about '(20729) 1999 XS143' say regarding 'Diameter and albedo'? | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, between 50.96 kilometers in diameter and its surface has an albedo of 0.052, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diamete... | [
"(20729) 1999 XS143\n\n, provisional designation:, is a Jupiter trojan from the Greek camp, approximately 51 km in diameter. It was discovered on 15 December 1999, by American astronomer Charles Juels at the Fountain Hills Observatory in Arizona. The dark Jovian asteroid has a short rotation period of 5.72 hours an... |
(20729)_1999_XS143_11686104 | Reconstruct the content about 'Orbit and classification' from the article on '(20729) 1999 XS143'. | is a dark Jovian asteroid orbiting in the leading Greek camp at Jupiter's Lagrangian point, 60Β° ahead of the Gas Giant's orbit in a 1:1 resonance. It is also a non-family asteroid in the Jovian background population. It orbits the Sun at a distance of 4.9β5.5 AU once every 11 years and 11 months (4,352 days; semi-major... | [
"(20729) 1999 XS143\n\n, provisional designation:, is a Jupiter trojan from the Greek camp, approximately 51 km in diameter. It was discovered on 15 December 1999, by American astronomer Charles Juels at the Fountain Hills Observatory in Arizona. The dark Jovian asteroid has a short rotation period of 5.72 hours an... |
(20729)_1999_XS143_11686107 | What does the article about '(20729) 1999 XS143' say regarding 'Rotation period'? | In September 2008, a rotational lightcurve of was obtained from photometric observations. Lightcurve analysis gave a rotation period of 5.72 hours with a brightness variation of 0.33 magnitude (U=2). Observations by Stefano Mottola at the Calar Alto Observatory in October 2009 showed a divergent period of 7.631 hours ... | [
"(20729) 1999 XS143\n\n, provisional designation:, is a Jupiter trojan from the Greek camp, approximately 51 km in diameter. It was discovered on 15 December 1999, by American astronomer Charles Juels at the Fountain Hills Observatory in Arizona. The dark Jovian asteroid has a short rotation period of 5.72 hours an... |
(21601)_1998_XO89_11686036 | From the article on '(21601) 1998 XO89', restate the 'Physical characteristics' content. | is an assumed C-type asteroid. Its VβI color index of 0.97 is typical for that of D-type asteroids, the dominant spectral type among the Jupiter trojans. | [
"(21601) 1998 XO89 β Physical characteristics\n\nis an assumed C-type asteroid. Its VβI color index of 0.97 is typical for that of D-type asteroids, the dominant spectral type among the Jupiter trojans.",
"(21601) 1998 XO89 β Numbering and naming\n\nThis minor planet was numbered on 8 February 2001 (M.P.C. 22480)... |
(21601)_1998_XO89_11686037 | What information does the article about '(21601) 1998 XO89' provide on 'Rotation period'? | In April 2013, a rotational lightcurve of was obtained from photometric observations by Robert Stephens at the Center for Solar System Studies (CS3) in California. Lightcurve analysis gave a rotation period of 12.65 hours and a brightness variation of 0.30 magnitude (U=2+). Observations by his college Brian Warner at ... | [
"(21601) 1998 XO89 β Physical characteristics\n\nis an assumed C-type asteroid. Its VβI color index of 0.97 is typical for that of D-type asteroids, the dominant spectral type among the Jupiter trojans.",
"(21601) 1998 XO89 β Numbering and naming\n\nThis minor planet was numbered on 8 February 2001 (M.P.C. 22480)... |
(21601)_1998_XO89_11686034 | What information does the article about '(21601) 1998 XO89' provide on 'Orbit and classification'? | is a dark Jovian asteroid orbiting in the leading Greek camp at Jupiter's Lagrangian point, 60Β° ahead of the Gas Giant's orbit in a 1:1 resonance. It is also a non-family asteroid in the Jovian background population. It orbits the Sun at a distance of 5.0β5.4 AU once every 11 years and 11 months (4,356 days; semi-major... | [
"(21601) 1998 XO89 β Physical characteristics\n\nis an assumed C-type asteroid. Its VβI color index of 0.97 is typical for that of D-type asteroids, the dominant spectral type among the Jupiter trojans.",
"(21601) 1998 XO89 β Numbering and naming\n\nThis minor planet was numbered on 8 February 2001 (M.P.C. 22480)... |
(21601)_1998_XO89_11686038 | Reconstruct the content about 'Diameter and albedo' from the article on '(21601) 1998 XO89'. | According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 54.91 and 56.08 kilometers in diameter and its surface has an albedo of 0.064 and 0.100, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard albed... | [
"(21601) 1998 XO89 β Physical characteristics\n\nis an assumed C-type asteroid. Its VβI color index of 0.97 is typical for that of D-type asteroids, the dominant spectral type among the Jupiter trojans.",
"(21601) 1998 XO89 β Numbering and naming\n\nThis minor planet was numbered on 8 February 2001 (M.P.C. 22480)... |
(219774)_2001_YY145_13640052 | What information does the article about '(219774) 2001 YY145' provide on 'Slow rotator'? | In October 2013, a rotational lightcurve was obtained of this asteroid from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. It gave a rotation period of 1007.7 hours β or nearly 42 days β with an assigned error margin of Β±86 hours. According to the Light Curve Data ... | [
"(219774) 2001 YY145 β Slow rotator\n\nIn October 2013, a rotational lightcurve was obtained of this asteroid from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. It gave a rotation period of 1007.7 hours β or nearly 42 days β with an assigned error margin of Β±8... |
(219774)_2001_YY145_13640049 | Summarize the following section from the article on '(219774) 2001 YY145'. | ''', provisional designation ' is a stony background asteroid and exceptionally slow rotator from the central region of the asteroid belt, approximately 1.5 km in diameter. It was discovered on 18 December 2001, by astronomers with the Lowell Observatory Near-Earth-Object Search at Anderson Mesa Station near Flagstaff,... | [
"(219774) 2001 YY145 β Slow rotator\n\nIn October 2013, a rotational lightcurve was obtained of this asteroid from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. It gave a rotation period of 1007.7 hours β or nearly 42 days β with an assigned error margin of Β±8... |
(219774)_2001_YY145_13640053 | Based on the article about '(219774) 2001 YY145', describe the 'Diameter and albedo' section. | The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 1.54 kilometers, based on an absolute magnitude of 16.43. | [
"(219774) 2001 YY145 β Slow rotator\n\nIn October 2013, a rotational lightcurve was obtained of this asteroid from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. It gave a rotation period of 1007.7 hours β or nearly 42 days β with an assigned error margin of Β±8... |
(219774)_2001_YY145_13640050 | Reconstruct the content about 'Orbit and classification' from the article on '(219774) 2001 YY145'. | is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main-belt at a distance of 2.2β2.9 AU once every 4 years and 2 months (1,515 days; semi-major axis of 2.58 AU). Its orbit has an eccentricity of 0.13 and an inclination of 10Β° with respect to the ecliptic. A first prec... | [
"(219774) 2001 YY145 β Slow rotator\n\nIn October 2013, a rotational lightcurve was obtained of this asteroid from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. It gave a rotation period of 1007.7 hours β or nearly 42 days β with an assigned error margin of Β±8... |
(219774)_2001_YY145_13640054 | Summarize the 'Numbering and naming' part of '(219774) 2001 YY145'. | This minor planet was numbered by the Minor Planet Center on 4 October 2009. As of 2018, it has not been named. | [
"(219774) 2001 YY145 β Slow rotator\n\nIn October 2013, a rotational lightcurve was obtained of this asteroid from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. It gave a rotation period of 1007.7 hours β or nearly 42 days β with an assigned error margin of Β±8... |
(231937)_2001_FO32_4157579 | What does the article about '(231937) 2001 FO32' say regarding 'Discovery'? | was discovered on 23 March 2001 by the Lincoln Near-Earth Asteroid Research (LINEAR) at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico. The asteroid was first observed in the constellation Hydra at an apparent magnitude of 15.6. Shortly after discovery, follow-up observations were carried out by fou... | [
"(231937) 2001 FO32 β Discovery\n\nwas discovered on 23 March 2001 by the Lincoln Near-Earth Asteroid Research (LINEAR) at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico. The asteroid was first observed in the constellation Hydra at an apparent magnitude of 15.6. Shortly after discovery, follow-... |
(231937)_2001_FO32_4157582 | What does the article about '(231937) 2001 FO32' say regarding 'Close approaches'? | it was visible to observers using telescopes with apertures of at least 8 in. Due to its highly inclined and eccentric orbit, its relative velocity to Earth during the close approach is 34.4 km/s, making it one of the fastest asteroids to pass by Earth in 2021. By the time makes its closest approach to Earth, its solar... | [
"(231937) 2001 FO32 β Discovery\n\nwas discovered on 23 March 2001 by the Lincoln Near-Earth Asteroid Research (LINEAR) at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico. The asteroid was first observed in the constellation Hydra at an apparent magnitude of 15.6. Shortly after discovery, follow-... |
(231937)_2001_FO32_4157583 | From the article on '(231937) 2001 FO32', restate the 'Observations' content. | Preliminary observations by NEOWISE show that appears to be faint in infrared wavelengths of light, indicating that the asteroid is likely less than 1 kilometer in diameter. Based on this, the diameter is estimated around 550 Β± 110 m. Near-infrared spectral data obtained by NASA's Infrared Telescope Facility in 2018 su... | [
"(231937) 2001 FO32 β Discovery\n\nwas discovered on 23 March 2001 by the Lincoln Near-Earth Asteroid Research (LINEAR) at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico. The asteroid was first observed in the constellation Hydra at an apparent magnitude of 15.6. Shortly after discovery, follow-... |
(231937)_2001_FO32_4157580 | Summarize the 'Orbit and classification' part of '(231937) 2001 FO32'. | is a member of the dynamical Apollo group of Earth-crossing near-Earth asteroids with orbital semi-major axes greater than 1 astronomical unit (AU). It follows a highly elongated orbit around the Sun at a distance of 0.3β3.1 AU once every 2.22 years (810 days; semi-major axis of 1.7 AU). Its orbit has a high eccentrici... | [
"(231937) 2001 FO32 β Discovery\n\nwas discovered on 23 March 2001 by the Lincoln Near-Earth Asteroid Research (LINEAR) at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico. The asteroid was first observed in the constellation Hydra at an apparent magnitude of 15.6. Shortly after discovery, follow-... |
(231937)_2001_FO32_4157581 | What does the article about '(231937) 2001 FO32' say regarding 'Close approaches'? | Over the course of its highly eccentric orbit, makes numerous close encounters with the inner planetsβmost often Mercury, Venus, and Earth. Its MOIDs from Mercury and Venus are 0.036 AU and 0.075 AU, respectively. 's most recent close encounter with either one of those planets was on 16 January 2008, when it passed by ... | [
"(231937) 2001 FO32 β Discovery\n\nwas discovered on 23 March 2001 by the Lincoln Near-Earth Asteroid Research (LINEAR) at Lincoln Laboratory's Experimental Test Site in Socorro, New Mexico. The asteroid was first observed in the constellation Hydra at an apparent magnitude of 15.6. Shortly after discovery, follow-... |
(23958)_1998_VD30_15688063 | What does the article about '(23958) 1998 VD30' say regarding 'Physical characteristics'? | is an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical VβI color index of 0.99 and a BR-color of 1.15. | [
"(23958) 1998 VD30 β Physical characteristics\n\nis an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical VβI color index of 0.99 and a BR-color of 1.15.",
"(23958) 1998 VD30 β Numbering and naming\n\nThis minor planet w... |
(23958)_1998_VD30_15688062 | What does the article about '(23958) 1998 VD30' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 8 April 2001 (M.P.C. 42554). , it has not been named. | [
"(23958) 1998 VD30 β Physical characteristics\n\nis an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical VβI color index of 0.99 and a BR-color of 1.15.",
"(23958) 1998 VD30 β Numbering and naming\n\nThis minor planet w... |
(23958)_1998_VD30_15688065 | Reconstruct the content about 'Diameter and albedo' from the article on '(23958) 1998 VD30'. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, measures 46.00 and 47.91 kilometers in diameter and its surface has an albedo between 0.076 and 0.084, respectively. The Collaborative Asteroid Lightcurve Link assumes a standard a... | [
"(23958) 1998 VD30 β Physical characteristics\n\nis an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical VβI color index of 0.99 and a BR-color of 1.15.",
"(23958) 1998 VD30 β Numbering and naming\n\nThis minor planet w... |
(23958)_1998_VD30_15688060 | What information does the article about '(23958) 1998 VD30' provide? | , provisional designation:, is a Jupiter trojan from the Greek camp, approximately 47 km in diameter. It was discovered on 10 November 1998, by astronomers with the LINEAR survey at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The dark Jovian asteroid belongs to the 11... | [
"(23958) 1998 VD30 β Physical characteristics\n\nis an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical VβI color index of 0.99 and a BR-color of 1.15.",
"(23958) 1998 VD30 β Numbering and naming\n\nThis minor planet w... |
(23958)_1998_VD30_15688061 | From the article on '(23958) 1998 VD30', restate the 'Orbit and classification' content. | is a dark Jupiter trojan in a 1:1 orbital resonance with Jupiter. It is located in the leading Greek camp at the Gas Giant's Lagrangian point, 60Β° ahead of its orbit. It is also a non-family asteroid in the Jovian background population. It orbits the Sun at a distance of 4.7β5.7 AU once every 12 years (4,370 days; semi... | [
"(23958) 1998 VD30 β Physical characteristics\n\nis an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical VβI color index of 0.99 and a BR-color of 1.15.",
"(23958) 1998 VD30 β Numbering and naming\n\nThis minor planet w... |
(23958)_1998_VD30_15688064 | Reconstruct the content about 'Rotation period' from the article on '(23958) 1998 VD30'. | With a rotation period of 562 hours, this slow rotator belongs to the Top 100 slowest rotators known to exist. It is also the third-slowest rotator among the larger Jupiter trojans after 4902 Thessandrus (738 hours) and (7352) 1994 CO (648 hours). In August 2015, a rotational lightcurve of was obtained from photometri... | [
"(23958) 1998 VD30 β Physical characteristics\n\nis an assumed, carbonaceous C-type asteroid. Most Jupiter trojans are D-types, with the reminder being mostly C and P-type asteroids. It has a typical VβI color index of 0.99 and a BR-color of 1.15.",
"(23958) 1998 VD30 β Numbering and naming\n\nThis minor planet w... |
(24)7.ai_31468671 | Describe the 'Products' section of the article about '(24)7.ai'. | The product is sales and service-oriented software that encompasses big data, predictive analytics, virtual agents and real-time decisioning. It integrates different channels of communication, including web chat, mobile devices and interactive voice response, which incorporates the company's proprietary natural languag... | [
"(24)7.ai β Products\n\nThe product is sales and service-oriented software that encompasses big data, predictive analytics, virtual agents and real-time decisioning. It integrates different channels of communication, including web chat, mobile devices and interactive voice response, which incorporates the company's... |
(24)7.ai_31468670 | What does the article about '(24)7.ai' say regarding 'History'? | firm Shopalize for an undisclosed amount of money. [24]7.ai was also listed on Forbes list of America's Most Promising Companies in 2013. In November 2014, [24]7.ai acquired IntelliResponse, a provider of digital self-service technology, including virtual agent solutions. In August 2015, [24]7.ai acquired Campanja, a l... | [
"(24)7.ai β Products\n\nThe product is sales and service-oriented software that encompasses big data, predictive analytics, virtual agents and real-time decisioning. It integrates different channels of communication, including web chat, mobile devices and interactive voice response, which incorporates the company's... |
(24)7.ai_31468669 | Summarize the 'History' part of '(24)7.ai'. | which [24]7.ai and Microsoft would combine technologies for natural user interfaces (NUIs) and data analytics at cloud scale. Microsoft made an equity investor and transferred approximately 400 employees of the former Tellme Networks to [24]7.ai. At the same time, [24]7.ai acquired the call center automation developer ... | [
"(24)7.ai β Products\n\nThe product is sales and service-oriented software that encompasses big data, predictive analytics, virtual agents and real-time decisioning. It integrates different channels of communication, including web chat, mobile devices and interactive voice response, which incorporates the company's... |
(24)7.ai_31468668 | Describe the 'History' section of the article about '(24)7.ai'. | [24]7.ai was founded in April 2000 by P. V. Kannan and Shanmugam Nagarajan. Kannan previously founded Business Evolution, a software company, which was acquired by Kana Software in 1999. The company is headquartered in San Jose, California. Other offices are located in Toronto, London, and Sydney. [24]7.ai has customer... | [
"(24)7.ai β Products\n\nThe product is sales and service-oriented software that encompasses big data, predictive analytics, virtual agents and real-time decisioning. It integrates different channels of communication, including web chat, mobile devices and interactive voice response, which incorporates the company's... |
(24)7.ai_31468667 | Summarize the following section from the article on '(24)7.ai'. | [24]7.ai (full company name [24]7.ai, Inc.) is a customer experience software and services company based in California that uses artificial intelligence and machine learning to understand consumer intent. It helps companies create a personalized experience across channels. | [
"(24)7.ai β Products\n\nThe product is sales and service-oriented software that encompasses big data, predictive analytics, virtual agents and real-time decisioning. It integrates different channels of communication, including web chat, mobile devices and interactive voice response, which incorporates the company's... |
(242450)_2004_QY2_26255645 | Explain what '(242450) 2004 QY2' covers in the 'Close approaches' section. | With an absolute magnitude of 14.7, is one of the brightest potentially hazardous asteroids ever discovered (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0469 AU, which translates into 18.3 lunar distances. On 29 July 2012, it passed Earth at a distance of 0.4314 AU. | [
"(242450) 2004 QY2 β Close approaches\n\nWith an absolute magnitude of 14.7, is one of the brightest potentially hazardous asteroids ever discovered (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0469 AU, which translates into 18.3 lunar distances. On 29 July 2012, it passed Earth at a d... |
(242450)_2004_QY2_26255647 | Based on the article about '(242450) 2004 QY2', describe the 'Physical characteristics' section. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, has an albedo of 0.274, and it measures 2.914 and 3.320 kilometers in diameter, respectively. As of 2018, no rotational lightcurve of has been obtained from photometric observations. The body's rotation period, sha... | [
"(242450) 2004 QY2 β Close approaches\n\nWith an absolute magnitude of 14.7, is one of the brightest potentially hazardous asteroids ever discovered (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0469 AU, which translates into 18.3 lunar distances. On 29 July 2012, it passed Earth at a d... |
(242450)_2004_QY2_26255648 | What does the article about '(242450) 2004 QY2' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 26 June 2006. As of 2018, it has not been named. | [
"(242450) 2004 QY2 β Close approaches\n\nWith an absolute magnitude of 14.7, is one of the brightest potentially hazardous asteroids ever discovered (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0469 AU, which translates into 18.3 lunar distances. On 29 July 2012, it passed Earth at a d... |
(242450)_2004_QY2_26255643 | Describe the content of the article about '(242450) 2004 QY2'. | (prov. designation: ) is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 3 km in diameter. It was discovered on 20 August 2004 by the Siding Spring Survey at an apparent magnitude of 16.5 using the 0.5 m Uppsala Southern Schmidt Te... | [
"(242450) 2004 QY2 β Close approaches\n\nWith an absolute magnitude of 14.7, is one of the brightest potentially hazardous asteroids ever discovered (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0469 AU, which translates into 18.3 lunar distances. On 29 July 2012, it passed Earth at a d... |
(242450)_2004_QY2_26255646 | Describe the 'Sentry Risk Table' section of the article about '(242450) 2004 QY2'. | Due to its originally estimated size of 5.5 kilometers, was one of the largest objects to appear on the Sentry Risk Table. It was removed from the Sentry Risk Table on 25 August 2004. | [
"(242450) 2004 QY2 β Close approaches\n\nWith an absolute magnitude of 14.7, is one of the brightest potentially hazardous asteroids ever discovered (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0469 AU, which translates into 18.3 lunar distances. On 29 July 2012, it passed Earth at a d... |
(242450)_2004_QY2_26255644 | Describe the 'Orbit and classification' section of the article about '(242450) 2004 QY2'. | orbits the Sun at a distance of 0.6β1.6 AU once every 14 months (412 days; semi-major axis of 1.08 AU). Its orbit has an eccentricity of 0.48 and an inclination of 37Β° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Siding Spring. The object is a member of the ... | [
"(242450) 2004 QY2 β Close approaches\n\nWith an absolute magnitude of 14.7, is one of the brightest potentially hazardous asteroids ever discovered (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0469 AU, which translates into 18.3 lunar distances. On 29 July 2012, it passed Earth at a d... |
(251732)_1998_HG49_16122711 | Summarize the 'Description' part of '(251732) 1998 HG49'. | is an Amor asteroid because its perihelion is less than 1.3 AU and does not cross Earth's orbit. It is on a low-eccentricity and low-inclination orbit between the orbits of Earth and Mars. This is within a region of stability where bodies may survive for the age of the Solar System, and hence it may have formed near it... | [
"(251732) 1998 HG49 β Description\n\nis an Amor asteroid because its perihelion is less than 1.3 AU and does not cross Earth's orbit. It is on a low-eccentricity and low-inclination orbit between the orbits of Earth and Mars. This is within a region of stability where bodies may survive for the age of the Solar Sys... |
(251732)_1998_HG49_16122712 | Explain what '(251732) 1998 HG49' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 28 November 2010. As of 2018, it has not been named. | [
"(251732) 1998 HG49 β Description\n\nis an Amor asteroid because its perihelion is less than 1.3 AU and does not cross Earth's orbit. It is on a low-eccentricity and low-inclination orbit between the orbits of Earth and Mars. This is within a region of stability where bodies may survive for the age of the Solar Sys... |
(251732)_1998_HG49_16122710 | Summarize the following section from the article on '(251732) 1998 HG49'. | , provisional designation, is a sub-kilometer asteroid and near-Earth object of the Amor group, approximately 200 meters in diameter. It was discovered on 27 April 1998 by astronomers of the Spacewatch program at the Kitt Peak National Observatory near Tucson, Arizona, United States. | [
"(251732) 1998 HG49 β Description\n\nis an Amor asteroid because its perihelion is less than 1.3 AU and does not cross Earth's orbit. It is on a low-eccentricity and low-inclination orbit between the orbits of Earth and Mars. This is within a region of stability where bodies may survive for the age of the Solar Sys... |
(26308)_1998_SM165_4607603 | Reconstruct the content about 'Satellite' from the article on '(26308) 1998 SM165'. | On 22 December 2001, a minor-planet moon, provisionally designated, was discovered by American astronomer Michael Brown and Chad Trujillo using the Hubble Space Telescope. The discovery was announced in January 2002. The satellite measures approximately 96 +/- in diameter and orbits its primary at a distance of 11,310 ... | [
"(26308) 1998 SM165 β Satellite\n\nOn 22 December 2001, a minor-planet moon, provisionally designated, was discovered by American astronomer Michael Brown and Chad Trujillo using the Hubble Space Telescope. The discovery was announced in January 2002. The satellite measures approximately 96 +/- in diameter and orbi... |
(26308)_1998_SM165_4607602 | What does the article about '(26308) 1998 SM165' say regarding 'Physical characteristics'? | The observations with the infrared Spitzer Space Telescope combined with the orbits established using the Hubble Telescope allow the estimation of the density, assuming the components of equal albedo. The resulting estimate of 0.51 g/cm3 is similar to the density of the binary plutino 47171 Lempo (0.3β0.8 g/cm3 ) and S... | [
"(26308) 1998 SM165 β Satellite\n\nOn 22 December 2001, a minor-planet moon, provisionally designated, was discovered by American astronomer Michael Brown and Chad Trujillo using the Hubble Space Telescope. The discovery was announced in January 2002. The satellite measures approximately 96 +/- in diameter and orbi... |
(26308)_1998_SM165_4607604 | Explain what '(26308) 1998 SM165' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 5 July 2001. As of 2018, it has not been named. | [
"(26308) 1998 SM165 β Satellite\n\nOn 22 December 2001, a minor-planet moon, provisionally designated, was discovered by American astronomer Michael Brown and Chad Trujillo using the Hubble Space Telescope. The discovery was announced in January 2002. The satellite measures approximately 96 +/- in diameter and orbi... |
(26308)_1998_SM165_4607601 | Explain what '(26308) 1998 SM165' covers in the 'Twotino' section. | has a semi-major axis (average distance from the Sun) near the edge of the classical belt. The Deep Ecliptic Survey (DES) list this trans-Neptunian object as a twotino that stays in a 1:2 orbital resonance with the planet Neptune (for every one orbit that a twotino makes, Neptune orbits twice). | [
"(26308) 1998 SM165 β Satellite\n\nOn 22 December 2001, a minor-planet moon, provisionally designated, was discovered by American astronomer Michael Brown and Chad Trujillo using the Hubble Space Telescope. The discovery was announced in January 2002. The satellite measures approximately 96 +/- in diameter and orbi... |
(26308)_1998_SM165_4607600 | What information does the article about '(26308) 1998 SM165' provide? | is a resonant trans-Neptunian object and binary system from the Kuiper belt in the outermost regions of the Solar System. It was discovered on 16 September 1998, by American astronomer Nichole Danzl at the Kitt Peak National Observatory in Arizona. It is classified as a twotino and measures approximately 280 kilometers... | [
"(26308) 1998 SM165 β Satellite\n\nOn 22 December 2001, a minor-planet moon, provisionally designated, was discovered by American astronomer Michael Brown and Chad Trujillo using the Hubble Space Telescope. The discovery was announced in January 2002. The satellite measures approximately 96 +/- in diameter and orbi... |
(275809)_2001_QY297_17757487 | Based on the article about '(275809) 2001 QY297', describe the 'Discovery and orbit' section. | was discovered on 21 August 2001 by Marc William Buie from Cerro Tololo Observatory, La Serena, Chile. belongs to the dynamically cold population of the classical Kuiper belt objects, which have small orbital eccentricities and inclinations. Their semi-major axes reside mainly in the interval 40β45 AU. | [
"(275809) 2001 QY297 β Discovery and orbit\n\nwas discovered on 21 August 2001 by Marc William Buie from Cerro Tololo Observatory, La Serena, Chile. belongs to the dynamically cold population of the classical Kuiper belt objects, which have small orbital eccentricities and inclinations. Their semi-major axes reside... |
(275809)_2001_QY297_17757488 | From the article on '(275809) 2001 QY297', restate the 'Satellite' content. | is a binary system consisting of two components of approximately equal size. The satellite was discovered on 18 April 2006. Assuming that both components have the same albedo, the primary is estimated to be about 169 km in diameter. The size of the secondary (satellite) in this case is estimated at around 154 km. The t... | [
"(275809) 2001 QY297 β Discovery and orbit\n\nwas discovered on 21 August 2001 by Marc William Buie from Cerro Tololo Observatory, La Serena, Chile. belongs to the dynamically cold population of the classical Kuiper belt objects, which have small orbital eccentricities and inclinations. Their semi-major axes reside... |
(275809)_2001_QY297_17757486 | Summarize the following section from the article on '(275809) 2001 QY297'. | is a trans-Neptunian object from the classical Kuiper belt, located in the outermost region of the Solar System. The binary classical Kuiper belt object belongs to the cold population. | [
"(275809) 2001 QY297 β Discovery and orbit\n\nwas discovered on 21 August 2001 by Marc William Buie from Cerro Tololo Observatory, La Serena, Chile. belongs to the dynamically cold population of the classical Kuiper belt objects, which have small orbital eccentricities and inclinations. Their semi-major axes reside... |
(276033)_2002_AJ129_18876318 | From the article on '(276033) 2002 AJ129', restate the '2172 approach' content. | On 8 February 2172, the asteroid will pass about 0.00458 AU from Earth. The 2172 Earth approach distance is known with a 3-sigma accuracy of Β±4000 km. As we look even further into the future the known trajectory becomes more divergent. By the Earth approach of 0.24 AU on 19 February 2196 the uncertainty increases to Β±2... | [
"(276033) 2002 AJ129 β 2172 approach\n\nOn 8 February 2172, the asteroid will pass about 0.00458 AU from Earth. The 2172 Earth approach distance is known with a 3-sigma accuracy of Β±4000 km. As we look even further into the future the known trajectory becomes more divergent. By the Earth approach of 0.24 AU on 19 F... |
(276033)_2002_AJ129_18876315 | Reconstruct the content from the article about '(276033) 2002 AJ129'. | , provisional designation, is a Mercury-crossing asteroid. It has the ninth-smallest perihelion of all numbered asteroids, after asteroids such as, , and. It makes close approaches to all of the inner planets and asteroid 4 Vesta. The asteroid is estimated to be between 0.5 - 1.2 km across. In January 2018 there was mu... | [
"(276033) 2002 AJ129 β 2172 approach\n\nOn 8 February 2172, the asteroid will pass about 0.00458 AU from Earth. The 2172 Earth approach distance is known with a 3-sigma accuracy of Β±4000 km. As we look even further into the future the known trajectory becomes more divergent. By the Earth approach of 0.24 AU on 19 F... |
(276033)_2002_AJ129_18876317 | Summarize the '2018 approach' part of '(276033) 2002 AJ129'. | On 4 February 2018 at 21:31 UT, the asteroid passed about 0.028126 AU from Earth. The 2018 Earth approach distance was known with a 3-sigma accuracy of Β±200 km. Goldstone is scheduled to observe the asteroid from 3 to 6 February. By 4 February 2018 11:00 UT, the asteroid brightened to apparent magnitude 14 and had a so... | [
"(276033) 2002 AJ129 β 2172 approach\n\nOn 8 February 2172, the asteroid will pass about 0.00458 AU from Earth. The 2172 Earth approach distance is known with a 3-sigma accuracy of Β±4000 km. As we look even further into the future the known trajectory becomes more divergent. By the Earth approach of 0.24 AU on 19 F... |
(276033)_2002_AJ129_18876316 | What does the article about '(276033) 2002 AJ129' say regarding 'Description'? | was discovered on 15 January 2002 by astronomers of the NEAT team at Haleakala Observatory, Hawaii, United States. It was removed from the Sentry Risk Table on 3 February 2002. It is a Mercury-, Venus-, Earth- and Mars-crossing asteroid. With an observation arc of 14 years, it has a well determined orbit and was last o... | [
"(276033) 2002 AJ129 β 2172 approach\n\nOn 8 February 2172, the asteroid will pass about 0.00458 AU from Earth. The 2172 Earth approach distance is known with a 3-sigma accuracy of Β±4000 km. As we look even further into the future the known trajectory becomes more divergent. By the Earth approach of 0.24 AU on 19 F... |
(285263)_1998_QE2_201383 | Describe the content of the article about '(285263) 1998 QE2'. | , provisional designation, is a dark asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3 kilometers in diameter. It was discovered on 19 August 1998, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test S... | [
"(285263) 1998 QE2\n\n, provisional designation, is a dark asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3 kilometers in diameter. It was discovered on 19 August 1998, by astronomers of the LINEAR program at Lincoln Labora... |
(285263)_1998_QE2_201386 | Summarize the 'Satellite' part of '(285263) 1998 QE2'. | Goldstone radar observations on 29 May 2013 discovered that is orbited by a minor-planet moon approximately 600β800 meters in diameter. In radar images, the satellite appears brighter than because it is rotating significantly more slowly, which compresses the radar return of the satellite along the Doppler axis. This m... | [
"(285263) 1998 QE2\n\n, provisional designation, is a dark asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3 kilometers in diameter. It was discovered on 19 August 1998, by astronomers of the LINEAR program at Lincoln Labora... |
(285263)_1998_QE2_201387 | What does the article about '(285263) 1998 QE2' say regarding 'Surface, albedo and composition'? | The surface of is covered with a sooty substance, making it optically dark with a geometric albedo of 0.06, meaning it absorbs 94% of the light that hits it, which is indicative for a carbonaceous surface of a C-type asteroid. The asteroid is covered with craters and is dark, red, and primitive. | [
"(285263) 1998 QE2\n\n, provisional designation, is a dark asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3 kilometers in diameter. It was discovered on 19 August 1998, by astronomers of the LINEAR program at Lincoln Labora... |
(285263)_1998_QE2_201384 | Based on the article about '(285263) 1998 QE2', describe the 'Classification and orbital characteristics' section. | As an Amor asteroid the orbit of is entirely beyond Earth's orbit. The asteroid orbits the Sun at a distance of 1.0β3.8 AU once every 3 years and 9 months (1,378 days; semi-major axis of 2.42 AU). Its orbit has an eccentricity of 0.57 and an inclination of 13Β° with respect to the ecliptic. The Earth minimum orbit inter... | [
"(285263) 1998 QE2\n\n, provisional designation, is a dark asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3 kilometers in diameter. It was discovered on 19 August 1998, by astronomers of the LINEAR program at Lincoln Labora... |
(285263)_1998_QE2_201385 | From the article on '(285263) 1998 QE2', restate the 'Earth approach' content. | On 31 May 2013, approached within 0.039 AU (15 lunar distances) of Earth at 20:59 UT (4:59 pm EDT). This was the closest approach the asteroid will make to Earth for at least the next two centuries. It is a very strong radar target for Goldstone from May 30 to June 9 and will be one for Arecibo from June 6 to June 12. ... | [
"(285263) 1998 QE2\n\n, provisional designation, is a dark asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3 kilometers in diameter. It was discovered on 19 August 1998, by astronomers of the LINEAR program at Lincoln Labora... |
(285263)_1998_QE2_201388 | From the article on '(285263) 1998 QE2', restate the 'Diameter' content. | With a diameter between 2.7 and 3.2 kilometers, is one of largest known potentially hazardous asteroid (see PHA-list). Conversely, the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 1.08 kilometers based on an absolute magnitude of 17.2. | [
"(285263) 1998 QE2\n\n, provisional designation, is a dark asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3 kilometers in diameter. It was discovered on 19 August 1998, by astronomers of the LINEAR program at Lincoln Labora... |
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