id string | question string | answer string | documents list |
|---|---|---|---|
(82075)_2000_YW134_32126221 | From the article on '(82075) 2000 YW134', restate the 'Satellite' content. | On 25 October 2002, observations in the far-infrared with the NICMOS instrument of the Hubble Space Telescope revealed, that is a binary system with a satelite in its orbit. The discovery was announced on 6 October 2005. Johnston's Archive derives a diameter of 216 km for the primary and a diameter of 75 km for the se... | [
"(82075) 2000 YW134 — Orbit and classification\n\norbits the Sun at a distance of 41.0–73.8 AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its offic... |
(82075)_2000_YW134_32126216 | Summarize the following section from the article on '(82075) 2000 YW134'. | , provisional designation:, is a resonant trans-Neptunian object and binary system, located in the outermost region of the Solar System. It was discovered on 26 December 2000, by astronomers with the Spacewatch survey at Kitt Peak Observatory near Tucson, Arizona. The reddish object stays in a rare 3:8 resonance with N... | [
"(82075) 2000 YW134 — Orbit and classification\n\norbits the Sun at a distance of 41.0–73.8 AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its offic... |
(82075)_2000_YW134_32126220 | Reconstruct the content about 'Diameter and albedo' from the article on '(82075) 2000 YW134'. | In 2010, observations with the Herschel Space Observatory constrained the object's geometric albedo to no darker than 8%, and allowed to place an upper limit to its effective mean-diameter of 500 km, as no thermal radiation had been detected. However, according to 's dissertation in 2013, the object has a much higher a... | [
"(82075) 2000 YW134 — Orbit and classification\n\norbits the Sun at a distance of 41.0–73.8 AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its offic... |
(82075)_2000_YW134_32126219 | Explain what '(82075) 2000 YW134' covers in the 'Physical characteristics' section. | The surface of is moderately red in the visible part of the spectrum. Its IR spectral type transitions from the very red (RR) to the intermediate blue-red (BR). Alternatively a BR-spectral type has also been assumed. The object's B−V and V–R color indices have also been measured several times, giving an averaged value... | [
"(82075) 2000 YW134 — Orbit and classification\n\norbits the Sun at a distance of 41.0–73.8 AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its offic... |
(82075)_2000_YW134_32126218 | Explain what '(82075) 2000 YW134' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 4 May 2004, receiving the number in the minor planet catalog (M.P.C. 51853). , it has not been named. According to the established naming conventions, it will be given a mythological name associated with the underworld. | [
"(82075) 2000 YW134 — Orbit and classification\n\norbits the Sun at a distance of 41.0–73.8 AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic. The body's observation arc begins with its offic... |
(82158)_2001_FP185_32464502 | Reconstruct the content about 'Numbering and naming' from the article on '(82158) 2001 FP185'. | This minor planet was numbered by the Minor Planet Center on 4 May 2004. As of 2018, it has not been named. | [
"(82158) 2001 FP185 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 4 May 2004. As of 2018, it has not been named.",
"(82158) 2001 FP185 — Diameter and albedo\n\nAccording to astronomer Michael Brown and based on radiometric observations, measures 336 kilometers in diameter ... |
(82158)_2001_FP185_32464500 | Explain what '(82158) 2001 FP185' covers in the 'Diameter and albedo' section. | According to astronomer Michael Brown and based on radiometric observations, measures 336 kilometers in diameter and its surface has an (assumed) albedo of 0.05. Observations with the PACS-instrument of the Herschel Space Observatory during a survey of scattered-disc objects ("TNO are cool") found a similar diameter of... | [
"(82158) 2001 FP185 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 4 May 2004. As of 2018, it has not been named.",
"(82158) 2001 FP185 — Diameter and albedo\n\nAccording to astronomer Michael Brown and based on radiometric observations, measures 336 kilometers in diameter ... |
(82158)_2001_FP185_32464501 | Describe the 'Lightcurve' section of the article about '(82158) 2001 FP185'. | No rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole axis and brightness amplitude remains unknown. | [
"(82158) 2001 FP185 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 4 May 2004. As of 2018, it has not been named.",
"(82158) 2001 FP185 — Diameter and albedo\n\nAccording to astronomer Michael Brown and based on radiometric observations, measures 336 kilometers in diameter ... |
(82158)_2001_FP185_32464499 | Based on the article about '(82158) 2001 FP185', describe the 'Spectra and colors' section. | 's color has extensively been measured. The object has a determined BR and IR spectra, which are intermediate classes of the very blue BB and very red RR spectra. | [
"(82158) 2001 FP185 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 4 May 2004. As of 2018, it has not been named.",
"(82158) 2001 FP185 — Diameter and albedo\n\nAccording to astronomer Michael Brown and based on radiometric observations, measures 336 kilometers in diameter ... |
(82158)_2001_FP185_32464496 | Describe the content of the article about '(82158) 2001 FP185'. | , provisional designation, is a highly eccentric trans-Neptunian object from the scattered disc in the outermost part of the Solar System, approximately 330 kilometers in diameter. It was discovered on 26 March 2001, by American astronomer Marc Buie at Kitt Peak National Observatory in Arizona, United States. | [
"(82158) 2001 FP185 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 4 May 2004. As of 2018, it has not been named.",
"(82158) 2001 FP185 — Diameter and albedo\n\nAccording to astronomer Michael Brown and based on radiometric observations, measures 336 kilometers in diameter ... |
(84522)_2002_TC302_19662713 | What information does the article about '(84522) 2002 TC302' provide on 'Orbit and classification'? | orbits the Sun at a distance of 39.2–71.4 AU once every 410 years and 12 months (150,105 days; semi-major axis of 55.28 AU). Its orbit has an eccentricity of 0.29 and an inclination of 35° with respect to the ecliptic. In December 2058, It will come to perihelion (minimum distance from the Sun) at 39.2 AU, which is abo... | [
"(84522) 2002 TC302 — Orbit and classification\n\norbits the Sun at a distance of 39.2–71.4 AU once every 410 years and 12 months (150,105 days; semi-major axis of 55.28 AU). Its orbit has an eccentricity of 0.29 and an inclination of 35° with respect to the ecliptic. In December 2058, It will come to perihelion (m... |
(84522)_2002_TC302_19662712 | What information does the article about '(84522) 2002 TC302' provide? | , prov. designation:, is a mid-sized trans-Neptunian object located in the outermost region of the Solar System. It was discovered on 9 October 2002, by American astronomers Mike Brown, Chad Trujillo and David Rabinowitz at the Palomar Observatory in California. The resonant trans-Neptunian object stays in a 2:5 resona... | [
"(84522) 2002 TC302 — Orbit and classification\n\norbits the Sun at a distance of 39.2–71.4 AU once every 410 years and 12 months (150,105 days; semi-major axis of 55.28 AU). Its orbit has an eccentricity of 0.29 and an inclination of 35° with respect to the ecliptic. In December 2058, It will come to perihelion (m... |
(84522)_2002_TC302_19662716 | Reconstruct the content about 'Possible satellite' from the article on '(84522) 2002 TC302'. | The mean diameter of determined from occultations in 2018 is smaller than the larger diameter estimate of 584.1 km by Spitzer in 2008. Despite the large uncertainty in the Spitzer's estimate, the difference of ~84 km between the two diameters is significant, implying that may have a large satellite with a possible size... | [
"(84522) 2002 TC302 — Orbit and classification\n\norbits the Sun at a distance of 39.2–71.4 AU once every 410 years and 12 months (150,105 days; semi-major axis of 55.28 AU). Its orbit has an eccentricity of 0.29 and an inclination of 35° with respect to the ecliptic. In December 2058, It will come to perihelion (m... |
(84522)_2002_TC302_19662715 | Explain what '(84522) 2002 TC302' covers in the 'Physical characteristics' section. | 0.04 mag. However, this short rotation period was most likely an alias due to a bias for shorter and more easily discernable shorter periods. is highly oblate, and Ortiz et al. suggest a longer rotation period estimate of 56.1 hours. An occultation of a 15.3 magnitude star by on 28 January 2018 over Europe suggests tha... | [
"(84522) 2002 TC302 — Orbit and classification\n\norbits the Sun at a distance of 39.2–71.4 AU once every 410 years and 12 months (150,105 days; semi-major axis of 55.28 AU). Its orbit has an eccentricity of 0.29 and an inclination of 35° with respect to the ecliptic. In December 2058, It will come to perihelion (m... |
(84522)_2002_TC302_19662714 | Explain what '(84522) 2002 TC302' covers in the 'Physical characteristics' section. | has an absolute magnitude of 3.78. It has an estimated diameter of 584.1 km. Using the Spitzer Space Telescope, it was previously estimated to have a diameter of 1,145 km, which would have made it one of the largest TNOs. This overestimation was due to insufficient motion to allow for a good sky subtraction, and becaus... | [
"(84522) 2002 TC302 — Orbit and classification\n\norbits the Sun at a distance of 39.2–71.4 AU once every 410 years and 12 months (150,105 days; semi-major axis of 55.28 AU). Its orbit has an eccentricity of 0.29 and an inclination of 35° with respect to the ecliptic. In December 2058, It will come to perihelion (m... |
(85182)_1991_AQ_26180632 | From the article on '(85182) 1991 AQ', restate the 'Orbit and classification' content. | is a member of the Earth-crossing class of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. It is also a Venus- and Mars-crosser due to its extreme perihelion and aphelion, respectively. It orbits the Sun at a distance of 0.5–3.9 AU once every 3 years and 4 months ... | [
"(85182) 1991 AQ — Orbit and classification\n\nis a member of the Earth-crossing class of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. It is also a Venus- and Mars-crosser due to its extreme perihelion and aphelion, respectively. It orbits the Sun at a dist... |
(85182)_1991_AQ_26180634 | From the article on '(85182) 1991 AQ', restate the 'Physical characteristics' content. | In the Tholen classification, this object is an uncommon Q-type asteroid, that falls into the larger stony S-complex. As of 2018, no rotational lightcurve of this asteroid has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. It has a brightness variation of 0.69 ma... | [
"(85182) 1991 AQ — Orbit and classification\n\nis a member of the Earth-crossing class of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. It is also a Venus- and Mars-crosser due to its extreme perihelion and aphelion, respectively. It orbits the Sun at a dist... |
(85182)_1991_AQ_26180636 | What does the article about '(85182) 1991 AQ' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 30 August 2004 (M.P.C. 52517). As of 2018, it has not been named. | [
"(85182) 1991 AQ — Orbit and classification\n\nis a member of the Earth-crossing class of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. It is also a Venus- and Mars-crosser due to its extreme perihelion and aphelion, respectively. It orbits the Sun at a dist... |
(85182)_1991_AQ_26180635 | Based on the article about '(85182) 1991 AQ', describe the 'Diameter and albedo' section. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, this asteroid measures 1.1 kilometers in diameter and its surface has an albedo of 0.242. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.18 and derives a diameter of 1.14 kilometers based on an a... | [
"(85182) 1991 AQ — Orbit and classification\n\nis a member of the Earth-crossing class of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. It is also a Venus- and Mars-crosser due to its extreme perihelion and aphelion, respectively. It orbits the Sun at a dist... |
(85182)_1991_AQ_26180631 | Summarize the following section from the article on '(85182) 1991 AQ'. | (85182) 1991 AQ, provisional designation, is a stony asteroid on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 km in diameter. It was discovered on 14 January 1991, by American astronomer Eleanor Helin at the Palomar Observatory in Ca... | [
"(85182) 1991 AQ — Orbit and classification\n\nis a member of the Earth-crossing class of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. It is also a Venus- and Mars-crosser due to its extreme perihelion and aphelion, respectively. It orbits the Sun at a dist... |
(85182)_1991_AQ_26180633 | From the article on '(85182) 1991 AQ', restate the 'Close approaches' content. | The asteroid has currently an Earth minimum orbital intersection distance of 0.0165 AU, which corresponds to 6.4 lunar distances and makes it a potentially hazardous asteroid due to its notably large size. In 1991 and 1994, it approached Earth at a nominal distance of 0.054 AU. The asteroids closest encounter with Eart... | [
"(85182) 1991 AQ — Orbit and classification\n\nis a member of the Earth-crossing class of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. It is also a Venus- and Mars-crosser due to its extreme perihelion and aphelion, respectively. It orbits the Sun at a dist... |
(85640)_1998_OX4_10855606 | What information does the article about '(85640) 1998 OX4' provide? | , also written Astronomical naming conventions, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. | [
"(85640) 1998 OX4 — Notes\n\nThis is assuming an albedo of 0.25–0.05.",
"(85640) 1998 OX4\n\n, also written Astronomical naming conventions, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group.",
"(85640) 1998 OX4 — Description\n\nIt was discovered... |
(85640)_1998_OX4_10855607 | Summarize the 'Description' part of '(85640) 1998 OX4'. | It was discovered on 26 July 1998 by the Spacewatch program and subsequently lost. It was re-discovered by the Near-Earth Asteroid Tracking (NEAT) project on 31 August 2002, as. It was removed from the Sentry Risk Table on 8 August 2002. It has a well determined orbit with an observation arc of more than 10 years. It i... | [
"(85640) 1998 OX4 — Notes\n\nThis is assuming an albedo of 0.25–0.05.",
"(85640) 1998 OX4\n\n, also written Astronomical naming conventions, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group.",
"(85640) 1998 OX4 — Description\n\nIt was discovered... |
(85713)_1998_SS49_1179473 | Explain what '(85713) 1998 SS49' covers in the 'Diameter and albedo' section. | Surveys contrast: of the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer. These measure the object as between 2 and 3.484 kilometers lengthways (in diameter) and to have an albedo (optical wavelength reflectivity) between 0.076 and 0.237. The Collaborative Asteroid Lightcu... | [
"(85713) 1998 SS49 — Diameter and albedo\n\nSurveys contrast: of the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer. These measure the object as between 2 and 3.484 kilometers lengthways (in diameter) and to have an albedo (optical wavelength reflectivity) between 0.0... |
(85713)_1998_SS49_1179474 | Based on the article about '(85713) 1998 SS49', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named. | [
"(85713) 1998 SS49 — Diameter and albedo\n\nSurveys contrast: of the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer. These measure the object as between 2 and 3.484 kilometers lengthways (in diameter) and to have an albedo (optical wavelength reflectivity) between 0.0... |
(85713)_1998_SS49_1179469 | Based on the article about '(85713) 1998 SS49', describe the 'Orbit and classification' section. | is a member of the dynamical Apollo group, which are Earth-crossing asteroids. Apollo asteroids are the largest subgroup of near-Earth objects. It orbits the Sun at a distance of 0.7–3.2 AU once every 2 years and 8 months (975 days; semi-major axis of 1.92 AU). Its orbit has a high eccentricity of 0.64 and an inclinati... | [
"(85713) 1998 SS49 — Diameter and albedo\n\nSurveys contrast: of the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer. These measure the object as between 2 and 3.484 kilometers lengthways (in diameter) and to have an albedo (optical wavelength reflectivity) between 0.0... |
(85713)_1998_SS49_1179470 | What does the article about '(85713) 1998 SS49' say regarding 'Close approaches'? | At about absolute magnitude 15.6, is one of the brightest and presumably largest known potentially hazardous asteroid (see PHA-list). It has a very low Earth minimum orbital intersection distance of 0.0023 AU. On 26 November 1902, this asteroid made its closest near-Earth encounter since 1900 at a nominal distance of 0... | [
"(85713) 1998 SS49 — Diameter and albedo\n\nSurveys contrast: of the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer. These measure the object as between 2 and 3.484 kilometers lengthways (in diameter) and to have an albedo (optical wavelength reflectivity) between 0.0... |
(85713)_1998_SS49_1179472 | What does the article about '(85713) 1998 SS49' say regarding 'Rotation period'? | In 2014, two rotational lightcurves of were obtained from photometric observations by American astronomer Brian Warner at the CS3–Palmer Divide Station in California (U82). Lightcurve analysis gave a rotation period of 5.370 and 5.66 hours and a brightness variation of 0.18 and 0.06 magnitude, respectively (U=2/2), one... | [
"(85713) 1998 SS49 — Diameter and albedo\n\nSurveys contrast: of the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer. These measure the object as between 2 and 3.484 kilometers lengthways (in diameter) and to have an albedo (optical wavelength reflectivity) between 0.0... |
(85713)_1998_SS49_1179468 | What information does the article about '(85713) 1998 SS49' provide? | , provisional 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. The asteroid was discovered on 29 September 1998, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site n... | [
"(85713) 1998 SS49 — Diameter and albedo\n\nSurveys contrast: of the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer. These measure the object as between 2 and 3.484 kilometers lengthways (in diameter) and to have an albedo (optical wavelength reflectivity) between 0.0... |
(85990)_1999_JV6_24471325 | Explain what '(85990) 1999 JV6' covers in the 'Close approaches' section. | In January 2015, approached Earth within a distance of 0.0833 AU. During the encounter, was observed by radar from the Arecibo, Green Bank, and Goldstone observatories. In January 2016, has made another close approach at a distance of 0.032 AU, several times closer than the encounter in 2015. The Minor Planet Center ha... | [
"(85990) 1999 JV6 — Close approaches\n\nIn January 2015, approached Earth within a distance of 0.0833 AU. During the encounter, was observed by radar from the Arecibo, Green Bank, and Goldstone observatories. In January 2016, has made another close approach at a distance of 0.032 AU, several times closer than the e... |
(85990)_1999_JV6_24471326 | Explain what '(85990) 1999 JV6' covers in the 'Physical characteristics' section. | was discovered in May 1999 by the Lincoln Near-Earth Asteroid Research (LINEAR) program at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico. Most properties of have been determined through photometry, spectroscopy, infrared radiometry, and radar imaging. Binzel et al. (2001) have found that has ... | [
"(85990) 1999 JV6 — Close approaches\n\nIn January 2015, approached Earth within a distance of 0.0833 AU. During the encounter, was observed by radar from the Arecibo, Green Bank, and Goldstone observatories. In January 2016, has made another close approach at a distance of 0.032 AU, several times closer than the e... |
(85990)_1999_JV6_24471324 | Summarize the following section from the article on '(85990) 1999 JV6'. | ''', provisional designation ', is a sub-kilometer near-Earth asteroid and a potentially hazardous object of the Apollo group. It was discovered by astronomers of the LINEAR program at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico. is a contact binary object consisting of two distinct lobes, ... | [
"(85990) 1999 JV6 — Close approaches\n\nIn January 2015, approached Earth within a distance of 0.0833 AU. During the encounter, was observed by radar from the Arecibo, Green Bank, and Goldstone observatories. In January 2016, has made another close approach at a distance of 0.032 AU, several times closer than the e... |
(86039)_1999_NC43_18558852 | Based on the article about '(86039) 1999 NC43', describe the 'Discovery' section. | The asteroid was discovered on 14 July 1999, by the Lincoln Near-Earth Asteroid Research (LINEAR) team at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico, USA, at an apparent magnitude of 18, using a 1.0-meter reflector. Its first observation was made by the Catalina Sky Survey in June 1999, exten... | [
"(86039) 1999 NC43 — Discovery\n\nThe asteroid was discovered on 14 July 1999, by the Lincoln Near-Earth Asteroid Research (LINEAR) team at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico, USA, at an apparent magnitude of 18, using a 1.0-meter reflector. Its first observation was made by the C... |
(86039)_1999_NC43_18558851 | Summarize the following section from the article on '(86039) 1999 NC43'. | , is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 2 kilometers in diameter. This suspected tumbler and relatively slow rotator was discovered by LINEAR in 1999. | [
"(86039) 1999 NC43 — Discovery\n\nThe asteroid was discovered on 14 July 1999, by the Lincoln Near-Earth Asteroid Research (LINEAR) team at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico, USA, at an apparent magnitude of 18, using a 1.0-meter reflector. Its first observation was made by the C... |
(86039)_1999_NC43_18558853 | From the article on '(86039) 1999 NC43', restate the 'Orbit and classification' content. | has a well-determined orbit with an uncertainty of 0. The body orbits the Sun at a distance of 0.7–2.8 AU once every 2 years and 4 months (852 days). Its orbit has an eccentricity of 0.58 and an inclination of 7° with respect to the ecliptic. Its Earth minimum orbit intersection distance is 0.0243 AU, which corresponds... | [
"(86039) 1999 NC43 — Discovery\n\nThe asteroid was discovered on 14 July 1999, by the Lincoln Near-Earth Asteroid Research (LINEAR) team at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico, USA, at an apparent magnitude of 18, using a 1.0-meter reflector. Its first observation was made by the C... |
(86039)_1999_NC43_18558857 | Explain what '(86039) 1999 NC43' covers in the 'Chelyabinsk meteor fragment' section. | is suspected to be related to the 20-meter Chelyabinsk meteor, which exploded as a bright fireball over Russia on 15 February 2013. Analysis showed similar orbits for both bodies and suggested that they were once part of the same object. | [
"(86039) 1999 NC43 — Discovery\n\nThe asteroid was discovered on 14 July 1999, by the Lincoln Near-Earth Asteroid Research (LINEAR) team at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico, USA, at an apparent magnitude of 18, using a 1.0-meter reflector. Its first observation was made by the C... |
(86039)_1999_NC43_18558854 | From the article on '(86039) 1999 NC43', restate the 'Physical characteristics' content. | The rare Q-type asteroid is one of only 20 characterized bodies of this spectral type in the SMASS taxonomic scheme. | [
"(86039) 1999 NC43 — Discovery\n\nThe asteroid was discovered on 14 July 1999, by the Lincoln Near-Earth Asteroid Research (LINEAR) team at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico, USA, at an apparent magnitude of 18, using a 1.0-meter reflector. Its first observation was made by the C... |
(86039)_1999_NC43_18558858 | Based on the article about '(86039) 1999 NC43', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named. | [
"(86039) 1999 NC43 — Discovery\n\nThe asteroid was discovered on 14 July 1999, by the Lincoln Near-Earth Asteroid Research (LINEAR) team at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico, USA, at an apparent magnitude of 18, using a 1.0-meter reflector. Its first observation was made by the C... |
(86039)_1999_NC43_18558856 | Summarize the 'Diameter and albedo' part of '(86039) 1999 NC43'. | According to the survey carried out by the Japanese Akari satellite, the asteroid has a high albedo of 0.35 and a diameter of 1.43 kilometers. Observations by the Keck Observatory in the thermal infrared gave a refined albedo of 0.13–0.14 with a larger diameter of 2.22 kilometers. | [
"(86039) 1999 NC43 — Discovery\n\nThe asteroid was discovered on 14 July 1999, by the Lincoln Near-Earth Asteroid Research (LINEAR) team at Lincoln Laboratory's Experimental Test Site, near Socorro, New Mexico, USA, at an apparent magnitude of 18, using a 1.0-meter reflector. Its first observation was made by the C... |
(88710)_2001_SL9_30272006 | Describe the content of the article about '(88710) 2001 SL9'. | is a sub-kilometer asteroid and binary system, classified as near-Earth object of Apollo group discovered by NEAT at Palomar Observatory on 18 September 2001. It measures approximately 960 meters in diameter, while its 2001-discovered minor-planet moon has an estimated diameter of 200 meters based on a secondary to pri... | [
"(88710) 2001 SL9\n\nis a sub-kilometer asteroid and binary system, classified as near-Earth object of Apollo group discovered by NEAT at Palomar Observatory on 18 September 2001. It measures approximately 960 meters in diameter, while its 2001-discovered minor-planet moon has an estimated diameter of 200 meters ba... |
(88710)_2001_SL9_30272008 | Summarize the 'Moon' part of '(88710) 2001 SL9'. | has one minor-planet moon,. It was discovered from lightcurve observations made by Czech astronomer Petr Pravec and collaborators. This moon is approximately 200 m in diameter. Its semi-major axis is 1.6 km and its orbital period is 16.4 hours. | [
"(88710) 2001 SL9\n\nis a sub-kilometer asteroid and binary system, classified as near-Earth object of Apollo group discovered by NEAT at Palomar Observatory on 18 September 2001. It measures approximately 960 meters in diameter, while its 2001-discovered minor-planet moon has an estimated diameter of 200 meters ba... |
(88710)_2001_SL9_30272007 | What information does the article about '(88710) 2001 SL9' provide on 'Near-Earth asteroid'? | Although is classified as a near-Earth object, it does not pose any threats. It has never, nor will it ever in the next century, come closer than 0.1 AU from Earth or Venus. However, the asteroid would make a good target for a spacecraft flyby, as a flyby to would only require a delta-v of 5.4 km/s. | [
"(88710) 2001 SL9\n\nis a sub-kilometer asteroid and binary system, classified as near-Earth object of Apollo group discovered by NEAT at Palomar Observatory on 18 September 2001. It measures approximately 960 meters in diameter, while its 2001-discovered minor-planet moon has an estimated diameter of 200 meters ba... |
(89830)_2002_CE_1009948 | What does the article about '(89830) 2002 CE' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named. | [
"(89830) 2002 CE — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(89830) 2002 CE\n\n(89830) 2002 CE, provisional designation, is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the ... |
(89830)_2002_CE_1009942 | What information does the article about '(89830) 2002 CE' provide? | (89830) 2002 CE, provisional designation, is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3.1 kilometers in diameter. It was discovered on 1 February 2002, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near So... | [
"(89830) 2002 CE — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(89830) 2002 CE\n\n(89830) 2002 CE, provisional designation, is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the ... |
(89830)_2002_CE_1009943 | Summarize the 'Orbit and classification' part of '(89830) 2002 CE'. | is a member of the dynamical Amor group, which are Mars-crossing asteroids that approach the orbit of Earth from beyond, but do not cross it. It orbits the Sun at a distance of 1.0–3.1 AU once every 2 years and 12 months (1,094 days; semi-major axis of 2.08 AU). Its orbit has a high eccentricity of 0.51 and an inclinat... | [
"(89830) 2002 CE — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(89830) 2002 CE\n\n(89830) 2002 CE, provisional designation, is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the ... |
(89830)_2002_CE_1009945 | Based on the article about '(89830) 2002 CE', describe the 'Physical characteristics' section. | has been characterized as a common, stony S-type asteroid by astronomers conducting spectroscopic observations using the New Technology Telescope at La Silla, Chile, and the 2.2-meter telescope of the Calar Alto Observatory in Spain. | [
"(89830) 2002 CE — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(89830) 2002 CE\n\n(89830) 2002 CE, provisional designation, is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the ... |
(89830)_2002_CE_1009944 | What does the article about '(89830) 2002 CE' say regarding 'Close approaches'? | With an absolute magnitude of 14.9, is one of the brightest and largest known potentially hazardous asteroid (see PHA-list). It has an Earth minimum orbital intersection distance of 0.0277 AU, which corresponds to 10.8 lunar distances. | [
"(89830) 2002 CE — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(89830) 2002 CE\n\n(89830) 2002 CE, provisional designation, is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the ... |
(90075)_2002_VU94_1178936 | From the article on '(90075) 2002 VU94', restate the 'Numbering and naming' content. | This minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named. | [
"(90075) 2002 VU94 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(90075) 2002 VU94 — Physical characteristics\n\nis an assumed, stony S-type asteroid.",
"(90075) 2002 VU94 — Rotation period\n\nIn 2014 and 2017, severa... |
(90075)_2002_VU94_1178934 | Describe the 'Rotation period' section of the article about '(90075) 2002 VU94'. | In 2014 and 2017, several rotational lightcurves of were obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station (U82) in California. Lightcurve analysis gave a consolidated rotation period of 7.879 hours with a brightness amplitude between 0.31 and 0.64 magnitude (U=3-).... | [
"(90075) 2002 VU94 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(90075) 2002 VU94 — Physical characteristics\n\nis an assumed, stony S-type asteroid.",
"(90075) 2002 VU94 — Rotation period\n\nIn 2014 and 2017, severa... |
(90075)_2002_VU94_1178931 | Describe the 'Orbit and classification' section of the article about '(90075) 2002 VU94'. | is a member of the dynamical Apollo group, which are Earth-crossing asteroids. Apollo asteroids are the largest subgroup of near-Earth objects. It orbits the Sun at a distance of 0.9–3.4 AU once every 3 years and 1 month (1,138 days; semi-major axis of 2.13 AU). Its orbit has an eccentricity of 0.58 and an inclination ... | [
"(90075) 2002 VU94 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(90075) 2002 VU94 — Physical characteristics\n\nis an assumed, stony S-type asteroid.",
"(90075) 2002 VU94 — Rotation period\n\nIn 2014 and 2017, severa... |
(90075)_2002_VU94_1178935 | Based on the article about '(90075) 2002 VU94', describe the 'Diameter and albedo' section. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 2.233 kilometers in diameter and its surface has an albedo of 0.294, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20, and calculates a diameter of 2.5... | [
"(90075) 2002 VU94 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(90075) 2002 VU94 — Physical characteristics\n\nis an assumed, stony S-type asteroid.",
"(90075) 2002 VU94 — Rotation period\n\nIn 2014 and 2017, severa... |
(90075)_2002_VU94_1178930 | Describe the content of the article about '(90075) 2002 VU94'. | , provisional designation, is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 2.5 kilometers in diameter. It was discovered on 13 November 2002, by astronomers of the Near-Earth Asteroid Tracking program at Palomar Observatory in C... | [
"(90075) 2002 VU94 — Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 30 August 2004. As of 2018, it has not been named.",
"(90075) 2002 VU94 — Physical characteristics\n\nis an assumed, stony S-type asteroid.",
"(90075) 2002 VU94 — Rotation period\n\nIn 2014 and 2017, severa... |
(90568)_2004_GV9_18437101 | What information does the article about '(90568) 2004 GV9' provide? | is a trans-Neptunian object that was discovered on April 13, 2004 by NEAT. It has been listed as a cubewano by the Minor Planet Center. | [
"(90568) 2004 GV9\n\nis a trans-Neptunian object that was discovered on April 13, 2004 by NEAT. It has been listed as a cubewano by the Minor Planet Center.",
"(90568) 2004 GV9 — Orbit\n\n2004_GV9-orbit.png It has an orbital period of 273.88 years. Its maximum possible distance from the Sun (aphelion) is 45.62 AU... |
(90568)_2004_GV9_18437104 | What does the article about '(90568) 2004 GV9' say regarding 'Orbit'? | 2004_GV9-orbit.png It has an orbital period of 273.88 years. Its maximum possible distance from the Sun (aphelion) is 45.62 AU, and its closest (perihelion) is 38.7 AU, and currently 39.7 AU from he sun. It has an inclination of 21.9718, and eccentricity of 0.082. | [
"(90568) 2004 GV9\n\nis a trans-Neptunian object that was discovered on April 13, 2004 by NEAT. It has been listed as a cubewano by the Minor Planet Center.",
"(90568) 2004 GV9 — Orbit\n\n2004_GV9-orbit.png It has an orbital period of 273.88 years. Its maximum possible distance from the Sun (aphelion) is 45.62 AU... |
(90568)_2004_GV9_18437102 | Based on the article about '(90568) 2004 GV9', describe the 'Discovery' section. | It was discovered on 13 April 2004 by NEAT. It has been observed forty-seven times, with precovery images back to 1954. | [
"(90568) 2004 GV9\n\nis a trans-Neptunian object that was discovered on April 13, 2004 by NEAT. It has been listed as a cubewano by the Minor Planet Center.",
"(90568) 2004 GV9 — Orbit\n\n2004_GV9-orbit.png It has an orbital period of 273.88 years. Its maximum possible distance from the Sun (aphelion) is 45.62 AU... |
(90568)_2004_GV9_18437103 | Reconstruct the content about 'Size estimate' from the article on '(90568) 2004 GV9'. | Brown estimates that is very likely a dwarf planet. A diameter of 680 km has been determined from combined observations of the Herschel and Spitzer space telescopes. Tancredi notes that light-curve-amplitude analysis shows only small deviations, suggesting that could be a spheroid with small albedo spots and hence a dw... | [
"(90568) 2004 GV9\n\nis a trans-Neptunian object that was discovered on April 13, 2004 by NEAT. It has been listed as a cubewano by the Minor Planet Center.",
"(90568) 2004 GV9 — Orbit\n\n2004_GV9-orbit.png It has an orbital period of 273.88 years. Its maximum possible distance from the Sun (aphelion) is 45.62 AU... |
(91205)_1998_US43_17089249 | Summarize the following section from the article on '(91205) 1998 US43'. | , provisional designation, is a resonant trans-Neptunian object of the plutino group, located in the Kuiper belt in the outermost region of the Solar System. The rather bluish body measures approximately 111 km in diameter. It was discovered on 22 October 1998, by American astronomer Marc Buie at the Kitt Peak National... | [
"(91205) 1998 US43\n\n, provisional designation, is a resonant trans-Neptunian object of the plutino group, located in the Kuiper belt in the outermost region of the Solar System. The rather bluish body measures approximately 111 km in diameter. It was discovered on 22 October 1998, by American astronomer Marc Buie... |
(91205)_1998_US43_17089250 | From the article on '(91205) 1998 US43', restate the 'Classification and orbit' content. | belongs to the plutino population, which are named after the group's largest member, Pluto. Plutinos are resonant trans-Neptunian objects in 2:3 resonance with Neptune, orbiting the Sun twice for every three orbits Neptune does. It orbits the Sun at a distance of 33.9–44.2 AU once every 244 years and 2 months (89,179 d... | [
"(91205) 1998 US43\n\n, provisional designation, is a resonant trans-Neptunian object of the plutino group, located in the Kuiper belt in the outermost region of the Solar System. The rather bluish body measures approximately 111 km in diameter. It was discovered on 22 October 1998, by American astronomer Marc Buie... |
(91205)_1998_US43_17089252 | Summarize the 'Physical characteristics' part of '(91205) 1998 US43'. | Based on an absolute magnitude of 8.0 and an assumed albedo of 0.09, the Johnston's Archive estimates a diameter of 111 kilometers. The body's spectrum (BB–BR) suggests a somewhat bluish color. As of 2018, no rotational lightcurve of has been obtained from photometric observations. it an unlikely dwarf planet candidate... | [
"(91205) 1998 US43\n\n, provisional designation, is a resonant trans-Neptunian object of the plutino group, located in the Kuiper belt in the outermost region of the Solar System. The rather bluish body measures approximately 111 km in diameter. It was discovered on 22 October 1998, by American astronomer Marc Buie... |
(91205)_1998_US43_17089251 | Summarize the 'Numbering and naming' part of '(91205) 1998 US43'. | This minor planet was numbered by the Minor Planet Center on 28 October 2004 (M.P.C. 52912). As of 2018, it has not been named. | [
"(91205) 1998 US43\n\n, provisional designation, is a resonant trans-Neptunian object of the plutino group, located in the Kuiper belt in the outermost region of the Solar System. The rather bluish body measures approximately 111 km in diameter. It was discovered on 22 October 1998, by American astronomer Marc Buie... |
(9928)_1981_WE9_1474234 | Summarize the 'Diameter and albedo' part of '(9928) 1981 WE9'. | According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures between 2.44 and 3.00 kilometers in diameter, and its surface has an albedo between 0.283 and 0.428. The Collaborative Asteroid Lightcurve Link assumes an intermediate albedo of 0... | [
"(9928) 1981 WE9 — Diameter and albedo\n\nAccording to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures between 2.44 and 3.00 kilometers in diameter, and its surface has an albedo between 0.283 and 0.428. The Collaborative Asteroid Light... |
(9928)_1981_WE9_1474235 | Describe the 'Numbering and naming' section of the article about '(9928) 1981 WE9'. | This minor planet was numbered by the Minor Planet Center on 2 February 1999. As of 2018, it has not been named. | [
"(9928) 1981 WE9 — Diameter and albedo\n\nAccording to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures between 2.44 and 3.00 kilometers in diameter, and its surface has an albedo between 0.283 and 0.428. The Collaborative Asteroid Light... |
(9928)_1981_WE9_1474231 | Describe the content of the article about '(9928) 1981 WE9'. | , provisional designation, is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 3 kilometers in diameter. It was discovered on 16 November 1981, by astronomers at Perth Observatory in Bickley, Australia. | [
"(9928) 1981 WE9 — Diameter and albedo\n\nAccording to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures between 2.44 and 3.00 kilometers in diameter, and its surface has an albedo between 0.283 and 0.428. The Collaborative Asteroid Light... |
(9928)_1981_WE9_1474233 | Explain what '(9928) 1981 WE9' covers in the 'Physical characteristics' section. | In December 2014, astronomer Maurice Clark obtained a rotational lightcurve from photometric observations at Preston Gott Observatory. Lightcurve analysis gave an ambiguous rotation period of 18.3980 hours with a brightness variation of 0.41 magnitude, suggesting a non-spheroidal shape (U=2+). The alternative period so... | [
"(9928) 1981 WE9 — Diameter and albedo\n\nAccording to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures between 2.44 and 3.00 kilometers in diameter, and its surface has an albedo between 0.283 and 0.428. The Collaborative Asteroid Light... |
(9928)_1981_WE9_1474232 | Explain what '(9928) 1981 WE9' covers in the 'Orbit and classification' section. | The stony S-type asteroid is a member of the Flora family, one of the largest groups of asteroids in the main-belt. It orbits the Sun at a distance of 1.8–2.6 AU once every 3 years and 4 months (1,206 days). Its orbit has an eccentricity of 0.18 and an inclination of 3° with respect to the ecliptic. A first precovery w... | [
"(9928) 1981 WE9 — Diameter and albedo\n\nAccording to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures between 2.44 and 3.00 kilometers in diameter, and its surface has an albedo between 0.283 and 0.428. The Collaborative Asteroid Light... |
(9942)_1989_TM1_30701719 | From the article on '(9942) 1989 TM1', restate the 'Diameter and albedo' content. | The asteroid was predicted to cross the focal plane array of the Infrared Astronomical Satellite (IRAS). However, it was missed on each of its seven planned observation and was never detected. According to the "missed predictions file" of the supplemental IRAS minor planet survey (SIMPS), the body was expected to have ... | [
"(9942) 1989 TM1 — Diameter and albedo\n\nThe asteroid was predicted to cross the focal plane array of the Infrared Astronomical Satellite (IRAS). However, it was missed on each of its seven planned observation and was never detected. According to the \"missed predictions file\" of the supplemental IRAS minor plane... |
(9942)_1989_TM1_30701720 | Reconstruct the content about 'Rotation period' from the article on '(9942) 1989 TM1'. | In October 2010, a rotational lightcurve for this asteroid was obtained from photometric observations at the Palomar Transient Factory in California. It rendered a tentative rotation period of 3.071 hours with a brightness variation of 0.08 in magnitude (U=1). | [
"(9942) 1989 TM1 — Diameter and albedo\n\nThe asteroid was predicted to cross the focal plane array of the Infrared Astronomical Satellite (IRAS). However, it was missed on each of its seven planned observation and was never detected. According to the \"missed predictions file\" of the supplemental IRAS minor plane... |
(9942)_1989_TM1_30701718 | From the article on '(9942) 1989 TM1', restate the 'Numbering and naming' content. | This minor planet was numbered by the Minor Planet Center on 2 February 1999. As of 2018, it has not been named. | [
"(9942) 1989 TM1 — Diameter and albedo\n\nThe asteroid was predicted to cross the focal plane array of the Infrared Astronomical Satellite (IRAS). However, it was missed on each of its seven planned observation and was never detected. According to the \"missed predictions file\" of the supplemental IRAS minor plane... |
(9942)_1989_TM1_30701716 | What information does the article about '(9942) 1989 TM1' provide? | ''', provisional designation ', is a background asteroid from the central region of the asteroid belt, approximately 4.5 km in diameter. It was discovered on 8 October 1989, by Japanese astronomers Nobuhiro Kawasato and Tsutomu Hioki at the Okutama Observatory in Japan. The asteroid has a tentative rotation period of 3... | [
"(9942) 1989 TM1 — Diameter and albedo\n\nThe asteroid was predicted to cross the focal plane array of the Infrared Astronomical Satellite (IRAS). However, it was missed on each of its seven planned observation and was never detected. According to the \"missed predictions file\" of the supplemental IRAS minor plane... |
(9942)_1989_TM1_30701717 | Summarize the 'Orbit and classification' part of '(9942) 1989 TM1'. | The assumed stony S-type is a non-family asteroid from the main belt's background population. It orbits the Sun in the central main-belt at a distance of 2.2–3.0 AU once every 4 years and 2 months (1,527 days; semi-major axis of 2.6 AU). Its orbit has an eccentricity of 0.17 and an inclination of 10° with respect to th... | [
"(9942) 1989 TM1 — Diameter and albedo\n\nThe asteroid was predicted to cross the focal plane array of the Infrared Astronomical Satellite (IRAS). However, it was missed on each of its seven planned observation and was never detected. According to the \"missed predictions file\" of the supplemental IRAS minor plane... |
(9948)_1990_QB2_29335593 | Reconstruct the content from the article about '(9948) 1990 QB2'. | ''', provisional designation ', is a stony Nysian asteroid from the inner region of the asteroid belt, approximately 3.4 km in diameter. It was discovered on 22 August 1990, by American astronomer Henry Holt at the Palomar Observatory in California. The likely elongated S-type asteroid has a rotation period of 3.53 hou... | [
"(9948) 1990 QB2\n\n''', provisional designation ', is a stony Nysian asteroid from the inner region of the asteroid belt, approximately 3.4 km in diameter. It was discovered on 22 August 1990, by American astronomer Henry Holt at the Palomar Observatory in California. The likely elongated S-type asteroid has a rot... |
(9948)_1990_QB2_29335597 | Based on the article about '(9948) 1990 QB2', describe the 'Diameter and albedo' section. | According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 3.345 kilometers in diameter and its surface has an albedo of 0.250. The Collaborative Asteroid Lightcurve Link adopts Petr Pravec's revised WISE-result, that is, an albedo of 0.2232 and a diameter of 3.3... | [
"(9948) 1990 QB2\n\n''', provisional designation ', is a stony Nysian asteroid from the inner region of the asteroid belt, approximately 3.4 km in diameter. It was discovered on 22 August 1990, by American astronomer Henry Holt at the Palomar Observatory in California. The likely elongated S-type asteroid has a rot... |
(9948)_1990_QB2_29335594 | Reconstruct the content about 'Orbit and classification' from the article on '(9948) 1990 QB2'. | is member of the Nysa family (405), located in the Nysa–Polana complex. It is named after 44 Nysa and one of the largest families in the main belt. The asteroid orbits the Sun in the inner asteroid belt at a distance of 1.9–2.9 AU once every 3 years and 8 months (1,344 days; semi-major axis of 2.38 AU). Its orbit has a... | [
"(9948) 1990 QB2\n\n''', provisional designation ', is a stony Nysian asteroid from the inner region of the asteroid belt, approximately 3.4 km in diameter. It was discovered on 22 August 1990, by American astronomer Henry Holt at the Palomar Observatory in California. The likely elongated S-type asteroid has a rot... |
(99907)_1989_VA_32369637 | From the article on '(99907) 1989 VA', restate the 'Orbit and classification' content. | It is a member of the Aten asteroid, a subgroup of near-Earth objects that are located in the zone of influence of Venus. It has frequent, relatively close encounters with the Earth, as its minimum orbit intersection distance (MOID) is 0.16 AU or about 23 million kilometers. It was the eighth Aten asteroid discovered. ... | [
"(99907) 1989 VA — Orbit and classification\n\nIt is a member of the Aten asteroid, a subgroup of near-Earth objects that are located in the zone of influence of Venus. It has frequent, relatively close encounters with the Earth, as its minimum orbit intersection distance (MOID) is 0.16 AU or about 23 million kilom... |
(99907)_1989_VA_32369640 | What information does the article about '(99907) 1989 VA' provide on 'Orbit and classification'? | the first Aten asteroid discovered to get closer to the Sun (0.295 AU) than Mercury ever does. 2340 Hathor (the second Aten discovered, in 1976) had the smallest perihelion (0.464 AU) earlier, which was about the same distance as Mercury's aphelion (0.467 AU). It was not until (0.277 AU) was discovered that an Aten ast... | [
"(99907) 1989 VA — Orbit and classification\n\nIt is a member of the Aten asteroid, a subgroup of near-Earth objects that are located in the zone of influence of Venus. It has frequent, relatively close encounters with the Earth, as its minimum orbit intersection distance (MOID) is 0.16 AU or about 23 million kilom... |
(99907)_1989_VA_32369642 | What does the article about '(99907) 1989 VA' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 22 June 2005. As of 2018, it has not been named. | [
"(99907) 1989 VA — Orbit and classification\n\nIt is a member of the Aten asteroid, a subgroup of near-Earth objects that are located in the zone of influence of Venus. It has frequent, relatively close encounters with the Earth, as its minimum orbit intersection distance (MOID) is 0.16 AU or about 23 million kilom... |
(99907)_1989_VA_32369638 | From the article on '(99907) 1989 VA', restate the 'Orbit and classification' content. | an exceptionally high eccentricity of 0.59, it was the most eccentric Aten asteroid known at the time of discovery, more eccentric than previously discovered Aten, 3753 Cruithne. Since then, more eccentric Atens – such as, with an eccentricity of 0.665 – have been discovered. Due to this elongated orbit, the Aten aster... | [
"(99907) 1989 VA — Orbit and classification\n\nIt is a member of the Aten asteroid, a subgroup of near-Earth objects that are located in the zone of influence of Venus. It has frequent, relatively close encounters with the Earth, as its minimum orbit intersection distance (MOID) is 0.16 AU or about 23 million kilom... |
(A)_Senile_Animal_32868005 | Summarize the 'Critical reception' part of '(A) Senile Animal'. | AllMusic's Greg Prato wrote: "The transfusion of new blood has made one of rock's gnarliest beats even -- gnarlier!". Drowned in Sound's Grant Purdum stated: "In lieu of live albums and collaborations aplenty, A Senile Animal couldn't have snarled to life at a better time." | [
"(A) Senile Animal — Critical reception\n\nAllMusic's Greg Prato wrote: \"The transfusion of new blood has made one of rock's gnarliest beats even -- gnarlier!\". Drowned in Sound's Grant Purdum stated: \"In lieu of live albums and collaborations aplenty, A Senile Animal couldn't have snarled to life at a better ti... |
(A)_Senile_Animal_32868008 | Explain what '(A) Senile Animal' covers in the 'Additional personnel' section. | Toshi Kasai – engineer, mixing ; John Golden – mastering ; Mackie Osborne – art ; Kevin Willis – band photos | [
"(A) Senile Animal — Critical reception\n\nAllMusic's Greg Prato wrote: \"The transfusion of new blood has made one of rock's gnarliest beats even -- gnarlier!\". Drowned in Sound's Grant Purdum stated: \"In lieu of live albums and collaborations aplenty, A Senile Animal couldn't have snarled to life at a better ti... |
(A)_Senile_Animal_32868002 | Summarize the following section from the article on '(A) Senile Animal'. | (A) Senile Animal is the 15th album (not including split albums) by American rock band Melvins, released on October 10, 2006 on Ipecac Recordings. After bassist Kevin Rutmanis' departure the two remaining members of the Melvins joined forces with Big Business, a duo consisting of Jared Warren on bass and Coady Willis o... | [
"(A) Senile Animal — Critical reception\n\nAllMusic's Greg Prato wrote: \"The transfusion of new blood has made one of rock's gnarliest beats even -- gnarlier!\". Drowned in Sound's Grant Purdum stated: \"In lieu of live albums and collaborations aplenty, A Senile Animal couldn't have snarled to life at a better ti... |
(A)_Senile_Animal_32868006 | From the article on '(A) Senile Animal', restate the 'Vinyl edition' content. | The vinyl edition was released as a 4-LP box set from Hydra Head Records. Each LP featured music on one side and an etching on the other. This was limited to 300 copies in a variety of colors and designs. | [
"(A) Senile Animal — Critical reception\n\nAllMusic's Greg Prato wrote: \"The transfusion of new blood has made one of rock's gnarliest beats even -- gnarlier!\". Drowned in Sound's Grant Purdum stated: \"In lieu of live albums and collaborations aplenty, A Senile Animal couldn't have snarled to life at a better ti... |
(A)_Senile_Animal_32868007 | Describe the 'Personnel' section of the article about '(A) Senile Animal'. | Coady Willis – drums, vocals ; Dale Crover – drums, vocals ; Jared Warren – bass guitar, vocals ; King Buzzo – guitar, vocals | [
"(A) Senile Animal — Critical reception\n\nAllMusic's Greg Prato wrote: \"The transfusion of new blood has made one of rock's gnarliest beats even -- gnarlier!\". Drowned in Sound's Grant Purdum stated: \"In lieu of live albums and collaborations aplenty, A Senile Animal couldn't have snarled to life at a better ti... |
(Ain't_Nobody_Loves_You)_Like_I_Do_11804957 | Reconstruct the content from the article about '(Ain't Nobody Loves You) Like I Do'. | "(Ain't Nobody Loves You) Like I Do" is a 1987 single by American singer La Toya Jackson. The song is taken from her fifth album, La Toya. It is one of only four songs by Jackson to have an accompanying music video. The song features a bridge sung by Mike Stock. The single was released in 1987 throughout Europe, exclud... | [
"(Ain't Nobody Loves You) Like I Do\n\n\"(Ain't Nobody Loves You) Like I Do\" is a 1987 single by American singer La Toya Jackson. The song is taken from her fifth album, La Toya. It is one of only four songs by Jackson to have an accompanying music video. The song features a bridge sung by Mike Stock. The single w... |
(Ain't_Nobody_Loves_You)_Like_I_Do_11804958 | Reconstruct the content about 'Background' from the article on '(Ain't Nobody Loves You) Like I Do'. | However, the single did fairly well on the German DJ charts. It debuted at No. 17 and stayed on the charts for several months. She also performed the song on the German television show Die Verflixte Sieben (with Rudi Carrell). The music video for the single was given little airplay and was never released on video or DV... | [
"(Ain't Nobody Loves You) Like I Do\n\n\"(Ain't Nobody Loves You) Like I Do\" is a 1987 single by American singer La Toya Jackson. The song is taken from her fifth album, La Toya. It is one of only four songs by Jackson to have an accompanying music video. The song features a bridge sung by Mike Stock. The single w... |
(Ain't_Nobody_Loves_You)_Like_I_Do_11804959 | What information does the article about '(Ain't Nobody Loves You) Like I Do' provide on 'Music video'? | A music video was filmed and released to promote the single. The clip is similar to Jackson's 1983 music video "Heart Don't Lie" in its colourful, cartoon-like cinematography and dance routines. The video can be found on YouTube and on various Jackson fan Web sites. | [
"(Ain't Nobody Loves You) Like I Do\n\n\"(Ain't Nobody Loves You) Like I Do\" is a 1987 single by American singer La Toya Jackson. The song is taken from her fifth album, La Toya. It is one of only four songs by Jackson to have an accompanying music video. The song features a bridge sung by Mike Stock. The single w... |
(Almost)_Straight_Outta_Compton_6875762 | Explain what '(Almost) Straight Outta Compton' covers in the 'Origin' section. | stating that "Plagued by crime and riddled with street gangs, the troubled Los Angeles neighborhood that Doria Ragland, 60, calls home couldn't be more different to London's leafy Kensington. But social worker Ragland might now find herself welcoming a royal guest to downtrodden Crenshaw after Prince Harry was revealed... | [
"(Almost) Straight Outta Compton — Origin\n\nstating that \"Plagued by crime and riddled with street gangs, the troubled Los Angeles neighborhood that Doria Ragland, 60, calls home couldn't be more different to London's leafy Kensington. But social worker Ragland might now find herself welcoming a royal guest to do... |
(Almost)_Straight_Outta_Compton_6875764 | What information does the article about '(Almost) Straight Outta Compton' provide on 'Origin'? | Finlay Greig wrote in the Edinburgh Evening News that the headline insinuates that Meghan comes from a "life of crime", despite being brought up in a middle class area, which had suffered significant damage from both the 1992 Los Angeles riots and the 1994 Northridge earthquake, but was able to rebound in the late 2000... | [
"(Almost) Straight Outta Compton — Origin\n\nstating that \"Plagued by crime and riddled with street gangs, the troubled Los Angeles neighborhood that Doria Ragland, 60, calls home couldn't be more different to London's leafy Kensington. But social worker Ragland might now find herself welcoming a royal guest to do... |
(Almost)_Straight_Outta_Compton_6875763 | Based on the article about '(Almost) Straight Outta Compton', describe the 'Origin' section. | the area profiled in the article. A separate article by the British tabloid the Daily Star had a headline querying whether Harry would "marry into gangster royalty?". Markle grew up in the 1980s and 1990s. She became engaged to Prince Harry in 2017. Upon their marriage in 2018, she became the Duchess of Sussex. Their s... | [
"(Almost) Straight Outta Compton — Origin\n\nstating that \"Plagued by crime and riddled with street gangs, the troubled Los Angeles neighborhood that Doria Ragland, 60, calls home couldn't be more different to London's leafy Kensington. But social worker Ragland might now find herself welcoming a royal guest to do... |
(Almost)_Straight_Outta_Compton_6875768 | Based on the article about '(Almost) Straight Outta Compton', describe the 'Reaction' section. | her race". Activist and lawyer Shola Mos-Shogbamimu wrote for The Guardian that she "[could not] believe that we are still having this debate about whether the way that Meghan has been treated is racist. It is misogynoir, pure and simple. Look at the media coverage of her. The Daily Mail said that she was "(almost) str... | [
"(Almost) Straight Outta Compton — Origin\n\nstating that \"Plagued by crime and riddled with street gangs, the troubled Los Angeles neighborhood that Doria Ragland, 60, calls home couldn't be more different to London's leafy Kensington. But social worker Ragland might now find herself welcoming a royal guest to do... |
(Almost)_Straight_Outta_Compton_6875769 | Based on the article about '(Almost) Straight Outta Compton', describe the 'Reaction' section. | offensive and said that it was "not acceptable" to describe sections of the British press as "bigoted". Murray described the article as a "rags to riches" story. Murray has since stepped down from the Society of Editors, after releasing a statement headlined "UK media not bigoted: SoE responds to Sussexes' claims of ra... | [
"(Almost) Straight Outta Compton — Origin\n\nstating that \"Plagued by crime and riddled with street gangs, the troubled Los Angeles neighborhood that Doria Ragland, 60, calls home couldn't be more different to London's leafy Kensington. But social worker Ragland might now find herself welcoming a royal guest to do... |
(Almost)_Straight_Outta_Compton_6875761 | What information does the article about '(Almost) Straight Outta Compton' provide on 'Origin'? | The November 2016 MailOnline article is about the inferred family background of American actress Meghan Markle (born 1981) and her upbringing in the Los Angeles district of Crenshaw with her mother, Doria Ragland. It was published after Markle began dating Prince Harry. The full headline is "Harry's girl is (almost) st... | [
"(Almost) Straight Outta Compton — Origin\n\nstating that \"Plagued by crime and riddled with street gangs, the troubled Los Angeles neighborhood that Doria Ragland, 60, calls home couldn't be more different to London's leafy Kensington. But social worker Ragland might now find herself welcoming a royal guest to do... |
(Almost)_Straight_Outta_Compton_6875765 | Summarize the 'Reaction' part of '(Almost) Straight Outta Compton'. | The tone of this and other articles prompted Prince Harry's Communications Secretary to issue a statement that deplored the "racist" and "sexist" commentary and coverage received by Meghan. The statement described Meghan as having been "...subject to a wave of abuse and harassment. Some of this has been very public — t... | [
"(Almost) Straight Outta Compton — Origin\n\nstating that \"Plagued by crime and riddled with street gangs, the troubled Los Angeles neighborhood that Doria Ragland, 60, calls home couldn't be more different to London's leafy Kensington. But social worker Ragland might now find herself welcoming a royal guest to do... |
(Always_Be_My)_Sunshine_17852362 | Based on the article about '(Always Be My) Sunshine', describe the 'Music video' section. | The music video was directed by Hype Williams. Jay-Z is featured in the video rapping in a room resembling a Rubik's Cube & having a carnival theme to it with Foxy Brown rapping alongside of him. Jay-Z & co-founder of Roc-A-Fella, Damon Dash later regretted doing the video citing that the video wasn't their style. | [
"(Always Be My) Sunshine — A-side\n\n1) \"Sunshine (Album Version)\" ; 2) \"Sunshine (TV Track)\" ; 3) \"Sunshine (Radio Edit)\"",
"(Always Be My) Sunshine — Music video\n\nThe music video was directed by Hype Williams. Jay-Z is featured in the video rapping in a room resembling a Rubik's Cube & having a carnival... |
(Always_Be_My)_Sunshine_17852363 | Based on the article about '(Always Be My) Sunshine', describe the 'CD' section. | 1) "Sunshine (Radio Edit)" (3:15) ; 2) "Sunshine (Album Version)" (4:11) ; 3) "Sunshine (Clean Version)" (4:12) ; 4) "Sunshine (TV track)" (4:12) ; 5) "Sunshine (Acappella)" (3:49) | [
"(Always Be My) Sunshine — A-side\n\n1) \"Sunshine (Album Version)\" ; 2) \"Sunshine (TV Track)\" ; 3) \"Sunshine (Radio Edit)\"",
"(Always Be My) Sunshine — Music video\n\nThe music video was directed by Hype Williams. Jay-Z is featured in the video rapping in a room resembling a Rubik's Cube & having a carnival... |
(And_Now_the_Waltz)_C'est_La_Vie_7394698 | Describe the content of the article about '(And Now the Waltz) C'est La Vie'. | "(And Now the Waltz) C'est La Vie" is a song by the British rock band Slade, released in 1982 as the lead single from the band's eleventh studio album The Amazing Kamikaze Syndrome. It was also included on its 1984 American counterpart Keep Your Hands Off My Power Supply. The song was written by lead vocalist Noddy Hol... | [
"(And Now the Waltz) C'est La Vie\n\n\"(And Now the Waltz) C'est La Vie\" is a song by the British rock band Slade, released in 1982 as the lead single from the band's eleventh studio album The Amazing Kamikaze Syndrome. It was also included on its 1984 American counterpart Keep Your Hands Off My Power Supply. The ... |
(And_Now_the_Waltz)_C'est_La_Vie_7394704 | Based on the article about '(And Now the Waltz) C'est La Vie', describe the 'Critical reception' section. | Upon release, Malcolm Dome of Kerrang! described the song as an "excellent taster" of the band's new studio album. In a review of The Amazing Kamikaze Syndrome, Kerrang! said the song "tends to disappear into the clouds of its own long-winded ambition." Sounds said: "The "Sailing"-style scarves in the air of "My Oh My"... | [
"(And Now the Waltz) C'est La Vie\n\n\"(And Now the Waltz) C'est La Vie\" is a song by the British rock band Slade, released in 1982 as the lead single from the band's eleventh studio album The Amazing Kamikaze Syndrome. It was also included on its 1984 American counterpart Keep Your Hands Off My Power Supply. The ... |
(And_Now_the_Waltz)_C'est_La_Vie_7394702 | What information does the article about '(And Now the Waltz) C'est La Vie' provide on 'Release'? | "(And Now the Waltz) C'est La Vie" was released on 7" vinyl by RCA Records in the UK, Ireland, Australia, Germany and the Netherlands. The B-side, "Merry Xmas Everybody (Live & Kickin')", was exclusive to the single and would later appear on the band's 1985 studio/compilation album Crackers: The Christmas Party Album. ... | [
"(And Now the Waltz) C'est La Vie\n\n\"(And Now the Waltz) C'est La Vie\" is a song by the British rock band Slade, released in 1982 as the lead single from the band's eleventh studio album The Amazing Kamikaze Syndrome. It was also included on its 1984 American counterpart Keep Your Hands Off My Power Supply. The ... |
(And_Now_the_Waltz)_C'est_La_Vie_7394705 | Reconstruct the content about 'Formats' from the article on '(And Now the Waltz) C'est La Vie'. | 7" Single ; 1) "(And Now the Waltz) C'est La Vie" - 3:44 ; 2) "Merry Xmas Everybody (Live & Kickin')" - 4:03 | [
"(And Now the Waltz) C'est La Vie\n\n\"(And Now the Waltz) C'est La Vie\" is a song by the British rock band Slade, released in 1982 as the lead single from the band's eleventh studio album The Amazing Kamikaze Syndrome. It was also included on its 1984 American counterpart Keep Your Hands Off My Power Supply. The ... |
(And_Now_the_Waltz)_C'est_La_Vie_7394699 | Reconstruct the content about 'Background' from the article on '(And Now the Waltz) C'est La Vie'. | Slade started recording their second studio album for RCA in 1982, and in November that year, the album's first single, "(And Now the Waltz) C'est La Vie", was released. Attempting to appeal to the Christmas market, it reached No. 50 in the UK, but fared better in Poland, reaching No. 2 there in January 1983, while als... | [
"(And Now the Waltz) C'est La Vie\n\n\"(And Now the Waltz) C'est La Vie\" is a song by the British rock band Slade, released in 1982 as the lead single from the band's eleventh studio album The Amazing Kamikaze Syndrome. It was also included on its 1984 American counterpart Keep Your Hands Off My Power Supply. The ... |
(And_Now_the_Waltz)_C'est_La_Vie_7394706 | Reconstruct the content about 'Personnel' from the article on '(And Now the Waltz) C'est La Vie'. | Slade ; Noddy Holder - lead vocals, guitar ; Jim Lea - piano, organ, bass, backing vocals, producer of "(And Now the Waltz) C'est La Vie" ; Dave Hill - lead guitar, backing vocals ; Don Powell - drums Additional personnel ; Slade - producer of "Merry Xmas Everybody (Live & Kickin')" | [
"(And Now the Waltz) C'est La Vie\n\n\"(And Now the Waltz) C'est La Vie\" is a song by the British rock band Slade, released in 1982 as the lead single from the band's eleventh studio album The Amazing Kamikaze Syndrome. It was also included on its 1984 American counterpart Keep Your Hands Off My Power Supply. The ... |
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