id string | question string | answer string | documents list |
|---|---|---|---|
(42301)_2001_UR163_3107906 | Summarize the following section from the article on '(42301) 2001 UR163'. | , prov. designation:, is a resonant trans-Neptunian object and possible dwarf planet located in the outermost region of the Solar System. The object measures approximately 352 km in diameter with a high albedo and stays in an uncommon orbital resonance (4:9) with Neptune. It has the reddest color (RR-U) of any object i... | [
"(42301) 2001 UR163 β Classification and orbit\n\nhas been characterized as a dwarf planet candidate. Based on assumptions and estimates, Michael Brown gives it a \"likely\"-status on his website, which is the third highest status after \"near certainty\" and \"highly likely\" (also see his classification table). T... |
(42301)_2001_UR163_3107908 | From the article on '(42301) 2001 UR163', restate the 'Numbering and naming' content. | was numbered (42301) by the Minor Planet Center on 26 May 2002 (M.P.C. 45686). , it has not been named. Acoording to the established naming conventions, it will receive a mythological or mythic name (not necessarily from Classical mythology), in particular one associated with creation. | [
"(42301) 2001 UR163 β Classification and orbit\n\nhas been characterized as a dwarf planet candidate. Based on assumptions and estimates, Michael Brown gives it a \"likely\"-status on his website, which is the third highest status after \"near certainty\" and \"highly likely\" (also see his classification table). T... |
(42301)_2001_UR163_3107909 | From the article on '(42301) 2001 UR163', restate the 'Physical characteristics' content. | Lightcurve analysis shows only small deviations, suggesting that is a spheroid with small albedo spots. Observations with Spitzers Infrared Array Camera were used to study the body's surface composition. The analyzed data indicate the presence of 20% water ice, 60% amorphous silicates, and 20% organic compounds, inclu... | [
"(42301) 2001 UR163 β Classification and orbit\n\nhas been characterized as a dwarf planet candidate. Based on assumptions and estimates, Michael Brown gives it a \"likely\"-status on his website, which is the third highest status after \"near certainty\" and \"highly likely\" (also see his classification table). T... |
(432949)_2012_HH2_25132253 | What information does the article about '(432949) 2012 HH2' provide on 'Orbit and classification'? | is a resonant trans-Neptunian object in an uncommon 4:5 resonance with Neptune (DES: 5:4E). It orbits the Sun at a distance of 29.2β40.4 AU once every 205 years and 4 months (75,008 days; semi-major axis of 34.81 AU). Its orbit has an eccentricity of 0.16 and an inclination of 29Β° with respect to the ecliptic. It is cu... | [
"(432949) 2012 HH2 β Orbit and classification\n\nis a resonant trans-Neptunian object in an uncommon 4:5 resonance with Neptune (DES: 5:4E). It orbits the Sun at a distance of 29.2β40.4 AU once every 205 years and 4 months (75,008 days; semi-major axis of 34.81 AU). Its orbit has an eccentricity of 0.16 and an incl... |
(432949)_2012_HH2_25132252 | Summarize the following section from the article on '(432949) 2012 HH2'. | is a resonant trans-Neptunian object, approximately 255 km in diameter, located in the outermost region of the Solar System. It was discovered by Slovak astronomer TomΓ‘Ε‘ Vorobjov from images taken on the night of 19 April 2012, at the Astronomical Research Institute in Illinois, United States. | [
"(432949) 2012 HH2 β Orbit and classification\n\nis a resonant trans-Neptunian object in an uncommon 4:5 resonance with Neptune (DES: 5:4E). It orbits the Sun at a distance of 29.2β40.4 AU once every 205 years and 4 months (75,008 days; semi-major axis of 34.81 AU). Its orbit has an eccentricity of 0.16 and an incl... |
(432949)_2012_HH2_25132256 | What does the article about '(432949) 2012 HH2' say regarding 'Diameter and albedo'? | Johnstons Archive estimates a mean-diameter of 255 km, using a standard magnitude-to-diameter conversion with an assumed albedo of 0.09. Astronomer Mike Brown gives a nearly identical estimates of 253 km for the object's diameter with an albedo of 0.08 and an absolute magnitude of 6.3. | [
"(432949) 2012 HH2 β Orbit and classification\n\nis a resonant trans-Neptunian object in an uncommon 4:5 resonance with Neptune (DES: 5:4E). It orbits the Sun at a distance of 29.2β40.4 AU once every 205 years and 4 months (75,008 days; semi-major axis of 34.81 AU). Its orbit has an eccentricity of 0.16 and an incl... |
(432949)_2012_HH2_25132254 | What does the article about '(432949) 2012 HH2' say regarding 'Numbering and naming'? | This minor planet was numbered (432949) by the Minor Planet Center on 4 April 2015 (M.P.C. 93615). , it has not been named. | [
"(432949) 2012 HH2 β Orbit and classification\n\nis a resonant trans-Neptunian object in an uncommon 4:5 resonance with Neptune (DES: 5:4E). It orbits the Sun at a distance of 29.2β40.4 AU once every 205 years and 4 months (75,008 days; semi-major axis of 34.81 AU). Its orbit has an eccentricity of 0.16 and an incl... |
(433953)_1997_XR2_1066929 | Describe the 'Recovery' section of the article about '(433953) 1997 XR2'. | On 24 February 2006, was observed by the Mount Lemmon Survey after being lost for more than 8 years. The refinement of its orbit eliminated the possibility of impact in 2101. It is now known that on 20 November 2101, the asteroid will be 0.0392 AU from Earth. | [
"(433953) 1997 XR2 β Recovery\n\nOn 24 February 2006, was observed by the Mount Lemmon Survey after being lost for more than 8 years. The refinement of its orbit eliminated the possibility of impact in 2101. It is now known that on 20 November 2101, the asteroid will be 0.0392 AU from Earth.",
"(433953) 1997 XR2 ... |
(433953)_1997_XR2_1066927 | What does the article about '(433953) 1997 XR2' say regarding 'Orbit and classification'? | The asteroid orbits the Sun at a distance of 0.9β1.3 AU once every 13 months (408 days). Its orbit has an eccentricity of 0.20 and an inclination of 7Β° with respect to the ecliptic. It has an Earth minimum orbital intersection distance of 0.000135 AU, which corresponds to 0.05 lunar distances. The body's observation ar... | [
"(433953) 1997 XR2 β Recovery\n\nOn 24 February 2006, was observed by the Mount Lemmon Survey after being lost for more than 8 years. The refinement of its orbit eliminated the possibility of impact in 2101. It is now known that on 20 November 2101, the asteroid will be 0.0392 AU from Earth.",
"(433953) 1997 XR2 ... |
(433953)_1997_XR2_1066926 | What information does the article about '(433953) 1997 XR2' provide? | is a sub-kilometer sized asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered on 4 December 1997, by the Lincoln Near-Earth Asteroid Research (LINEAR) program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. | [
"(433953) 1997 XR2 β Recovery\n\nOn 24 February 2006, was observed by the Mount Lemmon Survey after being lost for more than 8 years. The refinement of its orbit eliminated the possibility of impact in 2101. It is now known that on 20 November 2101, the asteroid will be 0.0392 AU from Earth.",
"(433953) 1997 XR2 ... |
(433953)_1997_XR2_1066928 | What information does the article about '(433953) 1997 XR2' provide on 'Impact risk'? | Between 2002 and 2006, was considered to have about a 1 in 10,000 chance of colliding with Earth on 1 June 2101, based on a 27-day observation arc following its discovery. With an estimated mass of 17,000,000,000 kilograms, it was ranked at level 1 on the Torino scale (0β10) of impact risk, and was the only near-Earth ... | [
"(433953) 1997 XR2 β Recovery\n\nOn 24 February 2006, was observed by the Mount Lemmon Survey after being lost for more than 8 years. The refinement of its orbit eliminated the possibility of impact in 2101. It is now known that on 20 November 2101, the asteroid will be 0.0392 AU from Earth.",
"(433953) 1997 XR2 ... |
(434326)_2004_JG6_19864018 | Based on the article about '(434326) 2004 JG6', describe the 'Discovery' section. | was discovered on 11 May 2004, by leading astronomer Brian Skiff of the Lowell Observatory Near-Earth Object Search (LONEOS) at Anderson Mesa Station near Flagstaff, Arizona, United States. The body's observation arc begins with its official discovery observation at Anderson Mesa, as no precoveries were taken and no pr... | [
"(434326) 2004 JG6 β Physical characteristics\n\nBased on a generic conversion from absolute magnitude, the asteroid measures between 0.6 and 1.4 kilometers in diameter.",
"(434326) 2004 JG6 β Discovery\n\nwas discovered on 11 May 2004, by leading astronomer Brian Skiff of the Lowell Observatory Near-Earth Object... |
(434326)_2004_JG6_19864017 | Describe the content of the article about '(434326) 2004 JG6'. | , provisional designation is an eccentric, sub-kilometer sized asteroid, classified as near-Earth object and potentially hazardous asteroid of the Atira group, which is also known as "Apohele" and "interior-Earth objects". It is one of the closest orbiting objects to the Sun. | [
"(434326) 2004 JG6 β Physical characteristics\n\nBased on a generic conversion from absolute magnitude, the asteroid measures between 0.6 and 1.4 kilometers in diameter.",
"(434326) 2004 JG6 β Discovery\n\nwas discovered on 11 May 2004, by leading astronomer Brian Skiff of the Lowell Observatory Near-Earth Object... |
(434326)_2004_JG6_19864019 | What information does the article about '(434326) 2004 JG6' provide on 'Orbit and classification'? | It orbits the Sun at a distance of 0.3β1.0 AU once every 6 months (185 days). Its orbit has an eccentricity of 0.53 and an inclination of 19Β° with respect to the ecliptic. is the second known Atira asteroid β the first being the group's namesake 163693 Atira β which means its entire orbit lies within that of the Earth... | [
"(434326) 2004 JG6 β Physical characteristics\n\nBased on a generic conversion from absolute magnitude, the asteroid measures between 0.6 and 1.4 kilometers in diameter.",
"(434326) 2004 JG6 β Discovery\n\nwas discovered on 11 May 2004, by leading astronomer Brian Skiff of the Lowell Observatory Near-Earth Object... |
(434620)_2005_VD_31578914 | Based on the article about '(434620) 2005 VD', describe the 'Description' section. | This minor planet was discovered on 1 November 2005, by astronomers of the Mount Lemmon Survey at Mount Lemmon Observatory near Tucson, Arizona. Precovery images have been found by the Sloan Digital Sky Survey (SDSS) from September 2005 and December 2001. | [
"(434620) 2005 VD β Description\n\nThis minor planet was discovered on 1 November 2005, by astronomers of the Mount Lemmon Survey at Mount Lemmon Observatory near Tucson, Arizona. Precovery images have been found by the Sloan Digital Sky Survey (SDSS) from September 2005 and December 2001.",
"(434620) 2005 VD β D... |
(434620)_2005_VD_31578916 | What does the article about '(434620) 2005 VD' say regarding 'Dynamics'? | Being a highly dynamic object, even among centaurs, 's orbit has visibly changed even since its discovery. Between 1600 and 2400, its semimajor axis will slowly increase from 6.64 to 6.96 AU, its eccentricity slowly increasing from 0.27 to 0.34, and a decreasing inclination from 176.7Β° to 169.9Β°. As such, until about 1... | [
"(434620) 2005 VD β Description\n\nThis minor planet was discovered on 1 November 2005, by astronomers of the Mount Lemmon Survey at Mount Lemmon Observatory near Tucson, Arizona. Precovery images have been found by the Sloan Digital Sky Survey (SDSS) from September 2005 and December 2001.",
"(434620) 2005 VD β D... |
(434620)_2005_VD_31578913 | What information does the article about '(434620) 2005 VD' provide? | (434620) 2005 VD, provisional designation, is a centaur and damocloid on a retrograde orbit from the outer Solar System, known for having the second most highly inclined orbit of any small Solar System body, second to. It was the most highly inclined known object between 2005 and 2013. The unusual object measures appro... | [
"(434620) 2005 VD β Description\n\nThis minor planet was discovered on 1 November 2005, by astronomers of the Mount Lemmon Survey at Mount Lemmon Observatory near Tucson, Arizona. Precovery images have been found by the Sloan Digital Sky Survey (SDSS) from September 2005 and December 2001.",
"(434620) 2005 VD β D... |
(436724)_2011_UW158_16921138 | Explain what '(436724) 2011 UW158' covers in the 'Media attention' section. | It also attracted the media and even firms such as Planetary Resources for its alleged content of platinum worth as high as 5 trillion U.S. dollars. Commenters at StackExchange have denied these estimations as being "orders of magnitude too high", and radar observations have shown that the object contains no more metal... | [
"(436724) 2011 UW158 β Media attention\n\nIt also attracted the media and even firms such as Planetary Resources for its alleged content of platinum worth as high as 5 trillion U.S. dollars. Commenters at StackExchange have denied these estimations as being \"orders of magnitude too high\", and radar observations h... |
(436724)_2011_UW158_16921137 | Describe the 'Shape' section of the article about '(436724) 2011 UW158'. | Radar observations by the Arecibo Observatory on 14 July 2015, revealed that the asteroid's shape looks like an unshelled walnut with a diameter of 300 by 600 metres. The radiometric observations also agreed with the previously obtained photometric ones and gave a period of 37 minutes. | [
"(436724) 2011 UW158 β Media attention\n\nIt also attracted the media and even firms such as Planetary Resources for its alleged content of platinum worth as high as 5 trillion U.S. dollars. Commenters at StackExchange have denied these estimations as being \"orders of magnitude too high\", and radar observations h... |
(436724)_2011_UW158_16921132 | What does the article about '(436724) 2011 UW158' say regarding 'Orbital description'? | orbits the Sun at a distance of 1.0β2.2 AU once every 2 years and 1 month (753 days). Its orbit has an eccentricity of 0.38 and an inclination of 5Β° with respect to the ecliptic. Its observation arc begins with its official discovery observation by Pan-STARRS, as no precoveries were taken, and no prior identifications ... | [
"(436724) 2011 UW158 β Media attention\n\nIt also attracted the media and even firms such as Planetary Resources for its alleged content of platinum worth as high as 5 trillion U.S. dollars. Commenters at StackExchange have denied these estimations as being \"orders of magnitude too high\", and radar observations h... |
(436724)_2011_UW158_16921135 | What does the article about '(436724) 2011 UW158' say regarding 'Diameter and albedo'? | Bruce Gary at Hereford Arizona Observatory (G95) estimated a mean-diameter of 220 meters with a high albedo of 0.39, while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroid of 0.20 and calculates a mean-diameter of 311 meters based on an absolute magnitude of 19.9. | [
"(436724) 2011 UW158 β Media attention\n\nIt also attracted the media and even firms such as Planetary Resources for its alleged content of platinum worth as high as 5 trillion U.S. dollars. Commenters at StackExchange have denied these estimations as being \"orders of magnitude too high\", and radar observations h... |
(436724)_2011_UW158_16921131 | Describe the content of the article about '(436724) 2011 UW158'. | , provisionally known as, is a stony, walnut-shaped asteroid and fast rotator, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 300 meters in diameter. It was discovered on 25 October 2011, by Pan-STARRS at Haleakala Observatory on the island of Maui, Hawaii, in the ... | [
"(436724) 2011 UW158 β Media attention\n\nIt also attracted the media and even firms such as Planetary Resources for its alleged content of platinum worth as high as 5 trillion U.S. dollars. Commenters at StackExchange have denied these estimations as being \"orders of magnitude too high\", and radar observations h... |
(436724)_2011_UW158_16921136 | Summarize the 'Fast rotator' part of '(436724) 2011 UW158'. | In July and August 2015, rotational lightcurves of this asteroid were obtained from photometric observations by Bruce Gary at Hereford Arizona Observatory and by Brian Warner at the CS3βPalmer Divide Station in California (U82). Lightcurve analysis gave a rotation period of 0.6107 hours (36.6 minutes) with a brightness... | [
"(436724) 2011 UW158 β Media attention\n\nIt also attracted the media and even firms such as Planetary Resources for its alleged content of platinum worth as high as 5 trillion U.S. dollars. Commenters at StackExchange have denied these estimations as being \"orders of magnitude too high\", and radar observations h... |
(444004)_2004_AS1_22221683 | Describe the content of the article about '(444004) 2004 AS1'. | , provisional designation, and also known by the temporary name AL00667, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 300 meters in diameter. It was discovered on 13 January 2004, by astronomers of the LINEAR program at the Lincoln La... | [
"(444004) 2004 AS1\n\n, provisional designation, and also known by the temporary name AL00667, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 300 meters in diameter. It was discovered on 13 January 2004, by astronomers of the LINEAR... |
(444004)_2004_AS1_22221686 | What information does the article about '(444004) 2004 AS1' provide on 'Close approaches'? | Although rather ordinary, it caused some controversy in astronomical circles due to initial projections posted on the web by the Minor Planet Center (MPC) suggesting an imminent collision with Earth on or about January 15 with a likelihood of 1:4. These projections came from very early observations, and turned out to b... | [
"(444004) 2004 AS1\n\n, provisional designation, and also known by the temporary name AL00667, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 300 meters in diameter. It was discovered on 13 January 2004, by astronomers of the LINEAR... |
(444004)_2004_AS1_22221684 | Reconstruct the content about 'Description' from the article on '(444004) 2004 AS1'. | Based on the asteroids brightness and assumed proximity to Earth, the asteroid was originally estimated to be only 30 meters in diameter. | [
"(444004) 2004 AS1\n\n, provisional designation, and also known by the temporary name AL00667, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 300 meters in diameter. It was discovered on 13 January 2004, by astronomers of the LINEAR... |
(444004)_2004_AS1_22221685 | Based on the article about '(444004) 2004 AS1', describe the 'Orbit and classification' section. | orbits the Sun at a distance of 0.88β1.26 AU once every 13 months (405 days; semi-major axis of 1.07 AU). Its orbit has an eccentricity of 0.17 and an inclination of 17Β° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Socorro in January 2004. | [
"(444004) 2004 AS1\n\n, provisional designation, and also known by the temporary name AL00667, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 300 meters in diameter. It was discovered on 13 January 2004, by astronomers of the LINEAR... |
(444004)_2004_AS1_22221687 | Based on the article about '(444004) 2004 AS1', describe the 'Diameter and albedo' section. | Based on a generic magnitude-to-diameter conversion, measures between 240 and 480 meters in diameter, for a measured absolute magnitude of 20.5, and an assumed albedo of 0.20 and 0.05, which corresponds to a body with a stony and carbonaceous composition, respectively. | [
"(444004) 2004 AS1\n\n, provisional designation, and also known by the temporary name AL00667, is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 300 meters in diameter. It was discovered on 13 January 2004, by astronomers of the LINEAR... |
(445473)_2010_VZ98_17615076 | What does the article about '(445473) 2010 VZ98' say regarding 'Physical characteristics'? | A rotational lightcurve of was obtained from photometric observation by members of the Carnegie Institution for Science at Las Campanas Observatory, Chile. The light-curve gave a rotation period of 9.72 hours with a brightness variation of 0.18 magnitude (U=n.a.). | [
"(445473) 2010 VZ98 β Naming\n\nAs of 2018, this minor planet remains unnamed.",
"(445473) 2010 VZ98 β Physical characteristics\n\nA rotational lightcurve of was obtained from photometric observation by members of the Carnegie Institution for Science at Las Campanas Observatory, Chile. The light-curve gave a rota... |
(445473)_2010_VZ98_17615075 | Describe the 'Orbit and classification' section of the article about '(445473) 2010 VZ98'. | orbits the Sun at a distance of 34.3β266.6 AU once every 1846 years (674,262 days; semi-major axis of 150.5 AU). Its orbit has a high eccentricity of 0.77 and an inclination of 5Β° with respect to the ecliptic. Small number statistics suggest that this body may be trapped in a 3:2 orbital resonance with an unseen planet... | [
"(445473) 2010 VZ98 β Naming\n\nAs of 2018, this minor planet remains unnamed.",
"(445473) 2010 VZ98 β Physical characteristics\n\nA rotational lightcurve of was obtained from photometric observation by members of the Carnegie Institution for Science at Las Campanas Observatory, Chile. The light-curve gave a rota... |
(445473)_2010_VZ98_17615074 | Describe the content of the article about '(445473) 2010 VZ98'. | , provisional designation, is a trans-Neptunian object of the scattered disc, orbiting the Sun in the outermost region of the Solar System. It has a diameter of approximately 400 kilometers. It was discovered on 11 November 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's ... | [
"(445473) 2010 VZ98 β Naming\n\nAs of 2018, this minor planet remains unnamed.",
"(445473) 2010 VZ98 β Physical characteristics\n\nA rotational lightcurve of was obtained from photometric observation by members of the Carnegie Institution for Science at Las Campanas Observatory, Chile. The light-curve gave a rota... |
(445473)_2010_VZ98_17615077 | Describe the 'Diameter and albedo' section of the article about '(445473) 2010 VZ98'. | While American astronomer Michael E. Brown assumes a diameter of 471 kilometers and an albedo of 0.07, the Johnston Archive estimates a diameter of 443 kilometers with generic albedo of 0.09. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.10 and calculates a diameter of 401 kilometers. These estimate... | [
"(445473) 2010 VZ98 β Naming\n\nAs of 2018, this minor planet remains unnamed.",
"(445473) 2010 VZ98 β Physical characteristics\n\nA rotational lightcurve of was obtained from photometric observation by members of the Carnegie Institution for Science at Las Campanas Observatory, Chile. The light-curve gave a rota... |
(44594)_1999_OX3_28647670 | What does the article about '(44594) 1999 OX3' say regarding 'Physical characteristics'? | In July 2009, a rotational lightcurve of was obtained from photometric observations. Lightcurve analysis gave a rotation period of 9.26 hours with a brightness amplitude of 0.11 magnitude (U=2). The period, however, is ambiguous with alternative solutions (13.4 and 15.45 hours). | [
"(44594) 1999 OX3 β Physical characteristics\n\nIn July 2009, a rotational lightcurve of was obtained from photometric observations. Lightcurve analysis gave a rotation period of 9.26 hours with a brightness amplitude of 0.11 magnitude (U=2). The period, however, is ambiguous with alternative solutions (13.4 and 15... |
(44594)_1999_OX3_28647671 | Explain what '(44594) 1999 OX3' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 22 August 2002. As of 2018, it has not been named. | [
"(44594) 1999 OX3 β Physical characteristics\n\nIn July 2009, a rotational lightcurve of was obtained from photometric observations. Lightcurve analysis gave a rotation period of 9.26 hours with a brightness amplitude of 0.11 magnitude (U=2). The period, however, is ambiguous with alternative solutions (13.4 and 15... |
(44594)_1999_OX3_28647669 | What does the article about '(44594) 1999 OX3' say regarding 'Orbit and classification'? | orbits the Sun at a distance of 17.6β46.6 AU once every 181 years and 9 months (66,375 days). Its orbit has an eccentricity of 0.45 and an inclination of 3Β° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Mauna Kea in 1999. Neptune has a semi-major axis of 30 A... | [
"(44594) 1999 OX3 β Physical characteristics\n\nIn July 2009, a rotational lightcurve of was obtained from photometric observations. Lightcurve analysis gave a rotation period of 9.26 hours with a brightness amplitude of 0.11 magnitude (U=2). The period, however, is ambiguous with alternative solutions (13.4 and 15... |
(450894)_2008_BT18_32510003 | Reconstruct the content about 'Rotation period' from the article on '(450894) 2008 BT18'. | A rotational lightcurve for was obtained from photometric observations made by astronomer Alberto Silva Betzler at Salvador, Brazil, in July 2008. The lightcurve gave a rotation period of 2.726 hours with a brightness variation of 0.04 in magnitude (U=1). | [
"(450894) 2008 BT18 β Rotation period\n\nA rotational lightcurve for was obtained from photometric observations made by astronomer Alberto Silva Betzler at Salvador, Brazil, in July 2008. The lightcurve gave a rotation period of 2.726 hours with a brightness variation of 0.04 in magnitude (U=1).",
"(450894) 2008 ... |
(450894)_2008_BT18_32510000 | Describe the content of the article about '(450894) 2008 BT18'. | is a sub-kilometer asteroid and synchronous binary system, classified as near-Earth object and potentially hazardous asteroid of the Apollo group. It was discovered on 31 January 2008, by the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, United States. The eccentric asteroid me... | [
"(450894) 2008 BT18 β Rotation period\n\nA rotational lightcurve for was obtained from photometric observations made by astronomer Alberto Silva Betzler at Salvador, Brazil, in July 2008. The lightcurve gave a rotation period of 2.726 hours with a brightness variation of 0.04 in magnitude (U=1).",
"(450894) 2008 ... |
(450894)_2008_BT18_32510001 | Reconstruct the content about 'Orbit and classification' from the article on '(450894) 2008 BT18'. | orbits the Sun at a distance of 0.9β3.5 AU once every 3 years and 4 months (1,209 days). Its orbit has an eccentricity of 0.59 and an inclination of 8Β° with respect to the ecliptic. Published by the Digitized Sky Survey, a first precovery was taken at Palomar Observatory in 1955, extending the asteroid's observation ar... | [
"(450894) 2008 BT18 β Rotation period\n\nA rotational lightcurve for was obtained from photometric observations made by astronomer Alberto Silva Betzler at Salvador, Brazil, in July 2008. The lightcurve gave a rotation period of 2.726 hours with a brightness variation of 0.04 in magnitude (U=1).",
"(450894) 2008 ... |
(450894)_2008_BT18_32510004 | From the article on '(450894) 2008 BT18', restate the 'Binary system' content. | On 6 and 7 July 2008, research conducted using the Arecibo Observatory produced evidence that is a synchronous binary asteroid with a minor-planet moon in its orbit. The secondary component, provisionally designated, has a diameter of at least 200 meters, about 33% the size of and up to 1.5 kilometers apart from its pr... | [
"(450894) 2008 BT18 β Rotation period\n\nA rotational lightcurve for was obtained from photometric observations made by astronomer Alberto Silva Betzler at Salvador, Brazil, in July 2008. The lightcurve gave a rotation period of 2.726 hours with a brightness variation of 0.04 in magnitude (U=1).",
"(450894) 2008 ... |
(450894)_2008_BT18_32510005 | Based on the article about '(450894) 2008 BT18', describe the 'Mineralogy' section. | On 26 July 2008, observations at the IRTF using the SpeX-spectrograph showed that is a basaltic achondrite, suggesting that its parent body was subjected to sufficiently high temperatures to produce a eutectic melt. The body's surface is thought to be dominated by iron-rich orthopyroxenes with little or no olivine. | [
"(450894) 2008 BT18 β Rotation period\n\nA rotational lightcurve for was obtained from photometric observations made by astronomer Alberto Silva Betzler at Salvador, Brazil, in July 2008. The lightcurve gave a rotation period of 2.726 hours with a brightness variation of 0.04 in magnitude (U=1).",
"(450894) 2008 ... |
(454101)_2013_BP73_26676258 | Describe the 'Description' section of the article about '(454101) 2013 BP73'. | From discovery until August 2013 when Sentry updated to planetary ephemeris (DE431), it had the 4th highest impact threat on the Palermo Technical Impact Hazard Scale. It was discovered on 22 January 2013 by the Mount Lemmon Survey at an apparent magnitude of 21 using a 1.5 m reflecting telescope. It has an estimated d... | [
"(454101) 2013 BP73 β Description\n\nFrom discovery until August 2013 when Sentry updated to planetary ephemeris (DE431), it had the 4th highest impact threat on the Palermo Technical Impact Hazard Scale. It was discovered on 22 January 2013 by the Mount Lemmon Survey at an apparent magnitude of 21 using a 1.5 m re... |
(454101)_2013_BP73_26676260 | From the article on '(454101) 2013 BP73', restate the 'Numbering and naming' content. | This minor planet was numbered by the Minor Planet Center on 25 December 2015 (M.P.C. 97517). As of 2018, it has not been named. | [
"(454101) 2013 BP73 β Description\n\nFrom discovery until August 2013 when Sentry updated to planetary ephemeris (DE431), it had the 4th highest impact threat on the Palermo Technical Impact Hazard Scale. It was discovered on 22 January 2013 by the Mount Lemmon Survey at an apparent magnitude of 21 using a 1.5 m re... |
(454101)_2013_BP73_26676259 | Summarize the 'Description' part of '(454101) 2013 BP73'. | asteroid that fit the uncertainty region in the known trajectory showed a 1 in 588,000 chance that the asteroid could impact Earth on 11 December 2096. With a 2096 Palermo Technical Scale of β3.42, the odds of impact by in 2096 were about 2630 times less than the background hazard level of Earth impacts which is define... | [
"(454101) 2013 BP73 β Description\n\nFrom discovery until August 2013 when Sentry updated to planetary ephemeris (DE431), it had the 4th highest impact threat on the Palermo Technical Impact Hazard Scale. It was discovered on 22 January 2013 by the Mount Lemmon Survey at an apparent magnitude of 21 using a 1.5 m re... |
(454101)_2013_BP73_26676257 | What information does the article about '(454101) 2013 BP73' provide? | , provisional designation, is a sub-kilometer asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 310 m in diameter. | [
"(454101) 2013 BP73 β Description\n\nFrom discovery until August 2013 when Sentry updated to planetary ephemeris (DE431), it had the 4th highest impact threat on the Palermo Technical Impact Hazard Scale. It was discovered on 22 January 2013 by the Mount Lemmon Survey at an apparent magnitude of 21 using a 1.5 m re... |
(456938)_2007_YV56_24450870 | Based on the article about '(456938) 2007 YV56', describe the 'Diameter and albedo' section. | Based on a generic magnitude-to-diameter conversion, measures 190 - 360 m in diameter, for an absolute magnitude of 21.0, and an assumed albedo of 0.20 and 0.057, which represent typical values for stony and carbonaceous asteroids, respectively. | [
"(456938) 2007 YV56 β Diameter and albedo\n\nBased on a generic magnitude-to-diameter conversion, measures 190 - 360 m in diameter, for an absolute magnitude of 21.0, and an assumed albedo of 0.20 and 0.057, which represent typical values for stony and carbonaceous asteroids, respectively.",
"(456938) 2007 YV56 β... |
(456938)_2007_YV56_24450872 | Reconstruct the content about 'Numbering and naming' from the article on '(456938) 2007 YV56'. | This minor planet was numbered by the Minor Planet Center on 22 February 2016 (M.P.C. 98584). As of 2018, it has not been named. | [
"(456938) 2007 YV56 β Diameter and albedo\n\nBased on a generic magnitude-to-diameter conversion, measures 190 - 360 m in diameter, for an absolute magnitude of 21.0, and an assumed albedo of 0.20 and 0.057, which represent typical values for stony and carbonaceous asteroids, respectively.",
"(456938) 2007 YV56 β... |
(456938)_2007_YV56_24450871 | Summarize the 'Rotation period' part of '(456938) 2007 YV56'. | As of 2018, no rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. | [
"(456938) 2007 YV56 β Diameter and albedo\n\nBased on a generic magnitude-to-diameter conversion, measures 190 - 360 m in diameter, for an absolute magnitude of 21.0, and an assumed albedo of 0.20 and 0.057, which represent typical values for stony and carbonaceous asteroids, respectively.",
"(456938) 2007 YV56 β... |
(456938)_2007_YV56_24450867 | Reconstruct the content about 'Orbit and classification' from the article on '(456938) 2007 YV56'. | is an Apollo asteroid that crosses the orbit of Earth. Apollo's are the largest group of near-Earth objects with nearly 10 thousand known members. It orbits the Sun at a distance of 0.60β2.55 AU once every 2 years (722 days; semi-major axis of 1.58 AU). Its orbit has a high eccentricity of 0.62 and an inclination of 6Β°... | [
"(456938) 2007 YV56 β Diameter and albedo\n\nBased on a generic magnitude-to-diameter conversion, measures 190 - 360 m in diameter, for an absolute magnitude of 21.0, and an assumed albedo of 0.20 and 0.057, which represent typical values for stony and carbonaceous asteroids, respectively.",
"(456938) 2007 YV56 β... |
(456938)_2007_YV56_24450868 | Explain what '(456938) 2007 YV56' covers in the 'Close approaches' section. | has a minimum orbital intersection distance (MOID) with Earth of 0.0047 AU, which corresponds to 1.83 lunar distances (LD). It has an absolute magnitude of 21.0. This makes it a potentially hazardous asteroid, which are defined as having a MOID of less than 0.05 AU and an absolute magnitude brighter than 22. Besides Ea... | [
"(456938) 2007 YV56 β Diameter and albedo\n\nBased on a generic magnitude-to-diameter conversion, measures 190 - 360 m in diameter, for an absolute magnitude of 21.0, and an assumed albedo of 0.20 and 0.057, which represent typical values for stony and carbonaceous asteroids, respectively.",
"(456938) 2007 YV56 β... |
(457175)_2008_GO98_8680165 | Describe the 'Orbit and classification' section of the article about '(457175) 2008 GO98'. | is classified as a member of the dynamical Hilda group, as well as a main-belt comet that shows clear cometary activity, which has also been described as a "quasi Hilda comet". Orbital backward integration suggests that it might have been a centaur or trans-Neptunian object that ended its dynamical evolution as a quasi... | [
"(457175) 2008 GO98 β Orbit and classification\n\nis classified as a member of the dynamical Hilda group, as well as a main-belt comet that shows clear cometary activity, which has also been described as a \"quasi Hilda comet\". Orbital backward integration suggests that it might have been a centaur or trans-Neptun... |
(457175)_2008_GO98_8680169 | Summarize the 'Diameter and albedo' part of '(457175) 2008 GO98'. | The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous body of 0.057 and calculates a diameter of 14.64 kilometers based on an absolute magnitude of 12.9. Other estimates, taking into account several published magnitude measurements and a large range of albedo assumptions, estimate a di... | [
"(457175) 2008 GO98 β Orbit and classification\n\nis classified as a member of the dynamical Hilda group, as well as a main-belt comet that shows clear cometary activity, which has also been described as a \"quasi Hilda comet\". Orbital backward integration suggests that it might have been a centaur or trans-Neptun... |
(457175)_2008_GO98_8680166 | What does the article about '(457175) 2008 GO98' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 16 February 2016 (M.P.C. 98587). As of 2020, it has not been named. | [
"(457175) 2008 GO98 β Orbit and classification\n\nis classified as a member of the dynamical Hilda group, as well as a main-belt comet that shows clear cometary activity, which has also been described as a \"quasi Hilda comet\". Orbital backward integration suggests that it might have been a centaur or trans-Neptun... |
(457175)_2008_GO98_8680168 | Describe the 'Rotation period' section of the article about '(457175) 2008 GO98'. | In August 2017, a rotational lightcurve of was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station in California. Lightcurve analysis gave a rotation period of 10.74 hours with a small brightness amplitude of 0.12 magnitude (U=2). | [
"(457175) 2008 GO98 β Orbit and classification\n\nis classified as a member of the dynamical Hilda group, as well as a main-belt comet that shows clear cometary activity, which has also been described as a \"quasi Hilda comet\". Orbital backward integration suggests that it might have been a centaur or trans-Neptun... |
(457175)_2008_GO98_8680164 | Describe the content of the article about '(457175) 2008 GO98'. | ''', provisional designation ' with cometary number 362P, is a Hildian asteroid and rare main-belt comet from the outermost regions of the asteroid belt, approximately 15 km in diameter. It was discovered on 8 April 2008, by astronomers of the Spacewatch program at Kitt Peak National Observatory near Tucson, Arizona, i... | [
"(457175) 2008 GO98 β Orbit and classification\n\nis classified as a member of the dynamical Hilda group, as well as a main-belt comet that shows clear cometary activity, which has also been described as a \"quasi Hilda comet\". Orbital backward integration suggests that it might have been a centaur or trans-Neptun... |
(459883)_2014_JX55_26678340 | Reconstruct the content from the article about '(459883) 2014 JX55'. | is an asteroid from the central regions of the asteroid belt. After its first observations as in 2007, it was considered an inner heliospheric asteroid and near-Earth object with one of the closest perihelion ever observed of any body orbiting the Sun, until further observations invalidated the conclusions from early o... | [
"(459883) 2014 JX55\n\nis an asteroid from the central regions of the asteroid belt. After its first observations as in 2007, it was considered an inner heliospheric asteroid and near-Earth object with one of the closest perihelion ever observed of any body orbiting the Sun, until further observations invalidated t... |
(459883)_2014_JX55_26678342 | What does the article about '(459883) 2014 JX55' say regarding 'Orbital determination as main-belt asteroid'? | The object remained listed as an inner heliospheric asteroid for several years, until identifications with and and a subsequent improvement of the orbital uncertainty completely overturned previous calculations. is now a secured central main-belt asteroid orbiting the Sun at a distance of 2.2β3.1 AU once every 4 years... | [
"(459883) 2014 JX55\n\nis an asteroid from the central regions of the asteroid belt. After its first observations as in 2007, it was considered an inner heliospheric asteroid and near-Earth object with one of the closest perihelion ever observed of any body orbiting the Sun, until further observations invalidated t... |
(459883)_2014_JX55_26678341 | Reconstruct the content about 'Inner heliospheric asteroid' from the article on '(459883) 2014 JX55'. | When the object was first observed as by the Mount Lemmon Survey in March 2007, it was considered to have the second-smallest positive semi-major axis (0.55 AU) of any known object orbiting the Sun, after Mercury. It was classified as an Apohele asteroid, which always stay inside of Earth's orbit, approaching within 0.... | [
"(459883) 2014 JX55\n\nis an asteroid from the central regions of the asteroid belt. After its first observations as in 2007, it was considered an inner heliospheric asteroid and near-Earth object with one of the closest perihelion ever observed of any body orbiting the Sun, until further observations invalidated t... |
(467336)_2002_LT38_18591434 | Explain what '(467336) 2002 LT38' covers in the 'Rotation period' section. | In July 2016, a first rotational lightcurve of was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Station in California (U82). Lightcurve analysis gave a longer-than average rotation period of 21.80 hours with a brightness variation of 1.16 magnitude (U=2+). A high brigh... | [
"(467336) 2002 LT38 β Rotation period\n\nIn July 2016, a first rotational lightcurve of was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Station in California (U82). Lightcurve analysis gave a longer-than average rotation period of 21.80 hours with a brightness var... |
(467336)_2002_LT38_18591431 | What information does the article about '(467336) 2002 LT38' provide on 'Orbit and classification'? | orbits the Sun at a distance of 0.6β1.1 AU once every 9 months (284 days; semi-major axis of 0.85 AU). Its orbit has an eccentricity of 0.31 and an inclination of 6Β° with respect to the ecliptic. The body's observation arc begins with a precovery taken at AMOS on 10 June 2002, two nights prior to its official discovery... | [
"(467336) 2002 LT38 β Rotation period\n\nIn July 2016, a first rotational lightcurve of was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Station in California (U82). Lightcurve analysis gave a longer-than average rotation period of 21.80 hours with a brightness var... |
(467336)_2002_LT38_18591435 | Based on the article about '(467336) 2002 LT38', 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 0.236 kilometers based on an absolute magnitude of 20.5. | [
"(467336) 2002 LT38 β Rotation period\n\nIn July 2016, a first rotational lightcurve of was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Station in California (U82). Lightcurve analysis gave a longer-than average rotation period of 21.80 hours with a brightness var... |
(467336)_2002_LT38_18591436 | Summarize the 'Numbering and naming' part of '(467336) 2002 LT38'. | This minor planet was numbered by the Minor Planet Center on 21 May 2016, after its orbit determination became sufficiently secure (M.P.C. 100286). As of 2018, it has not been named. | [
"(467336) 2002 LT38 β Rotation period\n\nIn July 2016, a first rotational lightcurve of was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Station in California (U82). Lightcurve analysis gave a longer-than average rotation period of 21.80 hours with a brightness var... |
(467336)_2002_LT38_18591432 | Summarize the 'Close approaches' part of '(467336) 2002 LT38'. | has an Earth minimum orbital intersection distance of 0.0344 AU which corresponds to 13.4 lunar distances. It will pass at that distance during its close encounter with Earth on 27 June 2030. | [
"(467336) 2002 LT38 β Rotation period\n\nIn July 2016, a first rotational lightcurve of was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Station in California (U82). Lightcurve analysis gave a longer-than average rotation period of 21.80 hours with a brightness var... |
(468861)_2013_LU28_17602615 | Reconstruct the content about 'Orbit and classification' from the article on '(468861) 2013 LU28'. | orbits the Sun at a distance of 8.7β353.1 AU once every 2434 years (888,879 days; semi-major axis of 180.92 AU). Its orbit has an exceptionally high eccentricity of 0.95 and an inclination of 125Β° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Mount Lemmon in ... | [
"(468861) 2013 LU28 β Orbit and classification\n\norbits the Sun at a distance of 8.7β353.1 AU once every 2434 years (888,879 days; semi-major axis of 180.92 AU). Its orbit has an exceptionally high eccentricity of 0.95 and an inclination of 125Β° with respect to the ecliptic. The body's observation arc begins with ... |
(468861)_2013_LU28_17602614 | What information does the article about '(468861) 2013 LU28' provide? | , provisional designation is a highly eccentric trans-Neptunian object, retrograde centaur and damocloid from the outer regions of the Solar System. It was discovered on 8 June 2013 by astronomers with the Mount Lemmon Survey at the Mount Lemmon Observatory in Arizona, United States. The object is unlikely a dwarf plan... | [
"(468861) 2013 LU28 β Orbit and classification\n\norbits the Sun at a distance of 8.7β353.1 AU once every 2434 years (888,879 days; semi-major axis of 180.92 AU). Its orbit has an exceptionally high eccentricity of 0.95 and an inclination of 125Β° with respect to the ecliptic. The body's observation arc begins with ... |
(468861)_2013_LU28_17602618 | What does the article about '(468861) 2013 LU28' say regarding 'Diameter and albedo'? | According to the Johnston's archive and astronomer Michael Brown, measures 106 and 114 kilometers in diameter, based on an absolute magnitude of 8.1 and an assumed albedo for the body's surface of 0.08 and 0.09, respectively. According to Brown, is "probably not" a dwarf planet. As of 2018, no physical characteristics ... | [
"(468861) 2013 LU28 β Orbit and classification\n\norbits the Sun at a distance of 8.7β353.1 AU once every 2434 years (888,879 days; semi-major axis of 180.92 AU). Its orbit has an exceptionally high eccentricity of 0.95 and an inclination of 125Β° with respect to the ecliptic. The body's observation arc begins with ... |
(468861)_2013_LU28_17602616 | Summarize the 'TNO, centaur and damocloid' part of '(468861) 2013 LU28'. | With a semi-major axis larger than that of Neptune, is generically classified as a trans-Neptunian object. It is also considered an (extended) centaur, due to its eccentric orbit with a low perihelion of 8.7 AU and a higher-than-90Β°-inclination, which gives it a retrograde orbit. There are only about a hundred known re... | [
"(468861) 2013 LU28 β Orbit and classification\n\norbits the Sun at a distance of 8.7β353.1 AU once every 2434 years (888,879 days; semi-major axis of 180.92 AU). Its orbit has an exceptionally high eccentricity of 0.95 and an inclination of 125Β° with respect to the ecliptic. The body's observation arc begins with ... |
(469306)_1999_CD158_13678963 | Describe the 'Orbit and classification' section of the article about '(469306) 1999 CD158'. | is candidate to the Haumea family, the only collisional group of trans-Neptunian objects currently determined. It is also sub-classified as a resonant trans-Neptunian object, as it stays in a 4:7 orbital resonance with the ice giant Neptune, which means, that for every seven orbits of Neptune around the Sun, it makes f... | [
"(469306) 1999 CD158 β Orbit and classification\n\nis candidate to the Haumea family, the only collisional group of trans-Neptunian objects currently determined. It is also sub-classified as a resonant trans-Neptunian object, as it stays in a 4:7 orbital resonance with the ice giant Neptune, which means, that for e... |
(469306)_1999_CD158_13678962 | Reconstruct the content from the article about '(469306) 1999 CD158'. | , provisional designation:, is a trans-Neptunian object from the circumstellar disc of the Kuiper belt, located in the outermost region of the Solar System. The relatively bright hot classical Kuiper belt object measures approximately 310 km in diameter. It was discovered on 10 February 1999, by American astronomers Ja... | [
"(469306) 1999 CD158 β Orbit and classification\n\nis candidate to the Haumea family, the only collisional group of trans-Neptunian objects currently determined. It is also sub-classified as a resonant trans-Neptunian object, as it stays in a 4:7 orbital resonance with the ice giant Neptune, which means, that for e... |
(469306)_1999_CD158_13678965 | What does the article about '(469306) 1999 CD158' say regarding 'Diameter and albedo'? | According to estimates by the Johnston's archive, the Collaborative Asteroid Lightcurve Link and American astronomer Michael Brown, measures between 420 and 477 kilometers in diameter. It is "probably" a dwarf planet" according to Brown's assessment (see ). | [
"(469306) 1999 CD158 β Orbit and classification\n\nis candidate to the Haumea family, the only collisional group of trans-Neptunian objects currently determined. It is also sub-classified as a resonant trans-Neptunian object, as it stays in a 4:7 orbital resonance with the ice giant Neptune, which means, that for e... |
(469306)_1999_CD158_13678964 | Reconstruct the content about 'Photometry' from the article on '(469306) 1999 CD158'. | Photometric observation of in March 2015, gave a classically shaped bimodal lightcurve with a rotation period of 6.88 hours and a large brightness variation of 0.49 magnitude (U=3-). Observations with the New Technology Telescope at ESO's La Silla Observatory in Chile in 2008, determined the body's BVRI colors to be 0.... | [
"(469306) 1999 CD158 β Orbit and classification\n\nis candidate to the Haumea family, the only collisional group of trans-Neptunian objects currently determined. It is also sub-classified as a resonant trans-Neptunian object, as it stays in a 4:7 orbital resonance with the ice giant Neptune, which means, that for e... |
(471240)_2011_BT15_26348964 | Reconstruct the content about 'Orbit' from the article on '(471240) 2011 BT15'. | Before the 2013 recovery it had an observation arc of 41 days with an uncertainty parameter of 7. Due to precovery images from 2007 it now has an observation arc of more than 5 years. It makes close approaches to Earth and Mars. On 28 December 2013, it passed 0.03222 AU from Earth. The December 2013 passage was studied... | [
"(471240) 2011 BT15 β Orbit\n\nBefore the 2013 recovery it had an observation arc of 41 days with an uncertainty parameter of 7. Due to precovery images from 2007 it now has an observation arc of more than 5 years. It makes close approaches to Earth and Mars. On 28 December 2013, it passed 0.03222 AU from Earth. Th... |
(471240)_2011_BT15_26348963 | What does the article about '(471240) 2011 BT15' say regarding 'Discovery'? | It was discovered on 24 January 2011, by a team of astronomers at Pan-STARRS, the Panoramic Survey Telescope and Rapid Response System at Haleakala Observatory on Hawaii, United States. The discovery was made using a 1.8-meter RitcheyβChrΓ©tien telescope. At the time of discovery, the object had an apparent magnitude of... | [
"(471240) 2011 BT15 β Orbit\n\nBefore the 2013 recovery it had an observation arc of 41 days with an uncertainty parameter of 7. Due to precovery images from 2007 it now has an observation arc of more than 5 years. It makes close approaches to Earth and Mars. On 28 December 2013, it passed 0.03222 AU from Earth. Th... |
(471240)_2011_BT15_26348965 | What information does the article about '(471240) 2011 BT15' provide on 'Impact risk'? | While listed on the Sentry Risk Table, virtual clones of the asteroid that fit the uncertainty region in the known trajectory showed a 1 in 71,000 chance that the asteroid could impact Earth on 5 January 2080. In 2013 it had the 5th highest impact threat on the Palermo Technical Impact Hazard Scale. It was removed from... | [
"(471240) 2011 BT15 β Orbit\n\nBefore the 2013 recovery it had an observation arc of 41 days with an uncertainty parameter of 7. Due to precovery images from 2007 it now has an observation arc of more than 5 years. It makes close approaches to Earth and Mars. On 28 December 2013, it passed 0.03222 AU from Earth. Th... |
(471240)_2011_BT15_26348968 | From the article on '(471240) 2011 BT15', restate the 'Diameter and albedo' content. | According to the CALL and JPL's impact-risk table, this near-Earth object measures 136 and 150 meters, respectively. For its size estimate, CALL uses a standard for stony asteroids of 0.20 with an absolute magnitude of 21.7. | [
"(471240) 2011 BT15 β Orbit\n\nBefore the 2013 recovery it had an observation arc of 41 days with an uncertainty parameter of 7. Due to precovery images from 2007 it now has an observation arc of more than 5 years. It makes close approaches to Earth and Mars. On 28 December 2013, it passed 0.03222 AU from Earth. Th... |
(471240)_2011_BT15_26348962 | Summarize the following section from the article on '(471240) 2011 BT15'. | , provisional designation, is a stony, sub-kilometer sized asteroid and fast rotator, classified as a near-Earth object and potentially hazardous asteroid of the Apollo group. It had been one of the objects with the highest impact threat on the Palermo Technical Impact Hazard Scale. | [
"(471240) 2011 BT15 β Orbit\n\nBefore the 2013 recovery it had an observation arc of 41 days with an uncertainty parameter of 7. Due to precovery images from 2007 it now has an observation arc of more than 5 years. It makes close approaches to Earth and Mars. On 28 December 2013, it passed 0.03222 AU from Earth. Th... |
(471240)_2011_BT15_26348967 | Explain what '(471240) 2011 BT15' covers in the 'Fast rotator' section. | In January 2014, a rotational lightcurve of was obtained from photometric observations by American astronomer Brian Warner at the CS3-Palmer Divide Station (U82) in California. Lightcurve analysis gave a well-defined rotation period of 0.109138 hours (393 seconds) with a brightness amplitude of 0.61 magnitude (U=3). | [
"(471240) 2011 BT15 β Orbit\n\nBefore the 2013 recovery it had an observation arc of 41 days with an uncertainty parameter of 7. Due to precovery images from 2007 it now has an observation arc of more than 5 years. It makes close approaches to Earth and Mars. On 28 December 2013, it passed 0.03222 AU from Earth. Th... |
(471325)_2011_KT19_4916948 | What information does the article about '(471325) 2011 KT19' provide on 'Details'? | was discovered by the Mount Lemmon Survey on 31 May 2011. Its rediscovery was announced in August 2016 by a team of astronomers using the Pan-STARRS telescope. It was soon linked with a supposed prograde centaur (inclination = 38Β° and semi-major axis = 28 AU) that had been lost due to a short observation arc. is in a 7... | [
"(471325) 2011 KT19 β Details\n\nwas discovered by the Mount Lemmon Survey on 31 May 2011. Its rediscovery was announced in August 2016 by a team of astronomers using the Pan-STARRS telescope. It was soon linked with a supposed prograde centaur (inclination = 38Β° and semi-major axis = 28 AU) that had been lost due ... |
(471325)_2011_KT19_4916947 | Describe the content of the article about '(471325) 2011 KT19'. | (nicknamed Niku; ) is a trans-Neptunian object that has an unusual 110Β° tilted solar orbital plane and retrograde orbit around the Sun. | [
"(471325) 2011 KT19 β Details\n\nwas discovered by the Mount Lemmon Survey on 31 May 2011. Its rediscovery was announced in August 2016 by a team of astronomers using the Pan-STARRS telescope. It was soon linked with a supposed prograde centaur (inclination = 38Β° and semi-major axis = 28 AU) that had been lost due ... |
(471325)_2011_KT19_4916949 | Reconstruct the content about 'Details' from the article on '(471325) 2011 KT19'. | been compared to those of (Drac). The orbits of, , , , , , appear to occupy a common plane, with three in prograde and three in retrograde orbits. The probability of this alignment occurring by chance is 0.016%. These orbits should leave a common plane in a few million years because the precession of prograde and retr... | [
"(471325) 2011 KT19 β Details\n\nwas discovered by the Mount Lemmon Survey on 31 May 2011. Its rediscovery was announced in August 2016 by a team of astronomers using the Pan-STARRS telescope. It was soon linked with a supposed prograde centaur (inclination = 38Β° and semi-major axis = 28 AU) that had been lost due ... |
(472651)_2015_DB216_8209410 | What information does the article about '(472651) 2015 DB216' provide on 'Notes'? | 1) Assuming an albedo from 0.05 (160 km) to 1 (40 km); is definitely somewhere within this range, and cannot be any smaller than 40 kilometers, assuming the absolute magnitude is correct. | [
"(472651) 2015 DB216 β Notes\n\n1) Assuming an albedo from 0.05 (160 km) to 1 (40 km); is definitely somewhere within this range, and cannot be any smaller than 40 kilometers, assuming the absolute magnitude is correct.",
"(472651) 2015 DB216\n\nis a centaur and Uranus co-orbital discovered on February 27, 2015... |
(472651)_2015_DB216_8209408 | Summarize the following section from the article on '(472651) 2015 DB216'. | is a centaur and Uranus co-orbital discovered on February 27, 2015, by the Mount Lemmon Survey. It is the second known centaur on a horseshoe orbit with Uranus, and the third Uranus co-orbital discovered after (a Trojan) and 83982 Crantor (a horseshoe librator). A second Uranian Trojan,, was announced in 2017. | [
"(472651) 2015 DB216 β Notes\n\n1) Assuming an albedo from 0.05 (160 km) to 1 (40 km); is definitely somewhere within this range, and cannot be any smaller than 40 kilometers, assuming the absolute magnitude is correct.",
"(472651) 2015 DB216\n\nis a centaur and Uranus co-orbital discovered on February 27, 2015... |
(472651)_2015_DB216_8209409 | From the article on '(472651) 2015 DB216', restate the 'Description' content. | An early orbital calculation of the asteroid with an observation arc of 10 days suggested an extremely close MOID to Neptune, but further observations on March 27 refined the orbit to show that the asteroid passes no less than several astronomical units away from Neptune, and show the orbit instead being that of a typi... | [
"(472651) 2015 DB216 β Notes\n\n1) Assuming an albedo from 0.05 (160 km) to 1 (40 km); is definitely somewhere within this range, and cannot be any smaller than 40 kilometers, assuming the absolute magnitude is correct.",
"(472651) 2015 DB216\n\nis a centaur and Uranus co-orbital discovered on February 27, 2015... |
(480808)_1994_XL1_18974660 | Reconstruct the content about 'Orbit and classification' from the article on '(480808) 1994 XL1'. | orbits the Sun at a distance of 0.3β1.0 AU once every 0 years and 7 months (201 days). Its orbit has an eccentricity of 0.53 and an inclination of 28Β° with respect to the ecliptic. No precoveries were taken, and no prior identifications were made. The body's observation arc begins with its official discovery observatio... | [
"(480808) 1994 XL1 β Orbit and classification\n\norbits the Sun at a distance of 0.3β1.0 AU once every 0 years and 7 months (201 days). Its orbit has an eccentricity of 0.53 and an inclination of 28Β° with respect to the ecliptic. No precoveries were taken, and no prior identifications were made. The body's observat... |
(480808)_1994_XL1_18974662 | Summarize the 'Physical characteristics' part of '(480808) 1994 XL1'. | has not been observed by any of the space-based surveys such as the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission. Based on a generic magnitude-to-diameter conversion, measures approximately 0.2 kilometers in diamet... | [
"(480808) 1994 XL1 β Orbit and classification\n\norbits the Sun at a distance of 0.3β1.0 AU once every 0 years and 7 months (201 days). Its orbit has an eccentricity of 0.53 and an inclination of 28Β° with respect to the ecliptic. No precoveries were taken, and no prior identifications were made. The body's observat... |
(480808)_1994_XL1_18974663 | Explain what '(480808) 1994 XL1' covers in the 'Naming and numbering' section. | After its first observation in 1994, this minor planet was numbered 23 year later by the Minor Planet Center on 12 January 2017 (M.P.C. 112958), after its last observation with the LCOβA 1-meter global telescope station at Sutherland, South Africa, on 6 December 2016. As of 2018, the asteroid has not been named. | [
"(480808) 1994 XL1 β Orbit and classification\n\norbits the Sun at a distance of 0.3β1.0 AU once every 0 years and 7 months (201 days). Its orbit has an eccentricity of 0.53 and an inclination of 28Β° with respect to the ecliptic. No precoveries were taken, and no prior identifications were made. The body's observat... |
(480808)_1994_XL1_18974661 | Explain what '(480808) 1994 XL1' covers in the 'Close encounter' section. | The asteroid has an Earth minimum orbital intersection distance of 0.0365 AU, which translates into 14.2 lunar distances. It passed 0.03709 AU from Earth on 6 December 1994. On 4 December 2044, it will pass again at 0.03637 AU from Earth. | [
"(480808) 1994 XL1 β Orbit and classification\n\norbits the Sun at a distance of 0.3β1.0 AU once every 0 years and 7 months (201 days). Its orbit has an eccentricity of 0.53 and an inclination of 28Β° with respect to the ecliptic. No precoveries were taken, and no prior identifications were made. The body's observat... |
(480808)_1994_XL1_18974659 | Reconstruct the content from the article about '(480808) 1994 XL1'. | is a sub-kilometer asteroid, classified as near-Earth object and potentially hazardous asteroid of the Aten group, approximately 200 m in diameter. It was discovered on 6 December 1994, by ScottishβAustralian astronomer Robert McNaught at Siding Spring Observatory in Australia. It was one of the first asteroids discove... | [
"(480808) 1994 XL1 β Orbit and classification\n\norbits the Sun at a distance of 0.3β1.0 AU once every 0 years and 7 months (201 days). Its orbit has an eccentricity of 0.53 and an inclination of 28Β° with respect to the ecliptic. No precoveries were taken, and no prior identifications were made. The body's observat... |
(481394)_2006_SF6_8079312 | Summarize the following section from the article on '(481394) 2006 SF6'. | is a sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group, approximately 300 m in diameter. It was discovered on 17 September 2006, by the Catalina Sky Survey at Catalina Station in Arizona. On 21 November 2019, it passed Earth at a distance of 0.0288 AU, which is the object's closest fl... | [
"(481394) 2006 SF6\n\nis a sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group, approximately 300 m in diameter. It was discovered on 17 September 2006, by the Catalina Sky Survey at Catalina Station in Arizona. On 21 November 2019, it passed Earth at a distance of 0.0288 AU, which ... |
(481394)_2006_SF6_8079318 | What information does the article about '(481394) 2006 SF6' provide on 'Diameter and albedo'? | According to the NEOSurvey carried out by NASA's Spitzer Space Telescope, the asteroid's surface has an albedo of 0.21, which gives a mean-diameter of roughly 300 meters based on an absolute magnitude of 19.9. The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.20 and a diameter of 0.311 kilometers using ... | [
"(481394) 2006 SF6\n\nis a sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group, approximately 300 m in diameter. It was discovered on 17 September 2006, by the Catalina Sky Survey at Catalina Station in Arizona. On 21 November 2019, it passed Earth at a distance of 0.0288 AU, which ... |
(481394)_2006_SF6_8079317 | What information does the article about '(481394) 2006 SF6' provide on 'Rotation period'? | In September 2018, a rotational lightcurve of was obtained from photometric observations by Brian Warner and Robert Stephens at the Center for Solar System Studies in California. Lightcurve analysis gave a rotation period of 11.517 hours with a very high brightness amplitude of 0.97 magnitude (U=3), indicative of a hi... | [
"(481394) 2006 SF6\n\nis a sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group, approximately 300 m in diameter. It was discovered on 17 September 2006, by the Catalina Sky Survey at Catalina Station in Arizona. On 21 November 2019, it passed Earth at a distance of 0.0288 AU, which ... |
(481394)_2006_SF6_8079315 | Based on the article about '(481394) 2006 SF6', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 12 January 2017 (M.P.C. 102964). As of 2020 it has not been named. | [
"(481394) 2006 SF6\n\nis a sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group, approximately 300 m in diameter. It was discovered on 17 September 2006, by the Catalina Sky Survey at Catalina Station in Arizona. On 21 November 2019, it passed Earth at a distance of 0.0288 AU, which ... |
(481394)_2006_SF6_8079313 | Reconstruct the content about 'Orbit and classification' from the article on '(481394) 2006 SF6'. | orbits the Sun at a distance of 0.7β1.2 AU once every 11 months (338 days; semi-major axis of 0.95 AU). Its orbit has an eccentricity of 0.28 and an inclination of 6Β° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Catalina Station in September 2006. | [
"(481394) 2006 SF6\n\nis a sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group, approximately 300 m in diameter. It was discovered on 17 September 2006, by the Catalina Sky Survey at Catalina Station in Arizona. On 21 November 2019, it passed Earth at a distance of 0.0288 AU, which ... |
(481394)_2006_SF6_8079316 | Explain what '(481394) 2006 SF6' covers in the 'Physical characteristics' section. | During its apparition in November 2007, spectro-photometric data obtained of allowed for an A/S/D-type classification. This classification could be further constrained to an A/S-type, as a D-type does not agree with the object's relatively high albedo value (see below). | [
"(481394) 2006 SF6\n\nis a sub-kilometer near-Earth object and potentially hazardous asteroid of the Aten group, approximately 300 m in diameter. It was discovered on 17 September 2006, by the Catalina Sky Survey at Catalina Station in Arizona. On 21 November 2019, it passed Earth at a distance of 0.0288 AU, which ... |
(48639)_1995_TL8_16321445 | Explain what '(48639) 1995 TL8' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 20 November 2002. As of 2018, it has not been named. | [
"(48639) 1995 TL8 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 20 November 2002. As of 2018, it has not been named.",
"(48639) 1995 TL8 β Discovery\n\nwas discovered on 15 October 1995, by American astronomer Arianna Gleason as part of UA's Spacewatch survey at Kitt Peak ... |
(48639)_1995_TL8_16321442 | From the article on '(48639) 1995 TL8', restate the 'Discovery' content. | was discovered on 15 October 1995, by American astronomer Arianna Gleason as part of UA's Spacewatch survey at Kitt Peak National Observatory, near Tucson, Arizona. It was the first of the bodies presently classified as a scattered-disc object (SDO) to be discovered, preceding the SDO prototype by almost a year. | [
"(48639) 1995 TL8 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 20 November 2002. As of 2018, it has not been named.",
"(48639) 1995 TL8 β Discovery\n\nwas discovered on 15 October 1995, by American astronomer Arianna Gleason as part of UA's Spacewatch survey at Kitt Peak ... |
(48639)_1995_TL8_16321443 | From the article on '(48639) 1995 TL8', restate the 'Satellite' content. | A companion was discovered by Denise C. Stephens and Keith S. Noll, from observations with the Hubble Space Telescope taken on 9 November 2002, and announced on 5 October 2005. The satellite, designated, is relatively large, having a likely mass of about 10% of the primary. Its orbit has not been determined, but it was... | [
"(48639) 1995 TL8 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 20 November 2002. As of 2018, it has not been named.",
"(48639) 1995 TL8 β Discovery\n\nwas discovered on 15 October 1995, by American astronomer Arianna Gleason as part of UA's Spacewatch survey at Kitt Peak ... |
(48639)_1995_TL8_16321444 | From the article on '(48639) 1995 TL8', restate the 'Scatteredβextended object' content. | is classified as detached object (scatteredβextended) by the Deep Ecliptic Survey, since its orbit appears to be beyond significant gravitational interactions with Neptune's current orbit. However, if Neptune migrated outward, there would have been a period when Neptune had a higher eccentricity. Simulations made in 20... | [
"(48639) 1995 TL8 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 20 November 2002. As of 2018, it has not been named.",
"(48639) 1995 TL8 β Discovery\n\nwas discovered on 15 October 1995, by American astronomer Arianna Gleason as part of UA's Spacewatch survey at Kitt Peak ... |
(48639)_1995_TL8_16321441 | Summarize the following section from the article on '(48639) 1995 TL8'. | is a binary trans-Neptunian object from the scattered disc in the outermost regions of the Solar System. It was discovered by Arianna Gleason in 1995 and measures approximately 176 kilometers in diameter. Its 80-kilometer minor-planet moon, provisionally designated, was discovered on 9 November 2002. | [
"(48639) 1995 TL8 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 20 November 2002. As of 2018, it has not been named.",
"(48639) 1995 TL8 β Discovery\n\nwas discovered on 15 October 1995, by American astronomer Arianna Gleason as part of UA's Spacewatch survey at Kitt Peak ... |
(4953)_1990_MU_31850788 | From the article on '(4953) 1990 MU', restate the 'Description' content. | it approached to 0.1418 AU. The Earth MOID of has been decreasing (becoming more hazardous) during the 20th century, while the Venus MOID (0.0455) has been increasing. Besides its original discovery at Siding Spring Observatory in Australia, has also been studied by radar at Goldstone Observatory in California, and Are... | [
"(4953) 1990 MU β Description\n\nit approached to 0.1418 AU. The Earth MOID of has been decreasing (becoming more hazardous) during the 20th century, while the Venus MOID (0.0455) has been increasing. Besides its original discovery at Siding Spring Observatory in Australia, has also been studied by radar at Goldsto... |
(4953)_1990_MU_31850786 | What does the article about '(4953) 1990 MU' say regarding 'Description'? | was first observed over three nights in 1990. By itself, this was not enough for the asteroid to be given a permanent number since the orbit could not be calculated accurately enough for the object to be subsequently recovered. However, the object was precovered by the Anglo-Australian Near-Earth Asteroid Survey on six... | [
"(4953) 1990 MU β Description\n\nit approached to 0.1418 AU. The Earth MOID of has been decreasing (becoming more hazardous) during the 20th century, while the Venus MOID (0.0455) has been increasing. Besides its original discovery at Siding Spring Observatory in Australia, has also been studied by radar at Goldsto... |
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