id string | question string | answer string | documents list |
|---|---|---|---|
(523706)_2014_HF200_29894408 | Describe the content of the article about '(523706) 2014 HF200'. | , provisional designation, is a trans-Neptunian object on an eccentric orbit from the scattered disc, located in the outermost region of the Solar System. It was discovered on 20 May 2012, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. The dwarf planet candidate measures appr... | [
"(523706) 2014 HF200 β Physical characteristics\n\nAccording to the Johnston's archive and American astronomer Michael Brown, measures 293 and 302 kilometers in diameter based on an assumed albedo of 0.09 and 0.08, respectively. On his website, Michael Brown lists this object as a \"possible\" dwarf planet (200β400... |
(523706)_2014_HF200_29894409 | Summarize the 'Orbit and classification' part of '(523706) 2014 HF200'. | is a scattered disc object and orbits the Sun at a distance of 35.5β88.0 AU once every 485 years and 4 months (177,277 days; semi-major axis of 61.76 AU). Its orbit has an eccentricity of 0.43 and an inclination of 10Β° with respect to the ecliptic. The body's observation arc begins with a precovery taken by Pan-STARRS ... | [
"(523706) 2014 HF200 β Physical characteristics\n\nAccording to the Johnston's archive and American astronomer Michael Brown, measures 293 and 302 kilometers in diameter based on an assumed albedo of 0.09 and 0.08, respectively. On his website, Michael Brown lists this object as a \"possible\" dwarf planet (200β400... |
(523719)_2014_LM28_24686031 | Describe the content of the article about '(523719) 2014 LM28'. | ''', provisional designation ', is a trans-Neptunian object and centaur, approximately 46 km in diameter. It was discovered on 16 May 2013, by the Pan-STARRS 1 survey at Haleakala Observatory, Hawaii, United States. The object's orbit is highly inclined and very eccentric, with a perihelion closer to the Sun than Uranu... | [
"(523719) 2014 LM28\n\n''', provisional designation ', is a trans-Neptunian object and centaur, approximately 46 km in diameter. It was discovered on 16 May 2013, by the Pan-STARRS 1 survey at Haleakala Observatory, Hawaii, United States. The object's orbit is highly inclined and very eccentric, with a perihelion c... |
(523719)_2014_LM28_24686032 | What does the article about '(523719) 2014 LM28' say regarding 'Orbit and classification'? | orbits the Sun at a distance of 16.8β538.9 AU once every 4631 years and 1 month (1,691,491 days; semi-major axis of 277.83 AU). Its orbit has an eccentricity of 0.94 and an inclination of 85Β° with respect to the ecliptic. The body's observation arc begins with its official discovery observation by Pan-STARRS at Haleaka... | [
"(523719) 2014 LM28\n\n''', provisional designation ', is a trans-Neptunian object and centaur, approximately 46 km in diameter. It was discovered on 16 May 2013, by the Pan-STARRS 1 survey at Haleakala Observatory, Hawaii, United States. The object's orbit is highly inclined and very eccentric, with a perihelion c... |
(523727)_2014_NW65_17601698 | Summarize the 'Diameter and albedo' part of '(523727) 2014 NW65'. | has an absolute magnitude of 6.6. According to the Johnston's archive and astronomer Michael Brown, it measures 212 and 225 kilometers in diameter, based on an assumed albedo for the body's surface of 0.09 and 0.08, respectively. It is one of the largest centaurs, comparable in size with 2060 Chiron, 10199 Chariklo, an... | [
"(523727) 2014 NW65 β Diameter and albedo\n\nhas an absolute magnitude of 6.6. According to the Johnston's archive and astronomer Michael Brown, it measures 212 and 225 kilometers in diameter, based on an assumed albedo for the body's surface of 0.09 and 0.08, respectively. It is one of the largest centaurs, compar... |
(523727)_2014_NW65_17601695 | Describe the content of the article about '(523727) 2014 NW65'. | , provisional designation:, is a large centaur from the outer Solar System, approximately 220 km in diameter. It was discovered on 14 July 2010 by astronomers with the Pan-STARRS-1 survey at Haleakala Observatory, Hawaii, in the United States. According to American astronomer Michael Brown, it is "possibly" a dwarf pla... | [
"(523727) 2014 NW65 β Diameter and albedo\n\nhas an absolute magnitude of 6.6. According to the Johnston's archive and astronomer Michael Brown, it measures 212 and 225 kilometers in diameter, based on an assumed albedo for the body's surface of 0.09 and 0.08, respectively. It is one of the largest centaurs, compar... |
(523727)_2014_NW65_17601697 | Based on the article about '(523727) 2014 NW65', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 25 September 2018, receiving the number in the minor planet catalog (M.P.C. 111779). , it has not been named. According to the established naming conventions, it will be named after one of the many centaurs from Greek mythology, which are creatures with the ... | [
"(523727) 2014 NW65 β Diameter and albedo\n\nhas an absolute magnitude of 6.6. According to the Johnston's archive and astronomer Michael Brown, it measures 212 and 225 kilometers in diameter, based on an assumed albedo for the body's surface of 0.09 and 0.08, respectively. It is one of the largest centaurs, compar... |
(523727)_2014_NW65_17601696 | Based on the article about '(523727) 2014 NW65', describe the 'Orbit and classification' section. | is a member of the centaurs, an inward-moving population of bodies transiting from the Kuiper belt to the group of Jupiter-family comets. Their eccentric orbits are often in between those of Jupiter and Neptune, that is, they have a semi-major axis of typically 5.5 to 30.1 AU. Centaurs are cometary-like bodies. They ha... | [
"(523727) 2014 NW65 β Diameter and albedo\n\nhas an absolute magnitude of 6.6. According to the Johnston's archive and astronomer Michael Brown, it measures 212 and 225 kilometers in diameter, based on an assumed albedo for the body's surface of 0.09 and 0.08, respectively. It is one of the largest centaurs, compar... |
(523731)_2014_OK394_3375725 | Describe the 'First observation and loss' section of the article about '(523731) 2014 OK394'. | was near perihelion 35.4 AU from the Sun when it was first observed in 1995, by astronomers Nichole Danzl and Arianna Gleason of the Spacewatch survey at Kitt Peak Observatory in Arizona, United States. It was only observed 14 times over 36 days, from 20 September to 26 October 1995. The discovery observations of were ... | [
"(523731) 2014 OK394 β First observation and loss\n\nwas near perihelion 35.4 AU from the Sun when it was first observed in 1995, by astronomers Nichole Danzl and Arianna Gleason of the Spacewatch survey at Kitt Peak Observatory in Arizona, United States. It was only observed 14 times over 36 days, from 20 Septembe... |
(523731)_2014_OK394_3375726 | Based on the article about '(523731) 2014 OK394', describe the 'Recovery' section. | On 30 November 2020, amateur astronomers S. Deen and K. Ly identified as the 3:5 resonant trans-Neptunian object, which was discovered by Pan-STARRS 1 in 2010. The identification was published by the Minor Planet Center on 27 January 2021. | [
"(523731) 2014 OK394 β First observation and loss\n\nwas near perihelion 35.4 AU from the Sun when it was first observed in 1995, by astronomers Nichole Danzl and Arianna Gleason of the Spacewatch survey at Kitt Peak Observatory in Arizona, United States. It was only observed 14 times over 36 days, from 20 Septembe... |
(523731)_2014_OK394_3375728 | What information does the article about '(523731) 2014 OK394' provide on 'Numbering and naming'? | was numbered by the Minor Planet Center on 25 September 2018 and received the number in the minor planet catalog. The alternate provisional designation was given by the Minor Planet Center on 27 January 2021 after the two objects were linked. , it has not been named. | [
"(523731) 2014 OK394 β First observation and loss\n\nwas near perihelion 35.4 AU from the Sun when it was first observed in 1995, by astronomers Nichole Danzl and Arianna Gleason of the Spacewatch survey at Kitt Peak Observatory in Arizona, United States. It was only observed 14 times over 36 days, from 20 Septembe... |
(523731)_2014_OK394_3375727 | From the article on '(523731) 2014 OK394', restate the 'Classification and orbit' content. | orbits the Sun at an average distance of 42.33 AU once every 275 years. Its orbit has an eccentricity of 0.16 and an inclination of 4Β° with respect to the ecliptic plane. Over the course of its orbit, its distance from the Sun ranges from 35.4 AU at perihelion to 49.3 AU at aphelion. is in a 3:5 mean-motion orbital res... | [
"(523731) 2014 OK394 β First observation and loss\n\nwas near perihelion 35.4 AU from the Sun when it was first observed in 1995, by astronomers Nichole Danzl and Arianna Gleason of the Spacewatch survey at Kitt Peak Observatory in Arizona, United States. It was only observed 14 times over 36 days, from 20 Septembe... |
(523731)_2014_OK394_3375724 | Reconstruct the content from the article about '(523731) 2014 OK394'. | ', also known as ', is a trans-Neptunian object that orbits in the outer Solar System beyond the orbit of Neptune. First observed as by Spacewatch on 20 September 1995, it was a lost minor planet with an insufficiently defined orbit with only 36 days of observations. On 8 October 2010, it was rediscovered by the Pan-ST... | [
"(523731) 2014 OK394 β First observation and loss\n\nwas near perihelion 35.4 AU from the Sun when it was first observed in 1995, by astronomers Nichole Danzl and Arianna Gleason of the Spacewatch survey at Kitt Peak Observatory in Arizona, United States. It was only observed 14 times over 36 days, from 20 Septembe... |
(523759)_2014_WK509_14468786 | What does the article about '(523759) 2014 WK509' say regarding 'Orbit and classification'? | belongs to the scattered disc population. It orbits the Sun at a distance of 40.1β61.6 AU once every 362 years and 6 months (132,399 days; semi-major axis of 50.8 AU). Its orbit has an eccentricity of 0.21 and an inclination of 15Β° with respect to the ecliptic. The body's observation arc begins on 14 September 2011 at ... | [
"(523759) 2014 WK509 β Orbit and classification\n\nbelongs to the scattered disc population. It orbits the Sun at a distance of 40.1β61.6 AU once every 362 years and 6 months (132,399 days; semi-major axis of 50.8 AU). Its orbit has an eccentricity of 0.21 and an inclination of 15Β° with respect to the ecliptic. The... |
(523759)_2014_WK509_14468787 | Based on the article about '(523759) 2014 WK509', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111779). As of 2018, it has not been named. | [
"(523759) 2014 WK509 β Orbit and classification\n\nbelongs to the scattered disc population. It orbits the Sun at a distance of 40.1β61.6 AU once every 362 years and 6 months (132,399 days; semi-major axis of 50.8 AU). Its orbit has an eccentricity of 0.21 and an inclination of 15Β° with respect to the ecliptic. The... |
(523759)_2014_WK509_14468788 | Summarize the 'Physical characteristics' part of '(523759) 2014 WK509'. | Based on an absolute magnitude of 4.4, and an assumed albedo of 0.09, the Johnston archive estimates a mean-diameter of approximately 584 km. As of 2018, no rotational lightcurve of this object has been obtained from photometric observations. The object's rotation period, pole and shape remain unknown. | [
"(523759) 2014 WK509 β Orbit and classification\n\nbelongs to the scattered disc population. It orbits the Sun at a distance of 40.1β61.6 AU once every 362 years and 6 months (132,399 days; semi-major axis of 50.8 AU). Its orbit has an eccentricity of 0.21 and an inclination of 15Β° with respect to the ecliptic. The... |
(523764)_2014_WC510_19765762 | What information does the article about '(523764) 2014 WC510' provide on 'Discovery'? | Before the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accredited observers using the telescope were... | [
"(523764) 2014 WC510 β Discovery\n\nBefore the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accre... |
(523764)_2014_WC510_19765766 | What does the article about '(523764) 2014 WC510' say regarding 'Binary system'? | Observations of the December 2018 occultation revealed that is a compact binary system consisting of two separate components in close orbit around each other. Of the six sites that reported positive detections of the occultation, one site located in Bishop, California, detected a shorter dimming event separate from the... | [
"(523764) 2014 WC510 β Discovery\n\nBefore the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accre... |
(523764)_2014_WC510_19765768 | Reconstruct the content about 'Physical characteristics' from the article on '(523764) 2014 WC510'. | Assuming a circular projected shape for the components' occultation profiles, the diameters of the primary and secondary are estimated to be 181 Β± 16 km and 138 Β± 32 km, respectively. The diameter ratio of the secondary to the primary is 0.76:1.00βthe secondary component is approximately 75% as large as the primary. Si... | [
"(523764) 2014 WC510 β Discovery\n\nBefore the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accre... |
(523764)_2014_WC510_19765764 | Based on the article about '(523764) 2014 WC510', describe the 'Occultation' section. | had only been observed by Pan-STARRS over an observation arc of 3 years. The calculated orbit from these Pan-STARRS observations had significant uncertainty, which would have been unreliable for predicting occultations. In an effort to reduce the orbital uncertainty, the RECON project collaborated with the Pan-STARRS p... | [
"(523764) 2014 WC510 β Discovery\n\nBefore the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accre... |
(523764)_2014_WC510_19765765 | Reconstruct the content about 'Orbit and classification' from the article on '(523764) 2014 WC510'. | is classified as a plutino, a subgroup of the resonant trans-Neptunian objects located in the inner region of Kuiper belt. Named after the group's largest member, Pluto, the plutinos are in a 2:3 mean-motion orbital resonance with Neptune. That is, they complete two orbits around the Sun for every three orbits that Nep... | [
"(523764) 2014 WC510 β Discovery\n\nBefore the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accre... |
(523764)_2014_WC510_19765767 | What information does the article about '(523764) 2014 WC510' provide on 'Binary system'? | milliarcseconds. Assuming a density of 1 g/cm3 for both components, their mutual orbital period would likely be under one day. has the third-smallest observed component separation of all known binary TNOs, after and. Such tight binary TNOs are difficult to resolve with direct imaging due to their characteristic small s... | [
"(523764) 2014 WC510 β Discovery\n\nBefore the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accre... |
(523764)_2014_WC510_19765763 | Describe the 'Occultation' section of the article about '(523764) 2014 WC510'. | On 1 December 2018, occulted a 15th-magnitude double star, blocking out its starlight for a maximal duration of approximately 11 seconds. The stellar occultation was observed by astronomers and citizen scientists across the West Coast of the United States and Canada. Of the 41 participating sites, six of them reported ... | [
"(523764) 2014 WC510 β Discovery\n\nBefore the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accre... |
(523764)_2014_WC510_19765761 | Describe the content of the article about '(523764) 2014 WC510'. | , is a binary trans-Neptunian object discovered on 8 September 2011 by the Pan-STARRS survey at the HaleakalΔ Observatory in Hawaii. It was found by Pan-STARRS on 20 November 2014 and was announced later in July 2016 after additional observations and precovery identifications. It is in the Kuiper belt, a region of icy ... | [
"(523764) 2014 WC510 β Discovery\n\nBefore the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accre... |
(523764)_2014_WC510_19765769 | What does the article about '(523764) 2014 WC510' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 25 September 2018 and received the number in the minor planet catalog. As of 2020, it has not been named. | [
"(523764) 2014 WC510 β Discovery\n\nBefore the announcement of its discovery, had been observed by the Pan-STARRS survey from 2011 to 2015. All of these observations were made with the Pan-STARRS 1 1.8-meter RitcheyβChrΓ©tien telescope, located at the HaleakalΔ Observatory atop the Hawaiian island of Maui. The accre... |
(523775)_2014_YB35_6624976 | Based on the article about '(523775) 2014 YB35', describe the 'Satellite' section. | The Goldstone Deep Space Communications Complex was scheduled to observe this object on 20 March 2015, at which time it was expected they could obtain coarse radar images and continuous wave spectra, which may help determine the asteroid's composition. These observations showed a small companion less than 150 meters ac... | [
"(523775) 2014 YB35 β Satellite\n\nThe Goldstone Deep Space Communications Complex was scheduled to observe this object on 20 March 2015, at which time it was expected they could obtain coarse radar images and continuous wave spectra, which may help determine the asteroid's composition. These observations showed a ... |
(523775)_2014_YB35_6624975 | What information does the article about '(523775) 2014 YB35' provide on 'Close encounters'? | It passed by Earth on 27 March 2015 at 06:21 UTC at a distance of 4473807 Β±, or 11.7 lunar distances, and a relative speed of 10.16 km/s. next encounter with Earth will be in 2033, at a distance of approximately 3330000 km. | [
"(523775) 2014 YB35 β Satellite\n\nThe Goldstone Deep Space Communications Complex was scheduled to observe this object on 20 March 2015, at which time it was expected they could obtain coarse radar images and continuous wave spectra, which may help determine the asteroid's composition. These observations showed a ... |
(523775)_2014_YB35_6624977 | Explain what '(523775) 2014 YB35' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111778). As of 2018, it has not been named. | [
"(523775) 2014 YB35 β Satellite\n\nThe Goldstone Deep Space Communications Complex was scheduled to observe this object on 20 March 2015, at which time it was expected they could obtain coarse radar images and continuous wave spectra, which may help determine the asteroid's composition. These observations showed a ... |
(523775)_2014_YB35_6624974 | Based on the article about '(523775) 2014 YB35', describe the 'Orbit and classification' section. | is a member of the Apollo asteroids, a group of near-Earth object with an Earth-crossing orbit. It orbits the Sun at a distance of 1.0β2.8 AU once every 2 years and 7 months (939 days; semi-major axis of 1.88 AU). Its orbit has an eccentricity of 0.48 and an inclination of 13Β° with respect to the ecliptic. The body's o... | [
"(523775) 2014 YB35 β Satellite\n\nThe Goldstone Deep Space Communications Complex was scheduled to observe this object on 20 March 2015, at which time it was expected they could obtain coarse radar images and continuous wave spectra, which may help determine the asteroid's composition. These observations showed a ... |
(523794)_2015_RR245_22861491 | Summarize the 'Satellite' part of '(523794) 2015 RR245'. | is suspected to be binary, though the size of the secondary body (moon) has not been determined. If the moon significantly contributes to the observed brightness of the primary, the size of may therefore be substantially smaller than estimates that assumed the system's total brightness was from a single object. Once th... | [
"(523794) 2015 RR245 β Satellite\n\nis suspected to be binary, though the size of the secondary body (moon) has not been determined. If the moon significantly contributes to the observed brightness of the primary, the size of may therefore be substantially smaller than estimates that assumed the system's total brig... |
(523794)_2015_RR245_22861486 | Based on the article about '(523794) 2015 RR245', describe the 'Discovery' section. | A first precovery of was taken at the Cerro Tololo Observatory in Chile on 15 October 2004. It was first observed by a research team led by Michele Bannister while poring over images that the CanadaβFranceβHawaii Telescope in Hawaii took in September 2015 as part of the Outer Solar System Origins Survey (OSSOS), and l... | [
"(523794) 2015 RR245 β Satellite\n\nis suspected to be binary, though the size of the secondary body (moon) has not been determined. If the moon significantly contributes to the observed brightness of the primary, the size of may therefore be substantially smaller than estimates that assumed the system's total brig... |
(523794)_2015_RR245_22861487 | Reconstruct the content about 'Numbering and naming' from the article on '(523794) 2015 RR245'. | This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111779). As of 2020, it has not been named. | [
"(523794) 2015 RR245 β Satellite\n\nis suspected to be binary, though the size of the secondary body (moon) has not been determined. If the moon significantly contributes to the observed brightness of the primary, the size of may therefore be substantially smaller than estimates that assumed the system's total brig... |
(523794)_2015_RR245_22861485 | Summarize the following section from the article on '(523794) 2015 RR245'. | , provisional designation, is a large trans-Neptunian object of the Kuiper belt in the outermost regions of the Solar System. It was discovered on 9 September 2015, by the Outer Solar System Origins Survey at Mauna Kea Observatories on the Big island of Hawaii, in the United States. The object is in a rare 2:9 resonanc... | [
"(523794) 2015 RR245 β Satellite\n\nis suspected to be binary, though the size of the secondary body (moon) has not been determined. If the moon significantly contributes to the observed brightness of the primary, the size of may therefore be substantially smaller than estimates that assumed the system's total brig... |
(523794)_2015_RR245_22861490 | Based on the article about '(523794) 2015 RR245', describe the 'Diameter and albedo' section. | Its exact size is uncertain, but the best estimate is around 670 km in diameter, assuming an albedo of 0.12 (within a wider range of 500 to 870 km, based on albedos of 0.21 to 0.07). For comparison, Pluto, the largest object in the Kuiper belt, is about 2374 km in diameter. Astronomer Michael Brown assumes an albedo of... | [
"(523794) 2015 RR245 β Satellite\n\nis suspected to be binary, though the size of the secondary body (moon) has not been determined. If the moon significantly contributes to the observed brightness of the primary, the size of may therefore be substantially smaller than estimates that assumed the system's total brig... |
(523794)_2015_RR245_22861488 | Explain what '(523794) 2015 RR245' covers in the 'Orbit and classification' section. | As of 2018, has a reasonably well defined orbit with an uncertainty of 3. It orbits the Sun at a distance of 33.8β128.6 AU once every 731 years and 6 months (for reference, Neptune's orbit is at 30 AU). Its orbit has an eccentricity of 0.58 and an inclination of 8Β° with respect to the ecliptic. is among the most distan... | [
"(523794) 2015 RR245 β Satellite\n\nis suspected to be binary, though the size of the secondary body (moon) has not been determined. If the moon significantly contributes to the observed brightness of the primary, the size of may therefore be substantially smaller than estimates that assumed the system's total brig... |
(523794)_2015_RR245_22861489 | Reconstruct the content about '2:9 resonance' from the article on '(523794) 2015 RR245'. | Additional precovery astrometry from the Sloan Digital Sky Survey and the Pan-STARRS1 survey shows that is a resonant trans-Neptunian object, securely trapped in a 2:9 mean motion resonance with Neptune, meaning that this minor planet orbits the Sun twice in the same amount of time it takes Neptune to complete 9 orbits... | [
"(523794) 2015 RR245 β Satellite\n\nis suspected to be binary, though the size of the secondary body (moon) has not been determined. If the moon significantly contributes to the observed brightness of the primary, the size of may therefore be substantially smaller than estimates that assumed the system's total brig... |
(523972)_1999_CW8_9161951 | Reconstruct the content from the article about '(523972) 1999 CW8'. | , provisional designation, is a bright carbonaceous asteroid and sub-kilometer near-Earth object of the Apollo group, first observed on 12 February 1999, by astronomers of the Lincoln Near Earth Asteroid Research program at Lincoln Laboratory ETS in New Mexico, United States. | [
"(523972) 1999 CW8\n\n, provisional designation, is a bright carbonaceous asteroid and sub-kilometer near-Earth object of the Apollo group, first observed on 12 February 1999, by astronomers of the Lincoln Near Earth Asteroid Research program at Lincoln Laboratory ETS in New Mexico, United States.",
"(523972) 199... |
(523972)_1999_CW8_9161953 | What information does the article about '(523972) 1999 CW8' provide on 'Orbit and classification'? | is an Apollo asteroid that crosses Earth's orbit. It orbits the Sun at a distance of 0.9β3.6 AU once every 3 years and 4 months (1,221 days; semi-major axis of 2.24 AU). Its orbit has an eccentricity of 0.60 and an inclination of 34Β° with respect to the ecliptic. The asteroid never approaches Earth closer than 0.2 AU i... | [
"(523972) 1999 CW8\n\n, provisional designation, is a bright carbonaceous asteroid and sub-kilometer near-Earth object of the Apollo group, first observed on 12 February 1999, by astronomers of the Lincoln Near Earth Asteroid Research program at Lincoln Laboratory ETS in New Mexico, United States.",
"(523972) 199... |
(523972)_1999_CW8_9161952 | Based on the article about '(523972) 1999 CW8', describe the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114615). As of 2019, it has not been named. | [
"(523972) 1999 CW8\n\n, provisional designation, is a bright carbonaceous asteroid and sub-kilometer near-Earth object of the Apollo group, first observed on 12 February 1999, by astronomers of the Lincoln Near Earth Asteroid Research program at Lincoln Laboratory ETS in New Mexico, United States.",
"(523972) 199... |
(523972)_1999_CW8_9161954 | From the article on '(523972) 1999 CW8', restate the 'Physical characteristics' content. | It is a carbonaceous B-type asteroid, relatively rare in the asteroid belt but common in the inner Solar System. Based on an absolute magnitude of 18.6, and an assumed albedo of 0.159 (derived from the B-type asteroid 2 Pallas), the asteroid can be estimated to have a mean-diameter of approximately 640 meters. If it im... | [
"(523972) 1999 CW8\n\n, provisional designation, is a bright carbonaceous asteroid and sub-kilometer near-Earth object of the Apollo group, first observed on 12 February 1999, by astronomers of the Lincoln Near Earth Asteroid Research program at Lincoln Laboratory ETS in New Mexico, United States.",
"(523972) 199... |
(524366)_2001_XR254_17527330 | From the article on '(524366) 2001 XR254', restate the 'Discovery and orbit' content. | was discovered on 10 December 2001 by David C. Jewitt, Scott S. Sheppard and Jan Kleyna using 2.2-meter University of Hawaii reflector on Mauna Kea. belongs to the dynamically cold population of the classical Kuiper belt objects, which small orbital eccentricities and inclinations. Their semi-major axes reside mainly i... | [
"(524366) 2001 XR254 β Discovery and orbit\n\nwas discovered on 10 December 2001 by David C. Jewitt, Scott S. Sheppard and Jan Kleyna using 2.2-meter University of Hawaii reflector on Mauna Kea. belongs to the dynamically cold population of the classical Kuiper belt objects, which small orbital eccentricities and i... |
(524366)_2001_XR254_17527329 | Summarize the following section from the article on '(524366) 2001 XR254'. | , provisional designation, is a trans-Neptunian object and binary system from the classical Kuiper belt, located in the outermost region of the Solar System. The cubewano belongs to the cold population and measures approximately 171 km. It was first observed on 10 December 2001, by astronomers at the Mauna Kea Observat... | [
"(524366) 2001 XR254 β Discovery and orbit\n\nwas discovered on 10 December 2001 by David C. Jewitt, Scott S. Sheppard and Jan Kleyna using 2.2-meter University of Hawaii reflector on Mauna Kea. belongs to the dynamically cold population of the classical Kuiper belt objects, which small orbital eccentricities and i... |
(524366)_2001_XR254_17527331 | Reconstruct the content about 'Satellite' from the article on '(524366) 2001 XR254'. | is a binary consisting of two components of approximately equal size. Assuming that both components have the same albedo, the primary is estimated to be about 170 km in diameter. The size of the secondary (satellite) in this case is estimated at about 140 km. The total mass of the system is about 4 kg. The average dens... | [
"(524366) 2001 XR254 β Discovery and orbit\n\nwas discovered on 10 December 2001 by David C. Jewitt, Scott S. Sheppard and Jan Kleyna using 2.2-meter University of Hawaii reflector on Mauna Kea. belongs to the dynamically cold population of the classical Kuiper belt objects, which small orbital eccentricities and i... |
(524435)_2002_CY248_28172119 | Based on the article about '(524435) 2002 CY248', describe the 'Physical characteristics' section. | Based on an absolute magnitude of 5.2, and an assumed albedo of 0.09, the Johnston archive estimates a mean-diameter of approximately 404 km, while astronomer Michael Brown assumes an albedo of 0.06 and calculates a diameter of 449 km using a fainter magnitude of 5.5. Brown also characterizes the object as a "probable ... | [
"(524435) 2002 CY248 β Physical characteristics\n\nBased on an absolute magnitude of 5.2, and an assumed albedo of 0.09, the Johnston archive estimates a mean-diameter of approximately 404 km, while astronomer Michael Brown assumes an albedo of 0.06 and calculates a diameter of 449 km using a fainter magnitude of 5... |
(524435)_2002_CY248_28172118 | Summarize the 'Orbit and classification' part of '(524435) 2002 CY248'. | orbits the Sun at a distance of 39.4β53.1 AU once every 314 years and 6 months (114,859 days; semi-major axis of 46.2 AU). Its orbit has an eccentricity of 0.15 and an inclination of 7Β° with respect to the ecliptic. The body's observation arc begins at Kitt Peak with its official first observation on 6 February 2002. A... | [
"(524435) 2002 CY248 β Physical characteristics\n\nBased on an absolute magnitude of 5.2, and an assumed albedo of 0.09, the Johnston archive estimates a mean-diameter of approximately 404 km, while astronomer Michael Brown assumes an albedo of 0.06 and calculates a diameter of 449 km using a fainter magnitude of 5... |
(524435)_2002_CY248_28172117 | Describe the content of the article about '(524435) 2002 CY248'. | , provisional designation, is a trans-Neptunian object and weak dwarf-planet candidate from the classical Kuiper belt in the outermost region of the Solar System, approximately 400 - 450 km in diameter. It was first observed on 6 February 2002, by American astronomer Marc Buie at the Kitt Peak National Observatory in A... | [
"(524435) 2002 CY248 β Physical characteristics\n\nBased on an absolute magnitude of 5.2, and an assumed albedo of 0.09, the Johnston archive estimates a mean-diameter of approximately 404 km, while astronomer Michael Brown assumes an albedo of 0.06 and calculates a diameter of 449 km using a fainter magnitude of 5... |
(524522)_2002_VE68_20928071 | From the article on '(524522) 2002 VE68', restate the 'Discovery, orbit and physical properties' content. | It was discovered on 11 November 2002 at Lowell Observatory. As of February 2013, has been observed telescopically 457 times with a data-arc span of 2,947 days and it was the target of Doppler observations in 5 occasions; therefore, its orbit is very well determined. Its semi-major axis of 0.7237 AU is very similar to ... | [
"(524522) 2002 VE68 β Discovery, orbit and physical properties\n\nIt was discovered on 11 November 2002 at Lowell Observatory. As of February 2013, has been observed telescopically 457 times with a data-arc span of 2,947 days and it was the target of Doppler observations in 5 occasions; therefore, its orbit is very... |
(524522)_2002_VE68_20928073 | Summarize the 'Potentially hazardous asteroid' part of '(524522) 2002 VE68'. | is included in the Minor Planet Center list of Potentially Hazardous Asteroids (PHAs) because it comes relatively frequently to within 0.05 AU of Earth. Approaches as close as 0.04 AU occur with a periodicity of 8 years due to its near 8:13 resonance with Earth. was discovered during the close approaches of 11 November... | [
"(524522) 2002 VE68 β Discovery, orbit and physical properties\n\nIt was discovered on 11 November 2002 at Lowell Observatory. As of February 2013, has been observed telescopically 457 times with a data-arc span of 2,947 days and it was the target of Doppler observations in 5 occasions; therefore, its orbit is very... |
(524522)_2002_VE68_20928074 | What does the article about '(524522) 2002 VE68' say regarding 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114620). As of 2020, it has not been named. | [
"(524522) 2002 VE68 β Discovery, orbit and physical properties\n\nIt was discovered on 11 November 2002 at Lowell Observatory. As of February 2013, has been observed telescopically 457 times with a data-arc span of 2,947 days and it was the target of Doppler observations in 5 occasions; therefore, its orbit is very... |
(524522)_2002_VE68_20928070 | What information does the article about '(524522) 2002 VE68' provide? | , provisional designation, is a sub-kilometer sized asteroid and temporary quasi-satellite of Venus. It was the first such object to be discovered around a major planet in the Solar System. In a frame of reference rotating with Venus, it appears to travel around it during one Venerean year but it actually orbits the Su... | [
"(524522) 2002 VE68 β Discovery, orbit and physical properties\n\nIt was discovered on 11 November 2002 at Lowell Observatory. As of February 2013, has been observed telescopically 457 times with a data-arc span of 2,947 days and it was the target of Doppler observations in 5 occasions; therefore, its orbit is very... |
(524522)_2002_VE68_20928072 | Based on the article about '(524522) 2002 VE68', describe the 'Quasi-satellite dynamical state and orbital evolution' section. | The existence of retrograde satellites or quasi-satellites was first considered by J. Jackson in 1913 but none was discovered until almost 100 years later. was the first quasi-satellite to be discovered, in 2002, although it was not immediately recognized as such. was identified as a quasi-satellite of Venus by Seppo M... | [
"(524522) 2002 VE68 β Discovery, orbit and physical properties\n\nIt was discovered on 11 November 2002 at Lowell Observatory. As of February 2013, has been observed telescopically 457 times with a data-arc span of 2,947 days and it was the target of Doppler observations in 5 occasions; therefore, its orbit is very... |
(527603)_2007_VJ305_18040053 | Describe the content of the article about '(527603) 2007 VJ305'. | , provisional designation, is an extrem trans-Neptunian object from the extended scattered disc on a highly eccentric orbit in the outermost region of the Solar System. It measures approximately 250 km in diameter and is "possibly" a dwarf planet. The rather reddish extended scattered disc object belongs to the group o... | [
"(527603) 2007 VJ305\n\n, provisional designation, is an extrem trans-Neptunian object from the extended scattered disc on a highly eccentric orbit in the outermost region of the Solar System. It measures approximately 250 km in diameter and is \"possibly\" a dwarf planet. The rather reddish extended scattered disc... |
(527603)_2007_VJ305_18040058 | Summarize the 'Rotation period and shape' part of '(527603) 2007 VJ305'. | As of 2019, no rotational lightcurve of has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. | [
"(527603) 2007 VJ305\n\n, provisional designation, is an extrem trans-Neptunian object from the extended scattered disc on a highly eccentric orbit in the outermost region of the Solar System. It measures approximately 250 km in diameter and is \"possibly\" a dwarf planet. The rather reddish extended scattered disc... |
(527603)_2007_VJ305_18040057 | Based on the article about '(527603) 2007 VJ305', describe the 'Diameter and albedo' section. | According to the Johnston's archive and to American astronomer Michael Brown, measures 202 and 279 kilometers in diameter based on an assumed albedo of 0.09 and 0.04, respectively. On his website, Michael Brown lists this object as "possibly" a dwarf planet (200β400 km) which is the least certain class in his 5-class ... | [
"(527603) 2007 VJ305\n\n, provisional designation, is an extrem trans-Neptunian object from the extended scattered disc on a highly eccentric orbit in the outermost region of the Solar System. It measures approximately 250 km in diameter and is \"possibly\" a dwarf planet. The rather reddish extended scattered disc... |
(527603)_2007_VJ305_18040055 | Describe the 'Numbering and naming' section of the article about '(527603) 2007 VJ305'. | This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114650). As of 2019, it has not been named. | [
"(527603) 2007 VJ305\n\n, provisional designation, is an extrem trans-Neptunian object from the extended scattered disc on a highly eccentric orbit in the outermost region of the Solar System. It measures approximately 250 km in diameter and is \"possibly\" a dwarf planet. The rather reddish extended scattered disc... |
(527603)_2007_VJ305_18040054 | What does the article about '(527603) 2007 VJ305' say regarding 'Orbit and classification'? | orbits the Sun at a distance of 35.1β347 AU once every 2640 years and 11 months (964,601 days; semi-major axis of 191.1 AU). Its orbit has an exceptionally high eccentricity of 0.82 and an inclination of 12Β° with respect to the ecliptic. The body's observation arc begins with a precovery taken during the Sloan Digital ... | [
"(527603) 2007 VJ305\n\n, provisional designation, is an extrem trans-Neptunian object from the extended scattered disc on a highly eccentric orbit in the outermost region of the Solar System. It measures approximately 250 km in diameter and is \"possibly\" a dwarf planet. The rather reddish extended scattered disc... |
(527604)_2007_VL305_29190371 | From the article on '(527604) 2007 VL305', restate the 'Numbering and naming' content. | This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114650). As of 2019, it has not been named. If named, it will follow the naming scheme already established with 385571 Otrera and 385695 Clete, which is to name these objects after figures related to the Amazons, an all-female warrior trib... | [
"(527604) 2007 VL305 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114650). As of 2019, it has not been named. If named, it will follow the naming scheme already established with 385571 Otrera and 385695 Clete, which is to name these objects after figures... |
(527604)_2007_VL305_29190369 | Based on the article about '(527604) 2007 VL305', describe the 'Orbit and classification' section. | Neptune trojans can be considered resonant trans-Neptunian objects in a 1:1 mean-motion orbital resonance with Neptune. These trojans have a semi-major axis and an orbital period very similar to Neptune's (30.10 AU; 164.8 years). belongs to the leading group, which orbits 60Β° ahead of Neptune's orbit. It orbits the Sun... | [
"(527604) 2007 VL305 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114650). As of 2019, it has not been named. If named, it will follow the naming scheme already established with 385571 Otrera and 385695 Clete, which is to name these objects after figures... |
(527604)_2007_VL305_29190368 | Describe the content of the article about '(527604) 2007 VL305'. | , provisional designation, is an inclined Neptune trojan that shares Neptune's orbit in the Lagrangian point. It was discovered on 4 November 2007, by astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica at the Apache Point Observatory in New Mexico, United States, although images from 2005 have also been recove... | [
"(527604) 2007 VL305 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114650). As of 2019, it has not been named. If named, it will follow the naming scheme already established with 385571 Otrera and 385695 Clete, which is to name these objects after figures... |
(527604)_2007_VL305_29190370 | What does the article about '(527604) 2007 VL305' say regarding 'Diameter'? | The discoverers estimate that has a mean-diameter of 160 kilometers based on a magnitude of 22.2. Based on a generic magnitude-to-diameter conversion, it measures approximately 110 kilometers in diameter using an absolute magnitude of 7.9 with an assumed albedo of 0.10. | [
"(527604) 2007 VL305 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114650). As of 2019, it has not been named. If named, it will follow the naming scheme already established with 385571 Otrera and 385695 Clete, which is to name these objects after figures... |
(52768)_1998_OR2_2910145 | Explain what '(52768) 1998 OR2' covers in the 'Close approaches' section. | With an absolute magnitude of approximately 15.8, is one of the brightest and presumably largest-known potentially hazardous asteroids (see PHA-list). It currently has an Earth minimum orbital intersection distance of 0.0154 AU, which translates into 6.0 lunar distances (LD). On 16 April 2079, this asteroid will make a... | [
"(52768) 1998 OR2 β Close approaches\n\nWith an absolute magnitude of approximately 15.8, is one of the brightest and presumably largest-known potentially hazardous asteroids (see PHA-list). It currently has an Earth minimum orbital intersection distance of 0.0154 AU, which translates into 6.0 lunar distances (LD).... |
(52768)_1998_OR2_2910144 | What does the article about '(52768) 1998 OR2' say regarding 'Orbit and classification'? | is a member of the dynamical Amor group of near-Earth asteroids, and therefore does not currently cross Earth's orbit. The asteroid's closest approach to the Sun is just outside Earth's farthest distance from the Sun. When the asteroid has a perihelion point less than 1.017 AU (Earth's aphelion), it is classified an Ap... | [
"(52768) 1998 OR2 β Close approaches\n\nWith an absolute magnitude of approximately 15.8, is one of the brightest and presumably largest-known potentially hazardous asteroids (see PHA-list). It currently has an Earth minimum orbital intersection distance of 0.0154 AU, which translates into 6.0 lunar distances (LD).... |
(52768)_1998_OR2_2910146 | Describe the 'Physical characteristics' section of the article about '(52768) 1998 OR2'. | According to observations by the NASA IRTF telescope during the ExploreNEOs Warm Spitzer program, is a rather rare L-type asteroid. Delay-Doppler radar observations by the Arecibo Observatory in April 2020 have shown that bears a large, crater-like concavity in its shape. These radar observations have also resolved sev... | [
"(52768) 1998 OR2 β Close approaches\n\nWith an absolute magnitude of approximately 15.8, is one of the brightest and presumably largest-known potentially hazardous asteroids (see PHA-list). It currently has an Earth minimum orbital intersection distance of 0.0154 AU, which translates into 6.0 lunar distances (LD).... |
(52768)_1998_OR2_2910143 | Reconstruct the content from the article about '(52768) 1998 OR2'. | (provisional designation ) is an asteroid on an eccentric orbit, classified as a near-Earth object and potentially hazardous asteroid of the Amor group, with a diameter of 2 km. It was discovered on 24 July 1998, by astronomers of the Near-Earth Asteroid Tracking (NEAT) program at the Haleakala Observatory, Hawaii. It ... | [
"(52768) 1998 OR2 β Close approaches\n\nWith an absolute magnitude of approximately 15.8, is one of the brightest and presumably largest-known potentially hazardous asteroids (see PHA-list). It currently has an Earth minimum orbital intersection distance of 0.0154 AU, which translates into 6.0 lunar distances (LD).... |
(52768)_1998_OR2_2910148 | Based on the article about '(52768) 1998 OR2', describe the 'Diameter and albedo' section. | The Collaborative Asteroid Lightcurve Link (CALL) assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 2.15 km based on an absolute magnitude of 15.7. | [
"(52768) 1998 OR2 β Close approaches\n\nWith an absolute magnitude of approximately 15.8, is one of the brightest and presumably largest-known potentially hazardous asteroids (see PHA-list). It currently has an Earth minimum orbital intersection distance of 0.0154 AU, which translates into 6.0 lunar distances (LD).... |
(52768)_1998_OR2_2910147 | Reconstruct the content about 'Rotation period' from the article on '(52768) 1998 OR2'. | In 2009, rotational lightcurves of were obtained from photometric observations by astronomers in Salvador, Brazil, and during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS). Lightcurve analysis gave a rotation period of 3.198 and 4.112 hours with a brightness amplitude of 0.29 and 0.16 magnitude,... | [
"(52768) 1998 OR2 β Close approaches\n\nWith an absolute magnitude of approximately 15.8, is one of the brightest and presumably largest-known potentially hazardous asteroids (see PHA-list). It currently has an Earth minimum orbital intersection distance of 0.0154 AU, which translates into 6.0 lunar distances (LD).... |
(528381)_2008_ST291_23515585 | Reconstruct the content about 'Numbering and naming' from the article on '(528381) 2008 ST291'. | This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114657). As of 2019, it has not been named. | [
"(528381) 2008 ST291 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114657). As of 2019, it has not been named.",
"(528381) 2008 ST291 β Orbit and classification\n\nis located at the 1:6 Neptune resonance of 99 AU meaning that it completes roughly 1 orbi... |
(528381)_2008_ST291_23515586 | What information does the article about '(528381) 2008 ST291' provide on 'Orbit and classification'? | is located at the 1:6 Neptune resonance of 99 AU meaning that it completes roughly 1 orbit for every 6 orbits Neptune makes. It orbits the Sun at a distance of 42.3β157.5 AU once every 998 years and 4 months (semi-major axis of 99.89 AU). Its orbit has an eccentricity of 0.58 and an inclination of 21Β° with respect to t... | [
"(528381) 2008 ST291 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114657). As of 2019, it has not been named.",
"(528381) 2008 ST291 β Orbit and classification\n\nis located at the 1:6 Neptune resonance of 99 AU meaning that it completes roughly 1 orbi... |
(528381)_2008_ST291_23515587 | Describe the 'Physical characteristics' section of the article about '(528381) 2008 ST291'. | Based on an absolute magnitude of 4.4, is estimated by the Johnston's Archive to be about 584 km in diameter, assuming a typical albedo of 0.09 for trans-Neptunian objects. Astronomer Mike Brown estimates a slightly smaller 549 km from the same albedo and a fainter 4.6 magnitude. The Asteroid Dynamic Site records a bri... | [
"(528381) 2008 ST291 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114657). As of 2019, it has not been named.",
"(528381) 2008 ST291 β Orbit and classification\n\nis located at the 1:6 Neptune resonance of 99 AU meaning that it completes roughly 1 orbi... |
(528381)_2008_ST291_23515584 | What information does the article about '(528381) 2008 ST291' provide? | , provisional designation, is a 1:6 resonant trans-Neptunian object located in the outermost region of the Solar System that takes almost a thousand years to complete an orbit around the Sun. It was discovered on 24 September 2008 by American astronomers Megan Schwamb, Michael Brown and David Rabinowitz at the Palomar ... | [
"(528381) 2008 ST291 β Numbering and naming\n\nThis minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114657). As of 2019, it has not been named.",
"(528381) 2008 ST291 β Orbit and classification\n\nis located at the 1:6 Neptune resonance of 99 AU meaning that it completes roughly 1 orbi... |
(529366)_2009_WM1_27586029 | Describe the content of the article about '(529366) 2009 WM1'. | , provisional designation, is a sub-kilometer asteroid and near-Earth object of the Apollo group, approximately 280 m in diameter. After its discovery by the Catalina Sky Survey at the Catalina Station in Arizona, United States, this potentially hazardous asteroid was briefly listed at a Torino Scale of 1 and a cumulat... | [
"(529366) 2009 WM1\n\n, provisional designation, is a sub-kilometer asteroid and near-Earth object of the Apollo group, approximately 280 m in diameter. After its discovery by the Catalina Sky Survey at the Catalina Station in Arizona, United States, this potentially hazardous asteroid was briefly listed at a Torin... |
(529366)_2009_WM1_27586030 | Explain what '(529366) 2009 WM1' covers in the 'Numbering and naming' section. | This minor planet was numbered by the Minor Planet Center on 18 May 2019 (M.P.C. 114667). As of 2019, it has not been named. | [
"(529366) 2009 WM1\n\n, provisional designation, is a sub-kilometer asteroid and near-Earth object of the Apollo group, approximately 280 m in diameter. After its discovery by the Catalina Sky Survey at the Catalina Station in Arizona, United States, this potentially hazardous asteroid was briefly listed at a Torin... |
(529366)_2009_WM1_27586031 | What information does the article about '(529366) 2009 WM1' provide on 'Orbit and classification'? | orbits the Sun at a distance of 0.98β1.38 AU once every 15 months (468 days; semi-major axis of 1.18 AU). Its orbit has an eccentricity of 0.17 and an inclination of 26Β° with respect to the ecliptic. Even though has an Earth MOID of 0.00009 AU, the orbit and future close approaches are well determined with an orbital u... | [
"(529366) 2009 WM1\n\n, provisional designation, is a sub-kilometer asteroid and near-Earth object of the Apollo group, approximately 280 m in diameter. After its discovery by the Catalina Sky Survey at the Catalina Station in Arizona, United States, this potentially hazardous asteroid was briefly listed at a Torin... |
(529366)_2009_WM1_27586032 | Describe the '2014 passage' section of the article about '(529366) 2009 WM1'. | The 21 May 2014 Earth close approach of 0.3622 AU should allow a refinement to the orbit. From 7 May 2014 until 2 June 2014 the asteroid will be brighter than apparent magnitude 20. The asteroid will come to opposition on 18 May 2014 when it will be up all night. | [
"(529366) 2009 WM1\n\n, provisional designation, is a sub-kilometer asteroid and near-Earth object of the Apollo group, approximately 280 m in diameter. After its discovery by the Catalina Sky Survey at the Catalina Station in Arizona, United States, this potentially hazardous asteroid was briefly listed at a Torin... |
(532037)_2013_FY27_28948726 | Describe the content of the article about '(532037) 2013 FY27'. | is a trans-Neptunian object and binary system that belongs to the scattered disc (like Eris). Its discovery was announced on 31 March 2014. It has an absolute magnitude (H) of 3.2. is a binary object, with two components approximately 740 km and 190 km in diameter. It is the ninth-intrinsically-brightest known trans-Ne... | [
"(532037) 2013 FY27\n\nis a trans-Neptunian object and binary system that belongs to the scattered disc (like Eris). Its discovery was announced on 31 March 2014. It has an absolute magnitude (H) of 3.2. is a binary object, with two components approximately 740 km and 190 km in diameter. It is the ninth-intrinsical... |
(532037)_2013_FY27_28948728 | Reconstruct the content about 'Physical properties' from the article on '(532037) 2013 FY27'. | has a diameter of about 740 km, placing it at a transition zone between medium-sized and large TNOs. Using the Atacama Large Millimeter Array and Magellan Telescopes, its albedo was found to be 0.17, and its colour to be moderately red. is one of the largest moderately red TNOs. The physical processes that lead to a la... | [
"(532037) 2013 FY27\n\nis a trans-Neptunian object and binary system that belongs to the scattered disc (like Eris). Its discovery was announced on 31 March 2014. It has an absolute magnitude (H) of 3.2. is a binary object, with two components approximately 740 km and 190 km in diameter. It is the ninth-intrinsical... |
(532037)_2013_FY27_28948729 | Based on the article about '(532037) 2013 FY27', describe the 'Satellite' section. | Using Hubble Space Telescope observations taken in January 2018, Scott Sheppard found a satellite around, 0.17 arcseconds away and 3 mag fainter than the primary. The discovery was announced on 10 August 2018. Assuming the two components have equal albedos, they are about 740 km and 190 km in diameter, respectively. Fo... | [
"(532037) 2013 FY27\n\nis a trans-Neptunian object and binary system that belongs to the scattered disc (like Eris). Its discovery was announced on 31 March 2014. It has an absolute magnitude (H) of 3.2. is a binary object, with two components approximately 740 km and 190 km in diameter. It is the ninth-intrinsical... |
(532037)_2013_FY27_28948727 | Explain what '(532037) 2013 FY27' covers in the 'Orbit' section. | orbits the Sun once every 449 years. It will come to perihelion around November 2202, at a distance of about 35.6 AU. It is currently near aphelion, 80 AU from the Sun, and, as a result, it has an apparent magnitude of 22. Its orbit has a significant inclination of 33Β°. The sednoid and the scattered-disc object were d... | [
"(532037) 2013 FY27\n\nis a trans-Neptunian object and binary system that belongs to the scattered disc (like Eris). Its discovery was announced on 31 March 2014. It has an absolute magnitude (H) of 3.2. is a binary object, with two components approximately 740 km and 190 km in diameter. It is the ninth-intrinsical... |
(53319)_1999_JM8_5396641 | Based on the article about '(53319) 1999 JM8', describe the 'Physical characteristics' section. | In the SMASS and Tholen classification, is an X-type asteroid. It has also been characterized as a carbonaceous C-type asteroid, which seems more likely due to its exceptionally low albedo (see below). | [
"(53319) 1999 JM8 β Physical characteristics\n\nIn the SMASS and Tholen classification, is an X-type asteroid. It has also been characterized as a carbonaceous C-type asteroid, which seems more likely due to its exceptionally low albedo (see below).",
"(53319) 1999 JM8 β Numbering and naming\n\nThis minor planet ... |
(53319)_1999_JM8_5396644 | What information does the article about '(53319) 1999 JM8' provide on 'Numbering and naming'? | This minor planet was numbered by the Minor Planet Center on 16 February 2003. As of 2018, it has not been named. | [
"(53319) 1999 JM8 β Physical characteristics\n\nIn the SMASS and Tholen classification, is an X-type asteroid. It has also been characterized as a carbonaceous C-type asteroid, which seems more likely due to its exceptionally low albedo (see below).",
"(53319) 1999 JM8 β Numbering and naming\n\nThis minor planet ... |
(53319)_1999_JM8_5396643 | Describe the 'Diameter and albedo' section of the article about '(53319) 1999 JM8'. | measures between 5 and 7 kilometers in diameter and its surface has an exceptionally low albedo of 0.02. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.03 and adopts a diameter of 7 kilometers based on an absolute magnitude of 15.2. | [
"(53319) 1999 JM8 β Physical characteristics\n\nIn the SMASS and Tholen classification, is an X-type asteroid. It has also been characterized as a carbonaceous C-type asteroid, which seems more likely due to its exceptionally low albedo (see below).",
"(53319) 1999 JM8 β Numbering and naming\n\nThis minor planet ... |
(53319)_1999_JM8_5396640 | What does the article about '(53319) 1999 JM8' say regarding 'Close approaches'? | has an Earth minimum orbital intersection distance of 0.0235 AU which translates into 9.2 lunar distances. It passed closer than 0.20 AU to the Earth five times in the last century (0.033 AU in 1990), but its next closest approach in the 21st century will be in 2075 at 0.256 au and in August 2137 at 0.0764 au. For comp... | [
"(53319) 1999 JM8 β Physical characteristics\n\nIn the SMASS and Tholen classification, is an X-type asteroid. It has also been characterized as a carbonaceous C-type asteroid, which seems more likely due to its exceptionally low albedo (see below).",
"(53319) 1999 JM8 β Numbering and naming\n\nThis minor planet ... |
(53319)_1999_JM8_5396642 | What does the article about '(53319) 1999 JM8' say regarding 'Rotation period'? | Radar imaging by Goldstone and Arecibo observatories revealed that has an unusually slow and possibly chaotic rotation period, similar to that of asteroid 4179 Toutatis. In July 1999, a rotational lightcurve of was obtained from photometric observations. It gave a period of 136 hours with a brightness amplitude of 0.7 ... | [
"(53319) 1999 JM8 β Physical characteristics\n\nIn the SMASS and Tholen classification, is an X-type asteroid. It has also been characterized as a carbonaceous C-type asteroid, which seems more likely due to its exceptionally low albedo (see below).",
"(53319) 1999 JM8 β Numbering and naming\n\nThis minor planet ... |
(533560)_2014_JM80_21935000 | Explain what '(533560) 2014 JM80' covers in the 'Orbit and classification' section. | celestial mechanics of a scattered-disc object. This has led to some uncertainty as to the current theoretical understanding of the outermost Solar System. The theories include close stellar passages, unseen planet/rogue planets/planetary embryos in the early Kuiper belt, and resonance interaction with an outward-migra... | [
"(533560) 2014 JM80 β Orbit and classification\n\ncelestial mechanics of a scattered-disc object. This has led to some uncertainty as to the current theoretical understanding of the outermost Solar System. The theories include close stellar passages, unseen planet/rogue planets/planetary embryos in the early Kuiper... |
(533560)_2014_JM80_21934999 | Explain what '(533560) 2014 JM80' covers in the 'Orbit and classification' section. | orbits the Sun at a distance of 46.0β80.2 AU once every 500 years and 11 months (182,969 days; semi-major axis of 63.07 AU). Its orbit has an eccentricity of 0.27 and an inclination of 20Β° with respect to the ecliptic. This distant minor planet is a trans-Neptunian object and a member of the scattered disc population. ... | [
"(533560) 2014 JM80 β Orbit and classification\n\ncelestial mechanics of a scattered-disc object. This has led to some uncertainty as to the current theoretical understanding of the outermost Solar System. The theories include close stellar passages, unseen planet/rogue planets/planetary embryos in the early Kuiper... |
(533560)_2014_JM80_21934998 | Summarize the following section from the article on '(533560) 2014 JM80'. | , provisional designation, is a trans-Neptunian object from the scattered disc in the outermost Solar System, approximately 340 km in diameter. It was discovered on 9 May 2010 by astronomers with the Pan-STARRS-1 survey at the Haleakala Observatory, Hawaii, in the United States. According to American astronomer Michael... | [
"(533560) 2014 JM80 β Orbit and classification\n\ncelestial mechanics of a scattered-disc object. This has led to some uncertainty as to the current theoretical understanding of the outermost Solar System. The theories include close stellar passages, unseen planet/rogue planets/planetary embryos in the early Kuiper... |
(5407)_1992_AX_19010094 | What information does the article about '(5407) 1992 AX' provide on 'Satellite'? | During the observations in January 1997, it was also revealed that is a synchronous binary asteroid with a minor-planet moon in its orbit. The satellite measures approximately 780 meters in diameter, or about 20% of its primary, and has an orbital period of 13.52 hours with an estimated semi-major axis of 5.8 kilomete... | [
"(5407) 1992 AX β Satellite\n\nDuring the observations in January 1997, it was also revealed that is a synchronous binary asteroid with a minor-planet moon in its orbit. The satellite measures approximately 780 meters in diameter, or about 20% of its primary, and has an orbital period of 13.52 hours with an estima... |
(5407)_1992_AX_19010095 | From the article on '(5407) 1992 AX', restate the 'Diameter and albedo' content. | According to the surveys carried out by the Japanese Akari satellite, the Spitzer Space Telescope and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), measures between 2.78 and 4.18 kilometers in diameter and its surface has an albedo between 0.199 and 0.40. In 2017, a study by WISE dedicated ... | [
"(5407) 1992 AX β Satellite\n\nDuring the observations in January 1997, it was also revealed that is a synchronous binary asteroid with a minor-planet moon in its orbit. The satellite measures approximately 780 meters in diameter, or about 20% of its primary, and has an orbital period of 13.52 hours with an estima... |
(5407)_1992_AX_19010092 | Based on the article about '(5407) 1992 AX', describe the 'Physical characteristics' section. | has been characterized as a common, stony S-type asteroid. In the SMASS taxonomy, it is an Sk-subtype, that transitions between the S and K-type asteroids. The body's color indices of 0.690 (BβV), 0.500 (VβR) and 0.840 (VβI) were also determined. | [
"(5407) 1992 AX β Satellite\n\nDuring the observations in January 1997, it was also revealed that is a synchronous binary asteroid with a minor-planet moon in its orbit. The satellite measures approximately 780 meters in diameter, or about 20% of its primary, and has an orbital period of 13.52 hours with an estima... |
(5407)_1992_AX_19010093 | Describe the 'Rotation period' section of the article about '(5407) 1992 AX'. | Since 1997, several rotational lightcurves of have been obtained from photometric observations by Petr Pravec and collaborating astronomers. Best-rated lightcurve analysis gave a rotation period of 2.5488 hours with a consolidated brightness amplitude between 0.10 and 0.12 magnitude (U=2/3). The results supersedes a t... | [
"(5407) 1992 AX β Satellite\n\nDuring the observations in January 1997, it was also revealed that is a synchronous binary asteroid with a minor-planet moon in its orbit. The satellite measures approximately 780 meters in diameter, or about 20% of its primary, and has an orbital period of 13.52 hours with an estima... |
(5407)_1992_AX_19010090 | Reconstruct the content about 'Orbit and classification' from the article on '(5407) 1992 AX'. | a member of the Mars-crossing asteroids, a dynamically unstable group between the main belt and the near-Earth populations, crossing the orbit of Mars at 1.66 AU. It orbits the Sun at a distance of 1.3β2.3 AU once every 2 years and 6 months (910 days; semi-major axis of 1.84 AU). Its orbit has an eccentricity of 0.28 a... | [
"(5407) 1992 AX β Satellite\n\nDuring the observations in January 1997, it was also revealed that is a synchronous binary asteroid with a minor-planet moon in its orbit. The satellite measures approximately 780 meters in diameter, or about 20% of its primary, and has an orbital period of 13.52 hours with an estima... |
(5407)_1992_AX_19010089 | What information does the article about '(5407) 1992 AX' provide? | ''', provisional designation ', is a stony asteroid and a synchronous binary Mars-crosser from the innermost region of the asteroid belt, approximately 3.6 km in diameter. It was discovered on 4 January 1992, by Japanese astronomers Seiji Ueda and Hiroshi Kaneda at the Kushiro Observatory on HokkaidΕ, Japan. The S-type... | [
"(5407) 1992 AX β Satellite\n\nDuring the observations in January 1997, it was also revealed that is a synchronous binary asteroid with a minor-planet moon in its orbit. The satellite measures approximately 780 meters in diameter, or about 20% of its primary, and has an orbital period of 13.52 hours with an estima... |
(543354)_2014_AN55_20456519 | What does the article about '(543354) 2014 AN55' say regarding 'Orbit and classification'? | belongs to the gravitationally perturbed population of scattered disc objects, which, at their closest approaches, come close to Neptune's orbit at 30 AU, but their farthest distances reach many times of that. It orbits the Sun at a distance of 34.3β77.6 AU once every 418 years and 2 months (152,739 days; semi-major ax... | [
"(543354) 2014 AN55 β Orbit and classification\n\nbelongs to the gravitationally perturbed population of scattered disc objects, which, at their closest approaches, come close to Neptune's orbit at 30 AU, but their farthest distances reach many times of that. It orbits the Sun at a distance of 34.3β77.6 AU once eve... |
(543354)_2014_AN55_20456521 | What does the article about '(543354) 2014 AN55' say regarding 'Diameter and albedo'? | Using an absolute magnitude of 4.3 from the AsteroidsβDynamic Site, and assuming an albedo in the range of 0.05 to 0.25, the object's mean-diameter may be as low as 370, and as high as 820 kilometers. Johnstonss Archive assumes a similar albedo of 0.9 and calculates a diameter of 671 kilometers using an absolute magnit... | [
"(543354) 2014 AN55 β Orbit and classification\n\nbelongs to the gravitationally perturbed population of scattered disc objects, which, at their closest approaches, come close to Neptune's orbit at 30 AU, but their farthest distances reach many times of that. It orbits the Sun at a distance of 34.3β77.6 AU once eve... |
(543354)_2014_AN55_20456520 | Reconstruct the content about 'Numbering and naming' from the article on '(543354) 2014 AN55'. | This minor planet was numbered by the Minor Planet Center on 5 February 2020 (M.P.C. 121072) and has not yet received a name. | [
"(543354) 2014 AN55 β Orbit and classification\n\nbelongs to the gravitationally perturbed population of scattered disc objects, which, at their closest approaches, come close to Neptune's orbit at 30 AU, but their farthest distances reach many times of that. It orbits the Sun at a distance of 34.3β77.6 AU once eve... |
(5496)_1973_NA_20217447 | What does the article about '(5496) 1973 NA' say regarding 'Physical characteristics'? | The stony S-type asteroid is also classified as a transitional C/X-type according to observations by the NASA IRTF telescope. A rotational lightcurve for this asteroid was obtained by American astronomer Brian Skiff from photometric observations made in June 2011. Lightcurve analysis gave a well-defined rotation period... | [
"(5496) 1973 NA β Physical characteristics\n\nThe stony S-type asteroid is also classified as a transitional C/X-type according to observations by the NASA IRTF telescope. A rotational lightcurve for this asteroid was obtained by American astronomer Brian Skiff from photometric observations made in June 2011. Light... |
(5496)_1973_NA_20217445 | Reconstruct the content about 'Parent of the Quadrantids' from the article on '(5496) 1973 NA'. | is a possible parent body of the Quadrantids, a major meteor shower that occurs every January. It may also be just a fragment of the parent or the dormant remains of the parent. Other possible parent bodies are and comet 96P/Machholz, as well as. | [
"(5496) 1973 NA β Physical characteristics\n\nThe stony S-type asteroid is also classified as a transitional C/X-type according to observations by the NASA IRTF telescope. A rotational lightcurve for this asteroid was obtained by American astronomer Brian Skiff from photometric observations made in June 2011. Light... |
(5496)_1973_NA_20217444 | Summarize the following section from the article on '(5496) 1973 NA'. | (5496) 1973 NA, is a very eccentric and heavily tilted asteroid, classified as near-Earth object of the Apollo group, approximately 2 kilometers in diameter. It was discovered on 4 July 1973, by American astronomer Eleanor Helin at the U.S. Palomar Observatory in California. At the time of its discovery, it was the mos... | [
"(5496) 1973 NA β Physical characteristics\n\nThe stony S-type asteroid is also classified as a transitional C/X-type according to observations by the NASA IRTF telescope. A rotational lightcurve for this asteroid was obtained by American astronomer Brian Skiff from photometric observations made in June 2011. Light... |
(55637)_2002_UX25_23681080 | Reconstruct the content from the article about '(55637) 2002 UX25'. | is a trans-Neptunian object that orbits the Sun in the Kuiper belt beyond Neptune. This TNO briefly garnered scientific attention when it was found to have an unexpectedly low density of about 0.82 g/cm3. has an absolute magnitude of about 4.0, and Spitzer Space Telescope results estimate it to be about 681 km in diame... | [
"(55637) 2002 UX25\n\nis a trans-Neptunian object that orbits the Sun in the Kuiper belt beyond Neptune. This TNO briefly garnered scientific attention when it was found to have an unexpectedly low density of about 0.82 g/cm3. has an absolute magnitude of about 4.0, and Spitzer Space Telescope results estimate it t... |
(55637)_2002_UX25_23681085 | From the article on '(55637) 2002 UX25', restate the 'Satellite' content. | The discovery of a minor-planet moon was reported in IAUC 8812 on 22 February 2007. The satellite was detected using the Hubble Space Telescope in August 2005. The satellite was found at 0.16 arcsec from the primary with an apparent magnitude difference of 2.5. It orbits the primary in 8.309 days, at a distance of 4,77... | [
"(55637) 2002 UX25\n\nis a trans-Neptunian object that orbits the Sun in the Kuiper belt beyond Neptune. This TNO briefly garnered scientific attention when it was found to have an unexpectedly low density of about 0.82 g/cm3. has an absolute magnitude of about 4.0, and Spitzer Space Telescope results estimate it t... |
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