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Zons [SEP] North of ferry slip and ship pier begins the nature reserve "Zonser Grind" on the western bank of the Rhine. The first time Zons was mentioned in a document is in the so-called last will and testament of Cunibert, Bishop of Cologne, which was written in the middle of the seventh century but is only known in a version of the late eleventh century. In the document the names of "Zuonizo" or "Zuonize" are mentioned with their origin still unclear until today.

Zons [SEP] In a deed of gift of Archbishop Heribert of Cologne the name of Zons appears in a location reference, „Burgula bei "Zünce"“ (Burgula near Zünce)., Burgula being the site of today's "Haus Bürgel", an old mansion built on the ruins of a Roman settlement. Archaeological finds indicate that there was a Merovingian settlement in Zons in the seventh century, yet its exact location is not determined.

Zons [SEP] Documents verify a "Fronhof" of the archbishop of Cologne (Fronhof = estate of a feudal lord receiving socage) existing in Zons at least since the beginning of the twelfth century . In the 1980s archaeological excavations in the castle area uncovered foundations of buildings which are regarded as remains of the proprietary church of the lord of the manor which was part of the building complex of the "Fronhof". At about the middle of the thirteenth century Zons "castrum" (castle) was fortified.

Zons [SEP] The location of the older rural settlement of Zons can only be presumed based on field-names and topography. The field-name „Im Hofstädtchen“ at today's Aldenhovenstraße near the Old Town could reference to this settlement with the crossing paths at this spot being a possible additional indicator. In 1372 the Archbishop of Cologne Friedrich III. of Saarwerden moved the Rhine toll castle from Neuss upstream to Zons protecting it with walls and moats and granting Zons the town privileges in 1373.

Zons [SEP] At the centre of the fortress was the thick fortified Friedestrom Castle which served the administration and protection of the toll and housed the administration of the new parish Zons. The obviously planned building of the toll fortress with town walls was finished probably in the 15th century. The rectangular to trapeziform town layout is surrounded by a wall strengthened with basalt stones. The wall stretches in north–south direction over about and in west–east direction over .

Zons [SEP] At the corners are towers built in different shapes: to the northeast the rectangular Rhein-, Zoll- or Peters-Turm (Rhine, Toll or Peters Tower); to the northwest the circular Krötschenturm (Krötschen Tower); to the southwest the circular Mühlenturm (Mill Tower), which was converted from a defensive tower to a tower mill as late as the Late Middle Ages; to the southeast the Schlossturm (Palace Tower) and in town at the castle wall the circular Juddeturm (Judde Tower: high, roof starts at height, baroque roof ).

Zons [SEP] The name "Juddeturm" probably refers to the patrician family Jude in Cologne. Two public gates gave access to the town: in the north the Rheintor (Rhine Gate), in the west the Feldtor (Field Gate). During the 19th century the first was partly, the latter almost entirely dismantled. A third outer gate, the Südtor (South Gate), which is preserved best, is the entrance from the "zwinger" (enclosed killing ground) to the Vorburg (lower ward).

Zons [SEP] The small town had only 124 plots for houses. The parish Zons comprised also the village Stürzelberg, part of the village Horrem and the village of Haus Bürgel, which is nowadays located on the opposite banks of the river Rhine. Regarding church and court of justice matters Haus Bürgel and Zons originally belonged together. The canon law for the parish Bürgel/Zons was governed by Brauweiler Abbey.

Zons [SEP] Already in 1374 Bürgel was moved from the west banks to east banks of the Rhine, probably due to a shift of the river. Zons, the Rhine toll town of the Prince-elector of Cologne is regarded as one of the best preserved Lower Rhine planned towns of the Late Middle Ages.

Zons [SEP] Until 1794 the parish Zons belonged to the Electorate of Cologne and was bordered in the south by Dormagen, an enclave ruled by the Duchy of Jülich; in the south-west by Hackenbroich, a lordship within the Electorate of Cologne; in the west by Nievenheim, a parish within the Electorate of Cologne; in the north-west by Uedesheim, another lordship within the Electorate of Cologne.

Zons [SEP] On the opposite banks of the Rhine were Urdenbach and Baumberg, "Honschaften" (lowest level administrative units similar to hundreds in England and Wales) within the Duchy of Berg. In 1463 Archbishop of Cologne Dietrich II. of Moers mortgaged town and parish Zons to the cathedral chapter of Cologne. Its reign lasted until 1794, when the French Revolutionary Army occupied the territory west of the Rhine. Zons became a French municipality and canton.

Zons [SEP] From 1798 to 1814 it was part of the canton Dormagen within the Arrondissement de Cologne which belonged to the Département de la Roer. With the Treaty of Lunéville in 1801 the occupied territory on the left bank of the Rhine came to France under public international law. As result of the Congress of Vienna Zons became part of the Prussian State in 1815.

Zons [SEP] The following year the district Neuss was set up with the "Bürgermeisterei" Zons (an administrative level similar to an Amt) which comprised the municipalities of Zons, Nachtigall, St. Peter and Stürzelberg. In 1882 the district Neuss became part of the Regierungsbezirk Düsseldorf in the Rhine Province. Since about 1900 Zons has been a popular destination for pleasure trips. In 1904 the municipality Zons was granted its own coat of arms.

Zons [SEP] Since then Zons was called again „Town”, despite the fact that it still belonged to the Prussian rural municipalities regarding administrative law. With the incorporation into the town limits of Dormagen with effect of 1 Januar 1975 Zons called itself „Feste“ (Fortress). In 1992 Zons again gained the description „Town”, though only as Titularstadt (titular town). Already in 1972 the whole Old Town underwent an extensive renovation in an exemplary project sponsored by Federal State and Federated State.

Zons [SEP] Since the 14th century Zons didn't change much regarding town area and population, probably due to its disadvantageous access to road traffic. During the course of the centuries the town was stricken three times by great fires: 1464, 1547 and 1620. Before the last great fire there were reports about a certain flourishing in economic terms due to trading. Yet the 17th century turned out to be a painful one for Zons.

Zons [SEP] Economic and demographic decline ensue after that great fire, an (unsuccessful) siege and heavy bombardment at the end of the Thirty Years' War, several disastrous plagues and frequent occupations by Cologne and French troops. 1648 Zons had a population of 172, Stürzelberg of 49. After a gradual increase in population in the parish Zons 255 people died due to the plague in 1666.

Zons [SEP] From about 1700 there was a noticeable increase in population: in 1692 the parish had a population of 308, in 1738 there were already 831 people who had received the First Communion and eventually in 1799 there was a population of 1,054. In the 18th century the population was almost entirely Catholic. During that time only a few Jewish families lived in Zons increasing in numbers to almost 50 people by 1806.

Zons [SEP] During the course of 19th century up to the beginning of the 20th century the population grew relatively slowly yet almost steadily in comparison to the overall demographic development. In 1849 Zons together with Stürzelberg counted for 2,012 people, in 1928 1,306 people lived in Zons and 1,428 in Stürzelberg, thus 2,734 in total. On 30 June 1964 the at that time “town” Zons (comprising also the villages of Stürzelberg, St. Peter und Nachtigall) had a population of 6,310 which increased to 9,715 on 30 June 1974.

Zons [SEP] Population Development in Quarter Zons: From 1904 until the incorporation into the town of Dormagen Zons had its own coat of arms. Blazon: “Gules a saint argent on a horse cutting his cloak with a sword to share it with a scantily clad man standing in front of him, on a canton argent a cross sable. “ As town coat of arms it is oftén depicted with a silver three-towered battlement coping including a black gate in the middle placed on the top (chief) of the escutcheon.

Zons [SEP] Coat of arms explanation: The saint is Martin of Tours, the black cross on a silver background is the coat of arms of the Electorate of Cologne. Up to the modern era the people of Zons earned their living in farming. In addition to that the trade of grain, beer and wine as well as some crafts like brick-making had partly an importance beyond the parish borders. The people of the village Stürzelberg worked mostly as fishermen or day labourers.

Zons [SEP] A privileged group by wealth and social background were the toll collectors until around 1800. They had no civil rights, therefore they were freed from serving civil duties. At the beginning of the 20th century an industrial plant was established near Stürzelberg and St. Peter. In Zons itself industrial activities didn't happen. Housing in Zons town expanded relatively late beyond the town walls. The first residential buildings "extra muros" were erected at the beginning of the 19th century.

Zons [SEP] First housing estates can be found only at the end of the 19th century. At first buildings were concentrated at the paths immediate to the fortress. Later, especially after World War II, housing spread out to the north and the west of the Old Town. Zons is located east of Bundesstraße 9. The distance from Zons to junction „Dormagen, Nievenheim, Zons“ of the Bundesautobahn 57 is . A car ferry runs frequently between Zons und Düsseldorf-Urdenbach.

Zons [SEP] The river cruise operator Köln-Düsseldorfer offers day excursions to Zons from Cologne and Düsseldorf on selected days during the summer. The following lines within the VRR run through Zons:

Uzarzewo [SEP] Uzarzewo () is a village in the administrative district of Gmina Swarzędz, within Poznań County, Greater Poland Voivodeship, in west-central Poland. It lies approximately north-east of Swarzędz and east of the regional capital Poznań. The village has a population of 580. It is the site of a Museum of Natural Environment and Hunting, under the auspices of the National Museum of Agriculture in Szreniawa. It also has a church which lies on the Wooden Churches Trail around Puszcza Zielonka. br

(225088) 2007 OR10 [SEP] , unofficially known as Gonggong, is a possible dwarf planet orbiting the Sun beyond Neptune. It is a member of the scattered disc, a high-eccentricity population of trans-Neptunian objects (TNOs). It was discovered in July 2007 by American astronomers Megan Schwamb, Michael Brown, and David Rabinowitz at the Palomar Observatory. The discovery was announced in January 2009.

(225088) 2007 OR10 [SEP] At in diameter, is the fifth-largest known body in the Solar System beyond the orbit of Neptune and is expected to have a gravitationally rounded shape, thereby qualifying for dwarf planet status. It is currently the largest known body in the Solar System without an official name. In 2019, the discoverers hosted an online poll for the general public to choose among three suggested names. Gonggong was announced as the winner. The discovery team plans to submit the name to the International Astronomical Union.

(225088) 2007 OR10 [SEP] was discovered by American astronomers Megan Schwamb, Michael Brown and David Rabinowitz on 17 July 2007. The discovery was part of the Palomar Distant Solar System Survey, a survey conducted to find distant objects in the region of , beyond 50 astronomical units (AU) from the Sun, using the Samuel Oschin telescope at Palomar Observatory near San Diego, California. The survey was designed to detect the movements of objects out to at least 1,000 astronomical units from the Sun.

(225088) 2007 OR10 [SEP] Schwamb identified by comparing multiple images using the blinking technique. In the discovery images, appeared to move slowly, suggesting that it is a distant object. The discovery was part of Schwamb's doctoral thesis. At that time, Schwamb was a graduate student of Michael Brown at Caltech. is currently the largest known object in the Solar System without an official name.

(225088) 2007 OR10 [SEP] Initially after the discovery of , Brown nicknamed the object "Snow White" for its presumed white color, because it would have to be very large or very bright to be detected by their survey. By that time, Brown's team had already discovered seven large trans-Neptunian objects which were collectively referred to as the "seven dwarfs": in 2002, in 2003, , and in 2004, and and in 2005.

(225088) 2007 OR10 [SEP] However, turned out to be very red in color, comparable to Quaoar, so the nickname was dropped. On 2 November 2009, two years after its discovery, the Minor Planet Center assigned the minor planet number 225088 to . The discoverers were given a 10-year period for naming proposals following the numbering of the object. was assigned its minor planet number in November 2009, hence the discoverers were given the privilege to propose a name until November 2019.

(225088) 2007 OR10 [SEP] Upon the discovery and announcement of , Brown did not consider naming it as he regarded it to be an unremarkable object despite its large size. In 2011, Brown declared that he now had enough information to justify giving it a name, in consideration of the discovery of water ice and the possibility of methane on its surface, which made it noteworthy enough to warrant further study.

(225088) 2007 OR10 [SEP] In 2016, in response to the larger size revisions of made in that same year, Schwamb remarked: In 2019, the discoverers of hosted an online poll for the general public to choose between three possible names they thought appropriate: Gonggong (Chinese), Holle (German), and Vili (Norse).

(225088) 2007 OR10 [SEP] These names were selected by the discoverers in accordance to the International Astronomical Union's (IAU's) minor planet naming criteria, which state that objects with orbits like that of must be given names related to mythological figures that are associated with creation. The three options were also picked because they are associated with water, ice, snow, and the color red, which are all characteristics of . The voting session ended on 10 May 2019, with Gonggong being the most voted name.

(225088) 2007 OR10 [SEP] The satellite of will not be named by the hosts of the naming poll as the naming privilege for the satellite of is reserved to the discoverers of the satellite. On 29 May 2019, the discovery team announced Gonggong as the winning name, with a plurality of 46 percent of the 280,000 votes casted during the voting session. The discovery team will propose the winning name to the IAU's Committee of Small Body Nomenclature, the institution that is responsible for naming minor planets.

(225088) 2007 OR10 [SEP] The name is derived from Gonggong, a Chinese water god depicted as having a red-haired human head and the body of a serpent. In Chinese mythology, Gonggong was responsible for creating chaos, causing flooding, and tilting the Earth, and was sent into exile. The surface of is red in color. It has an albedo (reflectivity) of .

(225088) 2007 OR10 [SEP] The surface composition and spectrum of is expected to be similar to that of , as both objects are red and display signs of water ice and possibly methane in their spectra. The spectrum of was first measured in 2011, at near-infrared wavelengths using the Folded port InfraRed Echellette (FIRE) spectrograph on the Magellan Baade Telescope at the Las Campanas Observatory in Chile. The observed spectrum of exhibits a strong red spectral slope along with broad absorption bands at wavelengths of 1.5 μm and 2 μm.

(225088) 2007 OR10 [SEP] Additional photometric measurements from the Hubble Space Telescope's Wide Field Camera 3 instrument display similar water ice absorption bands at 1.5 μm. These absorption bands are characteristic features of water ice, which is often found on large Kuiper belt objects. The presence of water ice on the surface of implies a brief period of cryovolcanism in the distant past when water erupted from its interior, deposited onto its surface, and subsequently froze.

(225088) 2007 OR10 [SEP] The red color of is unexpected for an object with a substantial amount of water ice on its surface. Objects with surfaces rich in water ice are typically neutral in color, hence was initially nicknamed "Snow White" for its presumed bright and reflective surface. is among the reddest objects known. Its red color implies that methane is present on its surface, although it was not directly detected in the spectrum of due to the low signal-to-noise ratio of the data.

(225088) 2007 OR10 [SEP] The red color results from methane frost that are irradiated by sunlight and cosmic rays. The photolysis of methane on its surface produces reddish organic compounds known as tholins. The size of an object can be calculated from its absolute magnitude (brightness) and albedo. has an absolute magnitude (H) of 2.34, which makes it the seventh-brightest trans-Neptunian object known.

(225088) 2007 OR10 [SEP] Other sources give an absolute magnitude of 1.8, which would make it the fifth brightest trans-Neptunian object, brighter than Sedna (H=1.83; D=995 km) and (H=2.31; D=917 km). Due to its large distance of 88 astronomical units from the Sun, the apparent magnitude of is only 21.5, too dim to be seen from Earth with the naked eye. It is dimmer than Sedna, which has an apparent magnitude of 20.9.

(225088) 2007 OR10 [SEP] The presence of tholins on the surface of implies the existence of a tenuous methane atmosphere slowly escaping into space, analogous to Quaoar. Although occasionally comes closer to the Sun than Quaoar, and is thus warm enough that a methane atmosphere should evaporate, its larger mass makes retention of an atmosphere just possible. Its low surface albedo may contribute to the loss of volatiles such as nitrogen, since a lower albedo corresponds to more light being absorbed by the surface rather than being reflected, thus resulting in greater surface heating.

(225088) 2007 OR10 [SEP] is thought to have had cryovolcanic activity along with a more substantial atmosphere shortly after its formation. Such cryovolcanic activity is expected to have been brief, and the resulting atmosphere gradually escaped over time. Volatile gases, such as nitrogen and carbon monoxide, were lost, while less volatile gases such as methane are likely to remain in its present tenuous atmosphere. As of 2019, is estimated to have a diameter of , derived from radiometric measurements, its calculated mass, and assuming a density similar to other similar bodies.

(225088) 2007 OR10 [SEP] This would make the fifth-largest trans-Neptunian object, after Pluto, Eris, Haumea, and Makemake. is probably larger than both Pluto's moon Charon and the large Kuiper belt object Quaoar, which have diameters of and , respectively. Due to its large size, it is very likely a dwarf planet. The International Astronomical Union has not addressed the possibility of accepting additional dwarf planets since before the announcement of the discovery of .

(225088) 2007 OR10 [SEP] Brown states that "must be a dwarf planet even if predominantly rocky", as his 2013 radiometric measurement of is large enough to certainly qualify as a dwarf planet.

(225088) 2007 OR10 [SEP] Scott Sheppard and his colleagues think that it is "likely" to be a dwarf planet, based on its minimum possible diameter (580 km under the assumption of an albedo of 1) 10^{-0.2H}, where formula_1 is the absolute magnitude of , and formula_2 is the albedo of , which in this case is assumed to be 1.|name=magnitude|group=lower-alpha}} and the expected lower size limit of around for hydrostatic equilibrium in cold icy-rocky bodies.

(225088) 2007 OR10 [SEP] In 2010, Tancredi initially estimated to have a very large diameter of , though its dwarf planet status was unclear as there was no lightcurve data and other information to ascertain its size. is too distant to be resolved directly; Brown placed a rough estimate of its diameter ranging from to , based on an albedo of 0.18 that is the best fit in his model.

(225088) 2007 OR10 [SEP] A survey led by a team of astronomers using the European Space Agency's Herschel Space Observatory in 2012 determined its diameter to be with an uncertainty of , based on the thermal properties of observed in the far infrared range. This measurement is consistent with Brown's estimate of . Later observations in 2013 using combined thermal emission data from "Herschel" and the Spitzer Space Telescope provided a smaller size estimate of , though this estimate had a larger range of uncertainty.

(225088) 2007 OR10 [SEP] In 2016, combined observations from the "Kepler" spacecraft and archival thermal emission data from "Herschel" suggested that was much larger than previously thought, giving a size estimate of based on an assumed equator-on view and a lower estimated albedo of 0.089. This would have made the third-largest trans-Neptunian object after Eris and Pluto, larger than Makemake (). These observations of were part of the "Kepler" spacecraft's K2 mission which includes studying small Solar System bodies.

(225088) 2007 OR10 [SEP] Subsequent measurements in 2018 revised the size of to , based on the mass and density of derived from the orbit of its satellite and the discovery that the viewing direction was almost pole-on. With this more recent size estimate, is again thought to be the fifth-largest trans-Neptunian object. Based on the orbit of its satellite, the mass of has been calculated to be , with a density of .

(225088) 2007 OR10 [SEP] From these mass and density estimates, the size of was calculated to be about , smaller than the previous 2016 size estimate of . Given the mass of , the 2016 size estimate of would have implied an unexpectedly low (and likely erroneous) density of . The rotation period of was first measured in March 2016, by observing variations in its brightness using the "Kepler" space telescope. The "Kepler" observations provided two possible values of and hours for the rotation period.

(225088) 2007 OR10 [SEP] The value of hours is thought to be the more plausible one. rotates slowly compared to other trans-Neptunian objects, which usually have rotation periods between 6 and 12 hours. Due to its slow rotation, it is expected to have a low oblateness of 0.03 or 0.007, for rotation periods of 22.4 or 44.81 hours, respectively. The slow rotation period led astronomers to speculate that the rotation of was slowed down by tidal forces exerted by an orbiting satellite, which was confirmed later that same year.

(225088) 2007 OR10 [SEP] orbits the Sun at an average distance of 67.4 AU and completes a full orbit in 553 years. The orbit of is highly inclined to the ecliptic, with an orbital inclination 30.7 degrees. Its orbit is also highly eccentric, with a measured orbital eccentricity of 0.503.

(225088) 2007 OR10 [SEP] Due to its highly eccentric orbit, the distance of from the Sun varies greatly over the course of its orbit, from 101.3 AU at aphelion, its furthest point from the Sun, to around 33.5 AU at perihelion, its closest point to the Sun. had approached its perihelion in 1857 and is currently moving farther from the Sun, toward its aphelion. The Minor Planet Center lists it as a scattered disc object for its eccentric and distant orbit.

(225088) 2007 OR10 [SEP] The Deep Ecliptic Survey shows the orbit of to be in a 3:10 resonance with Neptune; completes three orbits around the Sun for every ten orbits completed by Neptune. , is located from the Sun and is moving away at a speed of .

(225088) 2007 OR10 [SEP] It is currently the sixth-farthest known Solar System object from the Sun, preceding (89.5 AU), (90.4 AU), (96.1 AU), (~ 120 AU), and "FarFarOut" (~ 140 AU). is currently more distant than , which is located 84.8 AU from the Sun as of July 2019. It has been farther from the Sun than Sedna since 2013.

(225088) 2007 OR10 [SEP] will be farther than both Sedna and Eris by 2045, and will approach its aphelion in 2130. It was calculated that a flyby mission to could take just under 25 years using a Jupiter gravity assist, based on a launch date of 2030 or 2031. would be approximately 95 AU from the Sun when the spacecraft arrives. has a single known moon, S/2010 (225088) 1.

(225088) 2007 OR10 [SEP] It was first identified in 2016 by a team of astronomers led by Csaba Kiss, in archival images taken on 18 September 2010 with the Hubble Space Telescope. The discovery was announced on 17 October 2016. S/2010 (225088) 1 is estimated to be less than in diameter, implying an albedo above 0.2. The absolute magnitude of the moon is estimated to be , at least 4.59 magnitudes dimmer than (given an absolute magnitude of 2.34 for the primary).

(225088) 2007 OR10 [SEP] It is not yet possible to determine whether the orbit of the satellite is prograde or retrograde. Based on a prograde orbit model, the satellite orbits the primary at a distance of around and completes one orbit in 25.22 days. The satellite is believed to be tidally locked to the primary. Using the same prograde orbit model, the discovery team estimates that its orbit is inclined to the ecliptic by about 83 degrees.

(225088) 2007 OR10 [SEP] Assuming that the orbit has a low inclination to the primary's equator, this implies that is being viewed at a nearly pole-on configuration. The moon's orbit has an eccentricity of 0.29. Following the March 2016 discovery that was an unusually slow rotator, the possibility was raised that a satellite may have slowed it down via tidal forces. The indications of a possible satellite orbiting led Csaba Kiss and his team to analyze archival Hubble observations of .

(225088) 2007 OR10 [SEP] Their analysis of Hubble images taken on 18 September 2010 revealed a faint satellite orbiting at a distance of at least . Upon further analysis of archival images, the discovery team later also identified the satellite in Hubble images taken on 9 November 2009. From these images taken in 2009 and 2010, the mean brightness difference between the satellite and the primary was calculated to be magnitudes. The discovery team was unable to determine the satellite's exact orbit from these two images.

(225088) 2007 OR10 [SEP] Further observations in 2017 with the Hubble Space Telescope's Wide Field Camera 3 were carried out to determine the orbit of the moon as well as the mass and density of . From these observations, the absolute magnitude of the moon was estimated at , at least 4.59 magnitudes dimmer than (given an absolute magnitude of 2.34 for the primary). Based on Hubble images of and its satellite taken in 2009 and 2010, the discovery team constrained the satellite's orbital period to between 20 and 100 days.

(225088) 2007 OR10 [SEP] To further determine the orbit, they used Hubble in 2017 to observe the satellite's motion around . Because the observations of the satellite only span a small fraction of 's orbit around the Sun, it is not yet possible to determine whether the orbit of the satellite is prograde or retrograde. Based on a prograde orbit model, the satellite orbits the primary at a distance of around and completes one orbit in 25.22 days. The satellite is believed to be tidally locked to the primary.

(225088) 2007 OR10 [SEP] Using the same prograde orbit model, the discovery team estimates that its orbit is inclined to the ecliptic by about 83 degrees. Assuming that the orbit has a low inclination to the primary's equator, this implies that is being viewed at a pole-on configuration. The orbit of the moon is highly eccentric, with an eccentricity of 0.29. This high eccentricity is thought to be caused either by an intrinsically eccentric orbit and slow tidal evolution, or by the Kozai mechanism.

(225088) 2007 OR10 [SEP] The Kozai mechanism can be driven by perturbations either from the Sun's tidal forces, or from higher order terms in the gravitational potential of due to its oblate shape. The dynamics of the moon's orbit are similar to that of Quaoar's satellite Weywot, which has a moderate eccentricity of about 0.14. Based on dynamical models of the moon's orbit, it is estimated to be less than in diameter, implying an albedo above 0.2.

(225088) 2007 OR10 [SEP] Upon its discovery, the satellite's diameter was initially estimated at , under the assumption that the albedos of the satellite and the primary were equal. Photometric measurements in 2017 show that the satellite is far less red than the primary. The color difference of = between the primary (V–I=) and satellite (V–I=) is the largest among all known binary trans-Neptunian objects.

(225088) 2007 OR10 [SEP] This large color difference is atypical for trans-Neptunian binary systems; the components of most trans-Neptunian binaries display little color variation, unlike the system.

Bengtesgård meadow [SEP] Bengtesgård meadow () is a nature reserve in Falkenberg Municipality, Sweden. It has an area of and has been protected since 1972. Hawfinches nest in the area and another red-listed species, "Grifola frondosa", can be found on the ground.

Laughing kookaburra [SEP] The laughing kookaburra ("Dacelo novaeguineae") is a bird in the kingfisher subfamily Halcyoninae. It is a large robust kingfisher with a whitish head and a dark eye-stripe. The upperparts are mostly dark brown but there is a mottled light-blue patch on the wing coverts. The underparts are white and the tail is barred with rufous and black. The plumage of the male and female birds is similar.

Laughing kookaburra [SEP] The territorial call is a distinctive laugh that is often delivered by several birds at the same time, and is widely used as a stock sound effect in situations that involve a jungle setting. The laughing kookaburra is native to eastern mainland Australia, but has also been introduced to parts of New Zealand, Tasmania, and Western Australia. It occupies dry eucalypt forest, woodland, city parks and gardens. This species is sedentary and occupies the same territory throughout the year.

Laughing kookaburra [SEP] It is monogamous, retaining the same partner for life. A breeding pair can be accompanied by up to five fully grown non-breeding offspring from previous years that help the parents defend their territory and raise their young. The laughing kookaburra generally breeds in unlined tree holes or in excavated holes in arboreal termite nests. The usual clutch is three white eggs. The parents and the helpers incubate the eggs and feed the chicks. The youngest of the three nestlings or chicks is often killed by the older siblings.

Laughing kookaburra [SEP] When the chicks fledge they continue to be fed by the group for six to ten weeks until they are able to forage independently. A predator of a wide variety of small animals, the laughing kookaburra typically waits perched on a branch until it sees an animal on the ground and then flies down and pounces on its prey. Its diet includes lizards, insects, worms, snakes and are known to take goldfish out of garden ponds.

Laughing kookaburra [SEP] The International Union for Conservation of Nature (IUCN) has classed the laughing kookaburra as a species of least concern as it has a huge range and large population, with no widespread threats. The laughing kookaburra was first described and illustrated (in black and white) by the French naturalist and explorer Pierre Sonnerat in his "Voyage à la nouvelle Guinée" which was published in 1776. He claimed to have seen the bird in New Guinea.

Laughing kookaburra [SEP] In fact Sonnerat never visited New Guinea and the laughing kookaburra does not occur there. He probably obtained a preserved specimen from one of the naturalists who accompanied Captain James Cook to the east coast of Australia. Edme-Louis Daubenton and François-Nicolas Martinet included a coloured plate of the laughing kookaburra based on Sonnerat's specimen in their "Planches enluminées d'histoire naturelle". The plate has the legend in French ""Martin-pecheur, de la Nouvelle Guinée"" (Kingfisher from New Guinea).

Laughing kookaburra [SEP] In 1783, the French naturalist Johann Hermann provided a formal description of the species based the coloured plate by Daubenton and Martinet. He gave it the scientific name "Alcedo novæ Guineæ". The current genus "Dacelo" was introduced in 1815 by the English zoologist William Elford Leach, and is an anagram of "Alcedo", the Latin word for a kingfisher.

Laughing kookaburra [SEP] The specific name "novaeguineae" combines the Latin "novus" for new with Guinea, based on the erroneous belief that the specimen had originated from New Guinea. For many years it was believed that the earliest description was by the Dutch naturalist Pieter Boddaert and his scientific name "Dacelo gigas" was used in the scientific literature but in 1926 the Australian ornithologist Gregory Mathews showed that a description by Hermann had been published earlier in the same year, 1783, and thus had precedence.

Laughing kookaburra [SEP] In the 19th century this species was commonly called the "laughing jackass", a name first recorded (as Laughing Jack-Ass) in "An Account of the English Colony in New South Wales" by David Collins which was published in 1798. In 1858 the ornithologist John Gould used "great brown kingfisher", a name that had been coined by John Latham in 1782. Another popular name was "laughing kingfisher".

Laughing kookaburra [SEP] The name in several Australian indigenous languages were listed by European authors including "Go-gan-ne-gine" by Collins in 1798, "Cuck'anda" by René Lesson in 1828 and "Gogera" or "Gogobera" by George Bennett in 1834.

Laughing kookaburra [SEP] In the early years of the 20th century "kookaburra" was included as an alternative name in ornithological publications but it was not until 1926 in the second edition of the "Official Checklist of Birds of Australia" that the Royal Australasian Ornithologists Union officially adopted the name "laughing kookaburra". The name comes from Wiradhuri, an endangered Aboriginal language. The genus "Dacelo" contains four kookaburra species of which the rufous-bellied kookaburra and the spangled kookaburra are restricted to New Guinea and islands in the Torres Straits.

Laughing kookaburra [SEP] The blue-winged kookaburra and the laughing kookaburra are both widespread in Australia. Two subspecies are recognised: The laughing kookaburra is the largest kingfisher. It is a stout, stocky bird in length, with a large head, prominent brown eyes, and a very large bill. The sexes are very similar, although the female is usually larger and has less blue to the rump than the male. The male weighs and the female .

Laughing kookaburra [SEP] They have a white or cream-coloured body and head with a dark brown stripe across each eye and more faintly over the top of the head. The wings and back are brown with sky blue spots on the shoulders. The tail is rusty reddish-orange with dark brown bars and white tips on the feathers. The heavy bill is black on top and bone-coloured on the bottom. The subspecies "D. n. minor" has a similar plumage to the nominate but is smaller in size.

Laughing kookaburra [SEP] The laughing kookaburra can be distinguished from the similarly sized blue-winged kookaburra by its dark eye, dark eye-stripe, shorter bill and the smaller and duller blue areas on the wing and rump. Male blue-winged kookaburras also differ in having a barred blue and black tail. The name "laughing kookaburra" refers to the bird's "laugh", which it uses to establish territory among family groups. It can be heard at any time of day, but most frequently at dawn and dusk.

Laughing kookaburra [SEP] One bird starts with a low, hiccuping chuckle, then throws its head back in raucous laughter: often several others join in. If a rival tribe is within earshot and replies, the whole family soon gathers to fill the bush with ringing laughter. Hearing kookaburras in full voice is one of the more extraordinary experiences of the Australian bush, something even locals cannot ignore; some visitors, unless forewarned, may find their calls startling.

Laughing kookaburra [SEP] The laughing kookaburra is native to eastern Australia and has a range that extends from the Cape York Peninsula in the north to Cape Otway in the south. It is present on both the eastern and the western sides of the Great Dividing Range. In the south the range extends westwards from Victoria to the Yorke Peninsula and the Flinders Ranges in South Australia. It has been introduced into many other areas probably because of its reputation for killing snakes.

Laughing kookaburra [SEP] In Western Australia, laughing kookaburras were released near Mullewa in around 1896 and over the following decade hundreds of birds were imported from Victoria and released around Perth. By 1912 breeding populations had been established in a number of areas. The present range in Western Australia is southwest of a line joining Geraldton on the west coast and Hopetoun on the south coast. In Tasmania the laughing kookaburra was introduced at several locations beginning in 1906. It now mainly occurs northeast of a line joining Huonville, Lake Rowallan, Watatah and Marrawah.

Laughing kookaburra [SEP] It was introduced on Flinders Island in around 1940 where it is now widespread and on Kangaroo Island in 1926. In the 1860s, during his second term as governor of New Zealand, George Grey arranged for the release of laughing kookaburras on Kawau Island. The island lies in the Hauraki Gulf, about north of Auckland on the North Island of New Zealand. It was thought that the introduction had been unsuccessful but in 1916 some birds were discovered on the adjacent mainland.

Laughing kookaburra [SEP] It now breeds in a small region on the western side of the Hauraki Gulf between Leigh and Kumeu. The usual habitat is open sclerophyll forest and woodland. It is more common where the understory is open and sparse or where the ground is covered with grass. Tree-holes are needed for nesting. It also occurs near wetlands and in partly cleared areas or farmland with trees along roads and fences. In urban areas it is found in parks and gardens.

Laughing kookaburra [SEP] The range of the laughing kookaburra overlaps with that of the blue-winged kookaburra in an area of eastern Queensland that extends from the Cape York Peninsula south to near Brisbane. Around Cooktown the laughing kookaburra tends to favour areas near water while the blue-winged kookaburra keeps to drier habitats. Kookaburras occupy woodland territories (including forests) in loose family groups, and their laughter serves the same purpose as a great many other bird calls—to mark territorial borders.

Laughing kookaburra [SEP] Most species of kookaburras tend to live in family units, with offspring helping the parents hunt and care for the next generation of offspring. During mating season, the laughing kookaburra reputedly indulges in behaviour similar to that of a wattlebird. The female adopts a begging posture and vocalises like a young bird. The male then offers her his current catch accompanied with an "oo oo oo" sound.

Laughing kookaburra [SEP] However, some observers maintain that the opposite happens - the female approaches the male with her current catch and offers it to him. Either way, they start breeding around October/November. If the first clutch fails, they will continue breeding into the summer months. They generally lay three eggs at about two-day intervals. If the food supply is not adequate, the third egg will be smaller and the third chick will also be smaller and at a disadvantage relative to its larger siblings.

Laughing kookaburra [SEP] Chicks have a hook on the upper mandible, which disappears by the time of fledging. If the food supply to the chicks is not adequate, the chicks will quarrel, with the hook being used as a weapon. The smallest chick may even be killed by its larger siblings. If food is plentiful, the parent birds spend more time brooding the chicks, so the chicks are not able to fight.

Laughing kookaburra [SEP] Kookaburras hunt much as other kingfishers (or indeed Australasian robins) do, by perching on a convenient branch or wire and waiting patiently for prey to pass by. Common prey include mice and similar-sized small mammals, large insects, yabbies, lizards, small birds and nestlings, and most famously, snakes. Small prey are preferred, but kookaburras sometimes take large creatures, including venomous snakes, much longer than their bodies.

Laughing kookaburra [SEP] Laughing kookaburras are a common sight in suburban gardens and urban settings, even in built-up areas, and are so tame that they will often eat out of a person's hands. It is not uncommon for kookaburras to snatch food out of people's hands without warning, by swooping in from a distance. People often feed them pieces of raw meat. Laughing Kookaburras are often kept in zoos.

Laughing kookaburra [SEP] The kookaburra is also the subject of a popular Australian children's song, the "Kookaburra" which was written by Marion Sinclair in 1934. Recordings of this bird have been edited into Hollywood movies for decades, usually in jungle settings, beginning with the Tarzan series in the 1930s, and more recently in the film "" (1997). The population density of the laughing kookaburra in Australia varies between 0·04 and 0·8 birds/ha depending on the habitat.

Laughing kookaburra [SEP] Assuming an average of 0.3 birds/ha the total population may be as large as 65 million individuals. The population in New Zealand is relatively small and is probably less than 500 individuals. Given the extended range and the large stable population, the species is evaluated as of "least concern" by the International Union for Conservation of Nature.

Roman army of the mid-Republic [SEP] The Roman army of the mid-Republic (also known as the manipular Roman army or the "Polybian army"), refers to the armed forces deployed by the mid-Roman Republic, from the end of the Samnite Wars (290 BC) to the end of the Social War (88 BC). The first phase of this army, in its manipular structure (290–ca.

Roman army of the mid-Republic [SEP] 130 BC), is described in detail in the "Histories" of the ancient Greek historian Polybius, writing before 146 BC. The central feature of the mid-Republican army was the manipular organisation of its battle-line.

Roman army of the mid-Republic [SEP] Instead of a single, large mass (the phalanx) as in the Early Roman army, the Romans now drew up in three lines ("triplex acies") consisting of small units (maniples) of 120 men, arrayed in chessboard fashion, giving much greater tactical strength and flexibility. This structure was probably introduced in ca. 300 BC during the Samnite Wars.

Roman army of the mid-Republic [SEP] Also probably dating from this period was the regular accompaniment of each legion by a non-citizen formation of roughly equal size, the "ala", recruited from Rome's Italian allies, or "socii". The latter were about 150 autonomous states which were bound by a treaty of perpetual military alliance with Rome. Their sole obligation was to supply to the Roman army, on demand, a number of fully equipped troops up to a specified maximum each year.

Roman army of the mid-Republic [SEP] Evidence from Roman army camps near Numantia in Spain suggests that a much larger tactical unit, the cohort (480 men, equivalent to 4 maniples) already existed, alongside maniples, in the period 153-133 BC. By ca. 100 BC, cohorts appear to have fully replaced maniples as the basic tactical unit.

Roman army of the mid-Republic [SEP] The Second Punic War (218–201 BC) saw the addition of a third element to the existing dual Roman/Italian structure: non-Italian mercenaries with specialist skills lacking in the legions and "alae": Numidian light cavalry, Cretan archers, and slingers from the Balearic islands. From this time, these units always accompanied Roman armies.