|Discovered by||Marc Buie|
|Discovery site||Hubble Space Telescope|
|Discovery date||26 June 2014|
|MPC designation||(486958) Arrokoth|
|(486958) 2014 MU69|
Ultima Thule (unofficial)
|Epoch 2019 April 27 (JD 2458600.5)|
|Uncertainty parameter 2|
|Observation arc||2.33 yr (851 days)|
|0° 0m 11.92s / day|
|Dimensions||36 × 18 × 10 km|
± 0.5 × 0.5 × 2 km
Ultima 21.6 × 19.9 × 9.4 km
Thule 15.4 × 13.8 × 9.8 km
|18.3 km (volume equivalent)|
Ultima 15.9 km
Thule 12.9 km
Equatorial surface gravity
|~ 0.0001 g|
~ 0.001 m/s2
North pole right ascension
North pole declination
486958 Arrokoth[b] (provisional designation 2014 MU69) is a trans-Neptunian object located in the Kuiper belt. It is a contact binary 36 km (22 mi) long, composed of two planetesimals 22 km (14 mi) and 15 km (9 mi) across, nicknamed "Ultima" and "Thule", respectively, that are joined along their major axes. Ultima, which is flatter than Thule, appears to be an aggregate of 8 or so smaller units, each approximately 5 km (3 mi) across, that fused together before Ultima and Thule came into contact. Because there have been few to no disruptive impacts on Arrokoth since it formed, the details of its formation have been preserved. With the New Horizons space probe's flyby at 05:33 on 1 January 2019 (UTC time), Arrokoth became the farthest and most primitive object in the Solar System visited by a spacecraft. At the time of the New Horizons flyby, the object was originally nicknamed Ultima Thule[c] and was referred to as such in the media from the time.
Arrokoth was discovered on 26 June 2014 by astronomer Marc Buie and the New Horizons Search Team using the Hubble Space Telescope as part of a search for a Kuiper belt object for the New Horizons mission to target in its first extended mission; it was chosen over two other candidates to become the primary target of the mission. With an orbital period of 298 years and a low orbital inclination and eccentricity, Arrokoth is classified as a cold classical Kuiper belt object.
- 1 Nomenclature
- 2 Shape
- 3 Geology
- 4 Orbit and rotation
- 5 Mass and density
- 6 Formation
- 7 Observation
- 8 Exploration
- 9 See also
- 10 Notes
- 11 References
- 12 External links
Arrokoth was named for a word glossed as "sky", from the Powhatan language of the Tidewater region of Virginia and Maryland. The pronunciation and meaning of the word, however, are not entirely certain, as the language became extinct in the late 18th century and little was recorded of it. The only record of the word was collected in 1610–1611 by English writer William Strachey, who had a decent ear but bad handwriting, and scholars since have had considerable difficulty reading his notes. The meanings of the words are also often uncertain, as Strachey and the Powhatan had no language in common. Siebert (1975:324) used comparison with other Algonquian languages to interpret Strachey's handwriting, and deciphers Strachey's records as ⟨arrokoth⟩ 'sky' and ⟨arrahgwotuwss⟩ 'clouds'. He reconstructs these as the word /aːrahkwat/ 'cloud', pl. /aːrahkwatas/ (cf. Ojibwa /aːnakkwat/ 'cloud'), from the Proto-Algonquian *aːlaxkwatwi 'it is a cloud, it is cloudy'. Given that the first vowel is long (/aː/), that syllable would have been stressed, for ARR-o-koth.
Arrokoth's name was particularly chosen by the New Horizons team to represent the Powhatan people indigenous to the Tidewater region which included the state of Maryland, where Arrokoth's discovery took place. The Hubble Space Telescope and Johns Hopkins Applied Physics Laboratory were both operated at Maryland and were prominently involved in Arrokoth's discovery. In analogy, the Chesapeake Bay region of Maryland is significantly associated with the Powhatan people native to that particular region. With the permission of the elders of the Pamunkey Native American Tribe, the name Arrokoth was proposed to the International Astronomical Union (IAU) and was announced by the New Horizons team in a ceremony held at the NASA Headquarters in the District of Columbia on 12 November 2019. During the ceremony, New Horizons principal investigator Alan Stern justified their naming of Arrokoth, stating:
|“||The name 'Arrokoth' reflects the inspiration of looking to the skies, and wondering about the stars and worlds beyond our own. That desire to learn is at the heart of the New Horizons mission, and we're honored to join with the Powhatan community and people of Maryland in this celebration of discovery.||”|
In acknowledgement to the Powhatan people's significance to the Tidewater region of Virginia and Maryland, Lori Glaze, director of NASA's Planetary Science Division, asserted that Arrokoth's name "signifies the strength and endurance of the indigenous Algonquian people" and that their heritage "continues to be a guiding light for all who search for meaning and understanding of the origins of the universe and the celestial connection of humanity." Prior to the ceremony, the name was accepted by the IAU's Minor Planet Center on 8 November 2019 and the New Horizons team's naming citation was published in a Minor Planet Circular on 12 November 2019.
Nickname and designation
When Arrokoth was first observed, it was labelled 1110113Y, nicknamed "11" for short. Its existence as a potential target of the New Horizons probe was announced by NASA in October 2014 and it was unofficially designated as "Potential Target 1", or PT1. Its official designation, 2014 MU69, was assigned by the Minor Planet Center in March 2015, after sufficient orbital information was gathered. The provisional designation indicates that Arrokoth was the 1745th minor planet discovered during the second half of June 2014. After further observations refining its orbit, it was given the permanent minor planet number 486958 on 12 March 2017.
Before the flyby on 1 January 2019, NASA invited suggestions from the public on a nickname to be used. The campaign involved 115,000 participants from around the world, who suggested some 34,000 names. Of those, 37 reached the ballot for voting and were evaluated for popularity – this included eight names suggested by the New Horizons team and 29 suggested by the public. Ultima Thule,[c] which was selected on 13 March 2018, was proposed by about 40 different members of the public and obtained the seventh highest number of votes among the nominees. It is named after the Latin phrase ultima Thule (literally "farthest Thule"), an expression referencing the most distant place beyond the borders of the known world. Once it was determined the body was a bilobate contact binary object, the New Horizons team nicknamed the larger lobe "Ultima" and the smaller "Thule".
The nickname was criticized due to its use by Nazi occultists as the supposed mythical origin of the Aryan race, although it is commonly used in ancient Greek and Latin literature as well as to refer to the historical Inuit culture of the Thule people. The Thule Society was a key sponsor of what became the Nazi Party, and some modern-day neo-Nazis and members of the alt-right continue to use the term. A few members of the New Horizons team were aware of that association when they selected the nickname, and have since defended their choice. Responding to a question at a press conference, Alan Stern said, "Just because some bad guys once liked that term, we're not going to let them hijack it."
Arrokoth is a contact binary consisting of two lobes attached by a bright, narrow neck. The two lobes were likely once two objects that had merged in a slow collision. The larger lobe, nicknamed Ultima, is measured at about 21.6 km (13.4 mi) across its longest axis while the smaller lobe, Thule, is measured at 15.4 km (9.6 mi) across its longest axis. The larger lobe is lenticular in shape, being highly flattened and moderately elongated. Based on shape models of Arrokoth constructed from images taken by the New Horizons spacecraft, the dimensions of the larger lobe are approximately 21 km × 20 km × 9 km (13.0 mi × 12.4 mi × 5.6 mi). In contrast, the smaller lobe is less flattened, with dimensions of 15 km × 14 km × 10 km (9.3 mi × 8.7 mi × 6.2 mi). The volume ratio of the larger and smaller lobes is approximately 1.9:1, meaning that the larger lobe's volume is nearly twice as large as the smaller lobe's volume. Overall, the entire object is 36 km (22 mi) across its longest axis. The centers of the lobes are separated by 16 km (9.9 mi) from each other.
Prior to the New Horizons flyby of Arrokoth, stellar occultations by Arrokoth had provided evidence for its bilobate shape. The first detailed image of Arrokoth confirmed its double-lobed appearance and was described as a "snowman" by Alan Stern, as the two lobes appeared distinctively spherical. On 8 February, one month after the New Horizons flyby, Stern announced that Arrokoth was more flattened than initially thought, based on additional images of Arrokoth taken by New Horizons after its closest approach. The flattened larger lobe of Arrokoth was described as a "pancake", while the smaller lobe was described as a "walnut" as it appeared less flattened compared to the larger lobe. By observing how the unseen sections of Arrokoth occulted background stars, scientists were able to then outline the shapes of both lobes. The cause of Arrokoth's unexpectedly flattened shape is uncertain, though one possibility is that the two separate lobes were once rotating rapidly, causing them to become flattened due to centrifugal forces.
The longest axes of the two lobes are nearly aligned toward their rotational axis, which is situated between the two lobes. This near-parallel alignment of the two lobes suggests that they were mutually locked to each other, likely due to tidal forces, before merging. The alignment of the two lobes supports the idea that the two had individually formed from the coalescence of a cloud of icy particles.
Spectra and surface
Measurements of Arrokoth's absorption spectrum by the New Horizons' LEISA spectrometer show that Arrokoth's spectrum exhibits a strong red spectral slope extending from red to infrared wavelengths at 1.2–2.5 μm. Spectral measurements from LEISA have revealed the presence of methanol, water ice, and organic compounds on the surface of Arrokoth. An unidentified absorption band was also found in Arrokoth's spectrum at 1.8 μm. Arrokoth's spectrum shares similarities with that of 2002 VE95 and the centaur 5145 Pholus, which also display strong red spectral slopes along with signs of methanol present on their surfaces.
Preliminary observations with the Hubble Space Telescope in 2016 revealed that Arrokoth is red in color, similar to other Kuiper belt objects and centaurs like Pholus. Arrokoth's color is redder than that of Pluto, hence the New Horizons team informally classified it as an ultra red object. The red coloration of Arrokoth is caused by the presence of a mix of complex organic compounds called tholins on Arrokoth's surface. The tholins are thought to have been produced from the photolysis of simple organic compounds and volatiles irradiated by cosmic rays and ultraviolet solar radiation. The presence of tholins on Arrokoth's surface implies that volatiles such as methane and ammonia may be present on Arrokoth, although they would be lost on short timescales as Arrokoth is far too small to be able to retain these materials. However, less volatile materials such as methanol, acetylene, ethane, and hydrogen cyanide could be retained over a longer period of time, and may likely account for the reddening and production of tholins on Arrokoth. The photoionization of organic compounds and volatiles on Arrokoth is expected to also produce hydrogen gas, which would escape and interact with solar wind, though the New Horizons' SWAP and PEPSSI instruments did not detect any signature of solar wind interaction around Arrokoth.
From color and spectral measurements of Arrokoth, the surface displays subtle color variation among its surface features. Spectral images of Arrokoth show that the neck region and lineation features appear less red while the central region of the smaller lobe appears more red. The larger lobe also displays redder regions, which were informally known as "thumbprints" by the New Horizons team. The thumbprints are located near the larger lobe's limb. The surface albedo or reflectivity of Arrokoth varies from 5 percent to 12 percent due to various bright features on its surface. Its geometric albedo, the quantity of reflected light in visible spectrum, is measured at 16.5 percent, typical for most Kuiper belt objects. The overall Bond albedo (the quantity of reflected light of any wavelength) of Arrokoth is measured at 6.1 percent.
The surface of Arrokoth appears lightly cratered. Arrokoth's surface lacks small impact craters less than 1 km (0.62 mi) in size, implying a lack of impacts throughout its history. The occurrence of impact events in the Kuiper belt is thought to be uncommon, with a very low impact rate over the course of one billion years. Due to the slower orbital speeds of Kuiper belt objects, the speed of objects impacting Arrokoth is expected to be low, with impact speeds being at least 2 km/s (1.2 mi/s). At such slow impact speeds, large craters on Arrokoth are expected to be rare. With a low frequency of impact events along with the slow speeds of impacts, Arrokoth's surface would remain preserved since its formation. The preserved surface of Arrokoth could possibly give hints to its formation process, as well as signs of accreted material.
Numerous small pits on Arrokoth's surface were identified in high resolution images from the New Horizons spacecraft. The size of these pits are measured at about 700 m (2,300 ft) across. The exact cause of these pits is unknown; several explanations for these pits include impact events, the collapse of material, the sublimation of volatile materials, or the venting and escape of volatile gases from the interior of Arrokoth.
The surfaces of each lobe of Arrokoth display regions of varying brightness along with various geological features such as troughs and hills. These geological features are thought to have originated from the clumping of smaller planetesimals that come to form the lobes of Arrokoth. The brighter regions of Arrokoth's surface, especially its bright lineation features, are thought to have resulted from the deposition of material that have rolled down from hills on Arrokoth. The surface gravity on the hilltops of Arrokoth is weaker compared to the surface gravity at lower elevations, thus material is likely to roll down the hills toward lower elevations, where surface gravity is stronger.
The smaller lobe of Arrokoth, Thule, bears a large depression feature informally named "Maryland" by the New Horizons team, after the eponymous state where the Johns Hopkins University Applied Physics Laboratory is located and operated. The large depression feature is measured at 7 km (4.3 mi) to 8 km (5 mi) across and its depth is estimated at around 0.5–1 km (0.31–0.62 mi). The depression is likely an impact crater that was formed by an object 700 m (2,300 ft) in size. Two bright streaks of similar size are notably present in the depression feature, and may be associated with avalanches where bright material rolls down into the depression. Four subparallel troughs are present near the terminator of the small lobe, along with two possible kilometer-sized impact craters on the rim of the large depression feature. The surface of the small lobe exhibits bright mottled regions separated by broad, dark regions (labeled dm in the right image) which may have undergone scarp retreat, in which they were eroded due to the sublimation of volatiles, exposing lag deposits of darker material irradiated by sunlight. Another bright region (labeled rm in the right image), located at the equatorial end of the small lobe, exhibits rough terrain along with several topographic features that have been identified as possible pits, craters, or mounds. Unlike the larger lobe, the small lobe does not appear to display distinct subunits of rolling topography, likely as a result of resurfacing caused by the same impact event that created the large depression feature of the small lobe.
Like the smaller lobe, troughs and pit crater chains are also present along the terminator of the larger lobe of Arrokoth, nicknamed Ultima. The larger lobe consists of eight smaller subunits of rolling topography, each similarly sized at around 5 km (3.1 mi). Each distinctive subunit appears to be separated by relatively bright boundary regions. The similar sizes of the subunits of the large lobe suggests that each subunit was an individual small planetesimal, which eventually coalesced with other small planetesimals to form the large lobe of Arrokoth. These planetesimal units are expected to have accreted very slowly (at speeds of several meters per second), though they must have a very low mechanical strength in order to merge and form compact bodies at these speeds. The central subunit of the large lobe bears a bright ring-shaped feature informally called "The Road to Nowhere". From stereographic analysis, the central feature appears to be relatively flat compared to other topography units of the large lobe. Stereographic analysis of Arrokoth has also shown that one particular subunit located at the large lobe's limb (labeled md in the right image) appears to have a higher elevation and tilt compared to other subunits.
The neck region connecting both lobes of Arrokoth is considerably brighter and less red compared to the surfaces of both lobes. The brighter region in the neck is likely composed of a more reflective material different from the surfaces of Arrokoth's lobes. One hypothesis suggests the bright material in the neck region had likely originated from the deposition of small particles that had fallen from Arrokoth's lobes over time. Since Arrokoth's center of gravity lies between the two lobes, small particles are likely to roll down the steep slopes toward the center between each lobe. Another proposal suggests the bright material is produced by the deposition of ammonia ice. Ammonia vapor present on the surface of Arrokoth would solidify around the neck region, where gases cannot escape due to the concave shape of the neck. Arrokoth's neck region is also thought to be maintained by seasonal changes as it orbits around the Sun, due to its high axial tilt. Over the course of its orbit, the neck region of Arrokoth is shadowed when its lobes are coplanar to the direction of the Sun, in which the neck region no longer receives sunlight, cooling down and trapping volatiles in the region.
Topography variations at the limb of Arrokoth suggest that its interior is likely composed of mechanically strong material consisting of mostly amorphous water ice and rocky material. Trace amounts of methane and other volatile gases in the form of vapors may be also present in Arrokoth's interior, trapped in water ice. Under the assumption that Arrokoth has a low comet-like density of around 0.5 g/cm3, its internal structure is expected to be porous, as volatile gases trapped in Arrokoth's interior are thought to escape from the interior to the surface. Assuming that Arrokoth may have an internal heat source caused by the radioactive decay of radionuclides, the trapped volatile gases inside Arrokoth would migrate outward and escape from the surface, similarly to the scenario of outgassing of comets. The escaped gases may subsequently freeze and deposit on Arrokoth's surface, and could possibly account for the presence of ices and tholins on its surface.
Orbit and rotation
Arrokoth orbits the Sun at a distance of 44.6 AU (6.67×109 km) and completes a full orbit around the Sun in 298 years. Its orbit has a low orbital eccentricity of 0.04, as its perihelion (closest distance to the Sun) and aphelion (farthest distance from the Sun) differ by only about 2 AU. It has a low orbital inclination and eccentricity compared to other objects in the Kuiper belt. These orbital properties mean that Arrokoth is a cold classical Kuiper belt object (or cubewano) which is unlikely to have undergone significant perturbations. Observations in May and July 2015 as well as in July and October 2016 greatly reduced the uncertainties in the orbit, which prompted the Minor Planet Center to assign its permanent minor planet number.
Results from photometric Hubble Space Telescope observations show that the brightness of Arrokoth varies by around 0.3 magnitudes as it rotates. Though the rotation period and light curve amplitude of Arrokoth could not be determined from Hubble observations, the subtle brightness variations suggests that Arrokoth's rotational axis is either pointed toward the Earth or is being viewed at an equator-on configuration with a nearly spherical shape, with a constrained a/b ellipsoidal aspect ratio of 1–1.15.
Upon the New Horizons spacecraft's approach to Arrokoth, no rotational light curve amplitude was detected by the spacecraft despite Arrokoth's irregular shape. To explain the lack of its rotational light curve, scientists surmised that Arrokoth is rotating on its side, with its rotational axis pointing nearly directly at the approaching New Horizons spacecraft. Subsequent images of Arrokoth from New Horizons upon approach confirmed that its rotation is tilted, with its south pole facing towards the Sun. Based on images from New Horizons, the rotational axis of Arrokoth is estimated to be tilted at 99 degrees to its orbit. The rotation period of Arrokoth was initially constrained between roughly 15 to 30 hours based on initial images obtained from New Horizons after its flyby. Its rotation period was later refined to a value of 15.92 hours, consistent with a later constrained estimate of 15 to 16 hours.
Due to the high axial tilt of its rotation, the solar irradiance of the northern and southern hemispheres of Arrokoth varies greatly over the course of its orbit around the Sun. As it orbits around the Sun, one polar region of Arrokoth faces the Sun continuously while the other faces away. The solar irradiance of Arrokoth varies by 17 percent due to the low eccentricity of its orbit. The maximum equilibrium temperature of the illuminated face of Arrokoth is expected to reach 60 K (−213.2 °C). The surface temperature of the unilluminated face is predicted to be in the range of 10 K (−263.1 °C) to 14 K (−259.1 °C), although radiometric measurements from the New Horizons REX instrument indicated a higher average temperature of about 23 K (−250.2 °C). The REX instrument had likely measured the temperature 50 cm (1.6 ft) beneath the surface of the unilluminated face of Arrokoth.
Mass and density
The mass and density of Arrokoth is unknown. A definitive mass and density estimate cannot be given as the two lobes of Arrokoth are in contact rather than orbiting each other. Although a possible natural satellite orbiting Arrokoth could help determine its mass, no satellites were found orbiting Arrokoth. Under the assumption that both lobes of Arrokoth are bound by self-gravity, with the mutual gravity of the two lobes overcoming centrifugal forces that would otherwise separate the lobes, the entire body is estimated to have a very low density similar to that of comets, with an estimated minimum density of 0.29 g/cm3. In order to maintain the neck region's shape, the density of Arrokoth is expected to be less than the maximum possible density of 1 g/cm3, otherwise the neck region would be excessively compressed by the mutual gravity of the two lobes in which the entire object gravitationally collapses into a spheroid.
Arrokoth is thought to have originally been two objects, nicknamed "Ultima" and "Thule", that formed over time from a rotating cloud of small, icy bodies since the formation of the Solar System 4.6 billion years ago. Icy particles experienced streaming instability, in which they slowed down due to drag against the surrounding gas and dust, and gravitationally coalesced into clumps of larger particles. Based on the differing appearances of the two lobes, each were likely individual objects that had accreted separately and remained in a mutual orbit around each other after their formation. Both objects are believed to have formed from a single source of material as they appear to be homogeneous in albedo, color, and composition. The presence of rolling topography units on the larger object, Ultima, indicates that it had likely formed from the coalescence of smaller planetesimal units prior to merging with the smaller object.
Although it is unclear how the two constituents of Arrokoth became flattened during its formation, the New Horizons team suggests that the two objects were rotating rapidly, causing their shapes to become flattened due to centrifugal forces. Over time, the rotation rates of the two objects gradually slowed down as they experienced impacts by small objects and transferred their angular momentum to other orbiting debris left over from their formation. Eventually, loss of momentum, caused by impacts and momentum shifting to other bodies in the cloud, caused the pair to slowly spiral closer until they touched—where over time the joints fused together, forming its present bilobate shape. The present appearance of Arrokoth does not display any indication of deformation or compression fractures, suggesting that the two objects had merged very slowly at a speed of 2 m/s (6.6 ft/s)—comparable to the average walking speed of a person. There is a possible indication of shearing of the surface and terrain caused by the merging of the two objects.
The frequency of impact events occurring on Arrokoth over a period of at least four billion years were uncommon due to the slower speeds of objects in the Kuiper Belt. At such timescales since its formation, the effect of photon-induced sputtering of water ice on the surface of Arrokoth is estimated to be very minimal; over a period of 4.5 billion years, the amount of water ice lost by sputtering would reduce the size of Arrokoth by 1 cm (0.39 in). With the lack of frequent cratering events and perturbations of its orbit, the shape and appearance of Arrokoth would remain virtually pristine since the conjoining of two separate objects that formed its bilobate shape.
Arrokoth was discovered on 26 June 2014 using the Hubble Space Telescope during a preliminary survey to find a suitable Kuiper belt object for the New Horizons spacecraft to fly by. Scientists of the New Horizons team were searching for an object in the Kuiper belt that the spacecraft could study after Pluto, and their next target had to be reachable on New Horizons' remaining fuel. Using large ground-based telescopes on Earth, researchers began looking in 2011 for candidate objects and searched multiple times per year for several years. However, none of the objects found were reachable by the New Horizons spacecraft and most Kuiper belt objects that may be suitable were just too distant and faint to be seen through Earth's atmosphere. In order to find these fainter Kuiper belt objects, the New Horizons team initiated a search for suitable targets with the Hubble Space Telescope on 16 June 2014.
Arrokoth was first imaged by Hubble on 26 June 2014, 10 days since the New Horizons team began their search for potential targets. While digitally processing images from Hubble, Arrokoth was identified by astronomer Marc Buie, member of the New Horizons team. Buie reported his finding to the search team for subsequent analysis and confirmation. Arrokoth was the second object found during the search, after 2014 MT69. Three more candidate targets were later discovered with Hubble, though follow-up astrometric observations eventually ruled them out. Of the five potential targets found with Hubble, Arrokoth was deemed to be the most feasible target for the spacecraft as the flyby trajectory required the least amount of fuel compared to that for 2014 PN70, the second most feasible target for New Horizons. On 28 August 2015, Arrokoth was officially selected by NASA as a flyby target for the New Horizons spacecraft.
Arrokoth is too small and distant for its shape to be observed directly from Earth, but scientists were able to take advantage of an astronomical event called a stellar occultation, in which the object passes in front of a star from the vantage point of Earth. Since the occultation event is only visible from certain parts of the Earth, the New Horizons team combined data from Hubble and the European Space Agency's Gaia space observatory to figure out exactly when and where on Earth's surface Arrokoth would cast a shadow. They determined that occultations would occur on 3 June, 10 July, and 17 July in 2017, and set off for places around the world where they could see Arrokoth cover up a different star on each of these dates. Based on this string of three occultations, scientists were able to trace out the object's shape.
In June and July 2017, Arrokoth occulted three background stars. The team behind New Horizons formed a specialised "KBO Chasers" team to observe these stellar occultations from South America, Africa, and the Pacific Ocean. On 3 June 2017, two teams of NASA scientists tried to detect the shadow of Arrokoth from Argentina and South Africa. When they found that none of their telescopes had observed the object's shadow, it was initially speculated that Arrokoth might be neither as large nor as dark as previously expected, and that it might be highly reflective or even a swarm. Additional data taken with the Hubble Space Telescope in June and July 2017 revealed that the telescopes had been placed in the wrong location, and that these estimations were incorrect.
On 10 July 2017, the airborne telescope SOFIA was successfully placed close to the predicted centerline for the second occultation while flying over the Pacific Ocean from Christchurch, New Zealand. The main purpose of those observations was the search for hazardous material like rings or dust near Arrokoth that could threaten the New Horizons spacecraft during its flyby in 2019. Data collection was successful. A preliminary analysis suggested that the central shadow was missed; only in January 2018 was it realized that SOFIA had indeed observed a very brief dip from the central shadow. The data collected by SOFIA will also be valuable to put constraints on dust near Arrokoth. Detailed results of the search for hazardous material were presented on the 49th Meeting of the AAS Division for Planetary Sciences, on 20 October 2017.
On 17 July 2017, the Hubble Space Telescope was used to check for debris around Arrokoth, setting constraints on rings and debris within the Hill sphere of Arrokoth at distances of up to 75,000 km (47,000 mi) from the main body. For the third and final occultation, team members set up another ground-based "fence line" of 24 mobile telescopes along the predicted ground track of the occultation shadow in southern Argentina (Chubut and Santa Cruz provinces) to better constrain the size of Arrokoth. The average spacing between these telescopes was around 4 km (2.5 mi). Using the latest observations from Hubble, the position of Arrokoth was known with much better precision than for the June 3 occultation, and this time the shadow of Arrokoth was successfully observed by at least five of the mobile telescopes. Combined with the SOFIA observations, this put constraints on possible debris near Arrokoth.
Results from the occultation on 17 July showed that Arrokoth could have had a very oblong, irregular shape or be a close or contact binary. According to the duration of the observed chords, Arrokoth was shown to have two "lobes", with diameters of approximately 20 km (12 mi) and 18 km (11 mi), respectively. A preliminary analysis of all collected data suggested that Arrokoth was accompanied by an orbiting moonlet about 200–300 km (120–190 mi) away from the primary. It was later realized, however, that an error with the data processing software resulted in a shift in the apparent location of the target. After accounting for the bug, the short dip observed on 10 July was considered to be a detection of the primary body.
By combining data about its light curve, spectra (e.g. color), and stellar occultation data, illustrations could rely on known data to create a concept of what it might look like prior to spacecraft flyby.
There were two potentially useful Arrokoth occultations predicted for 2018: one on 16 July and one on 4 August. Neither of these were as good as the three 2017 events. No attempts were made to observe the 16 July 2018 occultation, which took place over the South Atlantic and the Indian Ocean. For the 4 August 2018 event, two teams, consisting of about 50 researchers in total, went to locations in Senegal and Colombia. The event gathered media attention in Senegal, where it was used as an opportunity for science outreach. Despite some stations being affected by bad weather, the event was successfully observed, as reported by the New Horizons team. Initially, it was unclear whether a chord on the target had been recorded. On 6 September 2018, NASA confirmed that the star had indeed been seen to dip by at least one observer, providing important information about the size and shape of Arrokoth.
Hubble observations were carried out on 4 August 2018, to support the occultation campaign. Hubble could not be placed in the narrow path of the occultation, but due to the favourable location of Hubble at the time of the event, the space telescope was able to probe the region down to 1,600 km (990 mi) from Arrokoth. This is much closer than the 20,000 km (12,000 mi) region that could be observed during the 17 July 2017 occultation. No brightness changes of the target star have been seen by Hubble, ruling out any optically thick rings or debris down to 1,600 km (990 mi) from Arrokoth. Results of the 2017 and 2018 occultation campaigns were presented at the 50th meeting of the American Astronomical Society Division for Planetary Sciences on 26 October 2018.
Having completed its flyby of Pluto in July 2015, the New Horizons spacecraft made four course changes in October and November 2015 to place itself on a trajectory towards Arrokoth. It is the first object to be targeted for a flyby that was discovered after the visiting spacecraft was launched, and is the farthest object in the Solar System ever to be visited by a spacecraft. New Horizons came within 3,500 km (2,200 mi) of Arrokoth, one third of the distance of the spacecraft's closest encounter with Pluto. Closest approach occurred on January 1, 2019, at 05:33 UTC (Spacecraft Event Time – SCET) at which point it was 43.4 AU from the Sun in the direction of the constellation Sagittarius. At this distance, the one-way transit time for radio signals between Earth and New Horizons was 6 hours.
The science objectives of the flyby include characterizing the geology and morphology of Arrokoth, mapping the surface composition (searching for ammonia, carbon monoxide, methane, and water ice). Surveys of the surrounding environment to detect possible orbiting moonlets, a coma, or rings, were conducted. Images with resolutions showing details of 30 m (98 ft) to 70 m (230 ft) are expected. From Hubble observations, faint, small satellites orbiting Arrokoth at distances greater than 2,000 km (1,200 mi) have been excluded to a depth of >29th magnitude. The object has no detectable atmosphere, and no large rings or satellites larger than 1.6 km (1 mi) in diameter. Nonetheless, a search for a related moon (or moons) continues, which may help better explain the formation of Arrokoth from two individual orbiting objects.
New Horizons made its first detection of Arrokoth on 16 August 2018, from a distance of 172 million km (107 million mi). At that time, Arrokoth was visible at magnitude 20, in the direction of the constellation Sagittarius. Arrokoth was expected to be magnitude 18 by mid-November, and magnitude 15 by mid-December. It reached naked eye brightness (magnitude 6) from the spacecraft's point of view just 3–4 hours before closest approach. If obstacles were detected, the spacecraft had the option of diverting to a more distant rendezvous, though no moons, rings or other hazards were seen. High-resolution images from New Horizons were taken on 1 January. The first images with medium resolution arrived the next day. The downlink of data collected from the flyby is expected to last 20 months, through to September 2020.
- Color MVIC image superimposed over a higher-resolution greyscale composite of nine 0.025 second exposures taken by the Long Range Reconnaissance Imager (LORRI) aboard New Horizons on 1 January 2019, from a distance of 6,628 kilometres (4,118 mi) at a resolution of 33 metres (108 ft) per pixel. The contact binary object is made up of two lobes nicknamed "Ultima" (top) and "Thule" (bottom). Its axis of rotation is located near the bright "neck" of the object and spins clockwise from this viewpoint.
- Pronounced // ARR-ə-koth
- Normally pronounced // THEW-lee [US // THOO-lee] The New Horizons team use this classical pronunciation, the pseudo-Latin pronunciation // TOO-lay, and the hybrid pronunciation // TOO-lee.
- Composite of black and while and color photographs taken respectively by the LORRI and MVIC instruments aboard New Horizons on 1 January 2019.
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...a resolution of about 110 feet (33 meters) per pixel. [...] This processed, composite picture combines nine individual images taken with the Long Range Reconnaissance Imager (LORRI), each with an exposure time of 0.025 seconds...
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This movie shows the propeller-like rotation of Ultima Thule in the seven hours between 20:00 UT (3 p.m. ET) on Dec. 31, 2018, and 05:01 UT (12:01 a.m.) on Jan. 1, 2019...
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