(523764) 2014 WC510

' (provisional designation ') is a binary trans-Neptunian object discovered on 8 September 2011 by the Pan-STARRS survey at the Haleakalā 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 objects orbiting beyond Neptune in the outer Solar System. It is classified as a plutino, a dynamical class of objects in a 2:3 orbital resonance with Neptune. On 1 December 2018, a team of astronomers observed a stellar occultation by the object, which revealed that it is a compact binary system consisting of two separate components in close orbit around each other. The primary and secondary components are estimated to have diameters of around 180 km and 140 km, respectively.

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 Ritchey–Chrétien telescope, located at the Haleakalā Observatory atop the Hawaiian island of Maui. The accredited observers using the telescope were B. Gibson, T. Goggia, N. Primak, A. Schultz, and M. Willman. The object was first identified on 20 November 2014, though it was announced later in a Minor Planet Electronic Circular published on 17 July 2016, after additional observations by Pan-STARRS had been found, preceding the team's original observation from 2014. While is the object's first and only provisional designation assigned by the Minor Planet Center, the date of discovery is considered to be on 8 September 2011, which was the earliest known observation of the object before it was assigned a minor planet number.

Occultation
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 dimmings in the star's brightness, signifying likely positive detections of the occultation. Five of these sites reported two consecutive dimmings due to the occulted star's double nature; occulted one of the two stars being observed. These observations were part of a campaign coordinated by the Research and Education Collaborative Occultation Network (RECON), a citizen science project dedicated to observing occultations by trans-Neptunian objects.

Prior to the occultation, 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 project to do a precovery search of archival Pan-STARRS images to gather extensive astrometric positions of. Follow-up observations by Pan-STARRS were also conducted through 2016–2018 and helped extend 's observation arc to 6.3 years. Although an observation arc of this length is generally unreliable for predicting occultations especially by distant objects, this was compensated by Pan-STARRS's highly accurate astrometric system, allowing for 's orbital uncertainty to be significantly reduced.

Orbit and classification
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 Neptune takes. orbits the Sun at an average distance of 39.24 AU, taking 245.8 years to complete a full orbit. This is characteristic of all plutinos, which have orbital periods around 250 years and semi-major axes around 39 AU.

Like Pluto, 's orbit is elongated and inclined to the ecliptic. has an orbital eccentricity of 0.25 and an orbital inclination of 19.5 degrees with respect to the ecliptic. Over the course of its orbit, 's distance from the Sun varies from 29.5 AU at perihelion (closest distance) to 48.9 AU at aphelion (farthest distance). has last passed aphelion in the early 20th century, and is now moving closer to the Sun, approaching perihelion by 2032. Simulations by the Deep Ecliptic Survey show that can acquire a perihelion distance (qmin) as small as 28.7 AU over the next 10 million years.

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 main detections by the other five sites located south of it. A 2020 study led by Rodrigo Leiva and Marc Buie analyzed the occultation data and determined that the detection from Bishop was most likely an occultation by a secondary component of.

Since the two components were only observed for a short period of time during the occultation, the binary system's orbital parameters have not been determined. The projected separation distance between the primary and secondary is 349 ± 29 km, derived from an angular separation of $181 km$ milliarcseconds. Assuming a density of $138 km$ 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 separation distances between their components.

Most models of the formation of the Solar System indicate that most TNOs have formed as binaries, hence they are expected to be common especially in the Kuiper belt population. While most known binary TNOs appear to have wide mutual orbits, tight binary TNOs similar to are thought to have a higher chance of survival after their formation. belongs to the population of smaller TNOs, which are expected to have a primordial origin similar to the classical Kuiper belt object 486958 Arrokoth.

Physical characteristics
Assuming a circular projected shape for the components' occultation profiles, the diameters of the primary and secondary are estimated to be 181 ± 16 km and 138 ± 32 km, respectively. The diameter ratio of the secondary to the primary is 0.76:1.00—the secondary component is approximately 75% as large as the primary. Since the mutual orbit of the components is undetermined, the mass and density of the system cannot be derived. The individual components of the system are among the smallest trans-Neptunian objects with sizes measured with stellar occultations, following the Kuiper belt object 486958 Arrokoth (~$0.051$).

Given the components' estimated diameters and their combined absolute magnitude of 7.2, their calculated geometric albedos indicate that they have dark surfaces, reflecting about 5% of incident visible light. However, the estimated geometric albedo may be subject to a systematic error depending on the true shapes and photometric properties of the components, resulting in a significant uncertainty of ±2%. Nonetheless, is one of the darkest objects measured with stellar occultations, being darker than 486958 Arrokoth.

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.