 2013 FY27 and its satellite, imaged by the Hubble Space Telescope on 15 January 2018 | |
| Discovery[1] | |
|---|---|
| Discovered by | |
| Discovery date | 17 March 2013 (announced on 31 March 2014) |
| Designations | |
| 2013 FY27 | |
| Orbital characteristics[3] | |
| Epoch 2023 Feb 25 (JD 2460000.5) | |
| Uncertainty parameter 4 | |
| Observation arc | 3953 days (10.82 yr) |
| Earliestprecovery date | 15 March 2011 (Pan-STARRS) |
| Aphelion | 81.912 AU (12.2539 Tm) |
| Perihelion | 35.199 AU (5.2657 Tm) |
| 58.555 AU (8.7597 Tm) | |
| Eccentricity | 0.3989 |
| 448.08 yr (163,660 d) | |
| 215.947° | |
| 0° 0m 7.92s /day | |
| Inclination | 33.290° |
| 186.922° | |
| ≈ 2202 June 15 ± 17 days | |
| 139.752° | |
| Knownsatellites | 1[4][5][6] |
| Physical characteristics | |
| 765+80 −85 km(effective diameter)[4] 742+78 −83 km(primary)[a][4] | |
| 0.170+0.045 −0.030[4] | |
| Temperature | 22 K (perihelion) to 16 K (aphelion) |
| |
| 22.5[7] | |
| 3.15±0.03[4][3] | |
(532037) 2013 FY27 (provisional designation2013 FY27) is atrans-Neptunian object andbinary system that belongs to thescattered disc (likeEris).[8] Its discovery was announced on 31 March 2014.[1] It has anabsolute magnitude (H) of 3.2.[3]2013 FY27 is a binary object, with two components approximately 740 kilometres (460 mi) and 190 kilometres (120 mi) in diameter. It is the ninth-intrinsically-brightest known trans-Neptunian system,[9] and is approximately tied with2002 AW197 and2002 MS4 (to within measurement uncertainties) as thelargest unnamed object in the Solar System.
2013 FY27 orbits the Sun once every 449 years. It will come toperihelion around November 2202,[3][b] at a distance of about 35.6 AU. It is currently nearaphelion, 80 AU from theSun, and, as a result, it has anapparent magnitude of 22.[1] Its orbit has a significant inclination of 33°.[3]Thesednoid2012 VP113 and the scattered-disc object2013 FZ27 were discovered by the same survey as2013 FY27 and were announced within about a week of one another.
2013 FY27 has a diameter of about 740 kilometres (460 mi), placing it at a transition zone between medium-sized and large TNOs. Using theAtacama Large Millimeter Array andMagellan Telescopes, itsalbedo was found to be 0.17, and its colour to be moderately red.2013 FY27 is one of the largest moderately red TNOs. The physical processes that lead to a lack of such moderately red TNOs larger than 800 kilometres (500 mi) are not yet well understood.
The brightness of2013 FY27 varies by less than0.06 mag over hours and days, suggesting that it either has a very long rotation period, an approximately spheroidal shape, or a rotation axis pointing towards Earth.[4]
2013 FY27 is apossible dwarf planet, though not a likely one. Grundy et al. calculate that bodies less than about 1000 km in diameter, with albedos less than ≈0.2 and densities less than ≈1.2 g/cm3, may retain a degree of porosity in their physical structure, having never collapsed into fully solid bodies, and therefore could not be dwarf planets.[10] However, the albedo of2013 FY27 may be around that limit, and there is no way to estimate its density.
The surface area of asteroid 532037 (2013 FY27) is similar to the area of the state of Texas.[11]
 Animation of2013 FY27 and its satellite, imaged by theHubble Space Telescope from January to July 2018 | |
| Discovery[4] | |
|---|---|
| Discovered by |
|
| Discovery date | 15 January 2018 |
| Orbital characteristics[4] | |
| >9800±40 km | |
| ≈19 d (for assumed density1.6 g/cm3)[12] | |
| Satellite of | 2013 FY27 |
| Physical characteristics | |
| ≈186 km (assuming equal albedos)[4] | |
| Albedo | 0.170+0.045 −0.030 (assumed) |
| 25.5[7] | |
| 6.15[c] | |
UsingHubble Space Telescope observations taken in January 2018,Scott Sheppard found asatellite around2013 FY27, that was 0.17arcseconds away and3.0±0.2 mag fainter than its primary. The discovery was announced on 10 August 2018.[13] The satellite does not have aprovisional designation nor a proper name.[3] Assuming the two components have equal albedos, they are about742+78
−83 km and186±20 km in diameter, respectively.[4] Follow-up observations were taken between May and July 2018 in order to determine the orbit of the satellite,[5] but the results of these observations remain yet to be published as of 2022[update].[7] Once the orbit is known, the mass of the system can be determined.
2014 in space | ||
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| Consensus | _(cropped).jpg)  | ||||||||||||||
| Candidate (for TNOs, D+1σ ≥ 700 km or H ≤ 4.2) |
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