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// Workers AI · dad joke modeWhat did (303775) 2005 QU182 say? It's an asteroid attraction.

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(303775) 2005 QU182
Discovery[1]
Discovered by
Discovery sitePalomar Obs.
Discovery date30 August 2005
Designations
TNO (SDO)[2][3]
Orbital characteristics[4]
Epoch 09 June 2026 (JD 2461200.5)
Uncertainty parameter 1
Observation arc18,818 days (51.52 yr)
Aphelion186.4 AU (27.89 Tm) (Q)
Perihelion37.0 AU (5.54 Tm) (q)
111.7 AU (16.71 Tm) (a)
Eccentricity0.669 (e)
1181 yr (431,400 d)
16.7° (M)
0° 0m 3.006s / day (n)
Inclination14.01° (i)
78.5° (Ω)
224.1° (ω)
Known satellites0
Earth MOID36.015 AU (5.3878 Tm)
Jupiter MOID31.959 AU (4.7810 Tm)
TJupiter6.732
Physical characteristics
584+155
−144 km[5]
976.31 km[6]
9.61 h (0.400 d)
9.61 hr[4]
0.129+0.115
−0.046[5]
Temperature45 K (perihelion)[7]: 11 
CO
2-type ("double-dip")[8]
B–V = 0.94±0.03
V–R = 0.54±0.03
R–I = 0.51±0.03
16 ± 2%/100 nm[9]
20.9[10]
3.75[4][2]
3.99±0.02[5]

(303775) 2005 QU182 is a large trans-Neptunian object in the scattered disk, estimated to be around 440 to 740 kilometres (270 to 460 miles) in diameter. It was discovered on 30 August 2005 by American astronomers Mike Brown, David Rabinowitz and Chad Trujillo at the Palomar Observatory in California,[1] with precovery images going back to 1974. It was assigned its permanent number in 2014.

2005 QU182 is scheduled for observation with the Hubble Space Telescope in 2026;[11] if those observations discover a moon, they could lead to a measurement of the mass and density of 2005 QU182.[12]: 1, 3 

Observation history

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It was discovered on 30 August 2005 by American astronomers Mike Brown, David Rabinowitz and Chad Trujillo at the Palomar Observatory in California,[1] with precovery images going back to 1974. As of 2026, it has been observed 626 times over 52 years, with precovery images back to 1974.[13]

2005 QU182 is scheduled for observation with the Hubble Space Telescope in 2026,[11] if those observations discover a moon, they could lead to a measurement of the mass and density of 2005 QU182.[12]: 1, 3 

Nomenclature

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The provisional designation of 2005 QU182 indicates its discovery date, the first letter represents the second half of August and the second letter and numbers means that it is the 4571st object discovered during that half-month.[14][a] 2005 QU182 was assigned its permanent number in 2014.

Orbit and classification

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2005 QU182 takes around 1,200 years to orbit the Sun. Among large TNOs, only Sedna, 2012 VP113, 2013 FS28, (445473) 2010 VZ98 and 2023 KQ14 have a longer orbit around the Sun.[15]

2005 QU182 is a trans-Neptunian object that orbits the Sun at a distance of 37.0–186.4 AU with an semi-major axis or average orbital distance of 111.7 AU once every 1181 years (for reference, Neptune's orbit is at 30 AU).[16] Its orbit has a high eccentricity of 0.669 and an inclination of 14.0° with respect to the ecliptic.[4] 2005 QU182 came to perihelion in 1971[4] and is currently 51.8 AU from the Sun.[10] In April 2013, it moved beyond 50 AU from the Sun.

2005 QU182 belongs to the scattered disc,[2][3] which is a population of TNOs that have distant, inclined, and eccentric orbits that come close to Neptune at perihelion. The scattered disc population, which includes the dwarf planets Eris and Gonggong, are strongly influenced by Neptune's gravitational perturbations and consequently experience gravitational scattering.[17]: 52  Both the Minor Planet Center (MPC) and Buie classify that 2005 QU182 is a scattered disc object.[2][3]

Physical characteristics

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Size

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In 2012, the diameter of 2005 QU182 was initially estimated to be 416±73 km using data from the Herschel Space Telescope.[18] Later in 2020, the data was reanalyzed, which yielded a notably larger nominal diameter and uncertainty of 584+155
−144 km.[5]

Mass and density

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2005 QU182 is not known to have any natural satellites or moons, which means there is currently no way to measure its mass and density.[12]: 1, 3 

Hypothesized interior

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Based on its size of approximately 440–740 km,[5] it belongs to the proposed class of "mid-sized" TNOs between 400 and 1,000 km (250 and 620 mi) in diameter, which are believed to represent the transition between small, low-density TNOs and large, high-density dwarf planets.[19][20]: 1  Planetary scientists have hypothesized that mid-sized TNOs should have highly porous and unheated interiors, because TNOs in this size range (such as Uni and Gǃkúnǁʼhòmdímà) have been found to have low densities around 1 g/cm3.[19]

Surface

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Color, albedo and brightness

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2005 QU182 has color indices of: B–V 0.94 ± 0.03; V–R 0.54 ± 0.03; R–I 0.51 ± 0.03. It also has a known spectral slope of 16 ± 2%/100 nm.[9] The surface temperature of 2005 QU182 at perihelion (closest point to the Sun) is estimated to be approximately 45 Kelvin.[7]: 11  2005 QU182 has a bright absolute magnitude of 3.74.[4]

Rotation

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2005 QU182 has a rotation period of 9.61 hours according to the Jet Propulsion Laboratory.[4]

Notes

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  1. ↑ The second letter 'U' indicates that it is the 21th object discovered on the 183th cycle of discoveries. Each completed cycle consists of 25 letters representing discoveries, hence 21 + (182 completed cycles × 25 letters) = 4571.[14]

References

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  1. 1 2 3 "MPEC 2007-R03 : 2004 PF115, 2004 PG115, 2004 XA192, 2005 QU182". IAU Minor Planet Center. 1 September 2007. Retrieved 26 August 2009.
  2. 1 2 3 4 "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 22 January 2009.
  3. 1 2 3 Marc W. Buie (24 October 2008). "Orbit Fit and Astrometric record for 05QU182". SwRI (Space Science Department). Retrieved 9 December 2008.
  4. 1 2 3 4 5 6 7 "JPL Small-Body Database Browser: (2005 QU182)" (last observation: 2009-09-18). Retrieved 7 April 2016.
  5. 1 2 3 4 5 Farkas-Takács, A.; Kiss, Cs.; Vilenius, E.; Marton, G.; Müller, T. G.; Mommert, M.; et al. (28 February 2020). "TNOs are Cool! A Survey of the transneptunian Region XV. Physical characteristics of 23 resonant transneptunian and scattered disk objects". Astronomy & Astrophysics. A23: 638. arXiv:2002.12712. Bibcode:2020A&A...638A..23F. doi:10.1051/0004-6361/201936183. S2CID 216193564.
  6. ↑ "MinorPlanet.info: One Asteroid Information". Asteroid Lightcurve Database (LCDB). Retrieved 7 March 2026. Search using Number = "303775"
  7. 1 2 Brunetto, R.; Hénault, E.; Cryan, S.; Pinilla-Alonso, N.; Emery, J. P.; Guilbert-Lepoutre, A.; et al. (March 2025). "Spectral Diversity of DiSCo's TNOs Revealed by JWST: Early Sculpting and Late Irradiation". The Astrophysical Journal Letters. 982 (1): L8. Bibcode:2025ApJ...982L...8B. doi:10.3847/2041-8213/adb977. S2CID 259287422.
  8. ↑ Pinilla-Alonso, Noemí; Brunetto, Rosario; De Prá, Mário N.; Holler, Bryan J.; Hénault, Elsa; Feliciano, Ana Carolina de Souza; et al. (December 2024). "A JWST/DiSCo-TNOs portrait of the primordial Solar System through its trans-Neptunian objects" (PDF). Nature Astronomy. 9 (2): 230–244. Bibcode:2025NatAs...9..230P. doi:10.1038/s41550-024-02433-2. S2CID 274932942.
  9. 1 2 H. Boehnhardt; Schulz, D.; Protopapa, S.; Götz, C. (1 November 2014). "Photometry of Transneptunian Objects for the Herschel Key Program 'TNOs are Cool'". Earth, Moon, and Planets. 114 (1): 35–57. doi:10.1007/s11038-014-9450-x. ISSN 1573-0794.
  10. 1 2 "AstDys 2005QU182 Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 26 May 2011. Retrieved 16 March 2009.
  11. 1 2 Proudfoot, Benjamin (August 2025). A search for the moons of mid-sized TNOs. Mikulski Archive for Space Telescopes (Report). HST Research Proposals. Space Telescope Science Institute. cycle 33, proposal 18010. Retrieved 17 August 2025 – via stsci.edu.
  12. 1 2 3 Grundy, W. M.; McKinnon, W. B.; Ammannito, E.; Aung, M.; Bellerose, J.; Brenker, F.; et al. (December 2009). Exploration Strategy for the Ice Dwarf Planets 2013-2022 (PDF). American Geophysical Union Fall Meeting 2009. Bibcode:2009AGUFM.P43D1471G. P43D-1471. Archived from the original (PDF) on 30 March 2025.
  13. ↑ MPC
  14. 1 2 "How Are Minor Planets Named?". Minor Planet Center. Retrieved 10 August 2026.
  15. ↑ "JPL Small-Body Database Search Engine: H < 6 (mag) and a > 80 (AU)". JPL Solar System Dynamics. Retrieved 14 June 2014.
  16. ↑ Yeomans, Donald K. "HORIZONS Web-Interface for Neptune Barycenter (Major Body=8)". JPL Horizons On-Line Ephemeris System. Archived from the original on 7 September 2021. Retrieved 18 July 2014.—Select "Ephemeris Type: Orbital Elements", "Time Span: 2000-01-01 12:00 to 2000-01-02". ("Target Body: Neptune Barycenter" and "Center: Solar System Barycenter (@0)".)
  17. ↑ Gladman, Brett; Marsden, Brian G.; VanLaerhoven, Christa (2008). "Nomenclature in the Outer Solar System" (PDF). The Solar System Beyond Neptune. University of Arizona Press. pp. 43–57. arXiv:astro-ph/0702538. Bibcode:2008ssbn.book...43G. ISBN 9780816527557. S2CID 14469199. Archived from the original (PDF) on 1 August 2023.
  18. ↑ Santos-Sanz, P.; Lellouch, E.; Fornasier, S.; Kiss, C.; Pal, A.; Müller, T. G.; Vilenius, E.; Stansberry, J.; Mommert, M.; Delsanti, A.; Mueller, M.; Peixinho, N.; Henry, F.; Ortiz, J. L.; Thirouin, A.; Protopapa, S.; Duffard, R.; Szalai, N.; Lim, T.; Ejeta, C.; Hartogh, P.; Harris, A. W.; Rengel, M. (2012). ""TNOs are Cool": A survey of the trans-Neptunian region IV. Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel-PACS". Astronomy & Astrophysics. 541: A92. arXiv:1202.1481. Bibcode:2012A&A...541A..92S. doi:10.1051/0004-6361/201118541. S2CID 118600525.
  19. 1 2 Grundy, W. M.; Noll, K. S.; Buie, M. W.; Benecchi, S. D.; Ragozzine, D.; Roe, H. G. (December 2019). "The Mutual Orbit, Mass, and Density of Transneptunian Binary Gǃkúnǁʼhòmdímà ((229762) 2007 UK126)" (PDF). Icarus. 334: 30–38. Bibcode:2019Icar..334...30G. doi:10.1016/j.icarus.2018.12.037. S2CID 126574999. Archived from the original (PDF) on 7 April 2019. Retrieved 7 May 2026.
  20. ↑ Sheppard, Scott; Fernandez, Yanga; Moullet, Arielle (6 September 2018). "The Albedos, Sizes, Colors and Satellites of Dwarf Planets Compared with Newly Measured Dwarf Planet 2013 FY27". The Astronomical Journal. 156 (6): 270. arXiv:1809.02184. Bibcode:2018AJ....156..270S. doi:10.3847/1538-3881/aae92a. S2CID 119522310.
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