Astronomy:90568 Goibniu

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90568 Goibniu
Goibniu imaged by the Hubble Space Telescope on 17 March 2010
Discovery[1]
Discovered byNEAT (obs. code 644)
Discovery sitePalomar Obs.
Discovery date13 April 2004
Designations
(90568) Goibniu
Pronunciation/ˈɡɔɪvnjuː/
Named afterGoibniu (mod. Gaibhne)
2004 GV9
Minor planet category
Orbital characteristics[6]
Epoch 5 May 2025 (JD 2460800.5)
Uncertainty parameter 0[2] or 1[1]
Observation arc70+ yr
Earliest precovery date21 December 1954[1]
|{{{apsis}}}|helion}}45.160 AU
|{{{apsis}}}|helion}}38.730 AU
41.945 AU
Eccentricity0.0766
Orbital period271.48 yr (99,158 d)
Mean anomaly48.258°
Mean motion0° 0m 13.07s / day
Inclination21.983°
Longitude of ascending node250.605°
292.116°
Known satellites0
Physical characteristics
Mean diameter680±34 km[3]
Mean density>0.37 g/cm3 (lower limit)[7]
Sidereal rotation period5.86±0.03
Geometric albedo0.077+0.0084
−0.0077[3]
Apparent magnitude19.9[10]
Absolute magnitude (H)


90568 Goibniu (provisional designation 2004 GV9) is a large trans-Neptunian object that was discovered in 2004 by the Near-Earth Asteroid Tracking survey at Palomar Observatory.[1] It is classified as a classical Kuiper belt object of the dynamically "hot" population, which follow highly inclined or eccentric orbits around the Sun.[3]: 2 

Goibniu is 680 ± 34 km (423 ± 21 mi) in diameter, according to measurements of its infrared thermal emission by the Herschel and Spitzer space telescopes.[3] It shows small variations in brightness (0.16 magnitudes) over its 5.86-hour rotation period.[7] Some astronomers have suggested that Goibniu is large enough that it could be a dwarf planet.[11][12] However, the shape of Goibniu is unknown–it could either be a spheroid with small albedo spots or an ellipsoid whose rotation axis is pointed towards Earth.[7] Furthermore, its low albedo suggests it has never been resurfaced and thus is unlikely to have the planetary geology thought to be typical of dwarf planets.[13]

History

Discovery

Goibniu was discovered on 13 April 2004 by the Near-Earth Asteroid Tracking (NEAT) survey,[14] which was a NASA-directed project for finding near-Earth asteroids in the sky using telescopes at various observatories across the United States.[15] The telescope that discovered Goibniu was the 1.22-meter (48 in) Samuel Oschin telescope at Palomar Observatory in San Diego County, California.[14] The people involved in making the discovery observations at Palomar included Steven Pravdo, D. MacDonald, Kenneth Lawrence and Michael D. Hicks.[14][15] The discovery of Goibniu was announced by the Minor Planet Center (MPC) on 14 April 2004, after several other observatories observed the object.[14]

Precovery

Precovery observations of Goibniu were first reported by astronomer Reiner Stoss and published by the MPC on 10 June 2004.[16] These precovery observations, which came from Digitized Sky Survey images from 1993–1997, allowed for an accurate determination of Goibniu's orbit without the need for follow-up observations.[16] Even earlier precovery observations have since been reported, from dates as early as December 1954.[1]

Number and name

Number

This object has the minor planet provisional designation 2004 GV9, which was given by the MPC in the discovery announcement.[14] The provisional designation indicates the year and half-month of the object's discovery date.[17] 2004 GV9 received its permanent minor planet catalog number of 90568 from the MPC on 30 August 2004.[18]

Name

Until 2025, 2004 GV9 did not have a proper name and the discoverers' privilege for naming this object expired ten years after it was numbered.[1][19]: 6  According to naming guidelines by the International Astronomical Union's Working Group for Small Bodies Nomenclature, 2004 GV9 was open for name suggestions that relate to creation myths, as recommended for Kuiper belt objects in general.[19]: 8  On 1 September 2025, it was officially named Goibniu, after the Irish god of metallurgy and hospitality.[20]

Orbit

Diagram showing Goibniu's orbit (gray) around the Sun, with the outer planets shown

Goibniu is a trans-Neptunian object orbiting the Sun at a semi-major axis or average distance of 41.9 astronomical units (AU).[6][lower-alpha 1] It has an orbital eccentricity of 0.08 and an inclination of 22° with respect to the ecliptic.[6] In its 271-year-long orbit, Goibniu comes as close as 38.7 AU from the Sun at perihelion and as far as 45.2 AU from the Sun at aphelion.[6]

Classification

Goibniu is located in the classical region of the Kuiper belt 39–48 AU from the Sun,[4]: 53  and is thus classified as a classical Kuiper belt object (sometimes known as a "cubewano").[4]: 55  The high orbital inclination of Goibniu makes it a dynamically "hot" member of the classical Kuiper belt.[3]: 3  The hot classical Kuiper belt objects are believed to have been scattered by Neptune's gravitational influence during the Solar System's early history.[22]: 230 

Physical characteristics

Size

History of size estimates for Goibniu
Year Diameter (km) References
2007 677.2+71.3
−69.3 		[23]
2008 636 [24]
2008 684+68
−78 		[25]
2010 677 [26]
2012 680±34 [27]

According to measurements of its infrared thermal emission by the Herschel and Spitzer space telescopes, Goibniu has a diameter of 680 ± 34 km (423 ± 21 mi)[3] Goibniu is large enough that some astronomers including Noemi Pinilla-Alonso and Michael Brown once considered it as a possible dwarf planet.[26][28][12][29]. Gonzalo Tancredi also considered it as a possible dwarf planet in 2010, though he did not propose its official classification to the IAU.[26] However, its low albedo suggests it has never been resurfaced and thus is unlikely to have the planetary geology thought to be typical of dwarf planets.[13]

Rotation, shape and density

Based on light curve observations, Goibniu rotates once on its axis every 5.86±0.03 hours. Goibniu has a fairly low light curve amplitude of 0.16±0.03,[7] which suggests that it could either be a spheroid with small albedo spots or an ellipsoid whose rotation axis is pointed towards Earth.[7] However light curve studies measured that it has an estimated b to a axis ratio being around b/a=1.16±0.03.[30] Its mass and density is unknown, because it has no known moons for scientists calculate the exact mass and density of it through Kepler's third law. However, we can still estimate its density through assuming it's a stable Jacobii ellipsoid. Then the results of its density will be approximately between 1.14 to 1.49 g/cm³ with an absolute lowest limit of 0.37 g/cm³.[30]

Surface and spectra

Goibniu is a moderately red trans-Neptunian object with a measured V-R color index of approximately 0.52.[8] It has a dark surface with a very low geometric albedo of about 0.077+0.0084
−0.0077.[3]

See also

Notes

  1. ↑ These orbital elements are expressed in terms of the Solar System Barycenter (SSB) as the frame of reference.[6] Due to planetary perturbations, the Sun revolves around the SSB at non-negligible distances, so heliocentric-frame orbital elements and distances can vary in short timescales as shown in JPL-Horizons.[21]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "(90568) Goibniu = 2004 GV9". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=90568. Retrieved 2025-08-18. 
  2. ↑ 2.0 2.1 2.2 "JPL Small-Body Database Lookup: 90568 Goibniu (2004 GV9)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=20090568. Retrieved 2025-08-18. 
  3. ↑ 3.00 3.01 3.02 3.03 3.04 3.05 3.06 3.07 3.08 3.09 Vilenius, E.Expression error: Unrecognized word "etal". (May 2012). ""TNOs are Cool": A survey of the trans-Neptunian region VI. Herschel/PACS observations and thermal modeling of 19 classical Kuiper belt objects". Astronomy & Astrophysics 541: 17. doi:10.1051/0004-6361/201118743. A94. Bibcode: 2012A&A...541A..94V. 
  4. ↑ 4.0 4.1 4.2 Gladman, Brett; Marsden, Brian G.; VanLaerhoven, Christa (2008). "Nomenclature in the Outer Solar System". The Solar System Beyond Neptune. University of Arizona Press. pp. 43–57. ISBN 9780816527557. Bibcode: 2008ssbn.book...43G. https://www.lpi.usra.edu/books/ssbn2008/7002.pdf. 
  5. ↑ Marc W. Buie. "Orbit Fit and Astrometric record for 90568". SwRI (Space Science Department). http://www.boulder.swri.edu/~buie/kbo/astrom/90568.html. Retrieved 2009-10-04. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 "JPL Horizons On-Line Ephemeris for 90568 Goibniu (2004 GV9) at epoch JD 2460800.5". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND='90568'&TABLE_TYPE='ELEMENTS'&START_TIME='JD2460800.5'&STOP_TIME='JD2460801.5'&STEP_SIZE='1y'&CENTER='@0'&OUT_UNITS='AU-D'. Retrieved 2025-08-18.  Solution using the Solar System Barycenter. Ephemeris Type: Elements and Center: @0)
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Dotto, E.; Perna, D.; Barucci, M. A.; Rossi, A.; de Bergh, C.; Doressoundiram, A. (November 2008). "Rotational properties of Centaurs and Trans-Neptunian Objects. Lightcurves and densities". Astronomy & Astrophysics 490 (2): 829–833. doi:10.1051/0004-6361:200809615. Bibcode: 2008A&A...490..829D. 
  8. ↑ 8.0 8.1 Tegler, Stephen C. (2007-02-01). "Kuiper Belt Object Magnitudes and Surface Colors". Archived from the original on 2006-09-01. https://web.archive.org/web/20060901063349/http://www.physics.nau.edu/~tegler/research/survey.htm. Retrieved 2009-12-30. 
  9. ↑ David L. Rabinowitz; Bradley E. Schaefer; Martha W. Schaefer; Suzanne W. Tourtellotte (2008). "The Youthful Appearance of the 2003 EL61 Collisional Family". The Astronomical Journal 136 (4): 1502–1509. doi:10.1088/0004-6256/136/4/1502. Bibcode: 2008AJ....136.1502R. 
  10. ↑ "AstDys (90568) 2004GV9 Ephemerides". Department of Mathematics, University of Pisa, Italy. https://newton.spacedys.com/astdys/index.php?pc=1.1.3.0&n=90568. Retrieved 2009-10-06. 
  11. ↑ Michael E. Brown (2013). "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. http://web.gps.caltech.edu/~mbrown/dps.html. Retrieved 30 August 2016. 
  12. ↑ 12.0 12.1 Pinilla-Alonso, Noemi (August 2015). "Icy Dwarf Planets: Colored Popsicles in the Outer Solar System". Proceedings of the International Astronomical Union 11: 241–246. doi:10.1017/S1743921316002970. A29A. Bibcode: 2016IAUFM..29A.241P. 
  13. ↑ 13.0 13.1 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)". Icarus 334: 30–38. doi:10.1016/j.icarus.2018.12.037. Bibcode: 2019Icar..334...30G. http://www2.lowell.edu/users/grundy/abstracts/preprints/2019.G-G.pdf. 
  14. ↑ 14.0 14.1 14.2 14.3 14.4 Yeung, W. K. Y.Expression error: Unrecognized word "etal". (2004-04-14). "MPEC 2004-G32 : 2004 GV9". Minor Planet Electronic Circular (Minor Planet Center) 2004-G32. Bibcode: 2004MPEC....G...32Y. https://www.minorplanetcenter.net/iau/mpec/K04/K04G32.html. Retrieved 2010-01-06. 
  15. ↑ 15.0 15.1 Bambery, Raymond J.; Helin, Eleanor F.; Pravdo, Steven H.; Lawrence, Kenneth J.; Hicks, Michael D. (September 2002). "An update of the Near-Earth Asteroid Tracking/Maui Space Surveillance System (NEAT/MSSS) collaboration". 2002 AMOS Technical Conference. Maui, Hawaii. https://dataverse.jpl.nasa.gov/file.xhtml?fileId=42940&version=2.0. 
  16. ↑ 16.0 16.1 Stoss, R.Expression error: Unrecognized word "etal". (2004-06-10). "MPEC 2004-L17 : 2004 GV9". Minor Planet Electronic Circular (Minor Planet Center) 2004-L17. Bibcode: 2004MPEC....L...17S. https://www.minorplanetcenter.net/iau/mpec/K04/K04L17.html. Retrieved 2025-08-24. 
  17. ↑ "New- And Old-Style Minor Planet Designations". Minor Planet Center. https://www.minorplanetcenter.net/iau/info/DesDoc.html. Retrieved 2025-08-24. 
  18. ↑ "M.P.C. 52569". Minor Planet Circulars (Minor Planet Center) (52569): 143. 2004-08-30. https://minorplanetcenter.net/iau/ECS/MPCArchive/2004/MPC_20040830.pdf#page=143. Retrieved 2025-08-24. 
  19. ↑ 19.0 19.1 "Rules and Guidelines for Naming Non-Cometary Small Solar-System Bodies". IAU Working Group for Small Bodies Nomenclature. 2025-02-22. https://www.wgsbn-iau.org/documentation/NamesAndCitations.pdf. Retrieved 2025-08-24. 
  20. ↑ "WGSBN Bulletin (Vol. 5, No. 20)". IAU. 2025-09-01. p. 7. https://www.wgsbn-iau.org/files/Bulletins/V005/WGSBNBull_V005_020.pdf. 
  21. ↑ "JPL Horizons On-Line Ephemeris for 90568 Goibniu (2004 GV9) at epochs JD 2460800.5–2461000.5". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND='90568'&TABLE_TYPE='ELEMENTS'&START_TIME='JD2460800.5'&STOP_TIME='JD2461000.5'&STEP_SIZE='200d'&CENTER='500@10'&OUT_UNITS='AU-D'. Retrieved 2025-08-18.  Solution using the Sun. Ephemeris Type: Elements and Center: @sun)
  22. ↑ Lykawka, Patryk Sofia; Tadashi, Mukai (July 2007). "Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation". Icarus 189 (1): 213–232. doi:10.1016/j.icarus.2007.01.001. Bibcode: 2007Icar..189..213L. 
  23. ↑ J. Stansberry u. a. (2007-02-20). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope (PDF; 1,3 MB)" (in en). University of Arizona Press 592 (161–179). Bibcode: 2008ssbn.book..161S. 
  24. ↑ G. Tancredi, S. Favre. "Which are the dwarfs in the solar system?" (in en). Dwarf Planets and Plutoid Headquarters, von. https://www.lpi.usra.edu/meetings/acm2008/pdf/8261.pdf. Retrieved 2019-03-12.  DPPH list:
  25. ↑ M. Brucker u. a. (2009-01-01). "High Albedos of Low Inclination Classical Kuiper Belt Objects (PDF)" (in en). Icarus: 26. doi:10.1016/j.icarus.2008.12.040. Bibcode: 2012A&A...546A..86P. https://pure.qub.ac.uk/portal/files/121297485/1206.3153v1.pdf. 
  26. ↑ 26.0 26.1 26.2 Tancredi, Gonzalo (6 April 2010). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Proceedings of the International Astronomical Union 5 (S263): 173–185. doi:10.1017/S1743921310001717. Bibcode: 2010IAUS..263..173T. 
  27. ↑ E. Vilenius u. a. (2012-04-04). "“TNOs are Cool”: A survey of the trans-Neptunian region VI. Herschel/PACS observations and thermal modeling of 19 classical Kuiper belt objects (PDF; 826 kB)" (in en). Astronomy and Astrophysics 541 (A94): 17. doi:10.1051/0004-6361/201118743. Bibcode: 2012A&A...541A..94V. https://arxiv.org/pdf/1204.0697.pdf. 
  28. ↑ Grundy, W. M.; McKinnon, W. B.; Ammannito, E.; Aung, M.; Bellerose, J.; Brenker, F. (December 2009). "Exploration Strategy for the Ice Dwarf Planets 2013-2022". American Geophysical Union Fall Meeting 2009. P43D-1471. Bibcode: 2009AGUFM.P43D1471G. https://www.lpi.usra.edu/decadal/sbag/community_wp/SB_Community_WP_Final_Dwarfs.pdf. 
  29. ↑ Pinilla-Alonso, Noemí; Stansberry, John; Holler, Bryan (2020). "Chapter 18 - Surface properties of large TNOs: Expanding the study to longer wavelengths with the James Webb Space Telescope". The Transneptunian Solar System. Elsevier. pp. 395–412. doi:10.1016/B978-0-12-816490-7.00018-7. ISBN 978-0-12-816490-7. Bibcode: 2019arXiv190512320P. 
  30. ↑ 30.0 30.1 Miville-Deschênes, M.-A.; Yvon, D.; Magneville, C.; Boulanger, F.; Lagache, G.; Piat, M.; Giard, M. (November 2008). "Separation of anomalous and synchrotron emissions using WMAP polarization data". Astronomy & Astrophysics 490 (3): 1135–1142. doi:10.1051/0004-6361:200809615. Bibcode: 2008A&A...490.1135M. https://www.aanda.org/articles/aa/pdf/2008/41/aa09615-08.pdf. Retrieved 2024-05-22. 



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