90568 Goibniu

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90568 Goibniu
2004-gv9 hst.jpg
Goibniu imaged by the Hubble Space Telescope on 17 March 2010
Discovery [1]
Discovered by NEAT (obs. code 644)
Discovery site Palomar Obs.
Discovery date13 April 2004
Designations
(90568) Goibniu
Pronunciation /ˈɡɔɪvnjuː/
Named after
 Goibniu
2004 GV9
Orbital characteristics   (barycentric) [6]
Epoch 5 May 2025 (JD 2460800.5)
Uncertainty parameter 0 [2] or 1 [1]
Observation arc 70+ yr
Earliest precovery date21 December 1954 [1]
Aphelion 45.160 AU
Perihelion 38.730 AU
41.945 AU
Eccentricity 0.0766
271.48  yr (99,158  d)
48.258°
0° 0m 13.07s / day
Inclination 21.983°
250.605°
292.116°
Known satellites 0
Physical characteristics
680±34 km [3]
Mean density
>0.37 g/cm3 (lower limit) [7]
5.86±0.03
0.077+0.0084
−0.0077 [3]
19.9 [10]

    90568 Goibniu (provisional designation 2004 GV9) is a large trans-Neptunian planetoid 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 

    Contents

    Goibniu is 680±34 km 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 including Noemi Pinilla-Alonso and Michael E. Brown 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 expected of a dwarf planet. [13]

    History

    Discovery

    Goibniu was discovered on 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 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

    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]

    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 2004 GV9-orbit.png
    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] [a] 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]

    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 

    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 2 3 4 5 6 7 "(90568) = 2004 GV9". Minor Planet Center. Retrieved 18 August 2025.
    2. 1 2 3 "JPL Small-Body Database Lookup: 90568 (2004 GV9)" (2025-06-22 last obs.). Jet Propulsion Laboratory . Retrieved 18 August 2025.
    3. 1 2 3 4 5 6 7 8 Vilenius, E.; Kiss, C.; Mommert, M.; Müller, T.; Santos-Sanz, P.; Pal, A.; et al. (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. arXiv: 1204.0697 . Bibcode:2012A&A...541A..94V. doi: 10.1051/0004-6361/201118743 . S2CID   54222700. A94.
    4. 1 2 3 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.
    5. ↑ Marc W. Buie. "Orbit Fit and Astrometric record for 90568" (2004-06-09 using 46 of 47 observations). SwRI (Space Science Department). Retrieved 4 October 2009.
    6. 1 2 3 4 5 "JPL Horizons On-Line Ephemeris for 90568 (2004 GV9) at epoch JD 2460800.5". JPL Horizons On-Line Ephemeris System . Jet Propulsion Laboratory. Retrieved 18 August 2025. Solution using the Solar System Barycenter. Ephemeris Type: Elements and Center: @0)
    7. 1 2 3 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. Bibcode:2008A&A...490..829D. doi: 10.1051/0004-6361:200809615 .
    8. ↑ Tegler, Stephen C. (1 February 2007). "Kuiper Belt Object Magnitudes and Surface Colors". Archived from the original on 1 September 2006. Retrieved 30 December 2009.
    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. arXiv: 0804.2864 . Bibcode:2008AJ....136.1502R. doi:10.1088/0004-6256/136/4/1502. S2CID   117167835.
    10. ↑ "AstDys (90568) 2004GV9 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 6 October 2009.
    11. ↑ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology . Retrieved 30 August 2016.
    12. ↑ Pinilla-Alonso, Noemi (August 2015). "Icy Dwarf Planets: Colored Popsicles in the Outer Solar System". Proceedings of the International Astronomical Union. 11: 241–246. Bibcode:2016IAUFM..29A.241P. doi: 10.1017/S1743921316002970 . A29A.
    13. ↑ 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.
    14. 1 2 3 4 5 Yeung, W. K. Y.; Stevens, B. L.; Sanchez, S.; Stoss, R.; Nomen, J.; Pravdo, S.; et al. (14 April 2004). "MPEC 2004-G32 : 2004 GV9". Minor Planet Electronic Circular. 2004-G32. Minor Planet Center. Bibcode:2004MPEC....G...32Y . Retrieved 6 January 2010.
    15. 1 2 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. hdl:2014/11237. S2CID   131088143.
    16. 1 2 Stoss, R.; McNaught, R. H.; Sanchez, S.; Nomen, J.; Holvorcem, P. R.; Schwartz, M.; et al. (10 June 2004). "MPEC 2004-L17 : 2004 GV9". Minor Planet Electronic Circular. 2004-L17. Minor Planet Center. Bibcode:2004MPEC....L...17S . Retrieved 24 August 2025.
    17. ↑ "New- And Old-Style Minor Planet Designations". Minor Planet Center. Retrieved 24 August 2025.
    18. ↑ "M.P.C. 52569" (PDF). Minor Planet Circulars (52569). Minor Planet Center: 143. 30 August 2004. Retrieved 24 August 2025.
    19. 1 2 "Rules and Guidelines for Naming Non-Cometary Small Solar-System Bodies" (PDF). IAU Working Group for Small Bodies Nomenclature. 22 February 2025. Retrieved 24 August 2025.
    20. ↑ "WGSBN Bulletin (Vol. 5, No. 20)" (PDF). IAU. 1 September 2025. p. 7.
    21. ↑ "JPL Horizons On-Line Ephemeris for 90568 (2004 GV9) at epochs JD 2460800.5–2461000.5". JPL Horizons On-Line Ephemeris System . Jet Propulsion Laboratory. Retrieved 18 August 2025. 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. Bibcode:2007Icar..189..213L. doi:10.1016/j.icarus.2007.01.001. S2CID   122671996.
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