(303775) 2005 QU182

Large scattered-disc object (202421) 2005 UQ 513 April 2020 yes possible dwarf planet (303775) 2005 QU 182 File:Ολόκληρο το σχεδιάγραμμα της τροχιάς του.gif (303775) 2005 QU 182's orbit M. E. Brown D. L. Rabinowitz C. A. Trujillo Palomar Obs. 30 August 2005 (303775) 2005 QU 182 TNOSDO (barycentric)barycentric 09 June 2026 (JD 2461200.5) 189.12 AU Tm on on (Q) 36.817 AU Tm on (q) 112.97 AU Tm on (a) 0.6741 (e) 1200.7 yr (438,600 d) 14.048° (i) 78.27° (Ω) 16.7° (M) 224.06° (ω) 0 584 155 144 km976.31 km416 73 km 5.256 19 kg (assumed) 9.61 hr 0.129 0.115 0.0460.3227 0.1133 CO 2-type ("double-dip") B–V 0.94 0.03V–R 0.54 0.03R–I 0.51 0.0316 ± 2%/100 nm 45 K (perihelion)11 20.9 3.99 0.023.75 0.01 0.000835 ms / day (n) 9.61 h d on on 18,818 days (51.52 yr) 1 36.015 AU Tm on 31.959 AU Tm on 6.732 (303775) 2005 QU 182 is a large trans-Neptunian object in the scattered disc. It was discovered on 30 August 2005 by American astronomers Mike Brown, David Rabinowitz and Chad Trujillo at the Palomar Observatory in California, with precovery images going back to 1974. It was assigned its permanent number in 2014. Its diameter is approximately 584 155 144 km, which makes it among the top 34 largest known trans-Neptunian objects. Its surface shows medium reddening and a composition rich in carbon dioxide ice. 2005 QU 182 completes one rotation every 9.61 hours. Simulations show that its orbit is unstable over a one-billion-year timeframe because of Neptune's gravity. The Hubble Space Telescope is scheduled to observe the object in 2026 to search for potential moons. If a moon is discovered, it could allow a direct measurement of its mass and density.1,3 History Discovery thumb|none|The 1.2-meter Samuel Oschin telescope that was used to discover 2005 QU 182 at Palomar Observatory 2005 QU 182 was discovered on 30 August 2005 by American astronomers Mike Brown, David Rabinowitz and Chad Trujillo at the Palomar Observatorydiscoverer The discoverer is labeled "Palomar" by the MPC. in California, United States. At the time, they were searching for distant trans-Neptunian objects using the observatory's 1.2-meter Samuel Oschin telescope. 2026, it has been observed 626 times over 52 years, with precovery images back to 1974. Further observations Following its discovery, 2005 QU 182 was tracked by multiple stations, including the Cerro Tololo Observatory, Las Campanas Observatory, and Mauna Kea Observatory. As of 2026, the object has been observed 626 times over an observation arc of 52 years. 2005 QU 182 is scheduled for observation with the Hubble Space Telescope in 2026, if those observations discover a moon, they could lead to a measurement of the mass and density of 2005 QU 182.1,3 Provisional designation and numbering The object was formally given the provisional designation 2005 QU 182 by the Minor Planet Center on 1 September 2007. The provisional designation of 2005 QU 182 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.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. 2005 QU 182 was assigned its permanent number 303775 in 2014.August 2026 Orbit and classification upright=2|thumb|right|2005 QU 182 takes around 1,200 years to orbit the Sun. Among large TNOs, only Sedna, 2012 VP 113, 2013 FS 28, (445473) 2010 VZ 98 and 2023 KQ 14 have a longer orbit around the Sun. 2005 QU 182 is a trans-Neptunian object that orbits the Sun at a distance of 36.8–189.1 AU with an semi-major axis or average orbital distance of 113.0 AU once every 1201 yearsbarycentric These orbital elements are expressed in terms of the Solar System Barycenter (SSB) as the frame of reference. Due to planetary perturbations, the Sun revolves around the SSB at non-negligible distances, so heliocentric-frame orbital elements and distances (such as those given in JPL's Small-Body Database) can vary on short timescales. (for reference, Neptune's orbit is at 30 AU).barycentric Its orbit has a high eccentricity of 0.674 and an inclination of 14.05° with respect to the ecliptic.barycentric 2005 QU 182 came to perihelion in 1971 and is currently 51.8 AU from the Sun. In April 2013, it moved beyond 50 AU from the Sun. 2005 QU 182 belongs to the scattered disc, 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.52 Both the Minor Planet Center (MPC) and Buie classify that 2005 QU 182 is a scattered disc object. Orbital stability In a 2021 study, scientists analyzed the orbital stability of 2005 QU 182 over a period of one billion years. At first, those models predicted that its orbit will be very stable, calculating a diffusion time of 68.272 billion years. However, a full 1 billion year simulation showed that the orbit is unstable, due to the object eventually entering the direct influence of Neptune's gravitational influence. In the simulations, none of its tracks managed to stay near its original orbit size. Even though its orbit size changes dramatically, none of the simulation tracks were completely lost or kicked out of the Solar System. Physical characteristics Size, mass and density thumb|180px|right|Second largest main belt asteroid 4 Vesta and 2005 QU 182 size and color comparison In 2012, the diameter of 2005 QU 182 was initially estimated to be 416 73 km using data from the Herschel Space Telescope. Later in 2020, the data was reanalyzed, which yielded a notably larger nominal diameter and uncertainty of 584 155 144 km, making it approximately ³/4 the size of the possible dwarf planet Aya.Aya Aya has a diameter of 768 km mi. ³/4 of Aya's diameter is 576 km mi, which is roughly around 2005 QU 182's size of 584 155 144 km. 2005 QU 182 is a relatively large trans-Neptunian object and is among the top 34 largest known TNOs.2 2005 QU 182 is not known to have any natural satellites or moons, which means there is currently no way to measure its mass and density.1,3 A 2021 study by Muñoz-Gutiérrez assumed a mass of 5.256 19 kg for 2005 QU 182. However, the true mass still remains unknown currently. 2005 QU 182's size is large enough that Mike Brown classify it as a possible dwarf planet, putting it in the 'probably' zone. However, based on its size of approximately 440 - 740 km, it belongs to the proposed class of "mid-sized" TNOs between 400 and 1000 km mi in diameter, which are believed to represent the transition between small, low-density TNOs and large, high-density dwarf planets.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.see List of possible dwarf planets talk page August 2026 Surface Composition and spectrum thumb|180px|right|Spectrum of 11 double dip (CO2) type large trans-Neptunian objects, 2005 QU 182 is the second from the top. 2005 QU 182 shares its composition with the CO 2-type (aka "double-dip") trans-Neptunian objects, which are commonly found on dynamically excited orbits such as those in the hot classical Kuiper belt.234, 236CO2-type The "double-dip" TNO spectral type were later renamed to the "CO 2-type" in 2025. The CO 2 type TNO exhibits two adjacent absorption minima in the 3 μm region, resulting in the “double dip” feature. Their spectra is dominated by carbon dioxide ices,carbon monoxide ices, and isotopologue ices, with other irradiation products like light hydrocarbons. The CO 2-type TNOs like 2005 QU 182 is the most common spectral type in the DiSco sample. Color, albedo and surface temperature 2005 QU 182 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, indicating a surface with medium reddening. Observations by the Herschel Space Telescope show that it has a geometric albedo of 0.129 0.115 0.046. The surface temperature of 2005 QU 182 at perihelion (closest point to the Sun) is estimated to be approximately 45 Kelvin.11 Brightness and visibility 2005 QU 182 has a bright absolute magnitude of 3.74. According to the Minor Planet Center, it is the seventh intrinsically brightest scattered-disc object. However, due to its very far distance from Earth, it has a dim apparent magnitude of 20.9 when viewed from Earth. Rotation According to a 2013 photometric survey, 2005 QU 182 has a rotation period of 9.61 hours, with its brightness varying by 0.12 magnitudes during each rotation, indicating an approximate spherical shape. Origin As a scattered-disc object, 2005 QU 182 is believed to have formed from a primordial disk of icy planetesimals surrounding the young Sun. During the early evolution of the Solar System, gravitational interactions with Neptune scattered the object into its current highly eccentric orbit. Exploration concepts 2005 QU 182 has not been visited by any spacecraft. A 2019 study on flyby mission opportunities between 2025 and 2040 calculated hypothetical trajectories to 2005 QU 182 using gravity assists from Jupiter, Saturn, and Neptune. These trajectories make launch windows between 2025 and 2033, with travel times ranging from 15.7 to 24.5 years. Two specific trajectories using swingbys of both Jupiter and Neptune have launch windows in April 2032, with arrival dates at 2005 QU 182 in 2048 and 2050. See also List of trans-Neptunian objects List of minor planets: 303001–304000 List of possible dwarf planets Scattered disc Notes References 30em 303775 2026-03-07 MPEC 2007-R03 : 2004 PF115, 2004 PG115, 2004 XA192, 2005 QU182 IAU Minor Planet Center 2007-09-01 http://minorplanetcenter.org/mpec/K07/K07R03.html 2009-08-26 List Of Centaurs and Scattered-Disk Objects Minor Planet Center http://www.minorplanetcenter.org/iau/lists/Centaurs.html 2009-01-22 Marc W. Buie Marc W. Buie 2008-10-24 Orbit Fit and Astrometric record for 05QU182 SwRI (Space Science Department) http://www.boulder.swri.edu/~buie/kbo/astrom/303775.html 2008-12-09 last observation: 2009-09-18 JPL Small-Body Database Browser: (2005 QU182) https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2005QU182 7 April 2016 AstDys 2005QU182 Ephemerides Department of Mathematics, University of Pisa, Italy https://newton.spacedys.com/astdys/index.php?pc=1.1.3.0&n=2005QU182 2009-03-16 https://web.archive.org/web/20110526232147/http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=2005QU182 2011-05-26 live http://ssd.jpl.nasa.gov/sbdb_query.cgi?obj_group=all;obj_kind=all;obj_numbered=all;OBJ_field=0;ORB_field=0;combine_mode=AND;c1_group=OBJ;c1_item=Ai;c1_op=%3C;c1_value=6;c2_group=ORB;c2_item=Bh;c2_op=%3E;c2_value=80;table_format=HTML;max_rows=200;format_option=comp;c_fields=AcBhBgBjBkBlBiBnBsCjCpCmCnCoAi;.cgifields=format_option;.cgifields=obj_kind;.cgifields=obj_group;.cgifields=obj_numbered;.cgifields=combine_mode;.cgifields=ast_orbit_class;.cgifields=table_format;.cgifields=com_orbit_class&query=1&c_sort=BhD JPL Small-Body Database Search Engine: H < 6 (mag) and a > 80 (AU) JPL Solar System Dynamics 2014-06-14 TNOs are Cool! 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Holler Elsa Hénault Ana Carolina de Souza Feliciano A JWST/DiSCo-TNOs portrait of the primordial Solar System through its trans-Neptunian objects https://hal.science/hal-04961629v1/file/s41550-024-02433-2.pdf Nature Astronomy December 2024 9 2 230–244 10.1038/s41550-024-02433-2 2025NatAs...9..230P 274932942 etal R. Brunetto E. Hénault S. Cryan N. Pinilla-Alonso J. P. Emery A. Guilbert-Lepoutre Spectral Diversity of DiSCo's TNOs Revealed by JWST: Early Sculpting and Late Irradiation The Astrophysical Journal Letters March 2025 982 1 L8 free 10.3847/2041-8213/adb977 2025ApJ...982L...8B 259287422 Donald K. Yeomans https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%278%27&TABLE_TYPE=%27ELEMENTS%27&START_TIME=%272000-01-01%27&STOP_TIME=%272000-01-02%27&STEP_SIZE=%27200%20years%27&CENTER=%27@0%27&OUT_UNITS=%27AU-D%27 HORIZONS Web-Interface for Neptune Barycenter (Major Body=8) JPL Horizons On-Line Ephemeris System 18 July 2014 7 September 2021 https://web.archive.org/web/20210907055935/https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%278%27&TABLE_TYPE=%27ELEMENTS%27&START_TIME=%272000-01-01%27&STOP_TIME=%272000-01-02%27&STEP_SIZE=%27200%20years%27&CENTER=%27%400%27&OUT_UNITS=%27AU-D%27 live —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)".) Brett Gladman Brian G. Marsden Christa VanLaerhoven Nomenclature in the Outer Solar System https://www.lpi.usra.edu/books/ssbn2008/7002.pdf The Solar System Beyond Neptune University of Arizona Press 2008 43–57 9780816527557 astro-ph/0702538 2008ssbn.book...43G 14469199 dead https://web.archive.org/web/20230801104434/https://www.lpi.usra.edu/books/ssbn2008/7002.pdf 1 August 2023 How Are Minor Planets Named? https://www.minorplanetcenter.net/iau/info/HowNamed.html Minor Planet Center 2026-08-10 H. Boehnhardt Schulz D. Protopapa S. Götz C. 2014-11-01 Photometry of Transneptunian Objects for the Herschel Key Program 'TNOs are Cool' https://doi.org/10.1007/s11038-014-9450-x Earth, Moon, and Planets en 114 1 35–57 10.1007/s11038-014-9450-x 1573-0794 subscription JPL/HORIZONS (303775) 2005 QU182 (Barycentric) https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%27303775%27&TABLE_TYPE=%27ELEMENTS%27&START_TIME=%27JD2461000.5%27&STOP_TIME=%27JD2461001.5%27&STEP_SIZE=%271y%27&CENTER=%27@0%27&OUT_UNITS=%27AU-D%27 JPL Horizons On-Line Ephemeris System Jet Propulsion Laboratory 2026-08-12 Solution using the Solar System Barycenter. Ephemeris Type: Elements and Center: @0) JPL/HORIZONS (303775) 2005 QU182 (Heliocentric) https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND='303775'&TABLE_TYPE='ELEMENTS'&START_TIME='JD2460800.5'&STOP_TIME='JD2461000.5'&STEP_SIZE='200d'&CENTER='500@10'&OUT_UNITS='AU-D' JPL Horizons On-Line Ephemeris System Jet Propulsion Laboratory 2026-08-12 Solution using the Sun. Ephemeris Type: Elements and Center: @sun) Gray Bill MPECs for 2007 Project Pluto https://www.projectpluto.com/mpecs/2007.htm az 2026-08-14 etal Bryan J. Holler Rosario Brunetto Dale P. Cruikshank Sasha Cryan Aurelie Guilbert-Lepoutre Brittany Harvison A Descriptive Taxonomic Nomenclature for Intermediate-sized Trans-Neptunian Object Spectra Research Notes of the American Astronomical Society September 2025 9 9 241 free 10.3847/2515-5172/ae03a2 2025RNAAS...9..241H IAU Minor Planet Center minorplanetcenter.net https://minorplanetcenter.net/db_search/show_object?object_id=303775 2026-08-14 Marco A. Muñoz-Gutiérrez Antoni Peimbert Matthew J. Lehner Shiang-Yu Wang Long-term Dynamical Stability in the Outer Solar System. I. The Regular and Chaotic Evolution of the 34 Largest Trans-Neptunian Objects The Astronomical Journal October 2021 162 4 164 free 10.3847/1538-3881/ac1102 2107.00240 2021AJ....162..164M 235694711 How many dwarf planets are there in the outer solar system? California Institute of Technology Michael E. Brown Michael E. Brown http://web.gps.caltech.edu/~mbrown/dps.html 13 September 2019 16 August 2026 https://web.archive.org/web/20191013130649/http://web.gps.caltech.edu/~mbrown/dps.html 13 October 2019 live etal E. Vilenius C. Kiss T. Müller M. Mommert P. Santos-Sanz A. Pál April 2014 "TNOs are Cool": A survey of the trans-Neptunian region. X. Analysis of classical Kuiper belt objects from Herschel and Spitzer observations Astronomy and Astrophysics 564 18 2014A&A...564A..35V 10.1051/0004-6361/201322416 free 1403.6309v1 118513049 List Of Centaurs and Scattered-Disk Objects https://www.minorplanetcenter.net/iau/lists/t_centaurs.html Minor Planet Center International Astronomical Union 29 December 2018 Benecchi Susan D. Sheppard Scott S. LIGHT CURVES OF 32 LARGE TRANSNEPTUNIAN OBJECTS The Astronomical Journal 145 5 2013-03-25 0004-6256 10.1088/0004-6256/145/5/124 124 https://iopscience.iop.org/article/10.1088/0004-6256/145/5/124 2026-08-19 1301.5791 Amanda M. Zangari Tiffany J. Finley S. Alan Stern Mark B. Tapley Return to the Kuiper Belt: Launch Opportunities from 2025 to 2040 Journal of Spacecraft and Rockets May 2019 56 3 919–930 10.2514/1.A34329 1810.07811 2019JSpRo..56..919Z 119033012 Éphémérides Formulaires https://ssp.imcce.fr/forms/ssocard fr 2026-09-09 Note: To get the physical parameters of 2005 QU 182, Search "2005 QU 182" in the search bar. External links 303775 303775 (303775) 2005 QU 182 303775 Category:Discoveries by Michael E. Brown Category:Discoveries by Chad Trujillo Category:Discoveries by David L. Rabinowitz 303775 20050830 Category:Possible dwarf planets