(523622) 2007 TG422

Trans-Neptunian object October 2018 yes (523622) 2007 TG 422 #C2E0FF Planet_nine-etnos_now.png Orbital diagram of extreme trans-Neptunian objects, including 2007 TG 422, together with the hypothetical Planet Nine A. C. Becker A. W. Puckett J. Kubica APO 3 October 2007 (523622) 2007 TG 422 TNO SDO ESDO p-DP distant 27 April 2019 (JD 2458600.5) 1 13.14 yr (4,800 d) 910.01 AU 35.532 AU 472.77 AU 0.9248 10279.78 yr (3,754,688 d) 0.4774° 0.0001 ms / day 18.620° 112.84° 285.54° 222 km 330 km 0.04 (est.) blue B–I 1.900 0.020 B–R 1.390 0.040 R–I 0.510 0.040 V–R 0.510 0.040 22.4 6.5 (523622) 2007 TG 422 is a trans-Neptunian object on a highly eccentric orbit in the scattered disc region at the edge of Solar System. Approximately 260 km mi off 2 us in diameter, it was discovered on 3 October 2007 by astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica during the Sloan Digital Sky Survey at Apache Point Observatory in New Mexico, United States. It belongs to a group of objects studied in 2014, which led to the proposition of the hypothetical Planet Nine. Orbit and classification 2007 TG 422 orbits the Sun at a distance of 35.5–910 AU once every 10279 years and 9 months (3,754,688 days; semi-major axis of 473 AU). Its orbit has an exceptionally high eccentricity of 0.92 and an inclination of 19° with respect to the ecliptic. 2007 TG 422 is an extended scattered disc object, as its large aphelion distance is similar to that of the detached objects such as the sednoids (e.g. 90377 Sedna), its perihelion distance, however, is much lower and still just inside the gravitational influence of Neptune. The object came to perihelion in 2005 at a heliocentric distance of 35.5 AU, and is currently 37.9 AU from the Sun. It was in the constellation of Taurus until 2018, and came to opposition 29 November 2017. The body's observation arc begins at Apache Point in September 2007, one month prior to its official discovery observation. It has since been observed over a hundred times and has an orbital uncertainty of 1. Unstable heliocentric solutions YearHeliocentric solution unstable due to the changing position of Jupiter over Jupiter's 12 year orbit which perturbs the eccentricity of the two-body solution of the Sun+asteroid. Barycentric solutions are more stable for objects that take thousands of years to orbit the Sun. footnoteB lower-alpha(epoch) Aphelion(AU) Orbitalperiodyears 28 August 2007 932 10652 30 September 2012 1099 13512 16 February 2017 917 10399 26 June 2018 901 10143 StableBarycentric2017 970 11300 Given the orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the aphelion (maximum distance from the Sun) of this object.Read osculating orbit for more details about heliocentric unperturbed two-body solutions With a 2007 epoch the object had an approximate period of about 10,611 years with aphelion at 930 AU. But using a 2012 epoch shows a period of about 13,512 years with aphelion at 1099 AU. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates. Using JPL Horizons with an observed orbital arc of 5 years, the barycentric orbital elements for epoch 2008-May-14 generate a semi-major axis of 503 AU and a period of 11,300 years. For comparison, Sedna has a barycentric semi-major axis of 506 AU and a period of 11,400 years. Both (308933) 2006 SQ 372 and (87269) 2000 OO 67 take longer than Sedna and 2007 TG 422 to orbit the Sun using barycentric coordinates. Numbering and naming This minor planet was numbered by the Minor Planet Center on 25 September 2018 (M.P.C. 111778). As of 2025, it has not been named. Physical characteristics 2007 TG 422 is expected to have a low albedo (see below) due to its blue (neutral) color. Diameter and albedo According to Johnston's Archive and to Michael Brown, 2007 TG 422 measures 222 and 331 kilometers in diameter, based on an absolute magnitude of 6.5 and an assumed standard albedo of 0.09 and 0.04 for the body's surface, respectively. As of 2018, no rotational lightcurve has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. Comparison thumb|center|500px|The orbits of Sedna, 2012 VP 113, Leleākūhonua, and other very distant objects along with the predicted orbit of Planet Nine. The three sednoids (pink) along with the red-colored extreme trans-Neptunian object (eTNO) orbits are suspected to be aligned with the hypothetical Planet Nine while the blue-colored eTNO orbits are anti-aligned. The highly elongated orbits colored brown include centaurs and damocloids with large aphelion distances over 200 AU. left Notes lower-alpha References 30em 2018-01-13 last obs. JPL Small-Body Database Browser: 523622 (2007 TG422) https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2523622 Jet Propulsion Laboratory 10 October 2018 523622 (2007 TG422) Minor Planet Center https://www.minorplanetcenter.net/db_search/show_object?object_id=523622 10 October 2018 MPC/MPO/MPS Archive Minor Planet Center https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html 10 October 2018 List Of Centaurs and Scattered-Disk Objects Minor Planet Center https://www.minorplanetcenter.net/iau/lists/t_centaurs.html 10 October 2018 List of Known Trans-Neptunian Objects Johnston's Archive 30 December 2017 Johnston Wm. Robert http://www.johnstonsarchive.net/astro/tnoslist.html 10 October 2018 How many dwarf planets are there in the outer solar system? California Institute of Technology Brown Michael E. http://web.gps.caltech.edu/~mbrown/dps.html 10 October 2018 Asteroid (523622) 2007 TG422 Small Bodies Data Ferret https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=2007+TG422 10 October 2018 3 November 2020 https://web.archive.org/web/20201103065711/https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=2007+TG422 dead Asteroid (523622) 2007 TG422 AstDyS-2, Asteroids Dynamic Site Department of Mathematics, University of Pisa, Italy https://newton.spacedys.com/astdys/index.php?pc=1.1.3.0&n=2007TG422 10 October 2018 https://web.archive.org/web/20160902015013/http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=2007TG422 2 September 2016 dead MPEC 2008-D39: 2007 TG422, 2007 TH422, 2007 TJ422, 2007 UL126, 2007 VH305 IAU Minor Planet Center 2008-02-26 http://minorplanetcenter.org/mpec/K08/K08D39.html 2011-01-30 (K07Tg2G) Marc W. Buie Marc W. Buie 2009-09-28 using 32 of 32 observations Orbit Fit and Astrometric record for 07TG422 SwRI (Space Science Department) http://www.boulder.swri.edu/~buie/kbo/astrom/523622.html https://web.archive.org/web/20150530210009/http://www.boulder.swri.edu/~buie/kbo/astrom/07TG422.html 2015-05-30 live 2011-01-30 https://archive.today/20121213135903/http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2007TG422 JPL Epoch 2012-Sep-30 solution 2011-01-30 Horizons output http://home.surewest.net/kheider/astro/2007TG422Barycenter.txt Barycentric Osculating Orbital Elements for 2007 TG422 2011-01-30 dead https://web.archive.org/web/20140328023855/http://home.surewest.net/kheider/astro/2007TG422Barycenter.txt March 28, 2014 (Horizons) 6 Nathan A. Kaib Andrew C. Becker R. Lynne Jones Andrew W. Puckett Dmitry Bizyaev Benjamin Dilday Joshua A. Frieman Daniel J. Oravetz Kaike Pan Thomas Quinn Donald P. Schneider Shannon Watters April 2009 2006 SQ372: A Likely Long-Period Comet from the Inner Oort Cloud The Astrophysical Journal 695 1 268–275 2009ApJ...695..268K 10.1088/0004-637X/695/1/268 0901.1690 16987581 Chadwick A. Trujillo Scott S. Sheppard March 2014 A Sedna-like body with a perihelion of 80 astronomical units Nature 507 7493 471–474 2014Natur.507..471T 10.1038/nature13156 24670765 4393431 External links Discovery Circumstances: Numbered Minor Planets (520001)–(525000) Minor Planet Center 523622 523622 (523622) 2007 TG 422 523622 523622 Category:Discoveries by Andrew C. Becker Category:Discoveries by Andrew W. Puckett Category:Discoveries by Jeremy Martin Kubica 20071003 Category:Inner Oort cloud