The following information shows the result of the orbit fit based on Gary Bernstein's method. Most of the information should be self-explanatory. Take special note that while the original Bernstein software works with barycentric coordinates, we convert these results into a heliocentric coordinate system.
# Object: 19GQ186 # Created Wed Nov 27 02:10:56 2024 # Orbit generated from Bernstein formalism # Fitting 9 observations of 9 # Arc: 83.94d # First observation: 2019/01/11 # Last observation: 2019/04/05 Preliminary a, adot, b, bdot, g, gdot: 0.000000 0.026797 -0.000001 0.007710 0.024561 0.000000 # WARNING Fitting with energy constraint # Chi-squared of fit: 4.39 DOF: 13 RMS: 0.12 # Min/Max residuals: -0.25 0.30 # Exact a, adot, b, bdot, g, gdot: 1.502370E-05 2.208319E-02 4.320987E-06 7.531126E-03 2.359949E-02 1.137452E-03 # Covariance matrix: 4.9171E-12 7.5008E-09 2.6343E-13 1.9535E-10 1.2752E-09 -9.1943E-09 7.5008E-09 1.2373E-05 4.3298E-10 3.2042E-07 2.0980E-06 -1.6274E-05 2.6343E-13 4.3298E-10 3.8115E-13 1.0022E-11 7.4592E-11 -3.0848E-10 1.9535E-10 3.2042E-07 1.0022E-11 8.7996E-09 5.5730E-08 -1.1062E-07 1.2752E-09 2.0980E-06 7.4592E-11 5.5730E-08 3.5975E-07 -1.8712E-06 -9.1943E-09 -1.6274E-05 -3.0848E-10 -1.1062E-07 -1.8712E-06 2.1892E-04 # lat0 lon0 xBary yBary zBary JD0 -7.277955 164.751731 0.802809 -0.073459 -0.575905 2458495.025361 # Heliocentric elements and errors Epoch: 2458490.5000 = 2019/01/07 Mean Anomaly: 22.08094 +/- 79.627 Argument of Peri: 313.06583 +/- 153.203 Long of Asc Node: 183.99230 +/- 2.648 Inclination: 19.94496 +/- 2.324 Eccentricity: 0.07133017 +/- 0.3069 Semi-Major Axis: 45.95496212 +/- 9.3119 Time of Perihelion: 2451511.1960 +/- 138940.2 Perihelion: 42.67698691 +/- 16.5426 Aphelion: 49.23293732 +/- 17.2742 Period (y) 311.5350 +/- 94.69 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X -40.90101048 +/- 1.0306 Ecliptic Y 11.97379137 +/- 0.2810 Ecliptic Z -5.36789186 +/- 0.1364 Ecliptic XDOT -0.00089896 +/- 0.0016 Ecliptic YDOT -0.00241010 +/- 0.0006 Ecliptic ZDOT 0.00084975 +/- 0.0002 # Distances at JD0 (AU) Heliocenter to KBO 42.95437814 +/- 0.9846 Geocenter to KBO 42.37380338 +/- 1.0770 # Hcoef: 8.83
The following table shows the complete astrometric record for 19GQ186. The first three columns show the date of observation. The next six columns are RA and DEC. The next column (when provided) is the observed magnitude and filter. The next column is the object name (19GQ186) followed by the observatory code and reference code for the source of the astrometry.
2019 01 11.52456 10 52 37.40 -00 42 49.3 25.0z 19GQ186 T09 C~870l 2019 01 11.57085 10 52 37.28 -00 42 49.1 25.1z 19GQ186 T09 C~870l 2019 01 11.61426 10 52 37.16 -00 42 48.4 24.8z 19GQ186 T09 C~870l 2019 01 11.65474 10 52 37.09 -00 42 48.3 25.5z 19GQ186 T09 C~870l 2019 04 04.38775 10 47 18.11 -00 06 32.9 25.5g 19GQ186 T09 C~870l 2019 04 04.42571 10 47 17.98 -00 06 31.6 25.8g 19GQ186 T09 C~870l 2019 04 05.38680 10 47 14.65 -00 06 01.2 25.2r 19GQ186 T09 C~870l 2019 04 05.43322 10 47 14.48 -00 05 59.5 24.9r 19GQ186 T09 C~870l 2019 04 05.46471 10 47 14.38 -00 05 58.8 24.8r 19GQ186 T09 C~870l
The following table shows the residuals to the orbit fit. The first coumn is the point number. The second column is the time, in years, measured from the first observation. The third and fifth columns are the regularized positions used in the orbit fit. The fourth and sixth columns are the residuals, in arc seconds, for RA and Dec respectively.
1 0.0000 0.00 -0.05 0.00 0.15
2 0.0001 -1.74 -0.00 -0.51 -0.13
3 0.0002 -3.67 -0.25 -0.55 0.04
4 0.0004 -4.68 0.30 -0.86 -0.07
5 0.2269 -5258.89 -0.02 171.10 -0.03
6 0.2270 -5261.19 0.02 171.55 0.09
7 0.2296 -5319.02 0.04 180.45 -0.06
8 0.2297 -5322.03 -0.14 181.04 0.11
9 0.2298 -5323.69 0.11 181.11 -0.11
The following table comes from a 10My integration of the orbit of the object. Three columns are shown. The first column is the result of integrating the nominal orbit. The other two columns are based on clones of the nominal orbit that are +/- 3 sigma from the nominal orbit. If all three types agree then the classificiation is deemed secure. The basis for these calculations is described in more detail in AJ, 129, 1117 (2005). Any use made of these calculations should refer to and credit this publication and the Deep Ecliptic Survey Team.