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: 19JX147 # Created Wed Nov 27 02:10:57 2024 # Orbit generated from Bernstein formalism # Fitting 10 observations of 10 # Arc: 54.04d # First observation: 2019/04/07 # Last observation: 2019/05/31 Preliminary a, adot, b, bdot, g, gdot: 0.000000 0.024490 0.000005 -0.002883 0.024040 0.000000 # WARNING Fitting with energy constraint # Chi-squared of fit: 7.95 DOF: 15 RMS: 0.16 # Min/Max residuals: -0.40 0.28 # Exact a, adot, b, bdot, g, gdot: 1.597010E-05 2.342688E-02 -1.263614E-06 -2.605856E-03 2.392636E-02 -9.367935E-03 # Covariance matrix: 7.4369E-13 6.3884E-12 1.1404E-14 -2.4928E-12 3.6372E-12 -1.9996E-10 6.3884E-12 4.4808E-09 1.5320E-11 -1.1580E-09 4.4629E-10 -5.0846E-07 1.1404E-14 1.5320E-11 6.5486E-13 -8.6289E-12 9.8677E-13 -1.9873E-09 -2.4928E-12 -1.1580E-09 -8.6289E-12 3.4991E-10 -1.0890E-10 1.3596E-07 3.6372E-12 4.4629E-10 9.8677E-13 -1.0890E-10 9.8283E-11 -2.8995E-08 -1.9996E-10 -5.0846E-07 -1.9873E-09 1.3596E-07 -2.8995E-08 6.7519E-05 # lat0 lon0 xBary yBary zBary JD0 -6.390943 160.195399 -0.592079 -0.089720 -0.801141 2458580.804461 # Heliocentric elements and errors Epoch: 2458580.5000 = 2019/04/07 Mean Anomaly: 321.45813 +/- 23.937 Argument of Peri: 307.46588 +/- 5.299 Long of Asc Node: 295.87169 +/- 0.241 Inclination: 8.81203 +/- 0.036 Eccentricity: 0.41083952 +/- 0.3681 Semi-Major Axis: 54.17959632 +/- 20.4905 Time of Perihelion: 2474175.3898 +/- 3942.5 Perihelion: 31.92047701 +/- 23.3130 Aphelion: 76.43871563 +/- 35.1209 Period (y) 398.8062 +/- 226.24 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X -40.03627862 +/- 0.0162 Ecliptic Y 13.78054839 +/- 0.0058 Ecliptic Z -4.65229749 +/- 0.0019 Ecliptic XDOT 0.00013356 +/- 0.0009 Ecliptic YDOT -0.00289531 +/- 0.0003 Ecliptic ZDOT -0.00017723 +/- 0.0001 # Distances at JD0 (AU) Heliocenter to KBO 42.59637299 +/- 0.0153 Geocenter to KBO 41.79491314 +/- 0.0173 # Hcoef: 8.53
The following table shows the complete astrometric record for 19JX147. 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 (19JX147) followed by the observatory code and reference code for the source of the astrometry.
2019 04 07.30366 10 37 13.40 +01 49 22.0 25.7g 19JX147 T09 C~8Mhu 2019 04 07.37920 10 37 13.16 +01 49 24.0 25.2g 19JX147 T09 C~8Mhu 2019 05 08.33595 10 36 03.01 +01 59 38.7 24.5i 19JX147 T09 C~8Mhu 2019 05 08.36272 10 36 02.97 +01 59 38.7 24.5i 19JX147 T09 C~8Mhu 2019 05 08.39224 10 36 02.94 +01 59 39.2 24.2i 19JX147 T09 C~8Mhu 2019 05 31.26312 10 36 00.85 +02 02 53.7 24.6r 19JX147 T09 C~8Mhu 2019 05 31.28833 10 36 00.89 +02 02 54.1 25.1r 19JX147 T09 C~8Mhu 2019 05 31.31241 10 36 00.93 +02 02 54.2 25.3r 19JX147 T09 C~8Mhu 2019 05 31.33334 10 36 00.93 +02 02 54.4 24.9r 19JX147 T09 C~8Mhu 2019 05 31.34382 10 36 00.93 +02 02 54.4 24.8r 19JX147 T09 C~8Mhu
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 -0.10 0.00 -0.09
2 0.0002 -4.09 0.10 0.51 0.14
3 0.0850 -1209.41 -0.01 176.81 0.20
4 0.0850 -1209.97 0.00 176.58 -0.20
5 0.0851 -1210.57 0.01 176.88 -0.10
6 0.1477 -1312.43 -0.13 345.52 -0.40
7 0.1478 -1312.02 0.01 346.11 0.01
8 0.1479 -1311.50 0.28 346.43 0.15
9 0.1479 -1311.58 -0.02 346.62 0.19
10 0.1480 -1311.58 -0.14 346.62 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.