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: 16EG397 # Created Wed Nov 27 02:10:35 2024 # Orbit generated from Bernstein formalism # Fitting 11 observations of 11 # Arc: 2.15d # First observation: 2016/03/07 # Last observation: 2016/03/09 # WARNING Fitting with energy constraint # WARNING and with gdot fixed = 0 # Chi-squared of fit: 6.27 DOF: 18 RMS: 0.13 # Min/Max residuals: -0.27 0.26 # Exact a, adot, b, bdot, g, gdot: 1.383758E-05 1.877403E-02 4.851167E-06 6.212288E-03 2.145318E-02 0.000000E+00 # Covariance matrix: 2.9746E-11 3.9815E-08 1.9164E-13 1.7580E-10 6.3116E-09 0.0000E+00 3.9815E-08 5.3856E-05 2.5889E-10 2.3744E-07 8.5251E-06 0.0000E+00 1.9164E-13 2.5889E-10 2.3717E-13 -4.2786E-11 4.0994E-11 0.0000E+00 1.7580E-10 2.3744E-07 -4.2786E-11 1.9894E-08 3.7599E-08 0.0000E+00 6.3116E-09 8.5251E-06 4.0994E-11 3.7599E-08 1.3499E-06 0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 1.2993E-04 # lat0 lon0 xBary yBary zBary JD0 -4.964815 170.283812 0.058184 -0.085313 -0.983893 2457454.939129 # Heliocentric elements and errors Epoch: 2457450.5000 = 2016/03/03 Mean Anomaly: 358.23057 +/- 349.863 Argument of Peri: 346.67374 +/- 56.441 Long of Asc Node: 184.62777 +/- 5.305 Inclination: 18.86778 +/- 6.342 Eccentricity: 0.02985428 +/- 0.5593 Semi-Major Axis: 49.06457422 +/- 25.6812 Time of Perihelion: 2458067.4931 +/- 373057.4 Perihelion: 47.59978680 +/- 37.0635 Aphelion: 50.52936163 +/- 38.1112 Period (y) 343.6847 +/- 269.84 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X -46.73962922 +/- 2.4789 Ecliptic Y 8.05880925 +/- 0.4247 Ecliptic Z -4.03385555 +/- 0.2185 Ecliptic XDOT -0.00047212 +/- 0.0014 Ecliptic YDOT -0.00235697 +/- 0.0008 Ecliptic ZDOT 0.00078985 +/- 0.0001 # Distances at JD0 (AU) Heliocenter to KBO 47.60051824 +/- 2.4352 Geocenter to KBO 46.61314144 +/- 2.5245 # Hcoef: 8.33
The following table shows the complete astrometric record for 16EG397. 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 (16EG397) followed by the observatory code and reference code for the source of the astrometry.
2016 03 07.43834 11 16 29.53 -00 43 03.0 25.1g 16EG397 T09 C~8McL 2016 03 07.45278 11 16 29.47 -00 43 02.5 25.1g 16EG397 T09 C~8McL 2016 03 07.51496 11 16 29.22 -00 43 00.8 25.3g 16EG397 T09 C~8McL 2016 03 07.52359 11 16 29.20 -00 43 00.3 25.8g 16EG397 T09 C~8McL 2016 03 07.55363 11 16 29.06 -00 42 59.8 25.8g 16EG397 T09 C~8McL 2016 03 09.35090 11 16 21.96 -00 42 07.8 25.2r 16EG397 T09 C~8McL 2016 03 09.36541 11 16 21.92 -00 42 07.4 25.0r 16EG397 T09 C~8McL 2016 03 09.39307 11 16 21.78 -00 42 06.8 25.1r 16EG397 T09 C~8McL 2016 03 09.43673 11 16 21.60 -00 42 05.7 24.6r 16EG397 T09 C~8McL 2016 03 09.53006 11 16 21.23 -00 42 02.9 25.3r 16EG397 T09 C~8McL 2016 03 09.58785 11 16 21.00 -00 42 01.0 24.7r 16EG397 T09 C~8McL
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 0.00 0.00 -0.06
2 0.0000 -1.02 -0.06 0.11 0.01
3 0.0002 -5.14 -0.01 0.20 -0.06
4 0.0002 -5.61 0.09 0.54 0.26
5 0.0003 -7.74 -0.03 0.18 -0.18
6 0.0052 -126.09 -0.02 6.26 0.16
7 0.0053 -126.80 0.24 6.39 0.25
8 0.0054 -128.97 -0.07 6.12 -0.10
9 0.0055 -131.88 -0.06 6.07 -0.27
10 0.0057 -138.09 -0.01 6.47 -0.13
11 0.0059 -142.01 -0.07 6.87 0.09
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.