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: 19CL31
# Created Wed Nov 27 02:10:54 2024
# Orbit generated from Bernstein formalism
# Fitting 9 observations of 9
# Arc: 26.02d
# First observation: 2019/02/05
# Last observation: 2019/03/03
Preliminary a, adot, b, bdot, g, gdot:
-0.000000 0.031282 -0.000000 0.011319 0.026521 0.000000
# WARNING Fitting with energy constraint
# Chi-squared of fit: 5.41 DOF: 13 RMS: 0.14
# Min/Max residuals: -0.22 0.28
# Exact a, adot, b, bdot, g, gdot:
1.657307E-05 2.747725E-02 7.008075E-06 1.145897E-02 2.566323E-02 -4.599775E-03
# Covariance matrix:
9.5555E-13 1.0186E-09 -4.4745E-14 -5.5468E-11 2.0366E-10 6.7889E-09
1.0186E-09 1.7645E-06 -7.7107E-11 -9.6120E-08 3.5010E-07 1.1094E-05
-4.4745E-14 -7.7107E-11 3.6371E-13 -1.1008E-12 -1.5298E-11 -4.8372E-10
-5.5468E-11 -9.6120E-08 -1.1008E-12 5.4775E-09 -1.8917E-08 -4.9321E-07
2.0366E-10 3.5010E-07 -1.5298E-11 -1.8917E-08 6.9709E-08 2.3747E-06
6.7889E-09 1.1094E-05 -4.8372E-10 -4.9321E-07 2.3747E-06 1.9411E-04
# lat0 lon0 xBary yBary zBary JD0
5.124326 -178.114303 0.712986 0.061658 -0.686863 2458520.072931
# Heliocentric elements and errors
Epoch: 2458520.5000 = 2019/02/06
Mean Anomaly: 346.81358 +/- 25.883
Argument of Peri: 46.97305 +/- 75.446
Long of Asc Node: 169.05638 +/- 0.686
Inclination: 23.29587 +/- 1.177
Eccentricity: 0.41811209 +/- 0.3062
Semi-Major Axis: 64.68997584 +/- 18.1429
Time of Perihelion: 2465481.6082 +/- 13345.9
Perihelion: 37.64231453 +/- 22.4461
Aphelion: 91.73763715 +/- 32.4706
Period (y) 520.3118 +/- 218.89
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -39.50113164 +/- 0.3991
Ecliptic Y -0.59531709 +/- 0.0131
Ecliptic Z 3.48061554 +/- 0.0358
Ecliptic XDOT 0.00070213 +/- 0.0015
Ecliptic YDOT -0.00291177 +/- 0.0001
Ecliptic ZDOT 0.00117356 +/- 0.0001
# Distances at JD0 (AU)
Heliocenter to KBO 39.65864960 +/- 0.3975
Geocenter to KBO 38.96626002 +/- 0.4009
# Hcoef: 8.47
The following table shows the complete astrometric record for 19CL31. 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 (19CL31) followed by the observatory code and reference code for the source of the astrometry.
2019 02 05.57213 12 15 04.84 +03 57 05.0 24.1i 19CL31 T09 C~89Vd 2019 02 05.60072 12 15 04.75 +03 57 05.8 24.1i 19CL31 T09 C~89Vd 2019 02 05.64110 12 15 04.64 +03 57 07.2 24.4i 19CL31 T09 C~89Vd 2019 02 05.64377 12 15 04.65 +03 57 07.3 24.7i 19CL31 T09 C~89Vd 2019 02 28.594670 12 13 46.92 +04 10 12.0 19CL31 T09 C~89Vd 2019 02 28.637324 12 13 46.72 +04 10 13.9 19CL31 T09 C~89Vd 2019 03 03.54189 12 13 34.93 +04 12 01.2 24.3z 19CL31 T09 C~89Vd 2019 03 03.55536 12 13 34.86 +04 12 01.7 24.1z 19CL31 T09 C~89Vd 2019 03 03.59555 12 13 34.70 +04 12 03.0 24.0z 19CL31 T09 C~89Vd
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 0.07 0.00 0.01
2 0.0001 -1.55 -0.06 0.20 -0.13
3 0.0002 -3.62 -0.13 0.83 0.02
4 0.0002 -3.52 0.10 0.98 0.14
5 0.0630 -1382.89 0.28 257.48 -0.21
6 0.0631 -1386.39 -0.22 258.03 -0.06
7 0.0711 -1590.91 0.04 286.24 0.17
8 0.0711 -1592.07 -0.14 286.29 0.09
9 0.0712 -1594.79 0.05 286.53 -0.03
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.