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: 17BP239
# Created Wed Nov 27 02:10:46 2024
# Orbit generated from Bernstein formalism
# Fitting 9 observations of 9
# Arc: 5.01d
# First observation: 2017/01/23
# Last observation: 2017/01/28
# WARNING Fitting with energy constraint
# WARNING and with gdot fixed = 0
# Chi-squared of fit: 2.67 DOF: 14 RMS: 0.10
# Min/Max residuals: -0.17 0.16
# Exact a, adot, b, bdot, g, gdot:
1.516560E-05 2.370503E-02 5.716209E-07 1.064200E-03 2.425011E-02 0.000000E+00
# Covariance matrix:
1.3048E-10 2.0034E-07 -1.1852E-11 -1.8313E-08 6.4539E-08 0.0000E+00
2.0034E-07 3.0832E-04 -1.8237E-08 -2.8180E-05 9.9313E-05 0.0000E+00
-1.1852E-11 -1.8237E-08 1.3477E-12 1.6475E-09 -5.8745E-09 0.0000E+00
-1.8313E-08 -2.8180E-05 1.6475E-09 2.5791E-06 -9.0771E-06 0.0000E+00
6.4539E-08 9.9313E-05 -5.8745E-09 -9.0771E-06 3.1990E-05 0.0000E+00
0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 1.8766E-04
# lat0 lon0 xBary yBary zBary JD0
2.914052 -173.363062 0.881289 0.022644 -0.441517 2457777.125121
# Heliocentric elements and errors
Epoch: 2457770.5000 = 2017/01/17
Mean Anomaly: 308.29211 +/- 3.747
Argument of Peri: 101.88970 +/- 19.503
Long of Asc Node: 137.79863 +/- 62.688
Inclination: 3.89842 +/- 3.871
Eccentricity: 0.02731284 +/- 0.6624
Semi-Major Axis: 42.38930606 +/- 24.0745
Time of Perihelion: 2472249.4538 +/- 404081.7
Perihelion: 41.23153372 +/- 36.5612
Aphelion: 43.54707841 +/- 37.4172
Period (y) 275.9896 +/- 235.12
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -41.45185993 +/- 9.5412
Ecliptic Y -3.94032375 +/- 1.1099
Ecliptic Z 2.09640747 +/- 0.4890
Ecliptic XDOT 0.00031822 +/- 0.0015
Ecliptic YDOT -0.00266437 +/- 0.0014
Ecliptic ZDOT 0.00011993 +/- 0.0002
# Distances at JD0 (AU)
Heliocenter to KBO 41.69145917 +/- 9.4870
Geocenter to KBO 41.23693474 +/- 9.6179
# Hcoef: 8.94
The following table shows the complete astrometric record for 17BP239. 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 (17BP239) followed by the observatory code and reference code for the source of the astrometry.
2017 01 23.62432 12 28 58.98 +00 02 30.2 25.2i 17BP239 T09 C~85Ir 2017 01 23.63574 12 28 58.95 +00 02 30.5 25.4i 17BP239 T09 C~85Ir 2017 01 23.64112 12 28 58.96 +00 02 30.4 25.4i 17BP239 T09 C~85Ir 2017 01 23.64921 12 28 58.94 +00 02 30.4 25.0i 17BP239 T09 C~85Ir 2017 01 23.65460 12 28 58.92 +00 02 30.7 24.8i 17BP239 T09 C~85Ir 2017 01 28.60612 12 28 50.68 +00 03 48.1 24.5z 17BP239 T09 C~85Ir 2017 01 28.61148 12 28 50.68 +00 03 48.1 25.1z 17BP239 T09 C~85Ir 2017 01 28.63649 12 28 50.63 +00 03 48.6 24.4z 17BP239 T09 C~85Ir 2017 01 28.63916 12 28 50.61 +00 03 48.5 25.1z 17BP239 T09 C~85Ir
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 0.06 0.00 0.03
2 0.0000 -0.53 -0.17 0.10 0.08
3 0.0000 -0.35 0.16 0.07 0.02
4 0.0001 -0.63 0.10 -0.05 -0.13
5 0.0001 -1.02 -0.15 0.10 0.01
6 0.0136 -145.15 -0.08 22.37 0.04
7 0.0137 -145.15 0.10 22.37 0.02
8 0.0137 -146.04 0.06 22.53 0.08
9 0.0137 -146.27 -0.09 22.32 -0.14
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.