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: 17DO171
# Created Sun Nov 24 02:10:50 2024
# Orbit generated by ELGB
# -->Covariance matrix from a Bernstein fit
# Fitting 14 observations of 14
# Arc: 7.05y
# First observation: 2012/03/16
# Last observation: 2019/04/03
# Chi-squared of fit: 8.64 DOF: 22 RMS: 0.14
# Min/Max residuals: -0.34 0.28
# Exact a, adot, b, bdot, g, gdot:
1.264566E-05 1.772157E-02 -1.052124E-05 -1.357821E-02 2.083986E-02 -7.759859E-03
# Covariance matrix:
7.1777E-13 -1.7838E-13 -2.0689E-14 3.9187E-14 -1.5659E-13 -4.7292E-13
-1.7838E-13 2.6836E-13 8.8943E-14 -1.7771E-13 -1.4788E-13 2.1260E-12
-2.0689E-14 8.8943E-14 7.0783E-13 -1.9655E-13 -3.9810E-14 7.9478E-13
3.9187E-14 -1.7771E-13 -1.9655E-13 1.6184E-13 9.1506E-14 -1.5852E-12
-1.5659E-13 -1.4788E-13 -3.9810E-14 9.1506E-14 1.1283E-12 -1.0718E-12
-4.7292E-13 2.1260E-12 7.9478E-13 -1.5852E-12 -1.0718E-12 1.8970E-11
# lat0 lon0 xBary yBary zBary JD0
8.543581 -177.477394 0.112348 0.147263 -0.980328 2456002.819169
# Heliocentric elements and errors
Epoch: 2456002.5000 = 2012/03/16
Mean Anomaly: 351.05392 +/- 0.009
Argument of Peri: 215.91069 +/- 0.025
Long of Asc Node: 13.10385 +/- 0.000
Inclination: 38.35997 +/- 0.000
Eccentricity: 0.64726219 +/- 0.0002
Semi-Major Axis: 119.70375300 +/- 0.0774
Time of Perihelion: 2467890.0018 +/- 452.7
Perihelion: 42.22404023 +/- 0.0380
Aphelion: 197.18346576 +/- 0.1302
Period (y) 1309.6940 +/- 1.27
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -48.39895074 +/- 0.0024
Ecliptic Y -2.01889817 +/- 0.0001
Ecliptic Z 7.12824311 +/- 0.0004
Ecliptic XDOT 0.00084007 +/- 0.0000
Ecliptic YDOT -0.00228926 +/- 0.0000
Ecliptic ZDOT -0.00191540 +/- 0.0000
# Distances at JD0 (AU)
Heliocenter to KBO 48.96298294 +/- 0.0024
Geocenter to KBO 47.98527281 +/- 0.0024
# Hcoef: 8.21
The following table shows the complete astrometric record for 17DO171. 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 (17DO171) followed by the observatory code and reference code for the source of the astrometry.
2012 03 16.318403 12 22 53.76 +06 50 01.6 17DO171 695 C~89Ua 2012 03 16.395671 12 22 53.42 +06 50 03.2 17DO171 695 C~89Ua 2017 01 30.623424 12 38 11.11 +00 49 00.1 17DO171 T09 C~89Ua 2017 01 30.626122 12 38 11.12 +00 49 00.1 17DO171 T09 C~89Ua 2017 01 30.640269 12 38 11.08 +00 49 00.1 17DO171 T09 C~89Ua 2017 02 02.624862 12 38 05.03 +00 49 28.7 17DO171 T09 C~89Ua 2017 02 21.50560 12 37 13.24 +00 53 39.4 24.6z 17DO171 T09 C~89Ua 2017 02 21.55007 12 37 13.08 +00 53 40.2 24.9z 17DO171 T09 C~89Ua 2017 02 21.59307 12 37 12.92 +00 53 41.1 24.5z 17DO171 T09 C~89Ua 2017 02 23.55566 12 37 06.37 +00 54 12.8 24.7r 17DO171 T09 C~89Ua 2017 02 23.62075 12 37 06.13 +00 54 13.6 25.0r 17DO171 T09 C~89Ua 2017 02 23.65038 12 37 06.06 +00 54 14.3 25.3r 17DO171 T09 C~89Ua 2017 04 02.485751 12 34 34.40 +01 05 47.6 17DO171 T09 C~89Ua 2019 04 03.472245 12 39 55.48 -01 21 20.5 17DO171 T09 C~89Ua
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 0.17 0.00 -0.02
2 0.0002 0.00 -0.12 0.00 0.05
3 4.8769 0.00 -0.08 0.00 -0.05
4 4.8770 0.00 0.15 0.00 -0.08
5 4.8770 0.00 -0.03 0.00 -0.20
6 4.8852 0.00 0.03 0.00 -0.06
7 4.9369 0.00 0.04 0.00 -0.03
8 4.9370 0.00 -0.12 0.00 0.06
9 4.9371 0.00 -0.34 0.00 0.27
10 4.9425 0.00 0.00 0.00 0.10
11 4.9426 0.00 -0.21 0.00 -0.17
12 4.9427 0.00 0.28 0.00 0.04
13 5.0463 0.00 0.05 0.00 0.10
14 7.0476 0.00 0.10 0.00 0.04
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.