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: 17DO166
# Created Wed Nov 27 02:10:49 2024
# Orbit generated from Bernstein formalism
# Fitting 10 observations of 10
# Arc: 11.15d
# First observation: 2017/02/21
# Last observation: 2017/03/04
Preliminary a, adot, b, bdot, g, gdot:
-0.000001 0.030757 -0.000000 0.003966 0.027393 0.000000
# WARNING MRQMIN stopped after 13 iterations -- oscilliatory solution
# WARNING Fitting with energy constraint
# Chi-squared of fit: 3.50 DOF: 15 RMS: 0.10
# Min/Max residuals: -0.18 0.16
# Exact a, adot, b, bdot, g, gdot:
1.512913E-05 2.628687E-02 2.305957E-06 4.138349E-03 2.651159E-02 3.956909E-03
# Covariance matrix:
3.0552E-12 5.3926E-09 -2.6363E-13 -2.1815E-10 1.0269E-09 5.0203E-08
5.3926E-09 1.0976E-05 -5.1125E-10 -4.4835E-07 2.0650E-06 7.1359E-05
-2.6363E-13 -5.1125E-10 2.8092E-13 1.0622E-11 -9.7083E-11 -4.6147E-09
-2.1815E-10 -4.4835E-07 1.0622E-11 1.9283E-08 -8.4166E-08 -2.6401E-06
1.0269E-09 2.0650E-06 -9.7083E-11 -8.4166E-08 3.8931E-07 1.4549E-05
5.0203E-08 7.1359E-05 -4.6147E-09 -2.6401E-06 1.4549E-05 2.0905E-03
# lat0 lon0 xBary yBary zBary JD0
4.010368 -171.052051 0.587069 0.055753 -0.792991 2457805.996261
# Heliocentric elements and errors
Epoch: 2457800.5000 = 2017/02/16
Mean Anomaly: 78.27718 +/- 241.552
Argument of Peri: 290.37863 +/- 123.429
Long of Asc Node: 164.64421 +/- 3.398
Inclination: 9.79297 +/- 1.311
Eccentricity: 0.13131246 +/- 1.6914
Semi-Major Axis: 38.89444950 +/- 22.8119
Time of Perihelion: 2438535.7860 +/- 56981.0
Perihelion: 33.78712366 +/- 68.7074
Aphelion: 44.00177534 +/- 70.6685
Period (y) 242.5714 +/- 213.40
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -38.04880863 +/- 0.8748
Ecliptic Y -5.40095857 +/- 0.1377
Ecliptic Z 2.63806133 +/- 0.0621
Ecliptic XDOT 0.00005222 +/- 0.0046
Ecliptic YDOT -0.00274702 +/- 0.0009
Ecliptic ZDOT 0.00045483 +/- 0.0003
# Distances at JD0 (AU)
Heliocenter to KBO 38.52066405 +/- 0.8643
Geocenter to KBO 37.71935864 +/- 0.8877
# Hcoef: 7.73
The following table shows the complete astrometric record for 17DO166. 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 (17DO166) followed by the observatory code and reference code for the source of the astrometry.
2017 02 21.49546 12 39 11.49 +00 08 25.0 23.3z 17DO166 T09 C~85Iz 2017 02 21.56347 12 39 11.23 +00 08 27.2 23.3z 17DO166 T09 C~85Iz 2017 02 21.61448 12 39 11.04 +00 08 28.5 23.2z 17DO166 T09 C~85Iz 2017 02 23.54142 12 39 04.00 +00 09 26.8 23.7r 17DO166 T09 C~85Iz 2017 02 23.57615 12 39 03.88 +00 09 27.6 23.5r 17DO166 T09 C~85Iz 2017 02 23.61010 12 39 03.75 +00 09 28.8 23.4r 17DO166 T09 C~85Iz 2017 02 23.65247 12 39 03.58 +00 09 30.3 23.3r 17DO166 T09 C~85Iz 2017 03 04.54977 12 38 28.23 +00 14 11.7 23.4y 17DO166 T09 C~85Iz 2017 03 04.59319 12 38 28.05 +00 14 13.4 23.6y 17DO166 T09 C~85Iz 2017 03 04.64464 12 38 27.82 +00 14 15.1 23.7y 17DO166 T09 C~85Iz
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 0.11 0.00 0.03
2 0.0002 -4.45 -0.09 0.49 0.13
3 0.0003 -7.58 -0.03 0.57 -0.09
4 0.0056 -127.60 -0.11 12.68 -0.00
5 0.0057 -129.57 0.16 12.71 -0.17
6 0.0058 -131.83 0.08 13.05 -0.02
7 0.0059 -134.76 -0.12 13.43 0.11
8 0.0303 -732.94 0.07 63.84 -0.18
9 0.0304 -736.09 0.04 64.34 0.12
10 0.0305 -739.93 -0.10 64.55 0.08
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.