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: 06TN147 # Created Wed Nov 27 02:08:53 2024 # Orbit generated from Bernstein formalism # Fitting 10 observations of 10 # Arc: 29.93d # First observation: 2006/10/12 # Last observation: 2006/11/11 Preliminary a, adot, b, bdot, g, gdot: -0.000001 0.359514 -0.000012 0.081510 0.141565 0.000000 # Chi-squared of fit: 16.66 DOF: 14 RMS: 0.23 # Min/Max residuals: -0.51 0.44 # Exact a, adot, b, bdot, g, gdot: 3.403128E-05 2.795359E-01 1.002068E-05 7.900255E-02 1.256057E-01 -2.188397E-02 # Covariance matrix: 5.5228E-13 6.8362E-10 -1.3245E-13 2.2493E-11 1.3842E-10 3.2510E-09 6.8362E-10 7.0823E-06 -1.0552E-09 1.8650E-07 1.3805E-06 2.6943E-05 -1.3245E-13 -1.0552E-09 4.8421E-13 -3.3045E-11 -2.0647E-10 -4.1300E-09 2.2493E-11 1.8650E-07 -3.3045E-11 5.1393E-09 3.6468E-08 7.2642E-07 1.3842E-10 1.3805E-06 -2.0647E-10 3.6468E-08 2.6919E-07 5.2683E-06 3.2510E-09 2.6943E-05 -4.1300E-09 7.2642E-07 5.2683E-06 1.0495E-04 # lat0 lon0 xBary yBary zBary JD0 -0.420229 57.354019 0.621563 -0.005653 -0.785734 2454020.923394 # Heliocentric elements and errors Epoch: 2454020.5000 = 2006/10/12 Mean Anomaly: 331.84213 +/- 4.917 Argument of Peri: 43.81448 +/- 8.990 Long of Asc Node: 54.62940 +/- 0.001 Inclination: 15.89913 +/- 0.171 Eccentricity: 0.23769906 +/- 0.0201 Semi-Major Axis: 10.84509410 +/- 0.0380 Time of Perihelion: 2455040.8420 +/- 178.1 Perihelion: 8.26722547 +/- 0.2200 Aphelion: 13.42296274 +/- 0.2231 Period (y) 35.7156 +/- 0.19 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X 5.23889232 +/- 0.0177 Ecliptic Y 7.02619389 +/- 0.0277 Ecliptic Z -0.05831287 +/- 0.0002 Ecliptic XDOT -0.00537613 +/- 0.0001 Ecliptic YDOT 0.00289134 +/- 0.0002 Ecliptic ZDOT 0.00172543 +/- 0.0000 # Distances at JD0 (AU) Heliocenter to KBO 8.76451902 +/- 0.0246 Geocenter to KBO 7.96142290 +/- 0.0329 # Hcoef: 12.16
The following table shows the complete astrometric record for 06TN147. 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 (06TN147) followed by the observatory code and reference code for the source of the astrometry.
2006 10 12.42264 03 40 42.13 +19 09 34.0 06TN147 691 C~8GkE 2006 10 12.43998 03 40 41.88 +19 09 33.9 06TN147 691 C~8GkE 2006 10 12.45741 03 40 41.57 +19 09 33.8 06TN147 691 C~8GkE 2006 10 20.44073 03 38 37.21 +19 08 34.6 21.5V 06TN147 691 C~8GkE 2006 10 20.45815 03 38 36.88 +19 08 34.1 21.8V 06TN147 691 C~8GkE 2006 10 20.47556 03 38 36.61 +19 08 33.9 21.7V 06TN147 691 C~8GkE 2006 11 11.34169 03 31 30.64 +19 01 06.2 22.2V 06TN147 G96 C~8GkE 2006 11 11.34619 03 31 30.54 +19 01 06.4 21.6V 06TN147 G96 C~8GkE 2006 11 11.35073 03 31 30.43 +19 01 06.8 20.8V 06TN147 G96 C~8GkE 2006 11 11.35520 03 31 30.32 +19 01 06.3 21.2V 06TN147 G96 C~8GkE
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 0.24 0.00 -0.02
2 0.0000 -3.47 0.27 0.71 -0.06
3 0.0001 -7.77 -0.51 1.61 0.08
4 0.0220 -1736.84 0.17 346.85 0.15
5 0.0220 -1741.51 -0.30 347.44 -0.03
6 0.0220 -1745.28 0.13 348.12 -0.11
7 0.0819 -7723.53 0.06 1332.67 -0.44
8 0.0819 -7724.86 0.10 1333.20 -0.11
9 0.0819 -7726.28 0.06 1333.97 0.44
10 0.0820 -7727.91 -0.21 1333.86 0.12
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.