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: 03WW218 # Created Wed Nov 27 02:08:30 2024 # Orbit generated from Bernstein formalism # Fitting 9 observations of 9 # Arc: 34.98d # First observation: 2003/11/24 # Last observation: 2003/12/29 Preliminary a, adot, b, bdot, g, gdot: -0.000001 1.101620 0.000011 0.054319 0.280971 0.000000 # Chi-squared of fit: 24.08 DOF: 12 RMS: 0.29 # Min/Max residuals: -0.50 0.54 # Exact a, adot, b, bdot, g, gdot: 4.632476E-05 5.858520E-01 2.884319E-06 5.486085E-02 1.991238E-01 -4.813297E-02 # Covariance matrix: 8.6896E-13 4.8978E-09 1.1527E-13 -2.2377E-11 7.4515E-10 -4.3991E-09 4.8978E-09 6.3616E-05 1.5373E-09 -2.9865E-07 9.6518E-06 -5.8731E-05 1.1527E-13 1.5373E-09 4.9035E-13 -1.2764E-11 2.3314E-10 -1.4301E-09 -2.2377E-11 -2.9865E-07 -1.2764E-11 1.5171E-09 -4.5290E-08 2.7787E-07 7.4515E-10 9.6518E-06 2.3314E-10 -4.5290E-08 1.4644E-06 -8.9065E-06 -4.3991E-09 -5.8731E-05 -1.4301E-09 2.7787E-07 -8.9065E-06 5.4650E-05 # lat0 lon0 xBary yBary zBary JD0 -0.331842 74.035572 0.216586 -0.005517 -0.962177 2452967.866563 # Heliocentric elements and errors Epoch: 2452960.5000 = 2003/11/17 Mean Anomaly: 347.78746 +/- 0.623 Argument of Peri: 23.21739 +/- 1.580 Long of Asc Node: 74.96368 +/- 0.027 Inclination: 5.36962 +/- 0.073 Eccentricity: 0.35268154 +/- 0.0179 Semi-Major Axis: 9.00586927 +/- 0.1639 Time of Perihelion: 2453295.3809 +/- 14.4 Perihelion: 5.82966543 +/- 0.1929 Aphelion: 12.18207312 +/- 0.2741 Period (y) 27.0269 +/- 0.74 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X 1.85062041 +/- 0.0084 Ecliptic Y 5.69688907 +/- 0.0293 Ecliptic Z -0.02907258 +/- 0.0002 Ecliptic XDOT -0.00792979 +/- 0.0001 Ecliptic YDOT 0.00157725 +/- 0.0001 Ecliptic ZDOT 0.00075828 +/- 0.0000 # Distances at JD0 (AU) Heliocenter to KBO 5.99000720 +/- 0.0280 Geocenter to KBO 5.02200133 +/- 0.0305 # Hcoef: 14.12
The following table shows the complete astrometric record for 03WW218. 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 (03WW218) followed by the observatory code and reference code for the source of the astrometry.
2003 11 24.36582 04 50 53.95 +22 09 18.5 21.3V 03WW218 691 C~8GiW 2003 11 24.39413 04 50 53.20 +22 09 17.4 21.9V 03WW218 691 C~8GiW 2003 11 24.44292 04 50 51.82 +22 09 17.1 21.2V 03WW218 691 C~8GiW 2003 12 17.35564 04 40 20.29 +22 02 33.1 22.3V 03WW218 691 C~8GiW 2003 12 17.38206 04 40 19.65 +22 02 32.3 22.3V 03WW218 691 C~8GiW 2003 12 17.41056 04 40 18.83 +22 02 32.2 21.6V 03WW218 691 C~8GiW 2003 12 29.26799 04 35 25.20 +21 59 12.2 21.4V 03WW218 691 C~8GiW 2003 12 29.30089 04 35 24.49 +21 59 11.7 22.2V 03WW218 691 C~8GiW 2003 12 29.34716 04 35 23.38 +21 59 11.0 22.0V 03WW218 691 C~8GiW
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 0.04 0.00 0.30
2 0.0001 -10.48 0.29 0.14 -0.41
3 0.0002 -29.55 -0.33 2.11 0.12
4 0.0629 -8792.24 -0.50 714.44 0.05
5 0.0630 -8801.18 0.54 714.85 -0.34
6 0.0631 -8812.51 -0.04 716.30 0.26
7 0.0956 -12895.34 -0.25 1088.19 0.03
8 0.0956 -12905.23 0.44 1089.11 -0.07
9 0.0958 -12920.67 -0.19 1090.64 0.05
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.