The following information shows the result of the orbit fit based on Gary Bernstein's method. Most of the information should be self-explanatory.
# Object: 02VV130 # Created Fri May 2 02:36:51 2008 # Orbit generated from Bernstein formalism # Fitting 14 observations of 14 # Arc: 1.86y # First observation: 2002/11/07 # Last observation: 2004/09/17 Preliminary a, adot, b, bdot, g, gdot: 0.000119 0.029988 -0.000003 -0.001104 0.027981 0.000000 # Chi-squared of fit: 23.51 DOF: 22 RMS: 0.23 # Min/Max residuals: -0.54 0.49 # Exact a, adot, b, bdot, g, gdot: 1.808154E-05 2.990775E-02 -2.256570E-06 -1.096876E-03 2.760179E-02 -3.874632E-03 # Covariance matrix: 4.7186E-13 -3.4109E-13 -3.2141E-15 -6.2569E-15 1.0337E-12 4.8536E-12 -3.4109E-13 1.5341E-12 4.4698E-15 -3.5209E-14 -6.4390E-16 1.8678E-11 -3.2141E-15 4.4698E-15 1.8663E-13 -1.3839E-13 -1.0257E-14 -1.2809E-14 -6.2569E-15 -3.5209E-14 -1.3839E-13 2.3653E-13 -4.7865E-14 -8.6609E-13 1.0337E-12 -6.4390E-16 -1.0257E-14 -4.7865E-14 4.2116E-12 3.1644E-11 4.8536E-12 1.8678E-11 -1.2809E-14 -8.6609E-13 3.1644E-11 5.0643E-10 # lat0 lon0 xBary yBary zBary JD0 -1.188649 19.962750 -0.406790 -0.018720 -0.900529 2452585.644793 # Heliocentric elements and errors Epoch: 2452580.5000 = 2002/11/02 Mean Anomaly: 323.09943 +/- 0.094 Argument of Peri: 260.18840 +/- 0.157 Long of Asc Node: 171.47335 +/- 0.011 Inclination: 2.38182 +/- 0.001 Eccentricity: 0.17246558 +/- 0.0008 Semi-Major Axis: 42.42165698 +/- 0.0228 Time of Perihelion: 2462925.0227 +/- 25.1 Perihelion: 35.10538134 +/- 0.0373 Aphelion: 49.73793262 +/- 0.0419 Period (y) 276.3056 +/- 0.22 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X 34.75188136 +/- 0.0025 Ecliptic Y 13.06190048 +/- 0.0009 Ecliptic Z -0.75162067 +/- 0.0001 Ecliptic XDOT -0.00138354 +/- 0.0000 Ecliptic YDOT 0.00265294 +/- 0.0000 Ecliptic ZDOT -0.00010060 +/- 0.0000 # Distances at JD0 (AU) Heliocenter to KBO 37.13315817 +/- 0.0024 Geocenter to KBO 36.22953367 +/- 0.0027 # Hcoef: 7.51
The following table shows the complete astrometric record for 02VV130. 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 (02VV130) followed by the observatory code and reference code for the source of the astrometry.
2002 11 07.14405 01 15 31.88 +06 42 15.0 22.7R 02VV130 695 Cg8319 2002 11 07.25151 01 15 31.39 +06 42 11.9 02VV130 695 Cg8319 2002 12 01.31020 01 14 00.14 +06 33 14.6 23.4R 02VV130 568 Cg8319 2002 12 01.35629 01 14 00.00 +06 33 13.6 02VV130 568 Cg8319 2002 12 02.32582 01 13 57.23 +06 32 57.6 02VV130 568 Cg8319 2002 12 05.08615 01 13 49.65 +06 32 15.0 22.7R 02VV130 695 Ch1653 2002 12 05.19676 01 13 49.35 +06 32 13.5 02VV130 695 Ch1653 2002 12 06.21327 01 13 46.78 +06 31 59.2 02VV130 695 Ch1653 2003 10 23.16899 01 23 17.04 +07 24 46.6 22.5R 02VV130 695 Cj4694 2003 10 23.26429 01 23 16.54 +07 24 43.6 02VV130 695 Cj4694 2003 11 20.13563 01 21 08.19 +07 12 03.0 22.8R 02VV130 695 Cj4694 2003 11 20.21942 01 21 07.86 +07 12 01.1 02VV130 695 Cj4694 2004 09 17.50381 01 32 43.07 +08 17 03.6 23.2R 02VV130 568 Cl5726 2004 09 17.54577 01 32 42.88 +08 17 02.6 02VV130 568 Cl5726
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 -0.20 0.00 0.34 2 0.0003 -7.93 -0.22 -0.12 0.13 3 0.0662 -1469.80 -0.03 14.49 -0.18 4 0.0663 -1472.11 -0.12 14.35 -0.39 5 0.0689 -1516.38 0.33 15.10 -0.54 6 0.0765 -1637.07 -0.14 18.26 0.00 7 0.0768 -1641.77 -0.12 18.56 0.13 8 0.0796 -1682.64 0.49 19.76 0.28 9 0.9583 7379.26 0.31 -227.85 0.20 10 0.9586 7371.23 0.11 -227.86 0.16 11 1.0349 5313.77 -0.23 -220.90 0.05 12 1.0351 5308.50 -0.14 -220.83 0.02 13 1.8627 16385.07 0.00 -426.56 -0.18 14 1.8628 16382.06 -0.04 -426.46 -0.03
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.
02VV130 quality flag:3 Type: 5:3EE 5:3EE 5:3EE axisobj 42.748 42.748 42.748 ecceobj 0.176 0.176 0.176 incobj 2.376 2.376 2.376 qmin 34.728 34.728 34.728 qmax 50.391 50.375 50.390 amean 42.328 42.328 42.328 amin 41.944 41.947 41.942 amax 42.758 42.763 42.757 emean 0.164 0.164 0.164 emin 0.149 0.149 0.149 emax 0.179 0.179 0.179 imean 2.630 2.630 2.630 imin 2.142 2.142 2.142 imax 3.198 3.198 3.199 fracstop 1.000 1.000 1.000 cjmean 3.048 3.048 3.048 libcent 0 180.1 180.3 180.2 libamp 0 48.8 49.0 48.9 libcent 1 -180.0 -180.0 -180.0 libamp 1 -180.0 -180.0 -180.0 libcent 2 -180.0 -180.0 -180.0 libamp 2 -180.0 -180.0 -180.0 libcent 3 -180.0 -180.0 -180.0 libamp 3 -180.0 -180.0 -180.0 libcent 4 -180.0 -180.0 -180.0 libamp 4 -180.0 -180.0 -180.0 kozaimean 185.8 185.6 185.9 kozaiamp 180.0 179.9 180.0