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: 13SX112
# Created Sat Apr 20 01:15:12 2024
# Orbit generated by ELGB
# -->Covariance matrix from a Bernstein fit
# Fitting 13 observations of 13
# Arc: 5.11y
# First observation: 2013/09/30
# Last observation: 2018/11/08
# Chi-squared of fit: 6.00 DOF: 20 RMS: 0.12
# Min/Max residuals: -0.25 0.26
# Exact a, adot, b, bdot, g, gdot:
1.757903E-05 2.817639E-02 -5.101588E-07 -9.370874E-04 2.560610E-02 3.285347E-03
# Covariance matrix:
4.5146E-13 -1.5536E-13 -5.3626E-16 2.5679E-15 2.3642E-13 -5.7719E-13
-1.5536E-13 3.6626E-13 5.8785E-15 -1.2079E-14 2.3232E-13 2.6332E-12
-5.3626E-16 5.8785E-15 3.2231E-13 -7.9828E-14 6.1053E-15 4.6247E-14
2.5679E-15 -1.2079E-14 -7.9828E-14 3.1107E-14 -8.7691E-15 -9.4800E-14
2.3642E-13 2.3232E-13 6.1053E-15 -8.7691E-15 9.0471E-13 1.8670E-12
-5.7719E-13 2.6332E-12 4.6247E-14 -9.4800E-14 1.8670E-12 2.0665E-11
# lat0 lon0 xBary yBary zBary JD0
0.620303 1.083767 -0.099677 0.010888 -0.996611 2456565.633408
# Heliocentric elements and errors
Epoch: 2456566.5000 = 2013/10/01
Mean Anomaly: 18.27174 +/- 0.020
Argument of Peri: 130.11147 +/- 0.038
Long of Asc Node: 198.86434 +/- 0.002
Inclination: 1.99584 +/- 0.000
Eccentricity: 0.26960833 +/- 0.0001
Semi-Major Axis: 53.03718591 +/- 0.0107
Time of Perihelion: 2449405.9476 +/- 8.1
Perihelion: 38.73791900 +/- 0.0111
Aphelion: 67.33645281 +/- 0.0157
Period (y) 386.2593 +/- 0.12
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X 40.03809822 +/- 0.0015
Ecliptic Y 0.86025792 +/- 0.0000
Ecliptic Z 0.42275643 +/- 0.0000
Ecliptic XDOT 0.00028913 +/- 0.0000
Ecliptic YDOT 0.00301747 +/- 0.0000
Ecliptic ZDOT -0.00009625 +/- 0.0000
# Distances at JD0 (AU)
Heliocenter to KBO 40.04949093 +/- 0.0015
Geocenter to KBO 39.05315295 +/- 0.0015
# Hcoef: 7.87
The following table shows the complete astrometric record for 13SX112. 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 (13SX112) followed by the observatory code and reference code for the source of the astrometry.
2013 09 30.13263 00 02 59.428 +01 00 00.73 24.5r 13SX112 W84 C~52RV 2013 09 30.13409 00 02 59.422 +01 00 00.63 23.6i 13SX112 W84 C~52RV 2013 11 22.06260 23 59 55.308 +00 39 03.53 24.1r 13SX112 W84 C~52RV 2013 11 23.08855 23 59 53.529 +00 38 50.78 24.4r 13SX112 W84 C~52RV 2015 11 07.07312 00 12 23.963 +01 53 33.28 24.1r 13SX112 W84 C~52RV 2015 11 07.07451 00 12 23.971 +01 53 33.25 23.5i 13SX112 W84 C~52RV 2016 09 10.32547 00 22 16.489 +02 54 41.90 23.2r 13SX112 W84 C~52RV 2016 12 05.08896 00 17 12.594 +02 20 41.55 23.5r 13SX112 W84 C~52RV 2017 10 22.17055 00 25 04.695 +03 08 51.90 23.9r 13SX112 W84 C~52RV 2017 10 22.17332 00 25 04.704 +03 08 51.59 24.2g 13SX112 W84 C~52RV 2018 09 09.32722 00 34 03.142 +04 03 26.30 24.1i 13SX112 W84 C~52RV 2018 11 07.13052 00 29 53.899 +03 36 09.91 23.7r 13SX112 W84 C~52RV 2018 11 08.13743 00 29 50.502 +03 35 47.18 24.0g 13SX112 W84 C~52RV
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 -0.03 0.00 -0.03
2 0.0000 0.00 -0.02 0.00 -0.08
3 0.1449 0.00 0.04 0.00 -0.06
4 0.1477 0.00 -0.04 0.00 0.23
5 2.1025 0.00 -0.02 0.00 -0.06
6 2.1025 0.00 0.17 0.00 -0.06
7 2.9465 0.00 0.04 0.00 0.03
8 3.1813 0.00 -0.04 0.00 -0.01
9 4.0603 0.00 -0.21 0.00 0.18
10 4.0603 0.00 0.10 0.00 -0.06
11 4.9424 0.00 0.05 0.00 -0.03
12 5.1033 0.00 -0.25 0.00 -0.13
13 5.1061 0.00 0.26 0.00 0.11
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.
13SX112 quality flag:3 Type: 7:3EEEE 7:3EEEE 7:3EEEE axisobj 53.464 53.464 53.464 ecceobj 0.276 0.276 0.276 incobj 1.993 1.993 1.993 qmin 38.169 38.169 38.169 qmax 68.774 68.782 68.776 amean 52.969 52.969 52.969 amin 52.324 52.322 52.326 amax 53.750 53.756 53.742 emean 0.268 0.268 0.268 emin 0.256 0.256 0.256 emax 0.280 0.280 0.280 imean 2.689 2.689 2.689 imin 2.521 2.521 2.521 imax 2.842 2.842 2.843 excite_mean 0.272 0.272 0.272 fracstop 1.000 1.000 1.000 cjmean 3.121 3.121 3.121 libcent 0 178.5 178.5 178.7 libamp 0 128.5 128.5 128.6 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 222.2 222.0 222.7 kozaiamp 180.0 180.0 180.0