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: 15GA89
# Created Sun Oct 19 01:10:57 2025
# Orbit generated from Bernstein formalism
# Fitting 8 observations of 8
# Arc: 41.92d
# First observation: 2015/04/13
# Last observation: 2015/05/25
Preliminary a, adot, b, bdot, g, gdot:
0.000001 0.027913 -0.000001 0.005035 0.024926 0.000000
# WARNING Fitting with energy constraint
# Chi-squared of fit: 0.91 DOF: 11 RMS: 0.06
# Min/Max residuals: -0.07 0.11
# Exact a, adot, b, bdot, g, gdot:
1.639876E-05 2.541213E-02 3.079397E-06 5.082344E-03 2.441527E-02 -8.253147E-03
# Covariance matrix:
8.8031E-13 6.2345E-10 -1.5344E-13 -1.6404E-11 1.1390E-10 4.1088E-09
6.2345E-10 1.4552E-06 -3.3216E-10 -4.0633E-08 2.5490E-07 5.5323E-06
-1.5344E-13 -3.3216E-10 6.0179E-13 4.0892E-12 -5.8637E-11 -1.4668E-09
-1.6404E-11 -4.0633E-08 4.0892E-12 1.2247E-09 -7.0658E-09 -1.3104E-07
1.1390E-10 2.5490E-07 -5.8637E-11 -7.0658E-09 4.4824E-08 1.0470E-06
4.1088E-09 5.5323E-06 -1.4668E-09 -1.3104E-07 1.0470E-06 5.6198E-05
# lat0 lon0 xBary yBary zBary JD0
7.888491 -125.590555 0.518247 0.117456 -0.846950 2457126.069098
# Heliocentric elements and errors
Epoch: 2457120.5000 = 2015/04/08
Mean Anomaly: 333.48642 +/- 11.621
Argument of Peri: 99.30495 +/- 25.509
Long of Asc Node: 199.95143 +/- 1.419
Inclination: 13.72848 +/- 0.490
Eccentricity: 0.43209164 +/- 0.2841
Semi-Major Axis: 60.86746139 +/- 16.5431
Time of Perihelion: 2469894.9480 +/- 2055.6
Perihelion: 34.56714017 +/- 19.6824
Aphelion: 87.16778260 +/- 29.3327
Period (y) 474.8823 +/- 193.60
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -24.53324229 +/- 0.2048
Ecliptic Y -33.38551948 +/- 0.2861
Ecliptic Z 5.62146775 +/- 0.0488
Ecliptic XDOT 0.00289318 +/- 0.0004
Ecliptic YDOT -0.00085531 +/- 0.0007
Ecliptic ZDOT 0.00043759 +/- 0.0001
# Distances at JD0 (AU)
Heliocenter to KBO 41.80997235 +/- 0.2582
Geocenter to KBO 40.95797546 +/- 0.3552
# Hcoef: 7.51
The following table shows the complete astrometric record for 15GA89. 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 (15GA89) followed by the observatory code and reference code for the source of the astrometry.
2015 04 13.56832 15 36 01.38 -11 12 53.7 23.5G 15GA89 T14 C~99u4 2015 04 13.60943 15 36 01.22 -11 12 52.8 15GA89 T14 C~99u4 2015 04 18.57833 15 35 42.02 -11 10 59.4 22.9G 15GA89 T14 C~99u4 2015 05 21.33898 15 33 15.29 -10 59 17.1 15GA89 T14 C~99u4 2015 05 21.38005 15 33 15.09 -10 59 16.4 23.7G 15GA89 T14 C~99u4 2015 05 21.42139 15 33 14.89 -10 59 15.7 15GA89 T14 C~99u4 2015 05 22.49770 15 33 09.87 -10 58 55.6 23.6G 15GA89 T14 C~99u4 2015 05 25.48844 15 32 55.98 -10 58 01.1 23.7G 15GA89 T14 C~99u4
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 0.01 0.00 0.04
2 0.0001 -2.50 -0.03 0.32 -0.01
3 0.0137 -303.81 0.01 43.80 -0.04
4 0.1034 -2568.78 0.05 213.57 0.11
5 0.1035 -2571.80 -0.00 213.55 0.02
6 0.1036 -2574.83 -0.03 213.52 -0.06
7 0.1066 -2651.42 0.06 215.43 -0.06
8 0.1148 -2863.10 -0.07 219.59 -0.01
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.