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: 19GN188
# Created Wed Nov 27 02:10:57 2024
# Orbit generated from Bernstein formalism
# Fitting 8 observations of 8
# Arc: 59.00d
# First observation: 2019/02/05
# Last observation: 2019/04/05
Preliminary a, adot, b, bdot, g, gdot:
-0.000000 0.016708 0.000000 -0.002159 0.021828 0.000000
# WARNING MRQMIN stopped after 13 iterations -- oscilliatory solution
# WARNING Fitting with energy constraint
# Chi-squared of fit: 0.90 DOF: 11 RMS: 0.06
# Min/Max residuals: -0.13 0.11
# Exact a, adot, b, bdot, g, gdot:
1.470278E-05 2.117340E-02 -1.537741E-06 -2.270465E-03 2.248362E-02 3.355375E-03
# Covariance matrix:
7.7559E-12 1.0327E-08 -2.5295E-13 -2.8738E-10 1.8436E-09 1.8215E-08
1.0327E-08 1.5192E-05 -3.7175E-10 -4.2238E-07 2.7087E-06 2.6055E-05
-2.5295E-13 -3.7175E-10 7.3788E-13 5.7718E-12 -6.6485E-11 -7.0522E-10
-2.8738E-10 -4.2238E-07 5.7718E-12 1.1800E-08 -7.5512E-08 -7.9205E-07
1.8436E-09 2.7087E-06 -6.6485E-11 -7.5512E-08 4.8521E-07 5.3994E-06
1.8215E-08 2.6055E-05 -7.0522E-10 -7.9205E-07 5.3994E-06 2.9682E-04
# lat0 lon0 xBary yBary zBary JD0
4.623234 -176.553602 0.731669 0.054050 -0.667588 2458520.059171
# Heliocentric elements and errors
Epoch: 2458520.5000 = 2019/02/06
Mean Anomaly: 61.31471 +/- 91.355
Argument of Peri: 65.50419 +/- 98.721
Long of Asc Node: 39.55679 +/- 4.027
Inclination: 7.53399 +/- 0.702
Eccentricity: 0.14633951 +/- 0.8475
Semi-Major Axis: 47.63066119 +/- 20.9207
Time of Perihelion: 2438070.6316 +/- 27328.3
Perihelion: 40.66041371 +/- 44.1421
Aphelion: 54.60090868 +/- 46.9545
Period (y) 328.7291 +/- 216.58
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -44.96341255 +/- 1.3710
Ecliptic Y -1.98307709 +/- 0.0825
Ecliptic Z 3.58488924 +/- 0.1111
Ecliptic XDOT -0.00026573 +/- 0.0021
Ecliptic YDOT -0.00260112 +/- 0.0005
Ecliptic ZDOT -0.00024285 +/- 0.0002
# Distances at JD0 (AU)
Heliocenter to KBO 45.14966771 +/- 1.3654
Geocenter to KBO 44.47683145 +/- 1.3779
# Hcoef: 7.45
The following table shows the complete astrometric record for 19GN188. 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 (19GN188) followed by the observatory code and reference code for the source of the astrometry.
2019 02 05.55837 12 19 59.87 +02 52 21.8 23.6i 19GN188 T09 C~8FzY 2019 02 05.63031 12 19 59.68 +02 52 23.3 23.8i 19GN188 T09 C~8FzY 2019 04 04.45230 12 16 23.64 +03 16 30.5 24.5g 19GN188 T09 C~8FzY 2019 04 04.46143 12 16 23.60 +03 16 30.8 24.4g 19GN188 T09 C~8FzY 2019 04 04.47412 12 16 23.56 +03 16 31.0 24.4g 19GN188 T09 C~8FzY 2019 04 04.49512 12 16 23.47 +03 16 31.5 24.4g 19GN188 T09 C~8FzY 2019 04 05.53497 12 16 19.14 +03 16 56.7 23.4r 19GN188 T09 C~8FzY 2019 04 05.55801 12 16 19.05 +03 16 57.2 24.3r 19GN188 T09 C~8FzY
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 -0.01
2 0.0002 -3.21 -0.04 0.24 0.01
3 0.1585 -3548.10 -0.08 43.16 -0.02
4 0.1585 -3548.77 -0.13 43.20 0.04
5 0.1586 -3549.40 0.11 43.15 0.03
6 0.1586 -3550.84 0.09 43.07 0.01
7 0.1615 -3620.38 -0.05 40.47 -0.02
8 0.1615 -3621.81 0.06 40.40 -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.