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: 19EO7
# Created Wed Nov 27 02:10:55 2024
# Orbit generated from Bernstein formalism
# Fitting 9 observations of 9
# Arc: 31.85d
# First observation: 2019/02/04
# Last observation: 2019/03/08
Preliminary a, adot, b, bdot, g, gdot:
-0.000000 0.017660 0.000001 -0.000170 0.023287 0.000000
# WARNING MRQMIN stopped after 13 iterations -- oscilliatory solution
# WARNING Fitting with energy constraint
# Chi-squared of fit: 12.89 DOF: 13 RMS: 0.21
# Min/Max residuals: -0.68 0.36
# Exact a, adot, b, bdot, g, gdot:
1.114242E-05 1.661344E-02 6.501274E-07 -1.616527E-04 2.302042E-02 1.422013E-02
# Covariance matrix:
8.4711E-12 1.1945E-08 -5.9486E-14 -8.8599E-11 2.0872E-09 -3.5795E-09
1.1945E-08 1.7878E-05 -8.8991E-11 -1.3254E-07 3.1222E-06 -5.4922E-06
-5.9486E-14 -8.8991E-11 4.8336E-13 -4.9824E-12 -1.5543E-11 2.6598E-11
-8.8599E-11 -1.3254E-07 -4.9824E-12 1.0820E-09 -2.3148E-08 4.0540E-08
2.0872E-09 3.1222E-06 -1.5543E-11 -2.3148E-08 5.4548E-07 -8.3853E-07
-3.5795E-09 -5.4922E-06 2.6598E-11 4.0540E-08 -8.3853E-07 7.1978E-05
# lat0 lon0 xBary yBary zBary JD0
0.912473 175.470656 0.644617 0.012068 -0.753720 2458519.085351
# Heliocentric elements and errors
Epoch: 2458510.5000 = 2019/01/27
Mean Anomaly: 52.84840 +/- 44.314
Argument of Peri: 351.31463 +/- 24.241
Long of Asc Node: 54.21661 +/- 2.137
Inclination: 1.04011 +/- 0.023
Eccentricity: 0.63722501 +/- 0.2636
Semi-Major Axis: 44.50069776 +/- 22.7238
Time of Perihelion: 2442592.8854 +/- 5430.6
Perihelion: 16.14374022 +/- 14.3359
Aphelion: 72.85765531 +/- 39.0089
Period (y) 296.8646 +/- 227.39
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -43.99809869 +/- 1.3891
Ecliptic Y 4.12414025 +/- 0.1102
Ecliptic Z 0.69179159 +/- 0.0222
Ecliptic XDOT -0.00183402 +/- 0.0010
Ecliptic YDOT -0.00183779 +/- 0.0005
Ecliptic ZDOT 0.00000750 +/- 0.0000
# Distances at JD0 (AU)
Heliocenter to KBO 44.19637764 +/- 1.3830
Geocenter to KBO 43.43968821 +/- 1.3937
# Hcoef: 8.76
The following table shows the complete astrometric record for 19EO7. 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 (19EO7) followed by the observatory code and reference code for the source of the astrometry.
2019 02 04.58455 11 44 49.30 +02 38 15.5 26.1g 19EO7 T09 C~83G9 2019 02 04.62894 11 44 49.15 +02 38 16.6 25.9g 19EO7 T09 C~83G9 2019 02 04.65831 11 44 49.06 +02 38 17.5 25.4g 19EO7 T09 C~83G9 2019 03 07.54864 11 42 47.07 +02 51 42.9 25.4y 19EO7 T09 C~83GA 2019 03 07.56472 11 42 47.00 +02 51 43.2 24.7y 19EO7 T09 C~83GA 2019 03 07.60483 11 42 46.79 +02 51 43.9 24.7y 19EO7 T09 C~83GA 2019 03 08.35603 11 42 43.52 +02 52 06.4 25.0r 19EO7 T09 C~83GA 2019 03 08.40222 11 42 43.32 +02 52 07.6 25.0r 19EO7 T09 C~83GA 2019 03 08.43185 11 42 43.17 +02 52 08.3 24.7r 19EO7 T09 C~83GA
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 0.06 0.00 -0.16
2 0.0001 -2.50 -0.03 0.12 -0.05
3 0.0002 -4.09 -0.03 0.41 0.23
4 0.0848 -2001.43 0.03 14.52 0.06
5 0.0848 -2002.51 0.12 14.38 -0.08
6 0.0849 -2005.68 -0.13 13.78 -0.68
7 0.0870 -2059.58 -0.05 15.01 0.36
8 0.0871 -2062.81 0.10 14.92 0.28
9 0.0872 -2065.15 -0.07 14.67 0.04
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.