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: 19EA9
# Created Wed Nov 27 02:10:55 2024
# Orbit generated from Bernstein formalism
# Fitting 9 observations of 9
# Arc: 31.84d
# First observation: 2019/02/04
# Last observation: 2019/03/08
Preliminary a, adot, b, bdot, g, gdot:
0.000000 0.028147 0.000000 -0.000211 0.025406 0.000000
# WARNING Fitting with energy constraint
# Chi-squared of fit: 4.71 DOF: 13 RMS: 0.13
# Min/Max residuals: -0.27 0.22
# Exact a, adot, b, bdot, g, gdot:
1.599094E-05 2.488308E-02 2.973632E-07 -1.134656E-04 2.469526E-02 -1.810942E-03
# Covariance matrix:
2.6584E-12 3.0709E-09 -2.2380E-13 -9.3772E-11 6.1436E-10 3.8049E-08
3.0709E-09 4.9016E-06 -3.5482E-10 -1.4932E-07 9.7510E-07 5.8946E-05
-2.2380E-13 -3.5482E-10 7.2356E-13 1.8947E-12 -7.0644E-11 -4.3009E-09
-9.3772E-11 -1.4932E-07 1.8947E-12 4.6974E-09 -2.9703E-08 -1.7937E-06
6.1436E-10 9.7510E-07 -7.0644E-11 -2.9703E-08 1.9410E-07 1.1793E-05
3.8049E-08 5.8946E-05 -4.3009E-09 -1.7937E-06 1.1793E-05 7.4910E-04
# lat0 lon0 xBary yBary zBary JD0
3.390948 177.401228 0.669739 0.043336 -0.730304 2458519.078231
# Heliocentric elements and errors
Epoch: 2458510.5000 = 2019/01/27
Mean Anomaly: 311.65136 +/- 250.751
Argument of Peri: 152.52221 +/- 12.492
Long of Asc Node: 82.92396 +/- 1.227
Inclination: 3.33689 +/- 0.003
Eccentricity: 0.11343792 +/- 0.9073
Semi-Major Axis: 44.20743091 +/- 3.3408
Time of Perihelion: 2472929.0993 +/- 74761.3
Perihelion: 39.19263207 +/- 40.2173
Aphelion: 49.22222975 +/- 40.2803
Period (y) 293.9349 +/- 33.32
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -41.08060138 +/- 0.7204
Ecliptic Y 2.52691227 +/- 0.0327
Ecliptic Z 2.39514119 +/- 0.0427
Ecliptic XDOT 0.00008243 +/- 0.0030
Ecliptic YDOT -0.00276656 +/- 0.0001
Ecliptic ZDOT -0.00002464 +/- 0.0002
# Distances at JD0 (AU)
Heliocenter to KBO 41.22787646 +/- 0.7178
Geocenter to KBO 40.49360537 +/- 0.7224
# Hcoef: 7.97
The following table shows the complete astrometric record for 19EA9. 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 (19EA9) followed by the observatory code and reference code for the source of the astrometry.
2019 02 04.57743 11 55 51.83 +04 08 40.2 24.9g 19EA9 T09 C~8FzV 2019 02 04.60152 11 55 51.76 +04 08 40.9 25.1g 19EA9 T09 C~8FzV 2019 03 02.45121 11 54 14.29 +04 20 24.9 23.4y 19EA9 T09 C~8FzV 2019 03 02.54583 11 54 13.89 +04 20 27.7 23.3y 19EA9 T09 C~8FzV 2019 03 02.54851 11 54 13.86 +04 20 28.2 23.8y 19EA9 T09 C~8FzV 2019 03 02.58871 11 54 13.71 +04 20 29.1 23.6y 19EA9 T09 C~8FzV 2019 03 08.37278 11 53 48.23 +04 23 21.9 24.3r 19EA9 T09 C~8FzV 2019 03 08.38324 11 53 48.19 +04 23 22.1 24.0r 19EA9 T09 C~8FzV 2019 03 08.41479 11 53 48.05 +04 23 23.3 24.1r 19EA9 T09 C~8FzV
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 -0.08
2 0.0001 -1.24 0.01 0.22 0.08
3 0.0708 -1619.06 -0.09 65.46 -0.19
4 0.0711 -1625.67 0.15 65.65 -0.09
5 0.0711 -1626.28 -0.27 65.93 0.19
6 0.0712 -1628.69 0.22 65.86 0.08
7 0.0871 -2047.11 -0.08 72.78 -0.04
8 0.0871 -2047.74 0.07 72.72 -0.11
9 0.0872 -2050.14 0.01 72.99 0.15
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.