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: 24CE30 # Created Sun Oct 19 01:12:26 2025 # Orbit generated from Bernstein formalism # Fitting 10 observations of 10 # Arc: 7.00d # First observation: 2024/02/07 # Last observation: 2024/02/14 Preliminary a, adot, b, bdot, g, gdot: 0.000000 0.027812 -0.000000 0.004447 0.026292 0.000000 # WARNING Fitting with energy constraint # Chi-squared of fit: 4.50 DOF: 15 RMS: 0.12 # Min/Max residuals: -0.24 0.24 # Exact a, adot, b, bdot, g, gdot: 1.594835E-05 2.583513E-02 1.693018E-06 3.580484E-03 2.580489E-02 -6.871569E-03 # Covariance matrix: 3.2720E-12 5.3832E-09 1.7026E-12 2.4185E-09 1.2227E-09 1.2335E-08 5.3832E-09 1.0167E-05 3.1981E-09 4.5456E-06 2.2975E-06 2.1633E-05 1.7026E-12 3.1981E-09 1.3996E-12 1.4054E-09 7.2306E-10 7.2638E-09 2.4185E-09 4.5456E-06 1.4054E-09 2.0354E-06 1.0275E-06 9.6163E-06 1.2227E-09 2.2975E-06 7.2306E-10 1.0275E-06 5.1937E-07 5.0277E-06 1.2335E-08 2.1633E-05 7.2638E-09 9.6163E-06 5.0277E-06 4.3312E-04 # lat0 lon0 xBary yBary zBary JD0 -25.721824 -173.634381 0.739337 -0.285796 -0.592910 2460347.744811 # Heliocentric elements and errors Epoch: 2460340.5000 = 2024/01/31 Mean Anomaly: 302.53595 +/- 54.586 Argument of Peri: 14.91274 +/- 35.257 Long of Asc Node: 257.86130 +/- 4.433 Inclination: 26.34736 +/- 0.534 Eccentricity: 0.28265022 +/- 0.7966 Semi-Major Axis: 42.90834904 +/- 18.8937 Time of Perihelion: 2476727.7053 +/- 11187.5 Perihelion: 30.78029493 +/- 36.7715 Aphelion: 55.03640316 +/- 41.9015 Period (y) 281.0742 +/- 185.65 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X -35.42548215 +/- 0.9690 Ecliptic Y -3.20648349 +/- 0.1081 Ecliptic Z -16.81860210 +/- 0.4697 Ecliptic XDOT 0.00078769 +/- 0.0020 Ecliptic YDOT -0.00266285 +/- 0.0004 Ecliptic ZDOT 0.00065871 +/- 0.0009 # Distances at JD0 (AU) Heliocenter to KBO 39.34605061 +/- 0.8953 Geocenter to KBO 38.75234343 +/- 1.0823 # Hcoef: 7.56
The following table shows the complete astrometric record for 24CE30. 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 (24CE30) followed by the observatory code and reference code for the source of the astrometry.
2024 02 07.24401 11 39 19.49 -25 58 16.90 23.5r 24CE30 W84 C~9A1j 2024 02 07.31390 11 39 19.20 -25 58 17.41 24CE30 W84 C~9A1j 2024 02 07.36007 11 39 19.01 -25 58 17.79 24CE30 W84 C~9A1j 2024 02 10.31026 11 39 06.93 -25 58 28.94 23.4r 24CE30 W84 C~9A1j 2024 02 10.34481 11 39 06.76 -25 58 29.09 24CE30 W84 C~9A1j 2024 02 13.21196 11 38 54.50 -25 58 32.17 24CE30 W84 C~9A1j 2024 02 13.28109 11 38 54.17 -25 58 32.06 23.6r 24CE30 W84 C~9A1j 2024 02 13.35413 11 38 53.86 -25 58 31.98 24CE30 W84 C~9A1j 2024 02 14.20912 11 38 50.07 -25 58 31.29 24CE30 W84 C~9A1j 2024 02 14.24376 11 38 49.93 -25 58 31.32 23.5r 24CE30 W84 C~9A1j
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 -0.02 0.00 0.10
2 0.0002 -3.29 -0.02 -2.18 -0.04
3 0.0003 -5.42 0.03 -3.65 -0.17
4 0.0084 -146.81 0.09 -85.32 0.17
5 0.0085 -148.80 -0.14 -86.46 -0.02
6 0.0163 -295.88 0.24 -162.02 0.04
7 0.0165 -299.92 -0.06 -163.88 -0.00
8 0.0167 -303.71 0.13 -165.65 0.13
9 0.0191 -349.90 -0.24 -187.54 -0.12
10 0.0192 -351.58 -0.01 -188.40 -0.09
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.