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: 24GG30 # Created Thu Jul 3 01:12:10 2025 # Orbit generated from Bernstein formalism # Fitting 10 observations of 10 # Arc: 15.05d # First observation: 2024/04/03 # Last observation: 2024/04/18 Preliminary a, adot, b, bdot, g, gdot: -0.000000 0.028453 0.000001 0.005813 0.027114 0.000000 # WARNING Fitting with energy constraint # Chi-squared of fit: 1.59 DOF: 15 RMS: 0.07 # Min/Max residuals: -0.11 0.17 # Exact a, adot, b, bdot, g, gdot: 1.600316E-05 2.688423E-02 3.610561E-06 6.131005E-03 2.688927E-02 -7.474622E-03 # Covariance matrix: 1.9036E-12 2.1352E-09 1.8627E-13 -4.0459E-10 3.6890E-10 2.4139E-10 2.1352E-09 3.0006E-06 2.8252E-10 -5.6929E-07 5.1033E-07 -5.9797E-06 1.8627E-13 2.8252E-10 3.2259E-13 -6.1970E-11 4.7208E-11 -1.4439E-09 -4.0459E-10 -5.6929E-07 -6.1970E-11 1.0851E-07 -9.6723E-08 1.2522E-06 3.6890E-10 5.1033E-07 4.7208E-11 -9.6723E-08 8.7045E-08 -7.7081E-07 2.4139E-10 -5.9797E-06 -1.4439E-09 1.2522E-06 -7.7081E-07 2.6752E-04 # lat0 lon0 xBary yBary zBary JD0 -28.736443 178.982112 -0.254753 -0.469080 -0.855074 2460403.635041 # Heliocentric elements and errors Epoch: 2460400.5000 = 2024/03/31 Mean Anomaly: 302.65967 +/- 47.522 Argument of Peri: 20.23362 +/- 20.176 Long of Asc Node: 242.72379 +/- 2.580 Inclination: 30.79399 +/- 0.577 Eccentricity: 0.26412040 +/- 0.6054 Semi-Major Axis: 41.48285885 +/- 15.7757 Time of Perihelion: 2475944.3695 +/- 9345.2 Perihelion: 30.52638954 +/- 27.6684 Aphelion: 52.43932816 +/- 32.0697 Period (y) 267.1845 +/- 152.41 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X -33.57641243 +/- 0.3577 Ecliptic Y 0.34483877 +/- 0.0064 Ecliptic Z -17.87992404 +/- 0.1962 Ecliptic XDOT 0.00031296 +/- 0.0015 Ecliptic YDOT -0.00273709 +/- 0.0002 Ecliptic ZDOT 0.00091334 +/- 0.0008 # Distances at JD0 (AU) Heliocenter to KBO 38.04189886 +/- 0.3289 Geocenter to KBO 37.18955149 +/- 0.4080 # Hcoef: 7.55
The following table shows the complete astrometric record for 24GG30. 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 (24GG30) followed by the observatory code and reference code for the source of the astrometry.
2024 04 03.13424 11 07 13.39 -25 46 46.94 23.3r 24GG30 W84 C~8vOd 2024 04 03.14380 11 07 13.35 -25 46 46.55 24GG30 W84 C~8vOd 2024 04 03.15335 11 07 13.30 -25 46 45.99 24GG30 W84 C~8vOd 2024 04 06.13645 11 06 59.56 -25 44 23.52 24GG30 W84 C~8vOd 2024 04 06.14598 11 06 59.52 -25 44 23.06 24GG30 W84 C~8vOd 2024 04 06.15550 11 06 59.47 -25 44 22.43 24GG30 W84 C~8vOd 2024 04 18.15525 11 06 09.99 -25 34 12.31 24GG30 W84 C~8vOd 2024 04 18.16527 11 06 09.95 -25 34 12.05 24GG30 W84 C~8vOd 2024 04 18.17528 11 06 09.92 -25 34 11.46 24GG30 W84 C~8vOd 2024 04 18.18028 11 06 09.90 -25 34 11.30 24GG30 W84 C~8vOd
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 -0.00
2 0.0000 -0.66 0.06 0.11 -0.02
3 0.0001 -1.51 -0.04 0.32 0.05
4 0.0082 -230.98 0.03 46.10 -0.06
5 0.0082 -231.67 0.08 46.28 -0.04
6 0.0083 -232.55 -0.07 46.54 0.07
7 0.0411 -1102.58 -0.11 297.38 0.17
8 0.0412 -1103.18 -0.02 297.37 -0.09
9 0.0412 -1103.81 0.05 297.72 0.01
10 0.0412 -1104.12 0.08 297.74 -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.