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: 19CC32
# Created Wed Nov 27 02:10:54 2024
# Orbit generated from Bernstein formalism
# Fitting 8 observations of 8
# Arc: 31.87d
# First observation: 2019/02/04
# Last observation: 2019/03/08
Preliminary a, adot, b, bdot, g, gdot:
0.000001 0.036904 0.000001 0.006680 0.028915 0.000000
# WARNING MRQMIN stopped after 13 iterations -- oscilliatory solution
# WARNING Fitting with energy constraint
# Chi-squared of fit: 7.19 DOF: 11 RMS: 0.17
# Min/Max residuals: -0.21 0.41
# Exact a, adot, b, bdot, g, gdot:
1.922403E-05 3.213134E-02 4.472911E-06 6.725551E-03 2.789985E-02 -1.834417E-03
# Covariance matrix:
1.7099E-12 3.3200E-09 -8.5012E-14 -6.2905E-11 6.1597E-10 1.2425E-08
3.3200E-09 7.9938E-06 -1.9922E-10 -1.5642E-07 1.4664E-06 2.2046E-05
-8.5012E-14 -1.9922E-10 3.0233E-13 2.8367E-13 -3.6991E-11 -7.8008E-10
-6.2905E-11 -1.5642E-07 2.8367E-13 3.3119E-09 -2.8258E-08 -2.0691E-07
6.1597E-10 1.4664E-06 -3.6991E-11 -2.8258E-08 2.7028E-07 4.7111E-06
1.2425E-08 2.2046E-05 -7.8008E-10 -2.0691E-07 4.7111E-06 4.0480E-04
# lat0 lon0 xBary yBary zBary JD0
2.355462 177.855960 0.675673 0.029907 -0.725497 2458519.066781
# Heliocentric elements and errors
Epoch: 2458510.5000 = 2019/01/27
Mean Anomaly: 349.93534 +/- 74.907
Argument of Peri: 30.32975 +/- 147.210
Long of Asc Node: 165.96313 +/- 1.069
Inclination: 12.09254 +/- 1.127
Eccentricity: 0.29716998 +/- 0.2234
Semi-Major Axis: 51.37037240 +/- 9.4869
Time of Perihelion: 2462270.2955 +/- 27963.0
Perihelion: 36.10463970 +/- 13.2736
Aphelion: 66.63610510 +/- 16.8277
Period (y) 368.1945 +/- 102.00
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -36.48644244 +/- 0.6669
Ecliptic Y 2.03398367 +/- 0.0250
Ecliptic Z 1.47323520 +/- 0.0275
Ecliptic XDOT 0.00009692 +/- 0.0020
Ecliptic YDOT -0.00316030 +/- 0.0002
Ecliptic ZDOT 0.00065182 +/- 0.0001
# Distances at JD0 (AU)
Heliocenter to KBO 36.57277667 +/- 0.6653
Geocenter to KBO 35.84248287 +/- 0.6679
# Hcoef: 10.05
The following table shows the complete astrometric record for 19CC32. 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 (19CC32) followed by the observatory code and reference code for the source of the astrometry.
2019 02 04.56598 11 55 52.85 +03 00 49.7 26.3g 19CC32 T09 C~8Mhg 2019 02 04.58875 11 55 52.78 +03 00 50.5 25.8g 19CC32 T09 C~8Mhg 2019 02 04.66250 11 55 52.58 +03 00 52.5 26.0g 19CC32 T09 C~8Mhg 2019 02 05.473907 11 55 49.93 +03 01 15.3 19CC32 T09 C~8Mhg 2019 02 05.514237 11 55 49.81 +03 01 16.4 19CC32 T09 C~8Mhg 2019 03 08.37278 11 53 41.00 +03 18 23.8 25.3r 19CC32 T09 C~8Mhg 2019 03 08.40641 11 53 40.85 +03 18 24.8 26.0r 19CC32 T09 C~8Mhg 2019 03 08.43604 11 53 40.69 +03 18 26.1 25.7r 19CC32 T09 C~8Mhg
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 -0.21 0.00 -0.14
2 0.0001 -1.28 -0.20 0.32 0.04
3 0.0003 -4.82 0.41 0.96 0.24
4 0.0025 -50.31 -0.11 6.07 -0.10
5 0.0026 -52.40 0.12 6.37 -0.05
6 0.0871 -2231.18 -0.09 181.54 0.04
7 0.0872 -2233.64 0.19 181.56 -0.08
8 0.0873 -2236.35 -0.10 181.80 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.