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: 17CW57
# Created Wed Nov 27 02:10:47 2024
# Orbit generated from Bernstein formalism
# Fitting 10 observations of 10
# Arc: 24.01d
# First observation: 2017/01/30
# Last observation: 2017/02/23
Preliminary a, adot, b, bdot, g, gdot:
-0.000000 0.023694 0.000000 -0.000935 0.023315 0.000000
# WARNING MRQMIN stopped after 13 iterations -- oscilliatory solution
# WARNING Fitting with energy constraint
# Chi-squared of fit: 5.00 DOF: 15 RMS: 0.12
# Min/Max residuals: -0.31 0.26
# Exact a, adot, b, bdot, g, gdot:
1.463033E-05 2.179807E-02 -1.153952E-07 -8.104597E-04 2.277474E-02 2.997245E-03
# Covariance matrix:
4.0128E-13 1.3579E-10 -2.8872E-14 -9.1194E-12 4.2136E-11 9.3081E-09
1.3579E-10 5.7409E-07 -7.5343E-11 -3.8746E-08 1.4135E-07 1.2402E-05
-2.8872E-14 -7.5343E-11 2.8333E-13 5.6937E-13 -1.9394E-11 -2.3212E-09
-9.1194E-12 -3.8746E-08 5.6937E-13 2.7759E-09 -9.5147E-09 -8.1403E-07
4.2136E-11 1.4135E-07 -1.9394E-11 -9.5147E-09 3.5422E-08 3.5574E-06
9.3081E-09 1.2402E-05 -2.3212E-09 -8.1403E-07 3.5574E-06 6.8400E-04
# lat0 lon0 xBary yBary zBary JD0
4.028045 -172.854635 0.824677 0.038149 -0.539489 2457784.143761
# Heliocentric elements and errors
Epoch: 2457780.5000 = 2017/01/27
Mean Anomaly: 56.88868 +/- 60.487
Argument of Peri: 46.59143 +/- 155.096
Long of Asc Node: 68.94613 +/- 1.044
Inclination: 4.46833 +/- 0.042
Eccentricity: 0.13015255 +/- 1.1999
Semi-Major Axis: 47.19231228 +/- 18.0681
Time of Perihelion: 2439068.1365 +/- 16744.1
Perihelion: 41.05011247 +/- 58.7662
Aphelion: 53.33451210 +/- 60.1949
Period (y) 324.2016 +/- 186.19
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -44.10210753 +/- 0.3591
Ecliptic Y -4.70190911 +/- 0.0450
Ecliptic Z 3.08431774 +/- 0.0255
Ecliptic XDOT -0.00003457 +/- 0.0031
Ecliptic YDOT -0.00265234 +/- 0.0004
Ecliptic ZDOT -0.00007194 +/- 0.0002
# Distances at JD0 (AU)
Heliocenter to KBO 44.45915940 +/- 0.3563
Geocenter to KBO 43.90829202 +/- 0.3629
# Hcoef: 8.67
The following table shows the complete astrometric record for 17CW57. 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 (17CW57) followed by the observatory code and reference code for the source of the astrometry.
2017 01 30.64296 12 32 36.47 +00 51 53.1 24.3z 17CW57 T09 C~85Iv 2017 01 30.64563 12 32 36.45 +00 51 53.3 24.7z 17CW57 T09 C~85Iv 2017 01 30.64832 12 32 36.46 +00 51 53.3 25.0z 17CW57 T09 C~85Iv 2017 02 02.63333 12 32 30.53 +00 52 45.7 25.0i 17CW57 T09 C~85Iv 2017 02 02.64170 12 32 30.50 +00 52 45.5 24.9i 17CW57 T09 C~85Iv 2017 02 02.65005 12 32 30.48 +00 52 45.8 24.9i 17CW57 T09 C~85Iv 2017 02 23.55287 12 31 32.15 +01 00 21.2 25.2r 17CW57 T09 C~85Iv 2017 02 23.57406 12 31 32.08 +01 00 21.8 25.3r 17CW57 T09 C~85Iv 2017 02 23.61866 12 31 31.89 +01 00 22.9 25.4r 17CW57 T09 C~85Iv 2017 02 23.64828 12 31 31.81 +01 00 23.6 25.6r 17CW57 T09 C~85Iv
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 0.10 0.00 -0.09
2 0.0000 -0.35 -0.16 0.07 -0.04
3 0.0000 -0.22 0.07 0.12 0.01
4 0.0082 -102.62 0.04 13.16 0.26
5 0.0082 -102.95 0.02 12.80 -0.13
6 0.0082 -103.35 -0.07 12.96 -0.00
7 0.0655 -1086.91 0.14 86.09 0.01
8 0.0655 -1088.11 0.16 86.23 0.10
9 0.0656 -1091.16 -0.31 86.12 -0.11
10 0.0657 -1092.54 0.02 86.29 -0.01
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.