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: 17CX57
# Created Wed Nov 27 02:10:47 2024
# Orbit generated from Bernstein formalism
# Fitting 11 observations of 11
# Arc: 23.99d
# First observation: 2017/01/30
# Last observation: 2017/02/23
Preliminary a, adot, b, bdot, g, gdot:
-0.000000 0.097732 -0.000002 -0.002685 0.058062 0.000000
# WARNING Fitting with energy constraint
# Chi-squared of fit: 4.40 DOF: 17 RMS: 0.11
# Min/Max residuals: -0.20 0.19
# Exact a, adot, b, bdot, g, gdot:
2.483506E-05 8.855162E-02 -4.000377E-07 -2.095816E-03 5.543715E-02 8.453636E-03
# Covariance matrix:
6.4121E-13 7.5082E-10 -1.8202E-13 -4.7057E-11 2.2688E-10 2.5107E-08
7.5082E-10 3.4477E-06 -6.8153E-10 -2.2490E-07 9.6214E-07 8.4353E-05
-1.8202E-13 -6.8153E-10 3.8084E-13 4.0087E-11 -1.9247E-10 -1.7604E-08
-4.7057E-11 -2.2490E-07 4.0087E-11 1.4843E-08 -6.2614E-08 -5.4408E-06
2.2688E-10 9.6214E-07 -1.9247E-10 -6.2614E-08 2.6963E-07 2.4000E-05
2.5107E-08 8.4353E-05 -1.7604E-08 -5.4408E-06 2.4000E-05 2.2518E-03
# lat0 lon0 xBary yBary zBary JD0
4.265507 -172.661858 0.826655 0.040161 -0.536311 2457784.126931
# Heliocentric elements and errors
Epoch: 2457780.5000 = 2017/01/27
Mean Anomaly: 9.89402 +/- 93.986
Argument of Peri: 89.60161 +/- 155.302
Long of Asc Node: 79.21014 +/- 0.692
Inclination: 4.29454 +/- 0.016
Eccentricity: 0.22281196 +/- 0.2477
Semi-Major Axis: 23.76060935 +/- 3.9782
Time of Perihelion: 2456617.8338 +/- 11040.7
Perihelion: 18.46646132 +/- 6.6478
Aphelion: 29.05475738 +/- 7.6354
Period (y) 115.8229 +/- 29.09
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -18.48338622 +/- 0.1671
Ecliptic Y -1.55096343 +/- 0.0215
Ecliptic Z 1.34165737 +/- 0.0126
Ecliptic XDOT 0.00014091 +/- 0.0023
Ecliptic YDOT -0.00439830 +/- 0.0003
Ecliptic ZDOT -0.00007223 +/- 0.0002
# Distances at JD0 (AU)
Heliocenter to KBO 18.59680344 +/- 0.1661
Geocenter to KBO 18.03844477 +/- 0.1690
# Hcoef: 12.28
The following table shows the complete astrometric record for 17CX57. 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 (17CX57) followed by the observatory code and reference code for the source of the astrometry.
2017 01 30.62613 12 33 41.37 +01 00 25.4 24.5z 17CX57 T09 C~85Iv 2017 01 30.64296 12 33 41.31 +01 00 26.1 25.0z 17CX57 T09 C~85Iv 2017 01 30.64563 12 33 41.29 +01 00 26.1 24.6z 17CX57 T09 C~85Iv 2017 02 02.61643 12 33 30.72 +01 02 10.1 24.9i 17CX57 T09 C~85Iv 2017 02 02.62487 12 33 30.67 +01 02 10.5 24.9i 17CX57 T09 C~85Iv 2017 02 02.63333 12 33 30.65 +01 02 10.6 24.9i 17CX57 T09 C~85Iv 2017 02 02.65005 12 33 30.58 +01 02 11.5 25.0i 17CX57 T09 C~85Iv 2017 02 23.55287 12 31 34.12 +01 18 09.3 25.0r 17CX57 T09 C~85Iv 2017 02 23.58469 12 31 33.90 +01 18 11.0 25.3r 17CX57 T09 C~85Iv 2017 02 23.58678 12 31 33.86 +01 18 11.0 24.9r 17CX57 T09 C~85Iv 2017 02 23.61866 12 31 33.65 +01 18 12.5 24.9r 17CX57 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 0.09 0.00 -0.04
2 0.0000 -1.10 0.01 0.29 0.08
3 0.0001 -1.38 -0.10 0.17 -0.07
4 0.0082 -188.08 0.09 33.18 0.01
5 0.0082 -188.92 -0.16 33.25 -0.00
6 0.0082 -189.24 0.11 33.23 -0.11
7 0.0083 -190.56 -0.04 33.64 0.14
8 0.0655 -2173.37 -0.08 224.78 0.09
9 0.0656 -2177.08 0.09 225.04 0.16
10 0.0656 -2177.63 -0.20 224.80 -0.09
11 0.0657 -2181.11 0.19 224.94 -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.