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: 17SQ385
# Created Wed Nov 27 02:10:52 2024
# Orbit generated from Bernstein formalism
# Fitting 9 observations of 9
# Arc: 13.99d
# First observation: 2017/09/13
# Last observation: 2017/09/27
# WARNING Fitting with energy constraint
# WARNING and with gdot fixed = 0
# Chi-squared of fit: 1.07 DOF: 14 RMS: 0.06
# Min/Max residuals: -0.15 0.10
# Exact a, adot, b, bdot, g, gdot:
1.409391E-05 2.441716E-02 8.319429E-06 1.409914E-02 2.720501E-02 0.000000E+00
# Covariance matrix:
5.7787E-11 9.8441E-08 1.4914E-13 3.1239E-10 1.5844E-08 0.0000E+00
9.8441E-08 1.6913E-04 2.5620E-10 5.3666E-07 2.7218E-05 0.0000E+00
1.4914E-13 2.5620E-10 4.7635E-13 -1.1753E-11 4.1231E-11 0.0000E+00
3.1239E-10 5.3666E-07 -1.1753E-11 2.2079E-09 8.6365E-08 0.0000E+00
1.5844E-08 2.7218E-05 4.1231E-11 8.6365E-08 4.3803E-06 0.0000E+00
0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 2.6495E-04
# lat0 lon0 xBary yBary zBary JD0
1.903787 -7.166827 0.034753 0.033563 -1.006459 2458009.873751
# Heliocentric elements and errors
Epoch: 2458000.5000 = 2017/09/04
Mean Anomaly: 1.38972 +/- 250.967
Argument of Peri: 2.19813 +/- 317.660
Long of Asc Node: 349.57227 +/- 1.692
Inclination: 30.10231 +/- 13.150
Eccentricity: 0.02427777 +/- 0.5862
Semi-Major Axis: 38.70204698 +/- 20.3510
Time of Perihelion: 2457661.0112 +/- 325135.2
Perihelion: 37.76244762 +/- 30.1490
Aphelion: 39.64164634 +/- 30.8088
Period (y) 240.7737 +/- 189.91
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X 37.44309640 +/- 2.8042
Ecliptic Y -4.74848728 +/- 0.3528
Ecliptic Z 1.22147573 +/- 0.0940
Ecliptic XDOT 0.00026474 +/- 0.0016
Ecliptic YDOT 0.00243832 +/- 0.0011
Ecliptic ZDOT 0.00141801 +/- 0.0001
# Distances at JD0 (AU)
Heliocenter to KBO 37.76275417 +/- 2.7808
Geocenter to KBO 36.75793789 +/- 2.8278
# Hcoef: 7.72
The following table shows the complete astrometric record for 17SQ385. 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 (17SQ385) followed by the observatory code and reference code for the source of the astrometry.
2017 09 13.37295 23 30 40.04 -01 05 43.8 23.8y 17SQ385 T09 C~8Aib 2017 09 13.38715 23 30 39.96 -01 05 44.2 23.2y 17SQ385 T09 C~8Aib 2017 09 13.40454 23 30 39.87 -01 05 44.5 23.0y 17SQ385 T09 C~8Aib 2017 09 27.27982 23 29 27.64 -01 11 34.2 23.6z 17SQ385 T09 C~8Aib 2017 09 27.29383 23 29 27.56 -01 11 34.6 23.4z 17SQ385 T09 C~8Aic 2017 09 27.30784 23 29 27.50 -01 11 35.0 23.0z 17SQ385 T09 C~8Aic 2017 09 27.32188 23 29 27.43 -01 11 35.2 23.4z 17SQ385 T09 C~8Aic 2017 09 27.35008 23 29 27.28 -01 11 36.0 22.4z 17SQ385 T09 C~8Aic 2017 09 27.36422 23 29 27.21 -01 11 36.4 23.1z 17SQ385 T09 C~8Aic
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 -0.03
2 0.0000 -1.26 -0.06 0.11 -0.04
3 0.0001 -2.62 0.04 0.36 0.07
4 0.0381 -1135.94 -0.03 106.60 0.05
5 0.0381 -1137.20 -0.15 106.71 0.05
6 0.0382 -1138.19 0.01 106.69 -0.07
7 0.0382 -1139.23 0.10 106.93 0.05
8 0.0383 -1141.61 0.02 107.08 -0.01
9 0.0383 -1142.74 0.05 107.12 -0.08
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.