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: 17BQ239
# Created Wed Jul 17 01:11:29 2024
# Orbit generated from Bernstein formalism
# Fitting 9 observations of 9
# Arc: 3.02d
# First observation: 2017/01/30
# Last observation: 2017/02/02
# WARNING Fitting with energy constraint
# WARNING and with gdot fixed = 0
# Chi-squared of fit: 1.91 DOF: 14 RMS: 0.08
# Min/Max residuals: -0.16 0.15
# Exact a, adot, b, bdot, g, gdot:
1.505333E-05 2.100380E-02 -1.844542E-06 -2.201926E-03 2.244077E-02 0.000000E+00
# Covariance matrix:
5.9666E-11 8.4128E-08 -6.5506E-12 -9.2978E-09 2.3287E-08 0.0000E+00
8.4128E-08 1.1935E-04 -9.2885E-09 -1.3184E-05 3.3020E-05 0.0000E+00
-6.5506E-12 -9.2885E-09 1.0329E-12 9.8810E-10 -2.5700E-09 0.0000E+00
-9.2978E-09 -1.3184E-05 9.8810E-10 1.4663E-06 -3.6478E-06 0.0000E+00
2.3287E-08 3.3020E-05 -2.5700E-09 -3.6478E-06 9.1362E-06 0.0000E+00
0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 1.4871E-04
# lat0 lon0 xBary yBary zBary JD0
4.361279 -172.760261 0.825618 0.041177 -0.537825 2457784.138401
# Heliocentric elements and errors
Epoch: 2457780.5000 = 2017/01/27
Mean Anomaly: 314.07402 +/- 239.836
Argument of Peri: 191.79146 +/- 308.975
Long of Asc Node: 42.25839 +/- 1.625
Inclination: 7.29199 +/- 0.262
Eccentricity: 0.02570295 +/- 0.6116
Semi-Major Axis: 45.91587529 +/- 24.1571
Time of Perihelion: 2472278.1843 +/- 416482.1
Perihelion: 44.73570199 +/- 36.6411
Aphelion: 47.09604858 +/- 37.4508
Period (y) 311.1376 +/- 245.54
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -44.72084614 +/- 5.9371
Ecliptic Y -4.85320946 +/- 0.7540
Ecliptic Z 3.38862028 +/- 0.4565
Ecliptic XDOT 0.00030557 +/- 0.0015
Ecliptic YDOT -0.00255137 +/- 0.0010
Ecliptic ZDOT -0.00026793 +/- 0.0002
# Distances at JD0 (AU)
Heliocenter to KBO 45.11086863 +/- 5.8864
Geocenter to KBO 44.56175003 +/- 6.0022
# Hcoef: 6.76
The following table shows the complete astrometric record for 17BQ239. 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 (17BQ239) followed by the observatory code and reference code for the source of the astrometry.
2017 01 30.63760 12 33 28.80 +01 08 01.6 22.9z 17BQ239 T09 C~85Ir 2017 01 30.64028 12 33 28.80 +01 08 01.4 22.8z 17BQ239 T09 C~85Ir 2017 01 30.64296 12 33 28.79 +01 08 01.7 23.4z 17BQ239 T09 C~85Ir 2017 01 30.64832 12 33 28.78 +01 08 01.7 23.1z 17BQ239 T09 C~85Ir 2017 02 02.61643 12 33 22.90 +01 08 52.0 23.4i 17BQ239 T09 C~85Ir 2017 02 02.62487 12 33 22.89 +01 08 52.0 23.3i 17BQ239 T09 C~85Ir 2017 02 02.63333 12 33 22.88 +01 08 52.1 23.1i 17BQ239 T09 C~85Ir 2017 02 02.64170 12 33 22.86 +01 08 52.3 23.1i 17BQ239 T09 C~85Ir 2017 02 02.65847 12 33 22.81 +01 08 52.6 23.1i 17BQ239 T09 C~85Ir
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 -0.05 0.00 0.06
2 0.0000 0.08 0.12 -0.18 -0.13
3 0.0000 -0.18 -0.05 0.03 0.07
4 0.0000 -0.32 -0.01 -0.03 -0.00
5 0.0082 -101.19 -0.16 11.39 0.07
6 0.0082 -101.33 0.01 11.33 -0.02
7 0.0082 -101.51 0.15 11.36 -0.02
8 0.0082 -101.86 0.10 11.43 0.02
9 0.0083 -102.67 -0.09 11.40 -0.05
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.