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: 16PY295
# Created Wed Jul 17 01:11:20 2024
# Orbit generated from Bernstein formalism
# Fitting 9 observations of 9
# Arc: 33.96d
# First observation: 2016/08/04
# Last observation: 2016/09/07
Preliminary a, adot, b, bdot, g, gdot:
-0.000001 0.029146 0.000000 -0.004737 0.027010 0.000000
# WARNING Fitting with energy constraint
# Chi-squared of fit: 3.14 DOF: 13 RMS: 0.10
# Min/Max residuals: -0.24 0.20
# Exact a, adot, b, bdot, g, gdot:
1.621282E-05 2.859376E-02 -2.284173E-06 -4.694817E-03 2.682247E-02 1.320748E-03
# Covariance matrix:
3.5899E-12 5.5943E-09 -2.5864E-13 -2.9924E-10 9.9852E-10 2.3130E-08
5.5943E-09 9.7205E-06 -4.4867E-10 -5.1924E-07 1.7315E-06 3.9010E-05
-2.5864E-13 -4.4867E-10 3.8422E-13 1.9927E-11 -8.0069E-11 -1.8764E-09
-2.9924E-10 -5.1924E-07 1.9927E-11 2.7836E-08 -9.2611E-08 -2.1455E-06
9.9852E-10 1.7315E-06 -8.0069E-11 -9.2611E-08 3.0925E-07 7.3738E-06
2.3130E-08 3.9010E-05 -1.8764E-09 -2.1455E-06 7.3738E-06 3.7289E-04
# lat0 lon0 xBary yBary zBary JD0
9.629967 -13.927269 0.562134 0.141462 -0.833076 2457604.866029
# Heliocentric elements and errors
Epoch: 2457600.5000 = 2016/07/31
Mean Anomaly: 12.69211 +/- 229.583
Argument of Peri: 117.39934 +/- 306.076
Long of Asc Node: 210.50841 +/- 2.650
Inclination: 13.13486 +/- 0.590
Eccentricity: 0.12863892 +/- 0.3609
Semi-Major Axis: 43.53766686 +/- 10.1899
Time of Perihelion: 2453901.1330 +/- 66904.0
Perihelion: 37.93702832 +/- 18.0485
Aphelion: 49.13830540 +/- 19.4725
Period (y) 287.2804 +/- 100.86
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X 36.35757657 +/- 0.7397
Ecliptic Y -9.59832017 +/- 0.1835
Ecliptic Z 6.23669640 +/- 0.1293
Ecliptic XDOT 0.00091062 +/- 0.0019
Ecliptic YDOT 0.00277456 +/- 0.0004
Ecliptic ZDOT -0.00044993 +/- 0.0003
# Distances at JD0 (AU)
Heliocenter to KBO 38.11689266 +/- 0.7073
Geocenter to KBO 37.28217198 +/- 0.7730
# Hcoef: 7.56
The following table shows the complete astrometric record for 16PY295. 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 (16PY295) followed by the observatory code and reference code for the source of the astrometry.
2016 08 04.36524 22 53 49.37 +03 23 15.0 23.8i 16PY295 T09 C~85IL 2016 08 04.38883 22 53 49.26 +03 23 14.5 24.2i 16PY295 T09 C~85IL 2016 08 04.46054 22 53 48.98 +03 23 13.5 23.2z 16PY295 T09 C~85IL 2016 08 04.50884 22 53 48.76 +03 23 12.3 23.1z 16PY295 T09 C~85IL 2016 09 05.30252 22 51 24.77 +03 09 19.8 22.6i 16PY295 T09 C~85IL 2016 09 05.31062 22 51 24.72 +03 09 19.5 22.7i 16PY295 T09 C~85IL 2016 09 05.31872 22 51 24.69 +03 09 19.3 22.7i 16PY295 T09 C~85IL 2016 09 07.31234 22 51 15.15 +03 08 14.3 23.0r 16PY295 T09 C~85IL 2016 09 07.32083 22 51 15.12 +03 08 14.0 23.1r 16PY295 T09 C~85IL
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 0.13 0.00 -0.10
2 0.0001 -1.71 -0.09 0.18 -0.07
3 0.0003 -5.97 0.20 0.88 0.16
4 0.0004 -9.47 -0.24 1.04 0.01
5 0.0874 -2320.05 0.06 68.01 -0.01
6 0.0875 -2320.85 -0.10 68.03 0.02
7 0.0875 -2321.35 0.05 68.02 0.02
8 0.0929 -2478.27 -0.07 63.43 0.03
9 0.0930 -2478.81 0.07 63.33 -0.06
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.