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: 15JF13 # Created Wed May 21 01:10:30 2025 # Orbit generated from Bernstein formalism # Fitting 8 observations of 8 # Arc: 1.96d # First observation: 2015/05/15 # Last observation: 2015/05/17 # WARNING Fitting with energy constraint # WARNING and with gdot fixed = 0 # Chi-squared of fit: 1.53 DOF: 12 RMS: 0.08 # Min/Max residuals: -0.14 0.11 # Exact a, adot, b, bdot, g, gdot: 1.481586E-05 2.578714E-02 -4.890321E-06 -8.726727E-03 2.657007E-02 0.000000E+00 # Covariance matrix: 4.9254E-11 8.2015E-08 3.9133E-12 6.5949E-09 1.4034E-08 0.0000E+00 8.2015E-08 1.3741E-04 6.5517E-09 1.1041E-05 2.3496E-05 0.0000E+00 3.9133E-12 6.5517E-09 5.5545E-13 4.8565E-10 1.1205E-09 0.0000E+00 6.5949E-09 1.1041E-05 4.8565E-10 9.1565E-07 1.8884E-06 0.0000E+00 1.4034E-08 2.3496E-05 1.1205E-09 1.8884E-06 4.0184E-06 0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 0.0000E+00 2.4683E-04 # lat0 lon0 xBary yBary zBary JD0 12.991536 -145.363924 -0.338023 0.213816 -0.926342 2457157.913320 # Heliocentric elements and errors Epoch: 2457150.5000 = 2015/05/08 Mean Anomaly: 22.39617 +/- 317.442 Argument of Peri: 121.29167 +/- 20.276 Long of Asc Node: 67.93063 +/- 14.565 Inclination: 22.55246 +/- 8.029 Eccentricity: 0.03074859 +/- 0.5837 Semi-Major Axis: 39.68979371 +/- 20.9450 Time of Perihelion: 2451468.6731 +/- 263156.7 Perihelion: 38.46938867 +/- 30.8038 Aphelion: 40.91019874 +/- 31.6675 Period (y) 250.0498 +/- 197.93 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X -30.76685833 +/- 2.2766 Ecliptic Y -21.66237211 +/- 1.5724 Ecliptic Z 8.46079170 +/- 0.6383 Ecliptic XDOT 0.00134106 +/- 0.0014 Ecliptic YDOT -0.00230728 +/- 0.0012 Ecliptic ZDOT -0.00087613 +/- 0.0004 # Distances at JD0 (AU) Heliocenter to KBO 38.56738172 +/- 2.0243 Geocenter to KBO 37.63633971 +/- 2.8395 # Hcoef: 8.90
The following table shows the complete astrometric record for 15JF13. 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 (15JF13) followed by the observatory code and reference code for the source of the astrometry.
2015 05 15.412542 14 26 47.503 -00 48 15.63 24.9r 15JF13 568 C~2TuN 2015 05 15.431048 14 26 47.404 -00 48 15.19 24.7r 15JF13 568 C~2TuN 2015 05 15.435977 14 26 47.383 -00 48 15.18 24.6r 15JF13 568 C~2TuN 2015 05 15.446581 14 26 47.329 -00 48 15.04 24.4r 15JF13 568 C~2TuN 2015 05 15.463998 14 26 47.232 -00 48 14.96 24.6r 15JF13 568 C~2TuN 2015 05 17.351168 14 26 38.043 -00 47 51.09 25.2g 15JF13 568 C~2TuN 2015 05 17.367074 14 26 37.971 -00 47 50.69 25.3g 15JF13 568 C~2TuN 2015 05 17.369180 14 26 37.965 -00 47 50.79 25.2g 15JF13 568 C~2TuN
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 0.11 0.00 -0.06
2 0.0001 -1.55 -0.05 -0.07 0.09
3 0.0001 -1.85 0.02 -0.16 0.06
4 0.0001 -2.66 0.01 -0.30 0.05
5 0.0001 -4.06 -0.09 -0.70 -0.14
6 0.0053 -142.10 -0.05 -23.25 -0.12
7 0.0054 -143.25 -0.03 -23.23 0.11
8 0.0054 -143.31 0.08 -23.35 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.