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: 15FC565 # Created Sun Oct 19 01:10:51 2025 # Orbit generated from Bernstein formalism # Fitting 10 observations of 10 # Arc: 11.00d # First observation: 2015/03/18 # Last observation: 2015/03/29 Preliminary a, adot, b, bdot, g, gdot: -0.000001 0.054496 0.000000 -0.007575 0.033876 0.000000 # WARNING Fitting with energy constraint # Chi-squared of fit: 225.81 DOF: 15 RMS: 0.84 # Min/Max residuals: -3.03 1.39 # Exact a, adot, b, bdot, g, gdot: 2.269828E-05 4.841696E-02 -2.844165E-06 -6.640207E-03 3.264571E-02 -7.937877E-03 # Covariance matrix: 1.3147E-12 2.3441E-09 -2.2180E-13 -3.6310E-10 4.4885E-10 5.4055E-09 2.3441E-09 5.3358E-06 -5.0200E-10 -8.2279E-07 1.0163E-06 1.1052E-05 -2.2180E-13 -5.0200E-10 3.2131E-13 6.7173E-11 -9.5685E-11 -1.1246E-09 -3.6310E-10 -8.2279E-07 6.7173E-11 1.2772E-07 -1.5673E-07 -1.7008E-06 4.4885E-10 1.0163E-06 -9.5685E-11 -1.5673E-07 1.9367E-07 2.2192E-06 5.4055E-09 1.1052E-05 -1.1246E-09 -1.7008E-06 2.2192E-06 1.9493E-04 # lat0 lon0 xBary yBary zBary JD0 13.723280 -145.238495 0.601206 0.187357 -0.766714 2457100.089728 # Heliocentric elements and errors Epoch: 2457100.5000 = 2015/03/19 Mean Anomaly: 358.89292 +/- 2.194 Argument of Peri: 141.57532 +/- 33.750 Long of Asc Node: 93.52412 +/- 0.449 Inclination: 15.37187 +/- 0.067 Eccentricity: 0.83742264 +/- 0.1696 Semi-Major Axis: 186.56017376 +/- 177.6715 Time of Perihelion: 2459962.7201 +/- 3933.2 Perihelion: 30.33046136 +/- 42.8407 Aphelion: 342.78988617 +/- 327.9870 Period (y) 2548.2182 +/- 3640.21 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X -25.44064852 +/- 0.3296 Ecliptic Y -16.92280748 +/- 0.2287 Ecliptic Z 7.26683400 +/- 0.0980 Ecliptic XDOT 0.00273449 +/- 0.0009 Ecliptic YDOT -0.00304821 +/- 0.0007 Ecliptic ZDOT -0.00069883 +/- 0.0003 # Distances at JD0 (AU) Heliocenter to KBO 31.40724258 +/- 0.2949 Geocenter to KBO 30.63189713 +/- 0.4129 # Hcoef: 10.06
The following table shows the complete astrometric record for 15FC565. 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 (15FC565) followed by the observatory code and reference code for the source of the astrometry.
2015 03 18.58895 14 28 12.62 -00 09 09.9 25.3r 15FC565 T09 C~99u3 2015 03 18.60439 14 28 12.55 -00 09 09.1 24.7r 15FC565 T09 C~99u3 2015 03 18.63105 14 28 12.45 -00 09 08.3 24.5r 15FC565 T09 C~99u3 2015 03 18.64048 14 28 12.40 -00 09 07.9 24.9r 15FC565 T09 C~99u4 2015 03 18.64474 14 28 12.40 -00 09 07.9 25.0r 15FC565 T09 C~99u4 2015 03 25.60942 14 27 44.24 -00 05 14.0 26.1g 15FC565 T09 C~99u4 2015 03 25.61869 14 27 44.19 -00 05 13.6 26.0g 15FC565 T09 C~99u4 2015 03 29.47724 14 27 26.81 -00 03 02.3 25.1y 15FC565 T09 C~99u4 2015 03 29.57488 14 27 26.61 -00 03 01.3 24.3z 15FC565 T09 C~99u4 2015 03 29.59028 14 27 26.53 -00 03 00.9 24.6z 15FC565 T09 C~99u4
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 0.16 0.00 -0.08
2 0.0000 -1.25 -0.09 0.41 0.14
3 0.0001 -2.93 -0.02 0.68 0.06
4 0.0001 -3.77 -0.24 0.81 0.07
5 0.0002 -3.77 0.04 0.81 0.02
6 0.0192 -479.42 0.31 83.83 -0.33
7 0.0192 -480.26 0.15 83.97 -0.29
8 0.0298 -769.55 -3.03 122.86 0.75
9 0.0301 -772.72 1.39 122.83 -0.10
10 0.0301 -773.98 1.32 122.81 -0.25
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.