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: 15LD75 # Created Wed Nov 27 02:10:22 2024 # Orbit generated from Bernstein formalism # Fitting 8 observations of 8 # Arc: 3.91d # First observation: 2015/06/05 # Last observation: 2015/06/09 Preliminary a, adot, b, bdot, g, gdot: -0.000000 0.529866 0.000001 -0.222076 0.201876 0.000000 # WARNING MRQMIN stopped after 13 iterations -- oscilliatory solution # WARNING Fitting with energy constraint # WARNING MRQMIN stopped after 13 iterations -- oscilliatory solution # Chi-squared of fit: 0.63 DOF: 11 RMS: 0.05 # Min/Max residuals: -0.08 0.09 # Exact a, adot, b, bdot, g, gdot: 3.995010E-05 4.796968E-01 -1.690910E-05 -2.063423E-01 1.899957E-01 -6.931895E-02 # Covariance matrix: 5.6605E-12 5.9834E-08 -9.8673E-13 -1.8840E-08 1.4324E-08 -7.4257E-07 5.9834E-08 7.1762E-04 -1.1615E-08 -2.2539E-04 1.7117E-04 -9.5069E-03 -9.8673E-13 -1.1615E-08 7.4464E-13 3.5906E-09 -2.7764E-09 1.4566E-07 -1.8840E-08 -2.2539E-04 3.5906E-09 7.0810E-05 -5.3772E-05 2.9731E-03 1.4324E-08 1.7117E-04 -2.7764E-09 -5.3772E-05 4.0842E-05 -2.2502E-03 -7.4257E-07 -9.5069E-03 1.4566E-07 2.9731E-03 -2.2502E-03 1.5010E-01 # lat0 lon0 xBary yBary zBary JD0 -16.061860 -153.870483 -0.753597 -0.187418 -0.651412 2457178.650857 # Heliocentric elements and errors Epoch: 2457170.5000 = 2015/05/28 Mean Anomaly: 351.73447 +/- 190.944 Argument of Peri: 226.22132 +/- 277.368 Long of Asc Node: 1.08183 +/- 4.591 Inclination: 25.08320 +/- 2.977 Eccentricity: 0.16520878 +/- 0.3457 Semi-Major Axis: 7.13040156 +/- 1.8007 Time of Perihelion: 2457330.1752 +/- 3688.2 Perihelion: 5.95239661 +/- 2.8869 Aphelion: 8.30840651 +/- 3.2368 Period (y) 19.0405 +/- 7.21 # Ecliptic coordinates at JD0 (AU and AU/d) Ecliptic X -4.82083897 +/- 0.1527 Ecliptic Y -3.20278794 +/- 0.0749 Ecliptic Z -1.45627948 +/- 0.0490 Ecliptic XDOT 0.00464201 +/- 0.0049 Ecliptic YDOT -0.00542716 +/- 0.0022 Ecliptic ZDOT -0.00258090 +/- 0.0015 # Distances at JD0 (AU) Heliocenter to KBO 5.96817299 +/- 0.1303 Geocenter to KBO 5.26327695 +/- 0.1770 # Hcoef: 14.32
The following table shows the complete astrometric record for 15LD75. 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 (15LD75) followed by the observatory code and reference code for the source of the astrometry.
2015 06 05.150079 13 11 29.803 -24 58 22.01 22.1r 15LD75 W84 C~89SI 2015 06 05.152832 13 11 29.773 -24 58 21.67 22.2r 15LD75 W84 C~89SI 2015 06 06.057410 13 11 19.663 -24 57 03.24 22.3r 15LD75 W84 C~89SI 2015 06 08.171272 13 10 57.987 -24 54 05.09 22.4r 15LD75 W84 C~89SI 2015 06 08.172985 13 10 57.974 -24 54 04.84 22.4r 15LD75 W84 C~89SI 2015 06 08.175055 13 10 57.944 -24 54 04.70 22.2r 15LD75 W84 C~89SI 2015 06 08.993808 13 10 50.514 -24 52 58.19 22.3g 15LD75 W84 C~89SI 2015 06 09.064838 13 10 49.820 -24 52 52.48 22.9g 15LD75 W84 C~89SI
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 -0.01 0.00 -0.05
2 0.0000 -0.51 -0.00 0.15 0.05
3 0.0025 -157.78 0.01 18.05 0.02
4 0.0083 -499.00 0.02 65.42 -0.07
5 0.0083 -499.26 0.03 65.58 0.05
6 0.0083 -499.69 -0.07 65.54 -0.03
7 0.0105 -618.84 0.09 86.72 0.06
8 0.0107 -629.77 -0.08 88.23 -0.02
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.