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: 17BH241
# Created Wed Nov 27 02:10:46 2024
# Orbit generated from Bernstein formalism
# Fitting 10 observations of 10
# Arc: 5.01d
# First observation: 2017/01/23
# Last observation: 2017/01/28
Preliminary a, adot, b, bdot, g, gdot:
0.000001 0.027059 -0.000000 -0.000157 0.025433 0.000000
# WARNING MRQMIN stopped after 13 iterations -- oscilliatory solution
# WARNING Fitting with energy constraint
# Chi-squared of fit: 3.02 DOF: 15 RMS: 0.10
# Min/Max residuals: -0.18 0.17
# Exact a, adot, b, bdot, g, gdot:
1.680524E-05 2.535231E-02 -2.929051E-08 -4.351164E-05 2.485473E-02 -6.521368E-04
# Covariance matrix:
3.9447E-12 6.2135E-09 -2.7438E-13 -4.2615E-10 2.0075E-09 8.8665E-09
6.2135E-09 1.0704E-05 -4.7044E-10 -7.3074E-07 3.4420E-06 1.4228E-05
-2.7438E-13 -4.7044E-10 3.2596E-13 5.6179E-12 -1.5135E-10 -6.6918E-10
-4.2615E-10 -7.3074E-07 5.6179E-12 5.4337E-08 -2.3507E-07 -9.4638E-07
2.0075E-09 3.4420E-06 -1.5135E-10 -2.3507E-07 1.1073E-06 4.8253E-06
8.8665E-09 1.4228E-05 -6.6918E-10 -9.4638E-07 4.8253E-06 1.2196E-03
# lat0 lon0 xBary yBary zBary JD0
2.185958 -173.570243 0.879798 0.017147 -0.444732 2457777.111061
# Heliocentric elements and errors
Epoch: 2457770.5000 = 2017/01/17
Mean Anomaly: 331.43240 +/- 274.514
Argument of Peri: 125.50762 +/- 70.344
Long of Asc Node: 93.82083 +/- 13.539
Inclination: 2.16195 +/- 0.011
Eccentricity: 0.09193970 +/- 0.7717
Semi-Major Axis: 44.16171167 +/- 5.8448
Time of Perihelion: 2466276.7568 +/- 188924.5
Perihelion: 40.10149704 +/- 34.4892
Aphelion: 48.22192629 +/- 34.6709
Period (y) 293.4790 +/- 58.26
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -40.49565898 +/- 1.6915
Ecliptic Y -3.68264006 +/- 0.1906
Ecliptic Z 1.53461688 +/- 0.0650
Ecliptic XDOT 0.00038672 +/- 0.0038
Ecliptic YDOT -0.00277378 +/- 0.0005
Ecliptic ZDOT -0.00000759 +/- 0.0001
# Distances at JD0 (AU)
Heliocenter to KBO 40.69171025 +/- 1.6834
Geocenter to KBO 40.23379372 +/- 1.7034
# Hcoef: 8.15
The following table shows the complete astrometric record for 17BH241. 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 (17BH241) followed by the observatory code and reference code for the source of the astrometry.
2017 01 23.61026 12 27 04.29 -00 32 43.1 24.4i 17BH241 T09 C~86um 2017 01 23.61293 12 27 04.30 -00 32 43.1 24.3i 17BH241 T09 C~86um 2017 01 23.64112 12 27 04.26 -00 32 42.8 24.1i 17BH241 T09 C~86um 2017 01 23.64653 12 27 04.23 -00 32 42.6 24.3i 17BH241 T09 C~86um 2017 01 26.62617 12 26 59.33 -00 32 01.5 23.6z 17BH241 T09 C~86um 2017 01 26.62885 12 26 59.34 -00 32 01.3 24.1z 17BH241 T09 C~86um 2017 01 26.65302 12 26 59.28 -00 32 01.0 23.8z 17BH241 T09 C~86um 2017 01 28.60345 12 26 55.66 -00 31 31.2 24.4z 17BH241 T09 C~86um 2017 01 28.60879 12 26 55.65 -00 31 31.2 24.0z 17BH241 T09 C~86um 2017 01 28.61691 12 26 55.64 -00 31 31.2 24.1z 17BH241 T09 C~86um
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 -0.14 0.00 0.00
2 0.0000 0.14 0.07 0.06 0.05
3 0.0001 -0.53 0.17 0.10 0.02
4 0.0001 -1.02 -0.18 0.10 0.01
5 0.0083 -84.78 -0.03 8.80 -0.18
6 0.0083 -84.72 0.11 9.05 0.05
7 0.0083 -85.67 -0.07 8.97 -0.09
8 0.0137 -147.32 -0.10 14.88 0.12
9 0.0137 -147.46 -0.06 14.82 0.05
10 0.0137 -147.60 0.08 14.76 -0.03
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.