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: 17BE241
# Created Wed Nov 27 02:10:46 2024
# Orbit generated from Bernstein formalism
# Fitting 8 observations of 8
# Arc: 31.03d
# First observation: 2017/01/23
# Last observation: 2017/02/23
Preliminary a, adot, b, bdot, g, gdot:
-0.000001 0.020988 0.000000 -0.001382 0.023160 0.000000
# WARNING Fitting with energy constraint
# WARNING MRQMIN stopped after 14 iterations -- oscilliatory solution
# Chi-squared of fit: 5.13 DOF: 11 RMS: 0.14
# Min/Max residuals: -0.20 0.41
# Exact a, adot, b, bdot, g, gdot:
1.397549E-05 2.128153E-02 -5.354302E-07 -1.391725E-03 2.305632E-02 -5.297386E-03
# Covariance matrix:
2.2945E-10 3.4008E-07 -1.0901E-11 -1.5859E-08 8.2451E-08 7.8533E-07
3.4008E-07 5.0485E-04 -1.6183E-08 -2.3543E-05 1.2240E-04 1.1657E-03
-1.0901E-11 -1.6183E-08 8.8045E-13 7.5042E-10 -3.9235E-09 -3.7383E-08
-1.5859E-08 -2.3543E-05 7.5042E-10 1.0980E-06 -5.7080E-06 -5.4380E-05
8.2451E-08 1.2240E-04 -3.9235E-09 -5.7080E-06 2.9676E-05 2.8340E-04
7.8533E-07 1.1657E-03 -3.7383E-08 -5.4380E-05 2.8340E-04 3.2097E-03
# lat0 lon0 xBary yBary zBary JD0
2.353453 -172.667861 0.886719 0.017874 -0.430738 2457777.108391
# Heliocentric elements and errors
Epoch: 2457770.5000 = 2017/01/17
Mean Anomaly: 287.95013 +/- 134.749
Argument of Peri: 250.00204 +/- 217.334
Long of Asc Node: 38.26499 +/- 9.429
Inclination: 4.37920 +/- 1.188
Eccentricity: 0.26091494 +/- 2.6229
Semi-Major Axis: 44.43108940 +/- 23.3654
Time of Perihelion: 2479420.5844 +/- 36712.5
Perihelion: 32.83835416 +/- 117.8108
Aphelion: 56.02382463 +/- 120.2047
Period (y) 296.1683 +/- 233.62
# Ecliptic coordinates at JD0 (AU and AU/d)
Ecliptic X -43.52511242 +/- 10.1553
Ecliptic Y -4.71075437 +/- 1.3062
Ecliptic Z 1.78098840 +/- 0.4208
Ecliptic XDOT 0.00094198 +/- 0.0066
Ecliptic YDOT -0.00243379 +/- 0.0029
Ecliptic ZDOT -0.00019101 +/- 0.0002
# Distances at JD0 (AU)
Heliocenter to KBO 43.81550567 +/- 10.0890
Geocenter to KBO 43.37205490 +/- 10.2476
# Hcoef: 9.08
The following table shows the complete astrometric record for 17BE241. 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 (17BE241) followed by the observatory code and reference code for the source of the astrometry.
2017 01 23.60759 12 30 38.99 -00 44 51.1 25.1i 17BE241 T09 C~86ul 2017 01 23.61026 12 30 38.97 -00 44 51.0 25.1i 17BE241 T09 C~86ul 2017 01 23.62432 12 30 38.96 -00 44 51.0 24.8i 17BE241 T09 C~86ul 2017 01 23.64653 12 30 38.93 -00 44 50.1 25.4i 17BE241 T09 C~86ul 2017 02 23.53583 12 29 19.97 -00 35 22.9 25.7r 17BE241 T09 C~86um 2017 02 23.56346 12 29 19.86 -00 35 22.4 26.0r 17BE241 T09 C~86um 2017 02 23.60592 12 29 19.71 -00 35 21.2 25.7r 17BE241 T09 C~86um 2017 02 23.63774 12 29 19.60 -00 35 20.6 25.2r 17BE241 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 0.13 0.00 -0.09
2 0.0000 -0.32 -0.12 -0.03 -0.12
3 0.0000 -0.45 0.10 -0.09 -0.20
4 0.0001 -1.22 -0.11 0.56 0.41
5 0.0847 -1313.27 0.05 54.42 0.09
6 0.0848 -1314.98 -0.03 54.23 -0.12
7 0.0849 -1317.53 -0.07 54.44 0.07
8 0.0850 -1319.28 0.06 54.34 -0.05
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.