(12104) Chesley orbit determination test

Let’s start by importing the necessary libraries

from grss import fit
import numpy as np
np.set_printoptions(precision=40, linewidth=np.inf)

We’ll then retrieve the cometary state of the asteroid (from JPL SBDB) plus any nongravitational accelerations acting on it.

body_id = '12104'
init_sol, init_cov, nongrav_info = fit.get_sbdb_info(body_id)
de_kernel = 440

Next, we’ll retrieve the observations from different sources (MPC, JPL, Gaia Data Releases) and prepare them for the orbit determination process.

add_gaia_obs = True
optical_obs_file = None
t_min_tdb = None
t_max_tdb = None
debias_lowres = True
deweight = True
eliminate = False
num_obs_per_night = 4
verbose = True
obs_df = fit.get_optical_obs(body_id, optical_obs_file, t_min_tdb, t_max_tdb, debias_lowres, deweight, eliminate, num_obs_per_night, verbose)
obs_df = fit.add_radar_obs(obs_df, t_min_tdb, t_max_tdb, verbose)
if add_gaia_obs:
    gaia_dr = 'gaiafpr'
    obs_df = fit.add_gaia_obs(obs_df, t_min_tdb, t_max_tdb, gaia_dr, verbose)

Read in 5586 observations from the MPC.
        WARNING: At least one unknown observation mode in the data.
        WARNING: At least one deprecated star catalog in the data.
        Filtered to 5586 observations that satisfy the time range and accepted observatory constraints.
Applying Eggl et al. (2020) debiasing scheme to the observations.
        Unknown star catalog: UNK
        No debiasing needed for 4275 observations.
        Debiased 1289 observations.
        No bias information for 22 observations.
Applying Vereš et al. (2017) weighting scheme to the observations.
        Using 3412 CCD observations with station-specific weight rules.
Applying sqrt(N/4) deweighting scheme.
        Deweighted 2666 observations.
Read in 459 Gaia observations from gaiafpr
        Filtered to 459 observations that satisfy the time range constraints.

All we need to do now is initialize the OD simulation and run the filter.

n_iter_max = 10
fit_sim = fit.FitSimulation(init_sol, obs_df, init_cov, n_iter_max=n_iter_max, de_kernel=de_kernel, nongrav_info=nongrav_info)

fit_sim.filter_lsq()

Iteration               Unweighted RMS          Weighted RMS            Chi-squared             Reduced Chi-squared
1                        0.743                   0.481                   2795.789                        0.231
2                        0.743                   0.481                   2795.773                        0.231
Converged without rejecting outliers. Starting outlier rejection now...
3                        0.710                   0.444                   2379.525                        0.198
Converged after rejecting outliers. Rejected 28 out of 6045 optical observations.

Let’s print some summary statistics and plot some results.

fit_sim.print_summary()

Summary of the orbit fit calculations after postfit pass:
==============================================================
RMS unweighted: 0.7100074619321145
RMS weighted: 0.4436413284570808
chi-squared: 2379.525126330326
reduced chi-squared: 0.19783215217245811
square root of reduced chi-squared: 0.44478326426750603
--------------------------------------------------------------
Solution Time: MJD 58122.000 TDB = 2018-01-04 00:00:00.000 TDB
Solution Observation Arc: 17721.12 days (48.52 years)
--------------------------------------------------------------
Fitted Variable         Initial Value                   Uncertainty                     Fitted Value                    Uncertainty                     Change                          Change (sigma)
e                       2.44896320089e-02               7.35000612766e-10               2.44896319457e-02               7.09160779128e-10               -6.32521292288e-11              -0.089
q                       2.93644529683e+00               3.42020021224e-09               2.93644529716e+00               3.30768440551e-09               +3.25952154157e-10              +0.099
tp                      5.87280803654e+04               6.74589596505e-06               5.87280803652e+04               6.52637683354e-06               -2.00343492907e-07              -0.031
om                      7.80640070842e+01               1.25609841342e-07               7.80640070802e+01               1.18383039626e-07               -4.04909883400e-09              -0.034
w                       1.83027495153e+02               1.33571798783e-06               1.83027495107e+02               1.29395463714e-06               -4.56345219391e-08              -0.035
i                       1.11526237797e+01               2.98360369954e-08               1.11526237812e+01               2.85056308612e-08               +1.48345158379e-09              +0.052

fit_sim.plot_summary(auto_close=True)

fit_sim.iters[-1].plot_iteration_summary(title='Postfit Residuals', auto_close=True)

mean_0 = np.array(list(init_sol.values())[1:])
cov_0 = init_cov
mean_f = np.array(list(fit_sim.x_nom.values()))
cov_f = fit_sim.covariance

maha_dist_f, maha_dist_0, bhattacharya, bhatt_coeff = fit.get_similarity_stats(mean_0, cov_0, mean_f, cov_f)
print(f'Mahalonobis distance between JPL and GRSS solution: {maha_dist_f:0.2f}')
print(f'Mahalonobis distance between GRSS and JPL solution: {maha_dist_0:0.2f}')
print(f'Bhattacharya distance between JPL and GRSS solution: {bhattacharya:0.4f}')
print(f'Bhattacharya coefficient between JPL and GRSS solution: {bhatt_coeff:0.4f}')

Mahalonobis distance between JPL and GRSS solution: 0.12
Mahalonobis distance between GRSS and JPL solution: 0.13
Bhattacharya distance between JPL and GRSS solution: 0.0031
Bhattacharya coefficient between JPL and GRSS solution: 0.9970

Finally, we’ll make sure the GRSS solution is statistically consistent with the JPL SBDB solution

assert maha_dist_f < 5.0
assert maha_dist_0 < 5.0
assert bhattacharya < 0.10
assert bhatt_coeff > 0.90