These programs will help perform the Gaussian method of OD for an asteroid. It is assumed that 5 star field images were taken during 3 evenly spaced observations. From these, the orbital elements of the asteroid will be determined.

This code was written for the. 2015 Summer Science Program at CU Boulder. If you are a current SSPer, please do not look at this! Remember the Honor Code! Afterward, feel free to try it out to see how your results compare! Also, feel free to contribute! Most of it was written in the wee hours of the morning on a month's worth of sleep deprivation, so do let me know if you spot any errors or find anything that can be improved.

This performs centroiding and least squares plate reduction on the star field images.

IMAGE CORRECTIONS: The star field image is first corrected using a flat image and the background pixels are subtracted (dark current should already be corrected for by MaxIm DL).

CENTROIDING: A weighted mean is taken using the dimensions and estimated centroid specified by the user. The location of the centroid pixel in the image is found.

ERROR: A variance array is generated to estimate maximum and minimum possible centroid values. (Note that this isn't really important as the error in the orbit determination program is what matters. This was mostly useful for developing the code.)

LSPR: Uses least squares plate reduction to find the RA and DEC of the asteroid given its centroid pixel values and the pixel, RA, and DEC values for six reference stars in the star field image. (The ESO-DSS I/II image server and PPMX optical catalogue on DS9 can be a good resource for finding reference stars.) There is more (not at all good) error analysis code here too.

Gauss' method of orbit determination based on Kepler's Second Law! Outputs a nice orbital elements chart.

Modified gaussianODWithMagellanData.py to run in py36 environment.
Visualize the orbits with poliastro libraries.
Use DE430 to compute precise Earth positions.