To measure the pixel locations (i.e. array orientation, scale) as a function of scan mirror angle for the 160 micron array. The goal of this task is to estimate the location of the 160 micron prime frame with repsect to the telescope boresight. The location of the MIPS instrument frames are found in the frame tables and are given as brown angles. In order to estimate the instrument pointing frame (IPF), a combinations of spacecraft moves and mirror motions places the star on several locations on the array. In addition, these observations are "sandwiched" between observations of stars with the two PCRS. The MIPS team calibrates data and centroids the star on the 160 micron array. These centroided values are passed to the IPF team who uses observations of stars with the PCRS to provide the final calibration and estimate brown angles need to locate the instrument frame.
The data from campaign K had a better S/N so we used that data instead of this data set.
With this data set the centroiding was difficult.
For a complete summary of frame table updates see :
Frame Table Updates: Meta task 2080