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.
This focal plane survey was done before the 160 spectral leak was understood.
The target used for this fps was a star (which is affected by the spectral leak).
Therefore the target that was centroided for this fps was dominated by the spectral leak and not the actual 160 micron source. This was corrected in 235-1MC.
The contamination of the data by the spectral leak was determined before any analysis was done for this survey. Therefore this survey was ignored and instead we used 235-1MC for the 160 FTU.
For a complete summary of frame table updates see :
Frame Table Updates: Meta task 2080