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 results from the IPF team recommended the following changes to the brown angles for the prime frame : delta_theta_Y (0.107 arc minutes), delta_theta_Z (0.13 arc minutes), delta_angle (0.000005 degrees). The IPF team gave an accuracy of the locating the 160 micron prime frame center as 0.6254 arc seconds. The requirement was 3.7 arc seconds. The results of this analysis was used to update frame table 14. However, these results are corrupted by the spectral leak (which we did not know about for this FTU - or we would not have done it).
The IPF results for this run gave the following brown angles. :
For a complete summary of frame table updates see :
Frame Table Updates: Meta task 2080
