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 results from the IPF team recommended the following changes to the brown angles for the prime frame : delta_theta_Y (-0.519604 arc minutes), delta_theta_Z (-0.050213 arc minutes), delta_angle (-0.000002 degrees). The IPF team gave an accuracy of the locating the 160 micron prime frame center as 3.7858 arc seconds. The requirement was 3.75 arc seconds. The results of this analysis was used to update frame table 12. However, the results were corrupted by the spectral leak (which was discoverd after Campaign Q).
For a complete summary of frame table updates see :
Frame Table Updates: Meta task 2080
Frame table upate 12 contained the following changes:
