To measure the pixel locations (i.e. array orientation, scale) as a function of scan mirror angle for the 24µm array. The goal of this task is to estimate the location of the 24 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 24 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 was nominal ( the flip in x, discovered in the first light campgain, had already occured).
This task was also performed in campaign F. The IPF team analyzed both the campaign F and campaign G results.
The results from both campaigns were consistent with eachother. Therefore the IPF team combined the results from both campaigns for a final run which was used to update frame table update 10.
The results from combining the 24 micron coarse FPS for campaign G and F is that the IPF team recommended the following changes to the brown angles for the prime frame : delta_theta_Y (-0.007896 arc minutes), delta_theta_Z (-0.012179 arc minutes), delta_angle (0.060630 degrees). The IPF team gave an accuracy of the locating the 24 micron prime frame center as 0.1054 rc seconds. The requirement was 1.0 arc seconds.
For a complete summary of frame table updates see :
Frame Table Updates: Meta task 2080
The resulting frame table update 10 contained the following changes:
