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.
This task was supposed to be cancelled because the previous 24 coarse surveys were sufficient.
Instead one run of the 24 micron fine FPS was done.
The 24 micron fine FPS is also done in campaign R. The results from campaign R were used for FTU 15.
The results from this run, campaign Q, and campaign R disagree by 1 arc second in the V direction.
This is a large amount and cause ssome concern. The IPF team believes that there is strong evidence that the actual frame changed by 1 arc seccond between to the two runs.
Below are the results from campaign Q.
Below are the results from camgaign R.
FTU 15 is based on campaign R.
For a complete summary of frame table updates see:
Frame Table Updates
