Analysis
The following steps were followed in analyzing the data:
1) I used V2.15 of mips_sloper to reduce the data. I used flags -b -d -l
on the darks.
For the standard star observations I used the following:
mips_sloper -w -j CamF filename
mips_caler -C CamF filename
Campaign F dark and flat calibration files were placed in the directory
Pipeline/Cal/CamF and the mips_param_flight_ce1 and mips_caler.param
were edited in that directory to use these dark and flat files.
2) We used get_rdnoise on the 24um data to calculate read noise and dark
current. We set n_dce_rej=2. James had to edit the get_rdnoise program
to reject the bias boost DCE and the first DCE after the boost. He also
added a median filter and sigma rejection algorithm to remove cosmic rays.
3) I performed photometry on the standard star AOT data using the IRAF
task imexamine with the following parameters:
radius = 6, inner radius of sky annulus = 11, width of sky annulus = 5,
center = yes, background = yes, iterations = 1
4) Calculate the mean and sigma of the standard star fluxes
5) Plot standard star brightness, dark current, read noise, and source
repeatability versus detector bias
6) These results can be combined with insights into the effects of bias
voltage on the cosmic ray hardness and the dynamic range of the detector
in deciding how to best set the detector bias.