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The data were reduced using the DAT version 2-41. Sensitive cosmic ray detection (mips_sloper comandline switch -q) was used and the electronic nonlinearity correction was not applied. The read niose input into mips_sloper was 100 electrons. No dark image was created due to the problems with the stim flashes.
No dark measurement were possible with this data.
The noise were determined for the d3 noise datasets. Many of the pixels on have many cosmic rays. Thus, we have measured the noise both with the new empirical method as well as the standard method. Our standard method of measuring noise is to determine the standard deviation of all the slopes of a pixel without detected cosmic rays. The empirical method is to do an iterative sigma rejection of deviant slopes. The results of the two methods are shown below. Given the middle reset each DCE, the noise measurement is for the average of two 5 MIPS second ramps. Thus, the effective exposure of the measurements is two times 5 MIPS seconds, not 10 MIPS seconds. This point is made as the noise we are measuring is 1/f noise and the specifics of how the data are taken are important. We have also quoted the noise on the good engineering pixels. These "pixelless" pixels give a good measure of the noise introduced by the electronics themselves. In the images below, the middle (non-existant) row has been removed.
The noise measurement given here is the noise in excess of that expected from photon statistics.
| Empirical Sigma Rejection (cut at 3*sigma) |
All DCEs with CR detected rejected plus empirical Sigma Rejection (cut at 3*sigma) |
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|---|---|---|---|
| Flight Data (mips_IER_7139584_d3_rn_A160_P24_10s) | |||
 scale = 0 - 30000 e counts = 11424.7 +/- 7159.2 e/s noise = 14434.5 +/- 6839.5 e DCEs used = 48.29 per pixel 34 pixels Eng. Pixels noise = 113.0 +/- 20.2 e 12 pixels |
 scale = 0 - 30000 e counts = 9971.4 +/- 6713.8 e/s noise = 9669.5 +/- 5455.4 e DCEs used = 9.31 per pixel 29 pixels Eng. Pixels noise = 94.8 +/- 13.2 e 11 pixels |
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The high responsivity means that very little of the 160 µm data in CamH can be calibrated so the lack of a 160 dark in not a problem.
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