Changeset 6555 for trunk/MagicSoft
- Timestamp:
- 02/16/05 20:01:55 (20 years ago)
- File:
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- 1 edited
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trunk/MagicSoft/TDAS-Extractor/Algorithms.tex
r6554 r6555 519 519 corresponding elements of both (bottom). The central regions of $\pm$3 FADC slices around the diagonal (which is used to 520 520 calculate the weights) deviate by less than 10\%. 521 Thus, the weights are to a very good approximation independent of the night sky background noise level in the high gain. 522 \par 523 Contrary to that in the low gain samples the correlated noise from the LONS is in the same order of magnitude as the white electronics and digitization noise. Moreover the noise autocorrelation for the low gain samples cannot be determined directly from the data. The low gain is only switched on if the pulse exceeds a preset threshold. There are no pedestals in the low gain available. Thus the noise auto-correlation determined from MC simulations for an extragalactic background is also used to compute the weights for cosmics and calibration pulses. 521 Thus, the weights are to a reasonable approximation independent of the night sky background noise level in the high gain. 522 \par 523 In the low gain samples the correlated noise from the LONS is in the same order of magnitude as the white electronics and digitization noise. 524 Moreover, the noise autocorrelation for the low gain samples cannot be determined directly from the data. The low gain is only switched on 525 if the pulse exceeds a preset threshold. There are no pedestals in the low gain available. Thus the noise auto-correlation determined from 526 MC simulations for an extragalactic background is also used to compute the weights for cosmics and calibration pulses. 524 527 525 528 %\begin{figure}[h!]
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