Index: trunk/MagicSoft/TDAS-Extractor/Algorithms.tex
===================================================================
--- trunk/MagicSoft/TDAS-Extractor/Algorithms.tex	(revision 6554)
+++ trunk/MagicSoft/TDAS-Extractor/Algorithms.tex	(revision 6555)
@@ -519,7 +519,10 @@
 corresponding elements of both (bottom). The central regions of $\pm$3 FADC slices around the diagonal (which is used to 
 calculate the weights) deviate by less than 10\%. 
-Thus, the weights are to a very good approximation independent of the night sky background noise level in the high gain.
-\par
-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.
+Thus, the weights are to a reasonable approximation independent of the night sky background noise level in the high gain.
+\par
+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.
 
 %\begin{figure}[h!]