Index: trunk/MagicSoft/TDAS-Extractor/Criteria.tex
===================================================================
--- trunk/MagicSoft/TDAS-Extractor/Criteria.tex	(revision 6601)
+++ trunk/MagicSoft/TDAS-Extractor/Criteria.tex	(revision 6602)
@@ -59,5 +59,7 @@
 In the case of MAGIC the background fluctuations are due to electronics noise  and the PMT response to LONS. The signals from the latter background are not distinguishable from the Cherenkov signals. Thus each algorithm which searches for the signals inside the recorded FADC time slices will have a bias. In case of no Cherenkov signal it will reconstruct the largest noise pulse. 
 
-Note that every sliding window extractor, the digital filter and the spline extractor has a bias, especially at low or vanishing signals $S$.
+Note that every sliding window extractor, the digital filter and the spline extractor have a bias, 
+especially at low or vanishing signals $S$, but usually a much smaller $R$ and in many cases a smaller $MSE$ than the fixed window 
+extractors.
 
 \subsection{Linearity}
@@ -86,5 +88,5 @@
 and low-gain pulse is small, thus for large pulses, 
 mis-interpretations between the tails of the high-gain pulse and the low-gain pulse might occur. Moreover, the total recorded time window 
-is relatively small and at late high-gain pulses, parts of the low-gain pulse might already reach out of the recorded FADC window. 
+is relatively small and for late high-gain pulses, parts of the low-gain pulse might already reach out of the recorded FADC window. 
 A good extractor must be 
 stably extracting the low-gain pulse without being confused by the above points. This is especially important since the low-gain 
@@ -109,4 +111,5 @@
 
 \subsection{Applicability for Different Sampling Speeds / No Pulse Shaping.}
+
 The current read-out system of the MAGIC telescope~\cite{Magic-DAQ} with 300~MSamples/s is relatively slow compared to the fast pulses of 
 about 2\,ns FWHM of Cherenkov pulses. 
@@ -119,25 +122,25 @@
 \subsection{CPU Requirements}
 
-Depending on the reconstruction algorithm the signal reconstruction can take a significant amount of CPU time. Especially the more  sophisticated signal extractors which search for the position of the Cherenkov signals in the recorded FADC time slices and perform a fit to these samples can be time consuming.
+Depending on the reconstruction algorithm the signal reconstruction can take a significant amount of CPU time. 
+Especially the more sophisticated signal extractors can be time consuming which search for the position of the Cherenkov signals 
+in the recorded FADC time slices and perform a fit to these samples. At any case, the extractor should not be significantly slower than 
+the reading and writing routines of the MARS software. 
 
-Thus for an online-analysis a different extraction algorithm might be chosen than for the final most accurate reconstruction of the signals offline.
-
-
-
+Thus, for an online-analysis a different extraction algorithm might be chosen than for the final most accurate 
+reconstruction of the signals offline.
 
 \subsection{Treatment of Calibration Pulses}
 
+The calibration pulse reconstruction sets two important constraints to the signal extractor:
 
-\subsection{Pulpo Pulses}
-
-\subsection{Cosmics Data?}
-The results of this subsection are based on the following runs taken
-on the 21st of September 2004.
-\begin{itemize}
-\item{Run 39000}: OffCrab11 at 19.1 degrees zenith angle and 106.2
-azimuth.
-\item{Run 39182}: CrabNebula at 19.0 degrees zenith angle and 106.0 azimuth.
-\end{itemize}
-
+\begin{enumerate}
+\item As the standard calibration uses the F-Factor method in order to reconstruct the number of impinging photo-electrons,
+the resolution of the extractor must be constant for different  signal heights, especially between the case: $S=0$ and 
+$S = 40\pm 7$~photo-electrons which is the default intensity of the current calibration pulses. This constraint is especially  
+non-trivial for extractors searching the signal in a sliding window.
+\item As the calibration pulses are slightly wider than the cosmics pulses, the obtained conversion factors must not be affected by 
+the difference in pulse shape. This puts severe contraints on all extractors which do not integrate the whole pulse or take the pulse 
+shape into account.
+\end{enumerate}
 
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