Index: /trunk/MagicSoft/GRB-Proposal/Introduction.tex
===================================================================
--- /trunk/MagicSoft/GRB-Proposal/Introduction.tex	(revision 6099)
+++ /trunk/MagicSoft/GRB-Proposal/Introduction.tex	(revision 6100)
@@ -43,5 +43,5 @@
 While the major energy from the prompt GRBs is emitted in $\gamma$-rays ($E_p \sim$ 200~keV), XRFs are characterized
 by peak energies below 50~keV and a dominated X-ray fluence. Because of similar properties a connection between XRFs and GRBs is strongly suggested. The most popular theories say that XRFs are produced from GRBs observed ''off-axis''.
-Alternativly, an increase of the baryon load within the fireball itself or low efficiency shocks can produce XRFs. If there is a connection between the XRFs and GRBs, they should originate at low redshifts (z < 0.6).\\
+Alternativly, an increase of the baryon load within the fireball itself or low efficiency shocks can produce XRFs. If there is a connection between the XRFs and GRBs, they should originate at low redshifts (z $<$ 0.6).\\
 
 Gamma-ray satellites react in the same way on XRFs and GRBs. In case of a detection the coordinates are distributed to other observatories (see section 2.1). Only from later analysis the difference can be established.
Index: /trunk/MagicSoft/GRB-Proposal/Strategies.tex
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--- /trunk/MagicSoft/GRB-Proposal/Strategies.tex	(revision 6099)
+++ /trunk/MagicSoft/GRB-Proposal/Strategies.tex	(revision 6100)
@@ -47,10 +47,41 @@
 to implement a new feature into the Steering System wich
 follow a different path while selwing must be considered.
-
+\par
+There was a shift observing the Crab-Nebula with half-moon at La Palma in December 2004. 
+The experience was that the nominal High-Voltages could be maintained and gave no 
+currents higher than 2\,$\mu$A. This means that moon-periods can be used for GRB-observations 
+without fundamental modifications except for full-moon periods. We want to stress that 
+these periods increase the chances to catch GRBs by 80\%, even if full-moon observations are excluded 
+\cite{NICOLA}. 
+It is therefore mandatory that the shifters keep the camera in fully operational conditions with high-voltages 
+already switched on from the beginning of a half-moon night until the end. 
+\par
+Because the background is higher with moon-light, we want to decrease then the maximun zenith angle from 
+$\theta^{max} = 70^\circ$ to $\theta^{max} = 65^\circ$. 
 
 \subsection{Calibration }
 
-\ldots {\bf MARKUS gAUG} \ldots
+For ordinary source observation, the calibration is currently performed in the following way: 
+\begin{itemize}
+\item At the beginning of the source observation, a dedicated pedestal run following by a calibration run is 
+taken.
+\item During the data runs, interlaced calibration events are taken with a rate of 50\,Hz.
+\end{itemize}
 
+We would like to continue taking the interlaced calibration events when a GRB
+alert is launched, but leave out the pedestal and calibration run in order not to loose valueable time.
+
+\subsection{Determine the maximum zenith angle}
+
+We determine the maximum zenith angle by requiring that the overwhelming majority of 
+possible GRBs will yield an in principle observable spectrum. Figure~\ref{fig:grh} 
+
+
+\begin{figure}
+\centering
+\includegraphics[width=0.99\linewidth]{f4.eps}
+\caption{
+\label{fig:grh}
+\end{figure}
 
 \subsection{In case of follow-up: Next steps}