Index: /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex
===================================================================
--- /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex	(revision 6161)
+++ /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex	(revision 6162)
@@ -96,6 +96,4 @@
 %------------------------------------------------------------
 
-\section{Calibrations}
-{\ldots \it \bf Crab data at different axis-offsets to calibrate off-axis sensitivity  \ldots \\}
 
 %%% BIBLIOGRAPHY %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
@@ -167,13 +165,14 @@
 \bibitem{KNEISKE} Kneiske T.M., Bretz T., Mannheim K., Hartmann D.H., A\&A 413, 807, 2004.
 \bibitem{GRB030329} Spectra of the burst: http://space.mit.edu/HETE/Bursts/GRB030329/
+\bibitem{ecl} Private communication with Lorenz E.
 
 %Not used references
 
-\bibitem{PAZCYNSKI} Pazcy\'{n}ski B., Astrophys. J. 308 L43 (1986)
-\bibitem{GOODMAN} Goodman J., Astrophys. J. 308 L47 (1986)
-\bibitem{SARI} Sari R., Piran T., Narayan R., Astrophys. J. 497 L17 (1998)
-\bibitem{XU} Pazcy\'{n}ski B., Xu G., Astrophys. J. 427 708 (1994)
-\bibitem{REES} Rees M., Meszaros P., MNRAS 258 P41 (1992)
-\bibitem{MESZAROS94} Meszaros P., Rees M., MNRAS 289 L41 (1994)
+%\bibitem{PAZCYNSKI} Pazcy\'{n}ski B., Astrophys. J. 308 L43 (1986)
+%\bibitem{GOODMAN} Goodman J., Astrophys. J. 308 L47 (1986)
+%\bibitem{SARI} Sari R., Piran T., Narayan R., Astrophys. J. 497 L17 (1998)
+%\bibitem{XU} Pazcy\'{n}ski B., Xu G., Astrophys. J. 427 708 (1994)
+%\bibitem{REES} Rees M., Meszaros P., MNRAS 258 P41 (1992)
+%\bibitem{MESZAROS94} Meszaros P., Rees M., MNRAS 289 L41 (1994)
 
 
Index: /trunk/MagicSoft/GRB-Proposal/Strategies.tex
===================================================================
--- /trunk/MagicSoft/GRB-Proposal/Strategies.tex	(revision 6161)
+++ /trunk/MagicSoft/GRB-Proposal/Strategies.tex	(revision 6162)
@@ -55,4 +55,9 @@
 $\theta_{max} = 70^\circ$ to $\theta_{max} = 65^\circ$.
 
+\subsection{Active Mirror Control behaviour}
+
+To reduce the time before starting of the observation, the use of the look-up tables (LUTs) is necessary.
+Once generated, the {\it AMC} will use the LUTs and automaticaly focus the panels for a given telescope position. The {\it CC} should send the burst coordinates to the {\it Drive} and the {\it AMC} software in the same time. In this way the panels could be focussed already during the telescope movement.
+
 \subsection{Calibration}
 
@@ -77,40 +82,34 @@
 
 Even the closest GRB with known redshift ever observed, GRB030329~\cite{GRB030329}, lies at a redshift
-of $z=0.1685$. In this case, gamma-rays above 200\,GeV get entirely absorbed.
+of $z=0.1685$. In this case $\gamma$-rays above 200\,GeV get entirely absorbed.
 
 \begin{figure}[htp]
 \centering
 \includegraphics[width=0.85\linewidth]{f4.eps}
-\caption{Gamma Ray Horizon, as derived in~\cite{KNEISKE}}
+\caption{Gamma Ray Horizon as derived in~\cite{KNEISKE}}
 \label{fig:grh}
 \end{figure}
 
 \par
-We assume now a current energy threshold of 50\,GeV for MAGIC at a zenith angle of $\theta = 0$\footnote{As 
-this proposal is going to be reviewed in a couple of months, improvements of the energy threshold will be taken 
-into account, then.}. According 
-to~\cite{eckart}, the energy threshold of a Cherenkov telescope scales with zenith angle like:
+
+We assume now a current energy threshold of 50\,GeV for \ma at a zenith angle of
+$\theta = 0$\footnote{As this proposal is going to be reviewed in a couple of months, improvements of the energy threshold will be taken into account then.}. According to~\cite{ecl}, the energy threshold of a Cherenkov telescope scales with zenith angle like:
 
 \begin{equation}
-E^{thr}(\theta) = E^{thr}(0) \cdot \cos(\theta)^{-2.7}
+E_{thr}(\theta) = E_{thr}(0) \cdot \cos(\theta)^{-2.7}
 \label{eq:ethrvszenith}
 \end{equation}
 
-Eq.~\ref{eq:ethrvszenith} leads to an energy threshold of about 5.6\,TeV at $\theta = 80^\circ$, 
-900\,GeV at $\theta = 70^\circ$ and 500\,GeV at $\theta = 65^\circ$. 
-Inserting these results into the GRH (figure~\ref{fig:grh}), one gets 
-a maximal observable GRB distance of $z = 0.1$ at $\theta = 70^\circ$ and $z = 0.2$ at $\theta = 65^\circ$. 
-We think that the probability for 
-GRBs to occur at these distances is sufficiently small in order to neglect the very difficult observations 
-beyond these limits.
+Eq.~\ref{eq:ethrvszenith} leads to an energy threshold of about 5.6\,TeV at $\theta = 80^\circ$,
+900\,GeV at $\theta = 70^\circ$ and 500\,GeV at $\theta = 65^\circ$.
+Inserting these results into the GRH (figure~\ref{fig:grh}), one gets a maximal observable GRB distance of $z = 0.1$ at $\theta = 70^\circ$ and $z = 0.2$ at $\theta = 65^\circ$.
+We think that the probability for GRBs to occur at these distances is sufficiently small in order to neglect the very difficult observations beyond these limits.
 
 \subsection{In case of follow-up: Next steps}
 
-We propose to analyse the GRB data at the following day in order to tell whether a follow-up observation during 
-the next night is useful. We think that a limit of 3\,$\sigma$ significance should be enough to start such a 
-follow-up observation of the same place. This follow-up observation can then be used in two ways:
+We propose to analyse the GRB data at the following day in order to tell whether a follow-up observation during the next night is useful. We think that a limit of 3\,$\sigma$ significance should be enough to start such a follow-up observation of the same place. This follow-up observation can then be used in two ways:
 
 \begin{itemize}
 \item In case of a repeated outbursts for a longer time period of direct observation
-\item In the other case for having Off-data at exactly the same location.
+\item In the other case for having Off-data at exactly the same sky location.
 \end{itemize}