Index: /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex
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--- /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex	(revision 6218)
+++ /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex	(revision 6219)
@@ -121,5 +121,4 @@
 Hartmann D.H., Kneiske T.M., Mannheim K.,Watanabe K., AIP Conference Proceedings, 662, 442, 2003.
 \bibitem{MANNHEIM} Mannheim K., Hartmann D., Burkhardt F., AsJ, 467, 532, 1996.
-\bibitem{SALOMON} Absorption of HE Gamma Rays by Interactions with Extragalactic Starlight Photons at High Redshifts and the HE Gamma-Ray Background, Salomon M.H., Stecker F.J., ApJ, 493, 547, 1998.
 \bibitem{DERMER} Beaming, Baryon loading, and the Synchrotron Self-Compton Component in Gamma-Ray Bursts,
 Dermer \& Chiang, ApJ, 537, 785, 2000.
@@ -177,4 +176,5 @@
 
 \bibitem{KNEISKE} Kneiske T.M., Bretz T., Mannheim K., Hartmann D.H., A\&A 413, 807, 2004.
+\bibitem{SALOMON} Absorption of HE Gamma Rays by Interactions with Extragalactic Starlight Photons at High Redshifts and the HE Gamma-Ray Background, Salomon M.H., Stecker F.J., ApJ, 493, 547, 1998.
 \bibitem{GRB030329} Spectra of the burst: http://space.mit.edu/HETE/Bursts/GRB030329/
 \bibitem{ecl} Private communication with Lorenz E.
Index: /trunk/MagicSoft/GRB-Proposal/Introduction.tex
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--- /trunk/MagicSoft/GRB-Proposal/Introduction.tex	(revision 6218)
+++ /trunk/MagicSoft/GRB-Proposal/Introduction.tex	(revision 6219)
@@ -7,13 +7,13 @@
 the objective to turn the telescope to the burst position within 10-30\,sec.
 in order to have a fair chance to detect a burst when the prompt $\gamma$--emission is still ongoing.
-During the commissioning phase it could be proven that our goal was reached.
-The telescope is able to turn 180 degrees in azimuth within 20\,sec. and 80 degrees in zenith within 10\,sec.\\
-
+During the commissioning phase, it could be proven that our goal was reached.
+The telescope is able to turn 180\,deg. in azimuth within 20\,sec. and 90\,deg. in zenith within 10\,sec.\\
 
 Very high energy (VHE) GRB observations have the potential to constrain the current GRB models
-on both the prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM,SALOMON}.
-Models based on both internal and external shocks predicts VHE fluence comparable to,
+on both the prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM}.
+Models based on both internal and external shocks predict VHE gamma-ray fluences comparable to,
 or in certain situations stronger than, the keV-MeV radiation,
-with duration ranging from shorter than the keV-MeV burst to extended TeV afterglows~\cite{DERMER, PILLA, ZHANG1, RAZZAQUE}.
+with durations ranging from shorter than the keV-MeV burst to extended TeV 
+afterglows~\cite{DERMER, PILLA, ZHANG1, RAZZAQUE}.
 
 \par
@@ -72,2 +72,7 @@
 
 
+
+%%% Local Variables: 
+%%% mode: latex
+%%% TeX-master: "GRB_proposal_2005"
+%%% End: 
Index: /trunk/MagicSoft/GRB-Proposal/Strategies.tex
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--- /trunk/MagicSoft/GRB-Proposal/Strategies.tex	(revision 6218)
+++ /trunk/MagicSoft/GRB-Proposal/Strategies.tex	(revision 6219)
@@ -73,5 +73,5 @@
 
 We determine the maximum zenith angle for GRB observations by requiring that the overwhelming majority of possible GRBs will have an in principle observable spectrum. Figure~\ref{fig:grh}
-shows the gamma-ray horizon (GRH) as computed in~\cite{KNEISKE}. The GRH is defined as the
+shows the gamma-ray horizon (GRH) as computed in~\cite{KNEISKE,SALOMON}. The GRH is defined as the
 gamma-ray energy at which a part of $1/e$ of a hypothesied mono-energetic flux gets absorbed after
 travelling a distance of $d$, expressed in redshift $z$ from the earth. One can see that at typical
@@ -113,2 +113,7 @@
 \item In the other case for having off-data at exactly the same sky location.
 \end{itemize}
+
+%%% Local Variables: 
+%%% mode: latex
+%%% TeX-master: "GRB_proposal_2005"
+%%% End: