Index: /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex
===================================================================
--- /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex	(revision 6160)
+++ /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex	(revision 6161)
@@ -166,4 +166,5 @@
 
 \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/
 
 %Not used references
Index: /trunk/MagicSoft/GRB-Proposal/Strategies.tex
===================================================================
--- /trunk/MagicSoft/GRB-Proposal/Strategies.tex	(revision 6160)
+++ /trunk/MagicSoft/GRB-Proposal/Strategies.tex	(revision 6161)
@@ -70,9 +70,11 @@
 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
-gamma-ray energy at which a part of $1/e$ of a hypothiszed mono-energetic flux gets absorbed after
+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
-GRB distances of $z=1$, all gamma-rays above 100\,GeV get absorbed before they reach the earth. 
+GRB distances of $z=1$, all gamma-rays above 100\,GeV get absorbed before they reach the earth.
+
 \par
-Even the closest GRB with known redshift ever observed, GRB030329~\cite{GRB030329}, lies at a redshift 
+
+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.