Index: /trunk/MagicSoft/GC-Proposal/GC.tex
===================================================================
--- /trunk/MagicSoft/GC-Proposal/GC.tex	(revision 6764)
+++ /trunk/MagicSoft/GC-Proposal/GC.tex	(revision 6765)
@@ -58,5 +58,5 @@
 like Kaluza-Klein dark matter are not ruled out. Moreover, assuming a 
 universal DM density profile, the GC is expected to yield the largest DM flux 
-amongst the favoured candidates, due to its proximity.
+amongst the favored candidates, due to its proximity.
 
 At La Palma, the GC culminates at about 58 deg zenith angle (ZA). It can be 
@@ -143,5 +143,5 @@
 3 EG J1745-2852 \cite{GC_egret}, which has a broken power law spectrum 
 extending up to at least 10 GeV, with the index 1.3 below the break at a few 
-GeV. Asssuming a distance of 8.5 kpc, the gamma ray luminosity of this source 
+GeV. Assuming a distance of 8.5 kpc, the gamma ray luminosity of this source 
 is very large $~2.2 \cdot 10^{37} \mathrm{erg}/\mathrm{s}$, which is 
 equivalent to about 10 Crab pulsars. An independent analysis of the EGRET data 
@@ -215,5 +215,5 @@
 \end{itemize}
 
-It is quite possible that some of these potentioal gamma-ray production sites contribute comparably to the the observed TeV flux.
+It is quite possible that some of these potential gamma-ray production sites contribute comparably to the the observed TeV flux.
 
 
@@ -235,10 +235,10 @@
 \includegraphics[totalheight=8cm]{total_spectrum.eps}
 \end{center}
-\caption[Total spectrum of the GC.]{Total spectrum of the gamma radiation from the Galactic Centrum, compiled by \cite{Aharonian2005}.} \label{fig:GC_source_location}
+\caption[Total spectrum of the GC.]{Total spectrum of the gamma radiation from the Galactic Center, compiled by \cite{Aharonian2005}.} \label{fig:GC_source_location}
 \end{figure}
 
 
 
-\subsection{Emission from SgrA$^*$}
+\subsection{Emission from Sgr A$^*$}
 
 
@@ -272,5 +272,5 @@
 Using fits of these dark matter profiles to the rotation data of the milky way predictions for the density distribution of the dark matter can be made \cite{Fornego2004,Evans2004}. Assuming parameters for the SUSY models determine the neutralino mass, the thermally averaged annihilation cross section and the gamma yield. Combining both models about the dark matter distribution and SUSY predictions for the gamma flux from SUSY particle dark matter annihilation are derived.
 
-Figure \ref{fig:exclusion_lmits} shows exclusion limits taking the sensitivity of MAGIC from MC simulations into account for different sources and predictions from typical allowed SUSY modells in the plane $N_{\gamma}(E_{\gamma}>E_{\mathrm{thresh}})\langle \sigma v \rangle$ vs $m_{\chi}$. Due to its relative vicinity the Galactic Center yield the largest expected flux from particle dark matter annihilation. Nevertheless this flux is more than one order of magnitude below the current MAGIC sensitivity. Also the observed flux from the HESS experiment way above the theoretical expectation.
+Figure \ref{fig:exclusion_lmits} shows exclusion limits taking the sensitivity of MAGIC from MC simulations into account for different sources and predictions from typical allowed SUSY models in the plane $N_{\gamma}(E_{\gamma}>E_{\mathrm{thresh}})\langle \sigma v \rangle$ vs. $m_{\chi}$. Due to its relative vicinity the Galactic Center yield the largest expected flux from particle dark matter annihilation. Nevertheless this flux is more than one order of magnitude below the current MAGIC sensitivity. Also the observed flux from the HESS experiment way above the theoretical expectation.
 
 
@@ -300,5 +300,5 @@
 \begin{tabular}{l|l|l|l}
  \hline
-   Date       & Time          & Az $[^\circ]$ & Zd $[^\circ]$\\ \hline
+   Date       & Time          & Az $[^\circ]$ & ZA $[^\circ]$\\ \hline
    09/08/2004 & 21:00 - 22:00 & 198.3 - 214.7 & 60.3 - 67.8
 \\ 09/09/2004 & 21:17 - 22:12 & 203.4 - 214.7 & 62.2 - 67.7
@@ -312,5 +312,5 @@
 In our preliminary analysis we used the Random Forest method for the gamma
 hadron separation. For this purpose high
-ZA (65$^\circ$ Zd and 205$^\circ$ Az) Monte Carlo gammas were generated, 
+ZA (65$^\circ$ ZA and 205$^\circ$ Az) Monte Carlo gammas were generated, 
 99500 events in all, with energies between 200
 and 30,000 GeV. The slope of the generated spectrum is $-2.6$, conforming the
@@ -319,5 +319,5 @@
 The MC sample is divided into training
 and test sample. Since there is no dedicated OFF data available, we used a
-subsample of Sgr A$^*$ ON data for the Random Forest training. As trainings
+subsample of Sgr A$^*$ ON data for the Random Forest training. As training
 parameters we used SIZE, DIST, WIDTH, LENGTH, CONC, and M3Long...
 
@@ -443,5 +443,5 @@
 \section{Acknowledgements}
 
-The authors thank A. Moralejo for helpfull discussions about the Monte Carlo simulations. 
+The authors thank A. Moralejo for helpful discussions about the Monte Carlo simulations.