Index: trunk/MagicSoft/GC-Proposal/GC.tex
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--- trunk/MagicSoft/GC-Proposal/GC.tex	(revision 6758)
+++ trunk/MagicSoft/GC-Proposal/GC.tex	(revision 6759)
@@ -106,5 +106,5 @@
 
 
-In fact, EGRET has detected a strong source in direction of the GC, 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 bread at a few GeV. If in the GC, the gamma ray luminosity of this source is very large $~2 \cdot 10^{37} \mathrm{erg}/\mathrm{s}$, which is equivalent to about 10 Crab pulsars. Up to now, the GC has been observed at energies above 200 GeV by Veritas, Cangaroo and HESS, \cite{GC_whipple,GC_cangaroo,GC_hess}. Figure \ref{fig:GC_gamma_flux} shows the reconstructed spectra by the other IACTs while figure \ref{fig:GC_source_location} shows the different reconstructed positions of the GC source. Recently a second TeV gamma source only about 1 degree away from the Galactic Center has been discovered \cite{SNR_G09+01}. Its integral flux above 200 GeV represents about 2\% of the gamma flux from the Crab nebula.
+In fact, EGRET has detected a strong source in direction of the GC, 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 bread at a few GeV. If in the GC, the gamma ray luminosity of this source is very large $~2 \cdot 10^{37} \mathrm{erg}/\mathrm{s}$, which is equivalent to about 10 Crab pulsars. Up to now, the GC has been observed at energies above 200 GeV by Veritas, Cangaroo and HESS, \cite{GC_whipple,GC_cangaroo,GC_hess}. Figure \ref{fig:GC_gamma_flux} shows the reconstructed spectra by the other IACTs while figure \ref{fig:GC_source_location} shows the different reconstructed positions of the GC source. Recently a second TeV gamma source only about 1 degree away from the Galactic Center has been discovered \cite{SNR_G09+01}. Its integral flux above 200 GeV represents about 2\% of the gamma flux from the Crab nebula with a photon-index of about 2.4.
 
 \begin{figure}[h!]
@@ -154,5 +154,5 @@
 
 
-High energy gamma rays can be produced in the GC in the non-thermal radio filaments by high-energy leptons which scatter background infrared photons from the nearby ionized clouds \cite{Pohl1997,Aharonian2005}, or by hadrons colliding with dense matter. These high energy hadrons can be accelerated by the massive black hole \cite{GC_black_hole}, associated with the Sgr A$^*$, supernovae or an energetic pulsar. Alternative mechanisms invoke the hypothetical annihilation of super-symmetric dark matter particles (for a review see \cite{jung96}) or curvature radiation of protons in the vicinity of the central super-massive black hole \cite{GC_black_hole}.
+High energy gamma rays can be produced in the GC in the non-thermal radio filaments by high-energy leptons which scatter background infrared photons from the nearby ionized clouds \cite{Pohl1997,Aharonian2005}, or by hadrons colliding with dense matter. These high energy hadrons can be accelerated by the massive black hole \cite{GC_black_hole}, associated with the Sgr A$^*$, supernovae or an energetic pulsar. Alternative mechanisms invoke the hypothetical annihilation of super-symmetric dark matter particles (for a review see \cite{jung96}) or curvature radiation of protons in the vicinity of the central super-massive black hole \cite{GC_black_hole,Melia2001}.
 
 
@@ -370,5 +370,5 @@
 \section{Acknowledgements}
 
-The authors thank ...  is acknowledged. 
+The authors thank A. Moralejo for helpfull discussions about the Monte Carlo simulations. 
 
 
Index: trunk/MagicSoft/GC-Proposal/bibbib.bib
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--- trunk/MagicSoft/GC-Proposal/bibbib.bib	(revision 6758)
+++ trunk/MagicSoft/GC-Proposal/bibbib.bib	(revision 6759)
@@ -1,2 +1,13 @@
+@ARTICLE{Melia2001,
+   author = {{Melia}, F. and {Falcke}, H.},
+    title = "{The Supermassive Black Hole at the Galactic Center}",
+  journal = "Ann. Rev. Astr. Astroph.",
+     year = 2001,
+   volume = 39,
+    pages = {309-352},
+   adsurl = {http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2001ARA%26A..39..309M&db_key=AST},
+  adsnote = {Provided by the NASA Astrophysics Data System}
+}
+
 @ARTICLE{Hayashida1999,
    author = {{Hayashida}, N. and {Nagano}, M. and {Nishikawa}, D. and {Ohoka}, H. and