Index: /trunk/MagicSoft/GRB-Proposal/Introduction.tex
===================================================================
--- /trunk/MagicSoft/GRB-Proposal/Introduction.tex	(revision 6238)
+++ /trunk/MagicSoft/GRB-Proposal/Introduction.tex	(revision 6239)
@@ -94,5 +94,5 @@
 The fluence was about $10^{-5}$\,erg/cm$^2$ in the range between 15 and 350\,keV. 
 This event was five orders of magnitude smaller than the giant flare from this source on the 
-December 27$^{th}$, 2004~\cite{GCN3002}. MAGIC have a enough sensitivity for observing the event which have a fluence more than 4.0 $\times$ 10 $^{-1}$ erg/cm$^{2} sec$ at SWIFT observable energy range, when power law index of -2.2 and 100 sec. observation time are assumpted. Therefore if a giant flare from SGR occurs as SGR1806-20, MAGIC would be able to detect the $\gamma$-ray emission from these source.
+December 27$^{th}$, 2004~\cite{GCN3002}. MAGIC have a enough sensitivity for observing the event which have a fluence more than 2.5 $\times$ 10 $^{-2}$ erg/cm$^{2} \cdot sec$ at 100keV, when power law index of -2.0 and 100 sec. observation time are assumpted. Therefore if a giant flare from SGR occurs as SGR1806-20, MAGIC would be able to detect the $\gamma$-ray emission from these source.