Index: /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex
===================================================================
--- /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex	(revision 6183)
+++ /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex	(revision 6184)
@@ -54,7 +54,7 @@
 %% elements: title, author, date, plus TDAScode
 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
-\title{Proposal for the Observation of Gamma-Ray Bursts with the MAGIC Telescope \\
-       {\it \Large DRAFT 2.1 }}
-\author{  N. Galante\\ \texttt{<nicola.galante@pi.infn.it>}\\
+\title{Proposal for the Observation of Gamma-Ray Bursts with the MAGIC Telescope} 
+%       {\it \Large DRAFT 2.1 }}
+\author{N. Galante\\ \texttt{<nicola.galante@pi.infn.it>}\\
   M. Garczarczyk\\ \texttt{<garcz@mppmu.mpg.de>}\\
   M. Gaug\\ \texttt{<markus@ifae.es>} \\
@@ -63,5 +63,5 @@
 
 \date{January, 2005\\}
-\TDAScode{MAGIC-TDAS 05-??\\ 0312??/NGalante}
+\TDAScode{MAGIC-TDAS 05-02\\ 050201/NGalante}
 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
 %% title %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
Index: /trunk/MagicSoft/GRB-Proposal/Introduction.tex
===================================================================
--- /trunk/MagicSoft/GRB-Proposal/Introduction.tex	(revision 6183)
+++ /trunk/MagicSoft/GRB-Proposal/Introduction.tex	(revision 6184)
@@ -22,7 +22,7 @@
 (low-energy) GRB, have been explored. Proton-synchrotron emission~\cite{TOTANI} have been suggested
 as well as photon-pion production~\cite{WAXMAN,BAHCALL,BOETTCHER} and inverse-Compton scattering
-in the burst environment~\cite{MESZAROS93,CHIANG,PILLA,ZHANG2}.
+in the burst environment~\cite{MESZAROS93,CHIANG,PILLA,ZHANG2,BELOBORODOV}.
 Long-term HE $\gamma$ emission from accelerated protons in the forward-shock has been predicted in~\cite{LI}. This model predicts GeV inverse Compton emission even one day after the burst.
-Even considering pure electron-synchrotron radiation predicts measurable GeV emission for a significant fraction of GRBs~\cite{ZHANG2}. In order to be able to describe prompt synchrotron optical flashes (like observed in GRB990123 by ROTSE), GeV--TeV emission by inverse Compton scattering of the MeV photons should be produced at the same time~\cite{BELOBORODOV}.\\
+Even considering pure electron-synchrotron radiation, measurable GeV emission for a significant fraction of GRBs is predicted~\cite{ZHANG2}.\\
 
 GeV emission in GRBs is particularly sensitive to the Lorentz factor and the photon density of the emitting material -
@@ -40,7 +40,6 @@
 Whipple Air Cherenkov Telescope~\cite{CONNAUGHTON1}, and coincident and monitoring studies by HEGRA-AIROBICC~\cite{PADILLA}, Whipple~\cite{CONNAUGHTON2} and the Milagro prototype Milagrito~\cite{MILAGRO}. The GRAND array has reported some excess of observed muons during seven BATSE bursts~\cite{GRAND}. In this context, especially the publication from the TASC detector on \eg is important~\cite{GONZALES}, finding a HE spectral component presumably due to ultra-relativistic acceleration of hadrons and producing a spectral index of $-1$ with no cut-off up to the detector energy limit (200\,MeV).\\
 
-Concerning estimates about the \ma observability of GRBs, a very detailed study of GRB spectra obtained from the
-third and fourth \ba catalogue has been made in~\cite{ICRC,NICOLA}. The spectra were extrapolated to GeV energies 
-with a simple continuation of the observed high-energy power law behaviour and the calculated fluxes compared with \ma sensitivities. Setting conservative cuts on observation times and significances,
+Concerning estimates of \ma GRB observability, a very detailed study of GRB spectra obtained from the
+third and fourth \ba catalogue has been made in~\cite{ICRC,NICOLA}. The spectra were extrapolated to GeV energies with a simple continuation of the observed high-energy power law behaviour and the calculated fluxes compared with \ma sensitivities. Setting conservative cuts on observation times and significances,
 and assuming an energy threshold of 15~GeV, a GRB detection rate of $0.5-2$ per year
 was obtained for an assumed observation delay between 15 and 60 sec. and a \ba trigger rate ($\sim$\,360/year).