Index: trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex =================================================================== --- trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6570) +++ trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6571) @@ -56,13 +56,13 @@ \title{Proposal for the Observation of Gamma-Ray Bursts with the MAGIC Telescope} % {\it \Large DRAFT 2.1 }} -\author{N. Galante\\ \texttt{}\\ +\author{D. Bastieri\\ \texttt{}\\ + N. Galante\\ \texttt{}\\ M. Garczarczyk\\ \texttt{}\\ M. Gaug\\ \texttt{}\\ S. Mizobuchi\\ \texttt{}\\ - D. Bastieri\\ \texttt{} } \date{February, 2005\\} -\TDAScode{MAGIC-TDAS 05-02\\ 050202/NGalante} +\TDAScode{MAGIC-TDAS 05-02\\ 050202/DBastieri} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %% title %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% @@ -72,11 +72,11 @@ \begin{abstract} We present a detailed strategy for the observation of Gamma Ray Bursts (GRBs) for the first -half year of 2005. -All observations will be mainly triggered by alerts from \sw. +half year of 2005. +All observations will be mainly triggered by alerts from \sw. In addition, the \he and \ig satellites can contribute a small number of alerts. -The \sw collaboration expects a total alert rate of about 15 per months -- +The \sw collaboration expects a total alert rate of about 15 per months -- although with big uncertainties -- out of which 1--2 should be observable due to our -duty cycle. The overlap in sky converages between \sw and \ma seems to be favorable for \ma. -As it is still unknown how many alerts \sw will deliver exactly, and how its sky coverage matches +duty cycle. The overlap in sky converages between \sw and \ma seems to be favorable for \ma. +As it is still unknown how many alerts \sw will deliver exactly, and how its sky coverage matches with the one of \ma, we cannot predict the alert frequency now to better than 100\% uncertainty. @@ -84,6 +84,6 @@ of 5$\pm$5 hours per month. This number includes observation during the moon-time. We give a detailed description of the observation procedures in La Palma and -propose to spend one dedicated night to test the automatic alert procedure -with the subsystem experts. +propose to spend one dedicated night to test the automatic alert procedure +with the subsystem experts. We suggest to review the situation in half a year from now. \end{abstract} Index: trunk/MagicSoft/GRB-Proposal/Monitor.tex =================================================================== --- trunk/MagicSoft/GRB-Proposal/Monitor.tex (revision 6570) +++ trunk/MagicSoft/GRB-Proposal/Monitor.tex (revision 6571) @@ -128,6 +128,6 @@ \begin{tabular}{lllcccl} -19th & December & 2004 & 1:44 am & INTEGRAL satellite & Zd $\sim 60^\circ$ & Time delay 71 sec.\\ -28th & January & 2005 & 5:36 am & HETE-2 satellite & Zd $\sim 65^\circ$ & Time delay 73 min. \\ \\ +19th & December & 2004 & 1:44 am & INTEGRAL & Zd $\sim 60^\circ$ & time delay 71 sec.\\ +28th & January & 2005 & 5:36 am & HETE-2 & Zd $\sim 65^\circ$ & time delay 73 min. \\ \\ \end{tabular} @@ -136,9 +136,6 @@ \subsection{Experience from SWIFT GRBs until now} -According to the \sw home page~\cite{SWIFT}, the satellite has detected 16 GRBs since mid-December last year. -The bursts were detected by chance during the commissioning phase. Since 15th of February the satellite sends -burst allerts to the \g in real time. The current sample contains three bursts -which could have been observed by \ma. The coordinates of the last burst from 15th February were send via an -alert within few seconds. The weather conditions did not allow any observation in this nights.\\ +According to the \sw home page~\cite{SWIFT}, the satellite has detected 16 GRBs since mid-December last year. The bursts were detected by chance during the commissioning phase. Since 15th of February the satellite sends burst allerts to the \g in real time. The current sample contains three bursts which could have been observed by \ma. The coordinates of the last burst from 15th February were send via an +alert within few seconds. Also in this cases the weather conditions did not allow any observation.\\ \begin{tabular}{lllcc} @@ -151,15 +148,15 @@ Figure~\ref{fig:orbit} shows the orbits of the \sw, \he and \ig satellites. -The \sw and \he satellites are situated in a circular orbit with +The \sw and \he satellites are situated in a circular orbit with 20.6$^\circ$ and 2$^\circ$ inclination, respectively. -One revolution of the \sw and \he satellites last about 100\,min. -The \ig satellite has a +One revolution of the \sw and \he satellites last about 100\,min. +The \ig satellite has a highly eccentric orbit with a revolution period of three sidereal days around the Earth. \par -It is difficult to draw strong conclusions from the individual satellites' orbits. -The orientation of the satellites' FOV is influenced by the scheduled targets. -However, \sw is the satellite with the largest inclination and overlaps mostly with the FOV of \ma. +It is difficult to draw strong conclusions from the individual satellites' orbits. +The orientation of the satellites' FoV is influenced by the scheduled targets. +However, \sw is the satellite with the largest inclination and overlaps mostly with the FoV of \ma. This increases the chance to receive {\bf Red Alarms} from this satellite. Index: trunk/MagicSoft/GRB-Proposal/Strategies.tex =================================================================== --- trunk/MagicSoft/GRB-Proposal/Strategies.tex (revision 6570) +++ trunk/MagicSoft/GRB-Proposal/Strategies.tex (revision 6571) @@ -100,14 +100,5 @@ \par -In December 2004, the shift in La Palma observed the Crab-Nebula even during half-moon. -During the observation, the nominal HV could be maintained while the currents were kept below -2\,$\mu$A. This means that only full-moon periods are not suitable for GRB-observations. -We want to stress the fact that observations at moon-time increase the chances to catch GRBs by 80\%. -It is therefore mandatory that the shifters keep the camera in fully operational conditions with -high-voltages switched on from the beginning of a half-moon night until the end. -This includes periods where no other half-moon observations are scheduled. -If no other data can be taken during those periods, the telescope should be pointed -to a Northern direction, close to the zenith. This increases the probability to overlap -with the FOV of \sw. +In December 2004, the shift in La Palma observed the Crab-Nebula even during half-moon. During the observation, the nominal HV could be maintained while the currents were kept below 2\,$\mu$A. This means that only full-moon periods are not suitable for GRB-observations. We want to stress the fact that observations at moon-time increase the chances to catch GRBs by 80\%. It is therefore mandatory that the shifters keep the camera in fully operational conditions with high-voltages switched on from the beginning of a half-moon night until the end. This includes periods where no other half-moon observations are scheduled. If no other data can be taken during those periods, the telescope should be pointed to a Southern direction, close to the Zenith. This increases the probability to overlap with the FoV of \sw. \par Index: trunk/MagicSoft/GRB-Proposal/Timing.tex =================================================================== --- trunk/MagicSoft/GRB-Proposal/Timing.tex (revision 6570) +++ trunk/MagicSoft/GRB-Proposal/Timing.tex (revision 6571) @@ -19,12 +19,10 @@ \item Regarding the fireball model~\cite{REES1,REES2}, -two efficient mechanisms are available for the generation of VHE photons~\cite{DERISHEV}. +two efficient mechanisms are available for the generation of HE photons (from sub-GeV to 100\,TeV)~\cite{DERISHEV}: \begin{enumerate} -\item The prompt emission of $\sim$100\,GeV photons is expected before and during the keV-MeV peak. -This emission should have their highest luminosity together with the main GRB peak. -\item VHE photons generated due to inverse Compton (IC) scattering in relativistic shocks -are strongly absorbed by infrared background radiation and -cannot be observed from cosmological distances. +\item The prompt emission of $\sim$100\,GeV photons is expected before and during the keV-MeV peak. +This emission should have their highest luminosity together with the main GRB peak. +\item VHE photons generated due to inverse Compton (IC) scattering in relativistic shocks. \end{enumerate}