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Timestamp:
02/17/05 19:03:00 (20 years ago)
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garcz
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trunk/MagicSoft/GRB-Proposal
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  • trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex

    r6550 r6571  
    5656\title{Proposal for the Observation of Gamma-Ray Bursts with the MAGIC Telescope}
    5757%       {\it \Large DRAFT 2.1 }}
    58 \author{N. Galante\\ \texttt{<nicola.galante@pi.infn.it>}\\
     58\author{D. Bastieri\\ \texttt{<denis.bastieri@pd.infn.it>}\\
     59  N. Galante\\ \texttt{<nicola.galante@pi.infn.it>}\\
    5960  M. Garczarczyk\\ \texttt{<garcz@mppmu.mpg.de>}\\
    6061  M. Gaug\\ \texttt{<markus@ifae.es>}\\
    6162  S. Mizobuchi\\ \texttt{<satoko@mppmu.mpg.de>}\\
    62   D. Bastieri\\ \texttt{<denis.bastieri@pd.infn.it>}
    6363}
    6464
    6565\date{February, 2005\\}
    66 \TDAScode{MAGIC-TDAS 05-02\\ 050202/NGalante}
     66\TDAScode{MAGIC-TDAS 05-02\\ 050202/DBastieri}
    6767%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
    6868%% title %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
    … …  
    7272\begin{abstract}
    7373We present a detailed strategy for the observation of Gamma Ray Bursts (GRBs) for the first
    74 half year of 2005. 
    75 All observations will be mainly triggered by alerts from \sw. 
     74half year of 2005.
     75All observations will be mainly triggered by alerts from \sw.
    7676In addition, the \he and \ig satellites can contribute a small number of alerts.
    77 The \sw collaboration expects a total alert rate of about 15 per months -- 
     77The \sw collaboration expects a total alert rate of about 15 per months --
    7878although with big uncertainties -- out of which 1--2 should be observable due to our
    79 duty cycle. The overlap in sky converages between \sw and \ma seems to be favorable for \ma. 
    80 As it is still unknown how many alerts \sw will deliver exactly, and how its sky coverage matches 
     79duty cycle. The overlap in sky converages between \sw and \ma seems to be favorable for \ma.
     80As it is still unknown how many alerts \sw will deliver exactly, and how its sky coverage matches
    8181with the one of \ma,
    8282we cannot predict the alert frequency now to better than 100\% uncertainty.
    … …  
    8484of 5$\pm$5 hours per month. This number includes observation during the moon-time.
    8585We give a detailed description of the observation procedures in La Palma and
    86 propose to spend one dedicated night to test the automatic alert procedure 
    87 with the subsystem experts. 
     86propose to spend one dedicated night to test the automatic alert procedure
     87with the subsystem experts.
    8888We suggest to review the situation in half a year from now.
    8989\end{abstract}

  • trunk/MagicSoft/GRB-Proposal/Monitor.tex

    r6550 r6571  
    128128
    129129\begin{tabular}{lllcccl}
    130 19th & December & 2004 & 1:44 am & INTEGRAL satellite & Zd $\sim 60^\circ$ & Time delay 71 sec.\\
    131 28th & January & 2005 & 5:36 am & HETE-2 satellite & Zd $\sim 65^\circ$ & Time delay 73 min. \\ \\
     13019th & December & 2004 & 1:44 am & INTEGRAL & Zd $\sim 60^\circ$ & time delay 71 sec.\\
     13128th & January & 2005 & 5:36 am & HETE-2 & Zd $\sim 65^\circ$ & time delay 73 min. \\ \\
    132132\end{tabular}
    133133
    … …  
    136136\subsection{Experience from SWIFT GRBs until now}
    137137
    138 According to the \sw home page~\cite{SWIFT}, the satellite has detected 16 GRBs since mid-December last year.
    139 The bursts were detected by chance during the commissioning phase. Since 15th of February the satellite sends
    140 burst allerts to the \g in real time. The current sample contains three bursts
    141 which could have been observed by \ma. The coordinates of the last burst from 15th February were send via an
    142 alert within few seconds. The weather conditions did not allow any observation in this nights.\\
     138According 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
     139alert within few seconds. Also in this cases the weather conditions did not allow any observation.\\
    143140
    144141\begin{tabular}{lllcc}
    … …  
    151148
    152149Figure~\ref{fig:orbit} shows the orbits of the \sw, \he and \ig satellites.
    153 The \sw and \he satellites are situated in a circular orbit with 
     150The \sw and \he satellites are situated in a circular orbit with
    15415120.6$^\circ$ and 2$^\circ$ inclination, respectively.
    155 One revolution of the \sw and \he satellites last about 100\,min. 
    156 The \ig satellite has a 
     152One revolution of the \sw and \he satellites last about 100\,min.
     153The \ig satellite has a
    157154highly eccentric orbit with a revolution period of three sidereal days around the Earth.
    158155
    159156\par
    160157
    161 It is difficult to draw strong conclusions from the individual satellites' orbits. 
    162 The orientation of the satellites' FOV is influenced by the scheduled targets.
    163 However, \sw is the satellite with the largest inclination and overlaps mostly with the FOV of \ma.
     158It is difficult to draw strong conclusions from the individual satellites' orbits.
     159The orientation of the satellites' FoV is influenced by the scheduled targets.
     160However, \sw is the satellite with the largest inclination and overlaps mostly with the FoV of \ma.
    164161This increases the chance to receive {\bf Red Alarms} from this satellite.
    165162

  • trunk/MagicSoft/GRB-Proposal/Strategies.tex

    r6550 r6571  
    100100\par
    101101
    102 In December 2004, the shift in La Palma observed the Crab-Nebula even during half-moon.
    103 During the observation, the nominal HV could be maintained while the currents were kept below
    104 2\,$\mu$A. This means that only full-moon periods are not suitable for GRB-observations.
    105 We want to stress the fact that observations at moon-time increase the chances to catch GRBs by 80\%.
    106 It is therefore mandatory that the shifters keep the camera in fully operational conditions with
    107 high-voltages switched on from the beginning of a half-moon night until the end.
    108 This includes periods where no other half-moon observations are scheduled.
    109 If no other data can be taken during those periods, the telescope should be pointed
    110 to a Northern direction, close to the zenith. This increases the probability to overlap
    111 with the FOV of \sw.
     102In 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.
    112103
    113104\par

  • trunk/MagicSoft/GRB-Proposal/Timing.tex

    r6550 r6571  
    1919
    2020\item Regarding the fireball model~\cite{REES1,REES2},
    21 two efficient mechanisms are available for the generation of VHE photons~\cite{DERISHEV}.
     21two efficient mechanisms are available for the generation of HE photons (from sub-GeV to 100\,TeV)~\cite{DERISHEV}:
    2222
    2323\begin{enumerate}
    24 \item The prompt emission of $\sim$100\,GeV photons is expected before and during the keV-MeV peak.
    25 This emission should have their highest luminosity together with the main GRB peak.
    26 \item VHE photons generated due to inverse Compton (IC) scattering in relativistic shocks
    27 are strongly absorbed by infrared background radiation and
    28 cannot be observed from cosmological distances.
     24\item The prompt emission of $\sim$100\,GeV photons is expected before and during the keV-MeV peak.
     25This emission should have their highest luminosity together with the main GRB peak.
     26\item VHE photons generated due to inverse Compton (IC) scattering in relativistic shocks.
    2927\end{enumerate}
    3028
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