source: trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex@ 6903

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%%%  Kopyleft (K) 2000 J C Gonzalez
%%%  Max-Planck-Institut fuer Physik,
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%%%  E-mail: gonzalez@mppmu.mpg.de
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\newcommand{\sw}{SWIFT\xspace}
\newcommand{\eg}{EGRET\xspace}
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\newcommand{\ma}{MAGIC\xspace}
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\title{Proposal for the Observation of Gamma-Ray Bursts with the MAGIC Telescope}
%       {\it \Large DRAFT 2.1 }}
\author{\begin{minipage} [c]{0.8\linewidth}
\begin{tabular}{l l l}
PI: & Nicola Galante & Universit{\`a} degli Studi di Siena \\
Co-I: & Denis Bastieri & Universit{\`a} degli Studi di Padova\\
      & Markus Gaug & IFAE Barcelona \\
      & Markus Garczarczyk & MPI Munich \\
      & Satoko Mizobuchi & MPI Munich \\
      & Riccardo Paoletti & Universit{\`a} degli Studi di Siena\\
      & Luigi Peruzzo  & Universit{\`a} degli Studi di Padova\\
Co-DA: & Martina Fagiolini & Universit{\`a} degli Studi di Siena\\
       & Tiziano Lenisa    & Universit{\`a} degli Studi di Udine \\
       & Abelardo Moralejo & Universit{\`a} degli Studi di Padova\\
       & Francesco Longo   & INFN Trieste \\
       & Alessio Piccioli  & Universit{\`a} degli Studi di Siena\\
Co-Th: & Steve Shore & Universit{\`a} degli Studi di Pisa \\
\end{tabular}
\end{minipage}
}

\date{March, 2005\\}
\TDAScode{MAGIC-TDAS 05-03\\ 050321/NGalante}
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\begin{abstract}
We ask for observations of Gamma-Ray Bursts (GRBs) for the next six months of the year 2005.
We present a detailed strategy for the observation of GRBs, X-Ray Flashes (XRFs) and 
Soft Gamma Repeaters (SGR)
(which are included in our proposal, given their similarities to GRB phenomena).
The observations will be mainly triggered by \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 month --
although with big uncertainties -- out of which 1--2 should be
observable by \ma 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, 
we cannot predict the alert frequency now to better than 100\%
uncertainty.  
This leads to an expected observation time 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 few dedicated nights to test the automatic alert procedure
with the subsystem experts. We suggest to review the situation in half a year from now.
\end{abstract}

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\include{ScientificCase}
\include{Alerts}
\include{Monitor}
\include{Strategies}
\include{Timing}
\include{Requirements}
\include{Tests}
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%%% BIBLIOGRAPHY %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

%%>>>> Use the following if you are using BibTeX for bibliography
%\theBibliography

%%>>>> Or the following if you include here by hand your
%%>>>> bibliographic entries
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%References used in chapter 2: Burst Alert System

\bibitem{GCN} The GCN homepage: http://gcn.gsfc.nasa.gov/
\bibitem{HETE} The HETE homepage: http://space.mit.edu/HETE/
\bibitem{INTEGRAL} The INTEGRAL homepage: http://astro.estec.esa.nl/Integral/isoc/
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%References used in Strategies

\bibitem{KNEISKE} Kneiske T.M., Bretz T., Mannheim K., Hartmann D.H., A\&A 413, 807, 2004.
\bibitem{SALOMON} Absorption of HE Gamma Rays by Interactions with Extragalactic Starlight Photons at High Redshifts and the HE Gamma-Ray Background, Salomon M.H., Stecker F.J., ApJ, 493, 547, 1998.
\bibitem{GRB030329} Spectra of the burst: http://space.mit.edu/HETE/Bursts/GRB030329/
\bibitem{ecl} Private communication with Lorenz E.
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%References used in Timing
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Formed by the Interaction with CMB Photons, Wang, at al., ApJ, 604, 306, 2004.

%Not used references

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%\bibitem{MESZAROS94} Meszaros P., Rees M., MNRAS 289 L41 (1994)

\end{thebibliography}

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