source: trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex@ 6796

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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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\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>}\\
  D. Bastieri\\ \texttt{<denis.bastieri@pd.infn.it>}\\
  M. Garczarczyk\\ \texttt{<garcz@mppmu.mpg.de>}\\
  M. Gaug\\ \texttt{<markus@ifae.es>}\\
  S. Mizobuchi\\ \texttt{<satoko@mppmu.mpg.de>}\\
}

\date{March, 2005\\}
\TDAScode{MAGIC-TDAS 05-02\\ 050314/NGalante}
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\begin{abstract}
We present a detailed strategy for the observation of Gamma Ray Bursts (GRBs) for the first
half year of 2005. Because of similarities, X-Ray Flashes (XRFs) and Soft Gamma Repeaters (SGR)
are also included in our proposal.
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 --
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
with the one of \ma, we cannot predict the alert frequency now to better than 100\% uncertainty.
This leads to an {\bf 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{Introduction}
\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
\begin{thebibliography}{900}

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using the TIBET Air Shower Array, Amenomori M., et al., A\&A, 311, 919, 1996.
\bibitem{CONNAUGHTON1} A Search for TeV Counterparts to BATSE GRBs,
Connaughton at al., ApJ, 479, 859, 1997.
\bibitem{PADILLA} Search for Gamma-Ray Bursts above 20~TeV with the HEGRA AIROBICC Cherenkov Array,
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\bibitem{CONNAUGHTON2} A Search for TeV GRBs on a 1-second time-scale,
Connaughton at al., Astroparticle Physics, vol. 8, no. 3, 179, 1998.
\bibitem{MILAGRO} The high-energy gamma-ray fluence and energy spectrum of GRB 970417A
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\bibitem{GCN3002} GCN GRB OBSERVATION REPORT, 3002, 2005

%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/
\bibitem{SWIFT} The SWIFT homepage: http://swift.gsfc.nasa.gov/docs/swift/
\bibitem{CONTROL} MAGIC-TDAS 00-07, Cortina J, 2004.

%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.


%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{XU} Pazcy\'{n}ski B., Xu G., Astrophys. J. 427 708 (1994)

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

\end{thebibliography}

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