Changeset 6162 for trunk/MagicSoft
- Timestamp:
- 01/31/05 20:47:44 (20 years ago)
- Location:
- trunk/MagicSoft/GRB-Proposal
- Files:
-
- 2 edited
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trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex
r6161 r6162 96 96 %------------------------------------------------------------ 97 97 98 \section{Calibrations}99 {\ldots \it \bf Crab data at different axis-offsets to calibrate off-axis sensitivity \ldots \\}100 98 101 99 %%% BIBLIOGRAPHY %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% … … 167 165 \bibitem{KNEISKE} Kneiske T.M., Bretz T., Mannheim K., Hartmann D.H., A\&A 413, 807, 2004. 168 166 \bibitem{GRB030329} Spectra of the burst: http://space.mit.edu/HETE/Bursts/GRB030329/ 167 \bibitem{ecl} Private communication with Lorenz E. 169 168 170 169 %Not used references 171 170 172 \bibitem{PAZCYNSKI} Pazcy\'{n}ski B., Astrophys. J. 308 L43 (1986)173 \bibitem{GOODMAN} Goodman J., Astrophys. J. 308 L47 (1986)174 \bibitem{SARI} Sari R., Piran T., Narayan R., Astrophys. J. 497 L17 (1998)175 \bibitem{XU} Pazcy\'{n}ski B., Xu G., Astrophys. J. 427 708 (1994)176 \bibitem{REES} Rees M., Meszaros P., MNRAS 258 P41 (1992)177 \bibitem{MESZAROS94} Meszaros P., Rees M., MNRAS 289 L41 (1994)171 %\bibitem{PAZCYNSKI} Pazcy\'{n}ski B., Astrophys. J. 308 L43 (1986) 172 %\bibitem{GOODMAN} Goodman J., Astrophys. J. 308 L47 (1986) 173 %\bibitem{SARI} Sari R., Piran T., Narayan R., Astrophys. J. 497 L17 (1998) 174 %\bibitem{XU} Pazcy\'{n}ski B., Xu G., Astrophys. J. 427 708 (1994) 175 %\bibitem{REES} Rees M., Meszaros P., MNRAS 258 P41 (1992) 176 %\bibitem{MESZAROS94} Meszaros P., Rees M., MNRAS 289 L41 (1994) 178 177 179 178 -
trunk/MagicSoft/GRB-Proposal/Strategies.tex
r6161 r6162 55 55 $\theta_{max} = 70^\circ$ to $\theta_{max} = 65^\circ$. 56 56 57 \subsection{Active Mirror Control behaviour} 58 59 To reduce the time before starting of the observation, the use of the look-up tables (LUTs) is necessary. 60 Once generated, the {\it AMC} will use the LUTs and automaticaly focus the panels for a given telescope position. The {\it CC} should send the burst coordinates to the {\it Drive} and the {\it AMC} software in the same time. In this way the panels could be focussed already during the telescope movement. 61 57 62 \subsection{Calibration} 58 63 … … 77 82 78 83 Even the closest GRB with known redshift ever observed, GRB030329~\cite{GRB030329}, lies at a redshift 79 of $z=0.1685$. In this case , gamma-rays above 200\,GeV get entirely absorbed.84 of $z=0.1685$. In this case $\gamma$-rays above 200\,GeV get entirely absorbed. 80 85 81 86 \begin{figure}[htp] 82 87 \centering 83 88 \includegraphics[width=0.85\linewidth]{f4.eps} 84 \caption{Gamma Ray Horizon ,as derived in~\cite{KNEISKE}}89 \caption{Gamma Ray Horizon as derived in~\cite{KNEISKE}} 85 90 \label{fig:grh} 86 91 \end{figure} 87 92 88 93 \par 89 We assume now a current energy threshold of 50\,GeV for MAGIC at a zenith angle of $\theta = 0$\footnote{As 90 this proposal is going to be reviewed in a couple of months, improvements of the energy threshold will be taken 91 into account, then.}. According 92 to~\cite{eckart}, the energy threshold of a Cherenkov telescope scales with zenith angle like: 94 95 We assume now a current energy threshold of 50\,GeV for \ma at a zenith angle of 96 $\theta = 0$\footnote{As this proposal is going to be reviewed in a couple of months, improvements of the energy threshold will be taken into account then.}. According to~\cite{ecl}, the energy threshold of a Cherenkov telescope scales with zenith angle like: 93 97 94 98 \begin{equation} 95 E ^{thr}(\theta) = E^{thr}(0) \cdot \cos(\theta)^{-2.7}99 E_{thr}(\theta) = E_{thr}(0) \cdot \cos(\theta)^{-2.7} 96 100 \label{eq:ethrvszenith} 97 101 \end{equation} 98 102 99 Eq.~\ref{eq:ethrvszenith} leads to an energy threshold of about 5.6\,TeV at $\theta = 80^\circ$, 100 900\,GeV at $\theta = 70^\circ$ and 500\,GeV at $\theta = 65^\circ$. 101 Inserting these results into the GRH (figure~\ref{fig:grh}), one gets 102 a maximal observable GRB distance of $z = 0.1$ at $\theta = 70^\circ$ and $z = 0.2$ at $\theta = 65^\circ$. 103 We think that the probability for 104 GRBs to occur at these distances is sufficiently small in order to neglect the very difficult observations 105 beyond these limits. 103 Eq.~\ref{eq:ethrvszenith} leads to an energy threshold of about 5.6\,TeV at $\theta = 80^\circ$, 104 900\,GeV at $\theta = 70^\circ$ and 500\,GeV at $\theta = 65^\circ$. 105 Inserting these results into the GRH (figure~\ref{fig:grh}), one gets a maximal observable GRB distance of $z = 0.1$ at $\theta = 70^\circ$ and $z = 0.2$ at $\theta = 65^\circ$. 106 We think that the probability for GRBs to occur at these distances is sufficiently small in order to neglect the very difficult observations beyond these limits. 106 107 107 108 \subsection{In case of follow-up: Next steps} 108 109 109 We propose to analyse the GRB data at the following day in order to tell whether a follow-up observation during 110 the next night is useful. We think that a limit of 3\,$\sigma$ significance should be enough to start such a 111 follow-up observation of the same place. This follow-up observation can then be used in two ways: 110 We propose to analyse the GRB data at the following day in order to tell whether a follow-up observation during the next night is useful. We think that a limit of 3\,$\sigma$ significance should be enough to start such a follow-up observation of the same place. This follow-up observation can then be used in two ways: 112 111 113 112 \begin{itemize} 114 113 \item In case of a repeated outbursts for a longer time period of direct observation 115 \item In the other case for having Off-data at exactly the same location.114 \item In the other case for having Off-data at exactly the same sky location. 116 115 \end{itemize}
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