| 1 | \section{Criteria for the Optimal Signal Extraction (STILL TO DO!!)}
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| 2 |
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| 3 | The goal for the optimal signal reconstruction algorithm is to compute an unbiased estimate of the strenght and arrival time of the Cherenkov signal with the highest possible resolution for all signal intensities. The algorithm shall be stable with respect to changes in observation conditions and background levels. Also the needed computing time is of concern.
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| 4 |
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| 5 | The reconstructed signal shall be proportional to the total integrated charge in the FADCs due to the PMT pulse from the Cherenkov signal.
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| 6 |
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| 7 | Discussion about the signal to noise for the image cleaning a la Maxim.
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| 8 |
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| 9 |
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| 10 |
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| 11 | \subsection{Resolution and Bias}
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| 12 | \ldots {\textit{The jitter to identical input pulses is measured, for times, amplitudes,
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| 13 | high-gain and low-gain pulses and different signal and background levels }}
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| 14 |
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| 15 | \subsection{Linearity}
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| 16 | \ldots {\textit The Nuria plots ... }
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| 17 |
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| 18 | \subsection{Low Gain Extraction}
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| 19 | \ldots {\textit The stability of the low-gain extraction w.r.t. the high-gain extraction}
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| 20 |
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| 21 |
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| 22 | \subsection{Stability}
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| 23 | \ldots {\textit The stability of an extractor to slightly varying pulse shapes is examined. }
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| 24 |
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| 25 |
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| 26 | \subsection{Treatment of Calibration Pulses}
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| 27 |
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| 28 |
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| 29 |
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| 30 | \subsection{Applicability for Different Sampling Speeds / No Pulse Shaping.}
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| 31 | The current read-out system of the MAGIC telescope \cite{Magic-DAQ} with 300 MSamples/s is relatively slow compared to the fast pulses of about 2 ns FWHM of Cherenkov pulses. To acquire the pulse shape an artificial pulse shaping to about 6.5 ns FWHM is used. Thereby also more LONS is integrated that acts as noise.
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| 32 |
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| 33 | For 2 ns FWHM fast pulses a 2 GSamples/s FADC provides at least 4 sampling points. This permits a reasonable reconstruction of the pulse shape. First prototype tests with fast digitization systems for MAGIC have been successfully conducted \cite{GSamlesFADC}. The signals have been reconstructed within the common MAGIC Mars software framework.
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| 34 |
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| 35 |
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| 36 | \ldots {\textit Some comments by Hendrik ...}
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| 37 |
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| 38 | \subsection{CPU Requirements}
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| 39 | \ldots {\textit The needed CPU time for each extractor}
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| 40 |
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| 41 |
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| 42 |
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| 43 |
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| 44 | \subsection{Pulpo Pulses}
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| 45 | \subsection{Cosmics Data?}
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| 46 | The results of this subsection are based on the following runs taken
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| 47 | on the 21st of September 2004.
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| 48 | \begin{itemize}
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| 49 | \item{Run 39000}: OffCrab11 at 19.1 degrees zenith angle and 106.2
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| 50 | azimuth.
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| 51 | \item{Run 39182}: CrabNebula at 19.0 degrees zenith angle and 106.0 azimuth.
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| 52 | \end{itemize}
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| 53 |
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| 54 |
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| 55 | %%% Local Variables:
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| 56 | %%% mode: latex
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| 57 | %%% TeX-master: "MAGIC_signal_reco"
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| 58 | %%% End:
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