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Timestamp:
02/16/05 19:35:35 (20 years ago)
Author:
gaug
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  • trunk/MagicSoft/TDAS-Extractor/Reconstruction.tex

    r6437 r6552  
    44signal samples varies  from event to event with respect to the position of the signal shape.
    55The time between the trigger decision and the first read-out sample is uniformly distributed in the range
    6 $t_{\text{rel}} \in [0,T_{\mathrm{FADC}}[$, where $T_{\mathrm{FADC}}=3.33$ ns is the digitization period of the MAGIC 300 MHz FADCs.
     6$t_{\text{rel}} \in [0,T_{\mathrm{FADC}}[$, where $T_{\mathrm{FADC}}=3.33$\,ns is the digitization period of the MAGIC 300\,MHz FADCs.
    77It can be determined using the reconstructed arrival time
    88$t_{\mathrm{arrival}}$.%directly by a time to digital converter (TDC) or
    … …  
    5252In figure~\ref{fig:pulpo_shape_high} the high and the low gain pulses are clearly visible. The low gain pulse is attenuated by a factor of about 10 and delayed by about 55\,ns with respect to the high gain pulse.
    5353
    54 Figure~\ref{fig:pulpo_shape_low} shows the averaged normalized (to an area of 1FADC count * $T_{FADC}=3.33$ ns) reconstructed pulse shapes for the ``pulpo''
     54Figure~\ref{fig:pulse_shapes} (left) shows the averaged normalized (to an area of 1FADC count * $T_{FADC}=3.33$ ns) reconstructed pulse shapes for the ``pulpo''
    5555pulses in the high and in the low gain, respectively. The input FWHM of the pulse generator pulses is
    5656about 2\,ns. The FWHM of the average reconstructed high gain pulse shape is about 6.3\,ns, while the FWHM of
    … …  
    6666\begin{center}
    6767\includegraphics[totalheight=7cm]{pulpo_shape_high_low_MC_TDAS.eps}%{pulpo_shape_low.eps}
     68\includegraphics[totalheight=7cm]{shape_green_UV_data_TDAS.eps}%{shape_green_high.eps}
    6869\end{center}
    69 \caption[Reconstructed pulpo low gain shape.]{Average normalized reconstructed high gain and low gain pulse
     70\caption[Reconstructed pulse shapes]{Left: Average normalized reconstructed high gain and low gain pulse
    7071shapes from a pulpo run.
    71 The FWHM of the low gain pulse is about 10 ns. The black line corresponds to the pulse shape implemented into the MC simulations \cite{MC-Camera}.}
    72 \label{fig:pulpo_shape_low}
     72The FWHM of the low gain pulse is about 10 ns.
     73The black line corresponds to the pulse shape implemented into the MC simulations \cite{MC-Camera}.
     74Right: Average reconstructed high gain pulse shape for one green LED calibration run.
     75The FWHM is about 6.5 ns.}
     76\label{fig:pulse_shapes}
    7377\end{figure}
    7478
    75 Figure \ref{fig:shape_green_high} shows the normalized average reconstructed pulse shapes for green and UV calibration LED pulses~\cite{MAGIC-calibration}
     79Figure~\ref{fig:pulse_shapes} (right) shows the normalized average reconstructed pulse shapes for green and UV calibration LED pulses~\cite{MAGIC-calibration}
    7680 as well as the normalized average reconstructed pulse shape for cosmics events. The pulse shape of the UV calibration pulses is quite similar to the
    7781reconstructed pulse shape for cosmics events, both have a FWHM of about 6.3 ns. As air showers due to hadronic cosmic rays trigger the telescope
    … …  
    8185
    8286% The pulses shape has a FWHM of about 6.5 ns and a significant tail.
    83 
    84 
    85 \begin{figure}[h!]
    86 \begin{center}
    87 \includegraphics[totalheight=7cm]{shape_green_UV_data_TDAS.eps}%{shape_green_high.eps}
    88 \end{center}
    89 \caption[Reconstructed green calibration high gain shape.]{Average reconstructed high gain pulse shape for one green LED calibration run.
    90 The FWHM is about 6.5 ns.}
    91 \label{fig:shape_green_high}
    92 \end{figure}
    93 
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    9588
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