Changeset 6112 for trunk

Timestamp:

01/29/05 14:39:52 (20 years ago)

Author:

gaug

Message:

*** empty log message ***

File:

• trunk/MagicSoft/TDAS-Extractor/Reconstruction.tex (modified) (5 diffs)

trunk/MagicSoft/TDAS-Extractor/Reconstruction.tex

@@ -3 +3 @@
 The FADC clock is not synchronized with the trigger. Therefore, the relative position of the recorded 
 signal samples varies  from event to event with respect to the position of the signal shape. 
-The time between the trigger decision and the first read-out sample is uniformly distributed in the range $t_{\text{rel}} \in [0,T_{\mathrm{FADC}}[$, where $T_{\mathrm{FADC}}=3.33$ ns is the digitization period of the MAGIC 300 MHz FADCs. It can be determined using the reconstructed arrival time 
+The time between the trigger decision and the first read-out sample is uniformly distributed in the range 
+$t_{\text{rel}} \in [0,T_{\mathrm{FADC}}[$, where $T_{\mathrm{FADC}}=3.33$ ns is the digitization period of the MAGIC 300 MHz FADCs. 
+It can be determined using the reconstructed arrival time 
 $t_{\mathrm{arrival}}$.%directly by a time to digital converter (TDC) or 
 \par
@@ -39 +41 @@
 delay line of the MAGIC receiver boards. 
 %   while the FWHM of the average reconstructed low gain pulse shape is 
-% Due to the electric delay line for the low gain pules on the receiver board the low gain pulse is widened with respect to the high gain. It has a FWHM of about 10 ns.
+% Due to the electric delay line for the low gain pules on the receiver board the low gain pulse is widened with respect to the high gain. 
+It has a FWHM of about 10 ns.
 
 
@@ -46 +49 @@
 \includegraphics[totalheight=7cm]{pulpo_shape_high_low_TDAS.eps}%{pulpo_shape_high.eps}
 \end{center}
-\caption[Reconstructed high gain shape.]{Average reconstructed high gain pulse shape from a pulpo run. The FWHM is about 6.2 ns.} \label{fig:pulpo_shape_high}
+\caption[Reconstructed high gain shape.]{Average reconstructed high gain pulse shape from a pulpo run. The FWHM is about 6.2 ns.} 
+\label{fig:pulpo_shape_high}
 \end{figure}
 
@@ -53 +57 @@
 \includegraphics[totalheight=7cm]{pulpo_shape_high_low_MC_TDAS.eps}%{pulpo_shape_low.eps}
 \end{center}
-\caption[Reconstructed pulpo low gain shape.]{Average normalized reconstructed high gain and low gain pulse shapes from a pulpo run. The FWHM of the low gain pulse is about 10 ns. The black line corresponds to the pulse shape implemented into the MC simulations.} \label{fig:pulpo_shape_low}
+\caption[Reconstructed pulpo low gain shape.]{Average normalized reconstructed high gain and low gain pulse shapes from a pulpo run. 
+The FWHM of the low gain pulse is about 10 ns. The black line corresponds to the pulse shape implemented into the MC simulations.} 
+\label{fig:pulpo_shape_low}
 \end{figure}
 
-Figure \ref{fig:shape_green_high} shows the normalized average reconstructed pulse shapes for green and UV calibration LED pulses \cite{MAGIC-calibration} 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 reconstructed 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 much more frequently than gamma showers the reconstructed pulse shape of the cosmics events corresponds mainly to hadron induced showers. The pulse shape due to electromagnetic air showers might be slightly different. The pulse shape for green calibration LED pulses is wider and has a pronounced tail.
-
+Figure \ref{fig:shape_green_high} shows the normalized average reconstructed pulse shapes for green and UV calibration LED pulses~\cite{MAGIC-calibration}
+ 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 
+reconstructed 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 
+much more frequently than gamma showers the reconstructed pulse shape of the cosmics events corresponds mainly to hadron induced showers. 
+The pulse shape due to electromagnetic air showers might be slightly different. The pulse shape for green calibration LED pulses is wider 
+and has a pronounced tail.
 
 % The pulses shape has a FWHM of about 6.5 ns and a significant tail.
@@ -66 +76 @@
 \includegraphics[totalheight=7cm]{shape_green_UV_data_TDAS.eps}%{shape_green_high.eps}
 \end{center}
-\caption[Reconstructed green calibration high gain shape.]{Average reconstructed high gain pulse shape for one green LED calibration run. The FWHM is about 6.5 ns.} \label{fig:shape_green_high}
+\caption[Reconstructed green calibration high gain shape.]{Average reconstructed high gain pulse shape for one green LED calibration run. 
+The FWHM is about 6.5 ns.} 
+\label{fig:shape_green_high}
 \end{figure}