Changeset 6383 for trunk/MagicSoft

Timestamp:

02/11/05 18:30:53 (20 years ago)

Author:

gaug

Message:

*** empty log message ***

File:

• trunk/MagicSoft/TDAS-Extractor/Pedestal.tex (modified) (6 diffs)

trunk/MagicSoft/TDAS-Extractor/Pedestal.tex

@@ -120 +120 @@
 \begin{figure}[htp]
 \centering
-\vspace{\floatsep}
 \includegraphics[width=0.3\linewidth]{MExtractTimeAndChargeSpline_Amplitude_Amplitude_Range_01_09_01_10_Run_38993_RelMean.eps}
 \vspace{\floatsep}
@@ -138 +137 @@
 \begin{figure}[htp]
 \centering
-\vspace{-\floatsep}
 \includegraphics[width=0.3\linewidth]{MExtractTimeAndChargeSpline_Rise-and-Fall-Time_0.5_1.5_Range_01_10_02_12_Run_38993_RelMean.eps}
 \vspace{\floatsep}
@@ -156 +154 @@
 \begin{figure}[htp]
 \centering
-\vspace{-\floatsep}
+\vspace{\floatsep}
 \includegraphics[width=0.3\linewidth]{MExtractTimeAndChargeDigitalFilter_Weights_cosmics_weights.dat_Range_01_14_02_14_Run_38993_RelMean.eps}
 \vspace{\floatsep}
@@ -200 +198 @@
 \end{description}
 
-Figures~\ref{fig:amp:relmean} through~\ref{fig:df:relmean} 
-show the calculated means obtained with this method for all pixels in the camera 
-and for different levels of night-sky background. 
-One can see that the bias vanishes to an accuracy of better than 1\% 
-for the extractors which are used in this TDAS. 
-
-\par
-
-The following plots~\ref{fig:sw:distped} through~\ref{fig:amp:relrms} show results 
+\par
+
+The following figures~\ref{fig:amp:relmean} through~\ref{fig:df:relrms} show results 
 obtained with the second method for three background intensities: 
 
@@ -214 +206 @@
 \item Closed camera and no (Poissonian) fluctuation due to photons from the night sky background
 \item The camera pointing to an extra-galactic region with stars in the field of view
-\item The camera illuminated by a continuous light source of high intensity causing much higher pedestal 
-fluctuations than in usual observation conditions.
+\item The camera illuminated by a continuous light source of intensity 100. 
 \end{enumerate}
 
+Figures~\ref{fig:amp:relmean} through~\ref{fig:df:relmean} 
+show the calculated biases obtained with this method for all pixels in the camera 
+and for the different levels of (night-sky) background. 
+One can see that the bias vanishes to an accuracy of better than 1\% 
+for the extractors which are used in this TDAS. 
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%1
+
+\begin{figure}[htp]
+\centering
+\includegraphics[width=0.47\linewidth]{MExtractTimeAndChargeSpline_Amplitude_Amplitude_Range_01_09_01_10_Run_38993_RMSDiff.eps}
+\vspace{\floatsep}
+\includegraphics[width=0.47\linewidth]{MExtractTimeAndChargeSpline_Amplitude_Amplitude_Range_01_09_01_10_Run_38995_RMSDiff.eps}
+\vspace{\floatsep}
+\includegraphics[width=0.47\linewidth]{MExtractTimeAndChargeSpline_Amplitude_Amplitude_Range_01_09_01_10_Run_38996_RMSDiff.eps}
+\caption{MExtractTimeAndChargeSpline with amplitude:  
+Difference in RMS (per FADC slice) between extraction algorithm
+applied on a fixed window and the corresponding pedestal RMS. 
+Closed camera (left), open camera observing extra-galactic star field (right) and 
+camera being illuminated by the continuous light (bottom). 
+Every entry corresponds to one pixel.}
+\label{fig:amp:relrms}
+\end{figure}
+
+
+\begin{figure}[htp]
+\centering
+\includegraphics[width=0.47\linewidth]{MExtractTimeAndChargeSpline_Rise-and-Fall-Time_0.5_1.5_Range_01_10_02_12_Run_38993_RMSDiff.eps}
+\vspace{\floatsep}
+\includegraphics[width=0.47\linewidth]{MExtractTimeAndChargeSpline_Rise-and-Fall-Time_0.5_1.5_Range_01_10_02_12_Run_38995_RMSDiff.eps}
+\vspace{\floatsep}
+\includegraphics[width=0.47\linewidth]{MExtractTimeAndChargeSpline_Rise-and-Fall-Time_0.5_1.5_Range_01_10_02_12_Run_38996_RMSDiff.eps}
+\caption{MExtractTimeAndChargeSpline with integral over 2 slices:  
+Difference in RMS (per FADC slice) between extraction algorithm
+applied on a fixed window and the corresponding pedestal RMS. 
+Closed camera (left), open camera observing extra-galactic star field (right) and 
+camera being illuminated by the continuous light (bottom). 
+Every entry corresponds to one 
+pixel.}
+\label{fig:amp:relrms}
+\end{figure}
+
+
+\begin{figure}[htp]
+\centering
+\includegraphics[width=0.47\linewidth]{MExtractTimeAndChargeDigitalFilter_Weights_cosmics_weights.dat_Range_01_14_02_14_Run_38993_RMSDiff.eps}
+\vspace{\floatsep}
+\includegraphics[width=0.47\linewidth]{MExtractTimeAndChargeDigitalFilter_Weights_cosmics_weights.dat_Range_01_14_02_14_Run_38995_RMSDiff.eps}
+\vspace{\floatsep}
+\includegraphics[width=0.47\linewidth]{MExtractTimeAndChargeDigitalFilter_Weights_cosmics_weights.dat_Range_01_14_02_14_Run_38996_RMSDiff.eps}
+\caption{MExtractTimeAndChargeDigitalFilter:  
+Difference in RMS (per FADC slice) between extraction algorithm
+applied on a fixed window and the corresponding pedestal RMS. 
+Closed camera (left), open camera observing extra-galactic star field (right) and 
+camera being illuminated by the continuous light (bottom). 
+Every entry corresponds to one pixel.}
+\label{fig:df:relrms}
+\end{figure}
+
+
+
 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+Figures~\ref{fig:amp:relrms} through~\ref{fig:amp:relrms} show the 
+differences in $R$ between the calculated pedestal RMS and 
+the one obtained by applying the extractor, converted to equivalent photo-electrons. One entry 
+corresponds to one pixel of the camera.
+The distributions have a negative mean in the case of the digital filter showing the 
+``filter'' capacity of that algorithm. It ``filters out'' between 0.12 photo-electrons night sky 
+background for the extra-galactic star-field until 0.2 photo-electrons for the continuous light.
+
+%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
+
+
+\subsubsection{ \label{sec:determiner} Application of the Signal Extractor to a Sliding Window
+of Pedestal Events}
+
+By applying the signal extractor to a global extraction window of pedestal events, allowing 
+it to ``slide'' and maximize the encountered signal, we 
+determine the bias $B$ and the mean-squared error $MSE$ for the case of no signal ($S=0$). 
+\par
+In MARS, this functionality is implemented with a function-call to: \\ 
+
+{\textit{\bf MJPedestal::SetExtractionWithExtractor()}} \\
+
+\par
+
+Figures~\ref{fig:amp:distped} through~\ref{fig:df:distped} show the 
+extracted pedestal distributions for the digital filter with cosmics weights (extractor~\#28) and the 
+spline amplitude (extractor~\#27), respectively for one examplary channel (corresponding to pixel 200). 
+One can see the (asymmetric) Poisson behaviour of the 
+night sky background photons for the distributions with open camera and the cutoff at the lower egde 
+for the distribution with high-intensity continuous light due to a limited pedestal offset and the cutoff 
+to negative fluctuations.
+\par
 
 \begin{figure}[htp]
@@ -286 +371 @@
 \end{figure}
 
-
-%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
-
-
-%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%1
-
-\begin{figure}[htp]
-\centering
-\includegraphics[height=0.3\textheight]{MExtractTimeAndChargeSpline_Amplitude_Amplitude_Range_01_09_01_10_Run_38993_RMSDiff.eps}
-\vspace{\floatsep}
-\includegraphics[height=0.3\textheight]{MExtractTimeAndChargeSpline_Amplitude_Amplitude_Range_01_09_01_10_Run_38995_RMSDiff.eps}
-\vspace{\floatsep}
-\includegraphics[height=0.3\textheight]{MExtractTimeAndChargeSpline_Amplitude_Amplitude_Range_01_09_01_10_Run_38996_RMSDiff.eps}
-\caption{MExtractTimeAndChargeSpline with amplitude:  
-Difference in pedestal RMS (per FADC slice) between extraction algorithm
-applied on a fixed window of 1 FADC slice (``extractor random'') and a simple addition of 
-2 FADC slices (``fundamental''). On the top, a run with closed camera has been taken, in the center
- an opened camera observing an extra-galactic star field and on the bottom, an open camera being 
-illuminated by the continuous light of the calibration (level: 100). Every entry corresponds to one 
-pixel.}
-\label{fig:amp:relrms}
-\end{figure}
-
-
-\begin{figure}[htp]
-\centering
-\includegraphics[height=0.3\textheight]{MExtractTimeAndChargeSpline_Rise-and-Fall-Time_0.5_1.5_Range_01_10_02_12_Run_38993_RMSDiff.eps}
-\vspace{\floatsep}
-\includegraphics[height=0.3\textheight]{MExtractTimeAndChargeSpline_Rise-and-Fall-Time_0.5_1.5_Range_01_10_02_12_Run_38995_RMSDiff.eps}
-\vspace{\floatsep}
-\includegraphics[height=0.3\textheight]{MExtractTimeAndChargeSpline_Rise-and-Fall-Time_0.5_1.5_Range_01_10_02_12_Run_38996_RMSDiff.eps}
-\caption{MExtractTimeAndChargeSpline with integral over 2 slices:  
-Difference in pedestal RMS (per FADC slice) between extraction algorithm
-applied on a fixed window of 2 FADC slices (``extractor random'') and a simple addition of 
-2 FADC slices (``fundamental''). On the top, a run with closed camera has been taken, in the center
- an opened camera observing an extra-galactic star field and on the bottom, an open camera being 
-illuminated by the continuous light of the calibration (level: 100). Every entry corresponds to one 
-pixel.}
-\label{fig:amp:relrms}
-\end{figure}
-
-
-\begin{figure}[htp]
-\centering
-\includegraphics[height=0.3\textheight]{MExtractTimeAndChargeDigitalFilter_Weights_cosmics_weights.dat_Range_01_14_02_14_Run_38993_RMSDiff.eps}
-\vspace{\floatsep}
-\includegraphics[height=0.3\textheight]{MExtractTimeAndChargeDigitalFilter_Weights_cosmics_weights.dat_Range_01_14_02_14_Run_38995_RMSDiff.eps}
-\vspace{\floatsep}
-\includegraphics[height=0.3\textheight]{MExtractTimeAndChargeDigitalFilter_Weights_cosmics_weights.dat_Range_01_14_02_14_Run_38996_RMSDiff.eps}
-\caption{MExtractTimeAndChargeDigitalFilter:  
-Difference in pedestal RMS (per FADC slice) between extraction algorithm
-applied on a fixed window of 6 FADC slices and time-randomized weights (``extractor random'') 
-and a simple addition of 6 FADC slices (``fundamental''). On the top, a run with closed camera 
-has been taken, in the center
- an opened camera observing an extra-galactic star field and on the bottom, an open camera being 
-illuminated by the continuous light of the calibration (level: 100). Every entry corresponds to one 
-pixel.}
-\label{fig:df:relrms}
-\end{figure}
-
-
-%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
-
-Figures~\ref{fig:df:distped},~\ref{fig:amp:distped}
-and~\ref{fig:amp:distped} show the 
-extracted pedestal distributions for the digital filter with cosmics weights (extractor~\#28) and the 
-spline amplitude (extractor~\#27), respectively for one examplary channel (corresponding to pixel 200). 
-One can see the (asymmetric) Poisson behaviour of the 
-night sky background photons for the distributions with open camera and the cutoff at the lower egde 
-for the distribution with high-intensity continuous light due to a limited pedestal offset and the cutoff 
-to negative fluctuations.
-\par
-Figures~\ref{fig:df:relmean}
-and~\ref{fig:amp:relmean} show the 
-relative difference between the calculated pedestal mean and 
-the one obtained by applying the extractor for 
-all channels of the MAGIC camera. One can see that in all cases, the distribution is centered around zero, 
-while its width is never larger than 0.01 which corresponds about to the precision of the extracted mean for 
-the number of used events. (A very similar distribution is obtained by comparing the results 
-of the same pedestal calculator applied to different ranges of FADC slices.)
-\par
-Figures~\ref{fig:df:relrms}
-and~\ref{fig:amp:relrms} show the 
-relative difference between the calculated pedestal RMS, normalized to an equivalent number of slices 
-(2.5 for the digital filter and 1. for the amplitude of the spline) and 
-the one obtained by applying the extractor for all channels of the MAGIC camera. 
-One can see that in all cases, the distribution is not centered around zero, but shows an offset depending 
-on the light intensity. The difference can be 10\% in the case of the digital filter and even 25\% for the 
-spline. This big difference for the spline is partly explained by the fact that the pedestals have to be 
-calculated from an even number of slices to account for the clock-noise. However, the (normalized) pedestal 
-RMS depends critically on the number of summed FADC slices, especially at very low numbers. In general, 
-the higher the number of summed FADC slices, the higher the (to the square root of the number of slices) 
-normalized pedestal RMS.
-
-
-\subsubsection{ \label{sec:determiner} Application of the Signal Extractor to a Sliding Window
-of Pedestal Events}
-
-In this section, we apply the signal extractor to a sliding window of pedestal events. 
-\par
-In MARS, this possibility can be used with a call to 
-{\textit{\bf MJPedestal::SetExtractionWithExtractor()}}. 
-\par
+\par
+
 Because the background is determined by the single photo-electrons from the night-sky background,
 the following possibilities can occur: