Changeset 827 for trunk/ICRC_01/mccontrib.tex

Timestamp:

06/01/01 10:36:02 (23 years ago)

Author:

blanch

Message:

Final version!!!

File:

• trunk/ICRC_01/mccontrib.tex (modified) (9 diffs)

trunk/ICRC_01/mccontrib.tex

@@ -233 +233 @@
 These stars will contribute locally to the noise in the 
 camera and have to be taken into account. 
-We developed a program that allows
-to simulate the star light together with the generated showers. 
+A program that allows to simulate the star light together 
+with the generated showers has been developed. 
 This program considers all stars in the field of view of the camera
 around a chosen direction. The light of these stars is traced up to 
@@ -251 +251 @@
                                             % pdfLatex allows .pdf, .jpg, .png and .tif
  \caption{The response of a pixel due to a star with magnitude
- $m=7$ in the field of view. On the left plot the response of the
- trigger system is plotted while on the right plot the content in the
+ $m=7$ in the field of view. On the left plot the analog signal that goes into
+ the trigger system is plotted while on the right plot the content in the
  FADC system is shown.}
  \label{fig_starresp}
@@ -300 +300 @@
 
  
-\subsubsection{Collection area}
-
-
-
-The trigger collection area is defined as the integral 
+\subsubsection{Effective trigger collection area}
+
+
+
+The effective trigger collection area is defined as the integral 
 \begin{equation} 
   A(E,\Theta)  = \int_{F}{ T(E,\Theta,F) dF}
@@ -313 +313 @@
 for different discriminator thresholds are shown in figure
 \ref{fig_collarea}.
-At low energies ($ E < 100 ~\mathrm{GeV}$), the collection area
-decreases with increasing zenith angle , and it decreases with 
+At low energies ($ E < 100 ~\mathrm{GeV}$), the effective trigger collection 
+area decreases with increasing zenith angle , and it decreases with 
 %
 %
@@ -322 +322 @@
  \includegraphics[width=8.3cm]{collarea.eps} % .eps for Latex,
                                             % pdfLatex allows .pdf, .jpg, .png and .tif
- \caption{The trigger collection area for gamma showers as a function
+ \caption{The effective trigger collection area for gamma showers as a function
  of energy $E$.}
  \label{fig_collarea}
@@ -334 +334 @@
 \subsubsection{Energy threshold}
 
-The threshold of the MAGIC telesope is defined as the peak 
+The threshold of the MAGIC telescope is defined as the peak 
 in the $dN/dE$ distribution for triggered showers. 
 This value is determined 
@@ -379 +379 @@
 Since we are aiming for a low energy threshold, 
 a low discriminator value is  preferred. 
-However, for 3 mV the expected rate due to protons increases a 
+However, for 3 mV the expected rate due to protons together with night 
+sky background light increases a 
 lot (see section ~\ref{sec-rates}), while it is kept
 under control at 4 mV. 
@@ -426 +427 @@
 \end{figure}
 
-The MAGIC telesope will use a disriminator
-threshold of about 4 mV. This value corresponds to a threshold of
-about 8 photo electrons. 
+Some improvement in the trigger rate reduction is needed to lower the 
+discriminator that the MAGIC telescope will use, below 4 mV. This value 
+corresponds to a threshold of about 8 photo electrons. 
 
 It has to be stressed, that these results are based on 
@@ -447 +448 @@
 this direction are ongoing. Also the development of the
 second-level-trigger is in progress. This should allow to lower the
-threshold. 
+threshold and achieve the aim of 30 GeV for the energy threshold. 
 The MAGIC collaboration is presently simulating air showers with 
 higher zenith angles.