Changeset 827 for trunk


Ignore:
Timestamp:
06/01/01 10:36:02 (23 years ago)
Author:
blanch
Message:
Final version!!!
File:
1 edited

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  • trunk/ICRC_01/mccontrib.tex

    r825 r827  
    233233These stars will contribute locally to the noise in the
    234234camera and have to be taken into account.
    235 We developed a program that allows
    236 to simulate the star light together with the generated showers.
     235A program that allows to simulate the star light together
     236with the generated showers has been developed.
    237237This program considers all stars in the field of view of the camera
    238238around a chosen direction. The light of these stars is traced up to
     
    251251                                            % pdfLatex allows .pdf, .jpg, .png and .tif
    252252 \caption{The response of a pixel due to a star with magnitude
    253  $m=7$ in the field of view. On the left plot the response of the
    254  trigger system is plotted while on the right plot the content in the
     253 $m=7$ in the field of view. On the left plot the analog signal that goes into
     254 the trigger system is plotted while on the right plot the content in the
    255255 FADC system is shown.}
    256256 \label{fig_starresp}
     
    300300
    301301 
    302 \subsubsection{Collection area}
    303 
    304 
    305 
    306 The trigger collection area is defined as the integral
     302\subsubsection{Effective trigger collection area}
     303
     304
     305
     306The effective trigger collection area is defined as the integral
    307307\begin{equation}
    308308  A(E,\Theta)  = \int_{F}{ T(E,\Theta,F) dF}
     
    313313for different discriminator thresholds are shown in figure
    314314\ref{fig_collarea}.
    315 At low energies ($ E < 100 ~\mathrm{GeV}$), the collection area
    316 decreases with increasing zenith angle , and it decreases with
     315At low energies ($ E < 100 ~\mathrm{GeV}$), the effective trigger collection
     316area decreases with increasing zenith angle , and it decreases with
    317317%
    318318%
     
    322322 \includegraphics[width=8.3cm]{collarea.eps} % .eps for Latex,
    323323                                            % pdfLatex allows .pdf, .jpg, .png and .tif
    324  \caption{The trigger collection area for gamma showers as a function
     324 \caption{The effective trigger collection area for gamma showers as a function
    325325 of energy $E$.}
    326326 \label{fig_collarea}
     
    334334\subsubsection{Energy threshold}
    335335
    336 The threshold of the MAGIC telesope is defined as the peak
     336The threshold of the MAGIC telescope is defined as the peak
    337337in the $dN/dE$ distribution for triggered showers.
    338338This value is determined
     
    379379Since we are aiming for a low energy threshold,
    380380a low discriminator value is  preferred.
    381 However, for 3 mV the expected rate due to protons increases a
     381However, for 3 mV the expected rate due to protons together with night
     382sky background light increases a
    382383lot (see section ~\ref{sec-rates}), while it is kept
    383384under control at 4 mV.
     
    426427\end{figure}
    427428
    428 The MAGIC telesope will use a disriminator
    429 threshold of about 4 mV. This value corresponds to a threshold of
    430 about 8 photo electrons.
     429Some improvement in the trigger rate reduction is needed to lower the
     430discriminator that the MAGIC telescope will use, below 4 mV. This value
     431corresponds to a threshold of about 8 photo electrons.
    431432
    432433It has to be stressed, that these results are based on
     
    447448this direction are ongoing. Also the development of the
    448449second-level-trigger is in progress. This should allow to lower the
    449 threshold.
     450threshold and achieve the aim of 30 GeV for the energy threshold.
    450451The MAGIC collaboration is presently simulating air showers with
    451452higher zenith angles.
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