Changeset 815 for trunk/ICRC_01/mccontrib.tex
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trunk/ICRC_01/mccontrib.tex
r814 r815 44 44 will be finished. The aim of this 45 45 detector is the observation of $\gamma$-ray sources in the 46 ener y region above $\approx 10~\mathrm{TeV}$.47 The size of the telesope mirro s will be around $250~\mathrm{m^2}$.46 energy region above $\approx 10~\mathrm{GeV}$. 47 The size of the telesope mirrors will be around $250~\mathrm{m^2}$. 48 48 The air showers induced by cosmic ray particles (hadrons and gammas) 49 49 will be detected with a "classical" camera consisting of 577 … … 51 51 be recorded by a FADC system running with a frequency of 52 52 $f = 333~\mathrm{MHz}$. 53 The readout of the FADCs by a dedicated trigger system containing 53 The readout of the FADCs will be started 54 by a dedicated trigger system containing 54 55 different trigger levels. 55 56 56 57 The goal of the trigger system is to reject the hadronic cosmic ray 57 background from the gamma rays, for which a lower threshold is aimed. 58 background from the gamma rays, for which the lowest threshold 59 is aimed. 58 60 For a better understanding of the MAGIC telescope and its different 59 61 systems (trigger, FADC) a detailed Monte Carlo (MC) study is 60 unavoidable. Such an study has to take into account the simulation62 neccessary. Such an study has to take into account the simulation 61 63 of air showers, the effect of absorption in the atmosphere, the 62 64 behaviour of the PMTs and the response of the trigger and FADC 63 system. 65 system. 66 64 67 For a big telescope like MAGIC there is an additional source of 65 68 noise, which is the light of the night sky. As a rude assumption 66 69 there will be around 50 stars with magnitude $m \le 9$ in the 67 field of view of the camera. So one other game of this 68 study is to invent methods to become rid of the light from 69 stars. 70 field of view of the camera. 71 Investigations are neccessary to invent methods which allows to 72 reduce the effect of the light from stars. The methods can be 73 tested before the MAGIC telescope exists by using monte carlo 74 data. 75 70 76 71 77 Here we present the first results of such an investigation. … … 81 87 Then the behaviour of the PMTs is simulated and the 82 88 response of the trigger and FADC system is generated. 83 In the followin subsections you find a more precise89 In the following subsections you find a more precise 84 90 description of all the programs. 85 91 … … 95 101 Gammas where simulated like a point source 96 102 whereas the hadrons are simulated isotropic around 97 the given zenith angle. We found that hadronic showers 98 have also for big impact parameters $I$ a non-zero 99 probability to trigger the telescope. Therefore we 103 the given zenith angle. 104 The trigger probality for hadronic showers with 105 a big impact parameter $I$ is not negliable. 106 Therefore we 100 107 simulate hadrons with $I < 400~\mathrm{m}$ and gammas 101 108 with $I < 200~\mathrm{m}$. … … 130 137 close to the telescope position are stored. 131 138 132 \subsection{ mirror simulation}139 \subsection{atmospheric and mirror simulation} 133 140 134 141 The output of the air shower simualition is used 135 as the input to the mirror simulation. But before 136 simulating the mirror themself, one has to take the 137 absorption in the atmosphere into account. For each 138 Cherenkov photon the height of production and 139 the wavelength is known. Taking the Rayleigh and 140 Mie scattering into account one is able to calculate 141 the effect of absorption in the atmosphere. 142 The next step in the simulation is the reflection of 143 the Cherenkov photons on the mirrors. Therefore one 144 has to define in that step the pointing of the 145 telescope. Each photon hitting one of the mirrors will 146 be tracked to the camera plane. Here we take an 147 reflectivity of around 90\% into account. 142 as the input to the mirror simulation. 143 First the absorption in the atmosphere is taken into 144 account. 145 By knowing the height of production and the 146 wavelength of each Cherenkov photen it is possible 147 to calculate the effect of Rayleigh and Mie scattering. 148 The second step is the simulation of the mirror dish. 149 We assume a reflectivity of the mirrors of around 90\%. 150 Each Cherenkov photon hitting one mirror is tracked back 151 to the camera plane of the telescope. This procedure 152 depends on the orientation of the telescope to the 153 shower axis. 148 154 All Cherenkov photons reaching the camera plane will be 149 stored.155 keeped for the next simulation program. 150 156 151 157 \subsection{camera simulation} … … 177 183 a given width. 178 184 The amplitude of the response function is randomized 179 by using the function of figure \ref{fig_ampl}.180 By superimpos e all photons of one pixel anby taking181 the arrival time into account we getthe response182 of the trigger and FADC system for that pixel (see183 also figure \ref{fig_starresp}).185 by using the distribution of figure \ref{fig_ampl}. 186 By superimposing all photons of one pixel and by taking 187 the arrival time into account the response 188 of the trigger and FADC system for that pixel is generated 189 (see also figure \ref{fig_starresp}). 184 190 This is done for all pixels in the camera. 185 191 186 192 Then the simulation of the trigger electronic is applied. 187 193 We look in the generated analog signal if the discriminator 188 threshold is achieved. If yes we will create a digital output 189 signal for that pixels. Then we decided if a first level trigger 190 occurs by looking for next neighbour (NN)conditions at a given 191 time. If a given NN condition (Multiplicity, Topology, ...) 192 is fullfilled, a first level trigger is generated and the 193 content of the FADC system is written to disk. An triggered 194 event is generated. 194 threshold is achieved. In that case a digital output 195 signal of a given length (We use in that study a gate length of 6 196 nsec.) 197 for that pixels. 198 By checking next neighbour conditions (NN) at a given time 199 the first level trigger is simulated. 200 If a given NN condition (Multiplicity, Topology, ...) 201 is fullfilled, a first level trigger signal is generated and 202 the 203 content of the FADC system is written to disk. 195 204 % 196 205 % … … 212 221 the position of an expected gamma ray source is contributing to 213 222 the noise in the camera. We developed a program that allows us 214 to simulate the star light together with the generated shower .223 to simulate the star light together with the generated showers. 215 224 This program takes all stars in the field of view of the camera 216 225 around chosen sky region. The light of these stars is track up to … … 219 228 get the number of emitted photo electrons per pixel and 220 229 time. 230 221 231 These number is used to generate a noise signal for all the pixels. 232 % 233 % 234 % 235 \begin{figure}[h] 236 \vspace*{2.0mm} % just in case for shifting the figure slightly down 237 \includegraphics[width=8.3cm]{signal.eps} % .eps for Latex, 238 % pdfLatex allows .pdf, .jpg, .png and .tif 239 \caption{The response of a pixel due to a star with magnitude 240 $m=7$ in the field of view. On the left plot the response of the 241 trigger system is plotted while on the right plot the content in the 242 FADC system is shown.} 243 \label{fig_starresp} 244 \end{figure} 245 % 246 % 247 % 222 248 In figure \ref{fig_starresp} the response of the trigger and the 223 249 FADC system can be seen for one pixel with a star of … … 225 251 These stars are typical, because there will 226 252 be always one $7^m$ star in the trigger area of the camera. 227 % 228 % 229 % 230 \begin{figure}[h] 231 \vspace*{2.0mm} % just in case for shifting the figure slightly down 232 \includegraphics[width=8.3cm]{signal.eps} % .eps for Latex, 233 % pdfLatex allows .pdf, .jpg, .png and .tif 234 \caption{The response of a pixel due to a star with magnitude 235 $m=7$ in the field of view. On the left plot the response of the 236 trigger system is plotted while on the right plot the content in the 237 FADC system is shown.} 238 \label{fig_starresp} 239 \end{figure} 240 % 241 % 242 % 253 243 254 244 255 \section{Results} … … 277 288 where T is the trigger probablity. F is perpendicular to 278 289 the shower axis. The results for different zenith angle $\Theta$ and 279 for different trigger settings are shown in figure290 for different discriminator thresholds are shown in figure 280 291 \ref{fig_collarea}. 281 292 % … … 294 305 % 295 306 As bigger the zenith angle the smaller becomes the collection area 296 for lower energies. 307 for lower energies. As bigger the discriminator threshold is set, as 308 lower is the trigger collection area for low energies. 297 309 298 310
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