Changeset 824 for trunk/ICRC_01/mccontrib.tex
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trunk/ICRC_01/mccontrib.tex
r823 r824 17 17 \author[3]{H. Kornmayer} 18 18 \affil[3]{Max-Planck-Institut f\"ur Physik, M\"unchen, Germany} 19 \correspondence{H. Kornmayer (h.kornmayer@web.de)} 19 \author[]{the MAGIC collaboration} 20 21 \correspondence{O.Blanch blanch@ifae.es), H. Kornmayer (h.kornmayer@web.de)} 22 \affil[ ]{ } 23 \affil[ ]{\large (for the MAGIC Collaboration)} 24 25 20 26 21 27 \firstpage{1} … … 55 61 different trigger levels. 56 62 57 The primary goal of the trigger system is the selction of showers ,63 The primary goal of the trigger system is the selction of showers. 58 64 For a better understanding of the MAGIC telescope and its different 59 65 systems (trigger, FADC) a detailed Monte Carlo (MC) study is 60 neccessary. Such a nstudy has to take into account the simulation66 neccessary. Such a study has to take into account the simulation 61 67 of the air showers, the effect of absorption in the atmosphere, the 62 68 behaviour of the PMTs and the response of the trigger and FADC … … 89 95 \subsection{Air shower simulation} 90 96 91 The simulation of gammas and of hadrons is done with 97 The simulation of gamma and of hadron showers in the 98 atmosphere is done with 92 99 the CORSIKA program, version 5.20. 93 For the simulation of had\-ro\-nic 94 showers we use the VENUS model. We simulate showers 100 As the had\-ro\-nic interaction model 101 we use the VENUS model. 102 We simulate showers 95 103 for different zenith angles 96 ($\Theta = 0^\circ, 5^\circ ,10^\circ, 15^\circ,97 20^\circ, 25^\circ $) at fixed azimuth angel$\Phi$.104 ($\Theta = 0^\circ, 5^\circ$, $ 10^\circ, 15^\circ, 105 20^\circ, 25^\circ $) at fixed azimuthal angle $\Phi$. 98 106 Gammas are assumed to originate from point sources 99 in the direction ($\Theta ,\Phi$)107 in the direction ($\Theta$,$\Phi$) 100 108 whereas the hadrons are simulated isotropically 101 around the given ($\Theta,\Phi$) direction. 109 around the given ($\Theta$,$\Phi$) direction in a 110 region of the solid angle corresponding to the FOV 111 of the camera. 102 112 The trigger probability for hadronic showers with 103 a big impact parameter $I$ is not Englischnegligible.113 a large impact parameter $I$ is not negligible. 104 114 Therefore we 105 115 simulate hadrons with $I < 400~\mathrm{m}$ and gammas … … 116 126 zenith angle & gammas & protons \\ 117 127 \hline \hline 118 $\Theta = 0^\circ$ & $\approx 5 \cdot 10^5$ & $\approx 5 \cdot 10^5$ \\119 $\Theta = 5^\circ$ & $\approx 5 \cdot 10^5$ & $\approx 5 \cdot 10^5$ \\120 $\Theta = 10^\circ$ & $\approx 5 \cdot 10^5$ & $\approx 5 \cdot 10^5$ \\128 $\Theta = 0^\circ$ & $\approx 5 \cdot 10^5$ & $\approx 1 \cdot 10^6$ \\ 129 $\Theta = 5^\circ$ & $\approx 5 \cdot 10^5$ & $\approx 1 \cdot 10^6$ \\ 130 $\Theta = 10^\circ$ & $\approx 5 \cdot 10^5$ & $\approx 1 \cdot 10^6$ \\ 121 131 $\Theta = 15^\circ$ & $\approx 2 \cdot 10^6$ & $\approx 5 \cdot 10^6$ \\ 122 132 $\Theta = 20^\circ$ & production & production \\ … … 125 135 \end{tabular} 126 136 \end{center} 127 \caption {Number of generated showers }137 \caption {Number of generated showers.} 128 138 \label{tab_showers} 129 139 \end{table} … … 132 142 % 133 143 For each simulated shower all 134 Cherenkov photons hitting a horizontal plane at observation level 144 Cherenkov photons hitting a horizontal plane at the 145 observation level 135 146 close to the telescope position are stored. 136 147 … … 141 152 First the absorption in the atmosphere is taken into 142 153 account. 143 By knowing the height of production and the144 wavelength of each Cherenkov photon the effect of Rayleigh145 and Mie scattering iscalculated.154 Using the height of production and the 155 wavelength of each Cherenkov photon the effects of Rayleigh 156 and Mie scattering are calculated. 146 157 Next the reflection at the mirrors is simulated. 147 We assume a reflectivity of the mirrors of around 90\%.148 Each Cherenkov photon hitting onemirror is propagated158 We assume a reflectivity of the mirrors of around 85\%. 159 Each Cherenkov photon hitting a mirror is propagated 149 160 to the camera plane of the telescope. This procedure 150 depends on the orientation of the telescope to the151 shower axis.161 depends on the orientation of the telescope relative 162 to the shower axis. 152 163 All Cherenkov photons reaching the camera plane will be 153 164 kept for the next simulation step. … … 181 192 a given width in time. 182 193 The amplitude of the response function is chosen randomly 183 according to the distribution offigure \ref{fig_ampl}194 according to the distribution shown in figure \ref{fig_ampl} 184 195 (\cite{ml97}). 185 196 186 197 By superimposing all photons of one pixel and by taking 187 198 the arrival times into account the response 188 of the trigger and FADC system for that pixel is generated199 of the trigger and FADC system for that pixel is computed 189 200 (see also figure \ref{fig_starresp}). 190 201 This is done for all pixels in the camera. … … 192 203 The simulation of the trigger electronic starts by checking 193 204 whether the generated analog signal exceeds the discriminator 194 level.205 threshold. 195 206 In that case a digital output 196 signal of a given length (We use in that study a gate length of 6 197 nsec.) 207 signal of a given length (6 nsec.) 198 208 for that pixels is generated. 199 209 By checking next neighbour conditions (NN) at a given time 200 210 the first level trigger is simulated. 201 If a given NN condition ( Multiplicity, Topology, ...)211 If a given NN condition (multiplicity, topology, ...) 202 212 is fullfilled, a first level trigger signal is generated and 203 213 the … … 220 230 \subsection{Starlight simulation} 221 231 222 Due to the big mirror area MAGIC will be sensitive up to223 $10^m$ stars.232 Due to the big mirror area MAGIC will be sensitive to stars up to a 233 magnitude of 10. 224 234 These stars will contribute locally to the noise in the 225 235 camera and have to be taken into account. 226 We developed a program that allows us236 We developed a program that allows 227 237 to simulate the star light together with the generated showers. 228 238 This program considers all stars in the field of view of the camera … … 283 293 on a pattern-recognition method. 284 294 This part is still in the design phase. 285 All results presented here are based on studies ofthe286 first-level-trigger. If not mentioned somewhere else,295 All results presented here refer to the 296 first-level-trigger. If not stated explicitly otherwise, 287 297 the MC data are produced with "standard" 288 298 values (discriminator threshold = 4 mV, gate length = 6 nsec, … … 300 310 \end{equation} 301 311 where T is the trigger probablity. F is a plane perpendicular 302 to the showeraxis.303 The results for different zenith angle $\Theta$ and312 to the telescope axis. 313 The results for different zenith angles $\Theta$ and 304 314 for different discriminator thresholds are shown in figure 305 315 \ref{fig_collarea}. … … 320 330 % 321 331 % 322 increasing dis kriminator threshold.332 increasing discriminator threshold. 323 333 324 334 325 \subsubsection{ Threshold of MAGIC telescope}335 \subsubsection{Energy threshold} 326 336 327 337 The threshold of the MAGIC telesope is defined as the peak 328 338 in the $dN/dE$ distribution for triggered showers. 329 For all different trigger settings 330 this value is determined. The energy threshold could 339 This value is determined 340 for all different trigger settings. 341 The energy threshold could 331 342 depend among other variables on the background conditions, 332 343 the threshold of the trigger discriminator and the zenith angle. We 333 check the influence ofthese three variables.344 check the dependence on these three variables. 334 345 335 346 For both, gammas and protons, some different background conditions … … 351 362 \includegraphics[width=8.3cm]{enerthres.eps} % .eps for Latex, 352 363 % pdfLatex allows .pdf, .jpg, .png and .tif 353 \caption{On the left upper plot the Energy Threshold for diffrent zenith angles is plotted while on the left bottom plot the Energy Threshold is plotted for several values of the trigger discriminator threshold. On the right plot a characteristic fit for $dN/dE$ is shown (for showers at $10^\circ$ with discriminator at 4 mV and diffuse NSB of 0.09 photo electrons per ns and pixel)} 364 \caption{On the left upper plot the energy threshold for diffrent 365 zenith angles is plotted while on the left bottom plot the energy 366 threshold is plotted for several values of the trigger discriminator 367 threshold. On the right plot a characteristic fit for $dN/dE$ is shown 368 (for showers at $10^\circ$ with discriminator at 4 mV and diffuse NSB 369 of 0.09 photo electrons per ns and pixel)} 354 370 \label{fig_enerthres} 355 371 \end{figure} 356 372 357 373 If one lowers the threshold of the trigger discriminator, then less 358 photons in the camera plane are needed to trigger the Telescope.359 And it helps the low energy showers to fulfil the required trigger374 photons in the camera plane are needed to trigger the telescope, 375 and it helps the low energy showers to fulfil the required trigger 360 376 conditions. 361 377 In figure \ref{fig_enerthres} one can see that the threshold 362 energy decreases when lowering the discriminator .378 energy decreases when lowering the discriminator threshold. 363 379 It is 29 GeV for 3 mV and 105 GeV for 7 mV. 364 380 Since we are aiming for a low energy threshold, 365 381 a low discriminator value is preferred. 366 382 However, for 3 mV the expected rate due to protons increases a 367 lot (see section ~\ref{sec-rates}), while it keeps under control at 4 mV. 368 Therefore, the threshold of the discriminator would be kept around 369 4 mV, which yields an energy threshold of 45 GeV. 383 lot (see section ~\ref{sec-rates}), while it is kept 384 under control at 4 mV. 385 Therefore, the threshold of the discriminator should be kept 386 around 4 mV, which yields an energy threshold of 45 GeV. 370 387 371 388 \subsubsection{Expected rates}\label{sec-rates} 372 389 373 Using the monte carlo data sample, it is possible to estimate 374 the expected rates from proton showers and background light. 390 Using the Monte Carlo data sample, it is possible to estimate 391 the expected rates for proton showers taking into account the 392 background light. 375 393 376 394 The numbers quoted in this section are calcuated for a zenith angle 377 $\Theta = 10^o$. Same studies have been done for $\Theta =0^o$ and378 for $\Theta = 15^o$ and we got similar results.395 of $10^\circ$. 396 The results for $0^o$ and $15^o$ were found to be similar. 379 397 We estimated the rate for the first level trigger 380 398 with the "standard" trigger conditions. 381 399 The first level trigger rate due to proton showers without any 382 400 background is $143 \pm 11~\mathrm{Hz}$. 383 This rate w ould increase due to other hadron showers (He, Li, ...) which384 we have not simulated yet. About 25 \% larger rate is expected due mainly385 to He.401 This rate will increase by $\approx 25$\% if heavier nuclei (He, 402 Li,...) are included. 403 386 404 387 405 However, to get a more reliable rate one must take into account 388 a realistic background situation. We take for the diffuse part of the 389 night sky background a value of 0.09 photo electrons per ns 390 \citep{ml94} 391 and use the star field around the Crab nebula. 392 Under this more realistic conditions the first level trigger 406 a realistic background situation. 407 From the total mirror area, the integration time, the FOV of a pixel 408 and the QE of the PMTs one obtains a value of 0.09 photo electrons per 409 ns and pixel \citep{ml94} due to the diffuse night sky background. 410 Added to this are the contributions from the star field around the 411 Crab nebula. 412 Under these more realistic conditions the first level trigger 393 413 background rate (protons and light of night sky) is $396 \pm 88$ Hz. 394 414 395 The dependence of the first level trigger rate fromthe discriminator415 The dependence of the first level trigger rate on the discriminator 396 416 threshold is shown in figure \ref{fig_rates}. 397 417 The trigger rate decreases 398 418 with increasing discriminator threshold as expected. 399 419 The rate for the discriminator threshold of 3 mV is more than 100 400 times larger than for the other values.420 times larger than that for higher thresholds. 401 421 \begin{figure}[hb] 402 422 \vspace*{2.0mm} % just in case for shifting the figure slightly down … … 407 427 \end{figure} 408 428 409 The se results show that theMAGIC telesope will use a disriminator429 The MAGIC telesope will use a disriminator 410 430 threshold of about 4 mV. This value corresponds to a threshold of 411 431 about 8 photo electrons. 412 432 413 It has to be mentioned here, that all the results hereare based on414 the first level trigger. There is a big pot iential to optimizethe415 settings here. I.e. the background rate can be reduced by433 It has to be stressed, that these results are based on 434 the first level trigger. There is a big potential in optimizing the 435 settings. I.e. the background rate can be reduced by 416 436 increasing the discriminator threshold for a few dedicated pixels, 417 437 that have a star in their field of view. Studies in this direction are … … 421 441 422 442 We presented the actual status of Monte Carlo simulation for the MAGIC 423 telescope. 443 telescope. The first level trigger rate for the background is for a 444 discriminator threshold of 4~mV well below the maximal trigger rate 445 (1000 Hz) that the MAGIC daq system will be able to handle. 446 For these standard settings the energy threshold is around 45 GeV. 447 There is a potential in optimizing the trigger system and studies in 448 this direction are ongoing. Also the development of the 449 second-level-trigger is in progress. This should allow to lower the 450 threshold. 451 The MAGIC collaboration is presently simulating air showers with 452 higher zenith angles. 453 The newest results will be presented on 454 the conference. 424 455 425 456 426 457 \begin{acknowledgements} 427 The authors thanks all the members of the MAGIC collaboration 428 for their support in production of the big amount of simulated data. 458 The authors thanks all the "simulators" of the MAGIC collaboration 459 for their support in the production of the big amount of Monte Carlo 460 data. The support of MAGIC by the BMBF (Germany) and the CYCIT (Spain) 461 is acknowledged. 462 463 429 464 \end{acknowledgements} 430 465 … … 438 473 \begin{thebibliography}{99} 439 474 440 \bibitem[(MAGIC Collaboration1998)]{mc98}475 \bibitem[(MAGIC 1998)]{mc98} 441 476 MAGIC Collaboration, "The MAGIC Telescope, Design Study for 442 477 the Construction of a 17m Cherenkov Telescope for Gamma … … 457 492 \end{document} 458 493 459
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