Changeset 815 for trunk


Ignore:
Timestamp:
05/30/01 08:49:22 (23 years ago)
Author:
harald
Message:
add new plot of collection area. And some changes in text.....
Location:
trunk/ICRC_01
Files:
2 edited

Legend:

Unmodified
Added
Removed
  • trunk/ICRC_01/collarea.eps

    r810 r815  
    33%%Title:
    44%%Creator: ROOT Version2.25/03
    5 %%CreationDate:Tue May 29 13:07:54 2001
     5%%CreationDate:Wed May 30 09:32:52 2001
    66%%EndComments
    77%%BeginProlog
     
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     217 1281 m 30 X s [] 0 sd 3 lw 1269 1281 m 30 X s [] 0 sd 3 lw 1 0 1 c 1258 1281 m25 [] 0 sd 3 lw [] 0 sd 3 lw black 1299 1297 m 30 X s [] 0 sd 3 lw 1351 1297 m 30 X s [] 0 sd 3 lw 1 0 1 c 1340 1297 m25 [] 0 sd 3 lw [] 0 sd 3 lw black 1381 1310 m 30 X s
     218 [] 0 sd 3 lw 1434 1310 m 30 X s [] 0 sd 3 lw 1 0 1 c 1422 1310 m25 [] 0 sd 3 lw [] 0 sd 3 lw black 1464 1315 m 30 X s [] 0 sd 3 lw 1516 1315 m 30 X s [] 0 sd 3 lw 1 0 1 c 1505 1315 m25 [] 0 sd 3 lw [] 0 sd 3 lw black 1546 1325 m 30 X s [] 0 sd 3 lw
     219 1599 1325 m 30 X s [] 0 sd 3 lw 1 0 1 c 1587 1325 m25 [] 0 sd 3 lw [] 0 sd 3 lw black 1629 1321 m 29 X s [] 0 sd 3 lw 1681 1321 m 30 X s [] 0 sd 3 lw 1 0 1 c 1670 1321 m25 [] 0 sd 3 lw [] 0 sd 3 lw black 1752 1306 m 10 Y s [] 0 sd 3 lw 1752 1339 m 7
     220 Y s [] 0 sd 3 lw 1711 1327 m 30 X s [] 0 sd 3 lw 1764 1327 m 30 X s [] 0 sd 3 lw 1 0 1 c 1752 1327 m25 [] 0 sd 3 lw [] 0 sd 3 lw black 1835 1285 m 36 Y s [] 0 sd 3 lw 1835 1344 m 24 Y s [] 0 sd 3 lw 1794 1332 m 29 X s [] 0 sd 3 lw 1846 1332 m 30 X s
     221 [] 0 sd 3 lw 1 0 1 c 1835 1332 m25 [] 0 sd 3 lw [] 0 sd 3 lw black 1917 1244 m 73 Y s [] 0 sd 3 lw 1917 1340 m 42 Y s [] 0 sd 3 lw 1876 1329 m 30 X s [] 0 sd 3 lw 1929 1329 m 29 X s [] 0 sd 3 lw 1 0 1 c 1917 1329 m25 [] 0 sd 3 lw [] 0 sd 3 lw black
     222 2000 1200 m 113 Y s [] 0 sd 3 lw 2000 1335 m 55 Y s [] 0 sd 3 lw 1958 1324 m 30 X s [] 0 sd 3 lw 2011 1324 m 30 X s [] 0 sd 3 lw 1 0 1 c 2000 1324 m25 [] 0 sd 3 lw
     223 gsave  1291 672
     224 t 0 r 0 0 m /Helvetica-Bold findfont 44 sf 0 0 m ( = 5 mV\040) show  gr
     225 gsave  1242 655
     226 t 0 r 0 0 m /Helvetica-Bold findfont 32 sf 0 0 m (Thr) show  gr
     227 gsave  1182 672
     228 t 0 r 0 0 m /Helvetica-Bold findfont 44 sf 0 0 m (, D) show  gr
     229 gsave  1162 695
     230 t 0 r 0 0 m /Helvetica-Bold findfont 32 sf 0 0 m (o) show  gr
     231 gsave  1085 672
     232 t 0 r 0 0 m /Helvetica-Bold findfont 44 sf 0 0 m ( = 0) show  gr
     233 gsave  1051 672
     234 t 0 r 0 0 m /Symbol findfont 44 sf 0 0 m (Q) show  gr  black [] 0 sd 3 lw 1 1 1 c 0 1 1 c [] 0 sd 3 lw black 392 163 m 30 X s [] 0 sd 3 lw 444 163 m 30 X s [] 0 sd 3 lw 0 1 1 c 433 163 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 474 163 m 30 X s [] 0 sd 3
     235 lw 527 163 m 30 X s [] 0 sd 3 lw 0 1 1 c 515 163 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 557 314 m 29 X s [] 0 sd 3 lw 609 314 m 30 X s [] 0 sd 3 lw 0 1 1 c 598 314 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 639 458 m 30 X s [] 0 sd 3 lw 692 458 m 30 X s
     236 [] 0 sd 3 lw 0 1 1 c 680 458 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 722 638 m 29 X s [] 0 sd 3 lw 774 638 m 30 X s [] 0 sd 3 lw 0 1 1 c 763 638 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 804 794 m 30 X s [] 0 sd 3 lw 857 794 m 29 X s [] 0 sd 3 lw 0 1 1 c 845
     237 794 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 886 945 m 30 X s [] 0 sd 3 lw 939 945 m 30 X s [] 0 sd 3 lw 0 1 1 c 928 945 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 969 1059 m 30 X s [] 0 sd 3 lw 1022 1059 m 29 X s [] 0 sd 3 lw 0 1 1 c 1010 1059 m23 [] 0 sd 3 lw
     238 [] 0 sd 3 lw black 1051 1159 m 30 X s [] 0 sd 3 lw 1104 1159 m 30 X s [] 0 sd 3 lw 0 1 1 c 1093 1159 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 1134 1218 m 30 X s [] 0 sd 3 lw 1186 1218 m 30 X s [] 0 sd 3 lw 0 1 1 c 1175 1218 m23 [] 0 sd 3 lw [] 0 sd 3 lw
     239 black 1216 1265 m 30 X s [] 0 sd 3 lw 1269 1265 m 30 X s [] 0 sd 3 lw 0 1 1 c 1258 1265 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 1299 1285 m 30 X s [] 0 sd 3 lw 1351 1285 m 30 X s [] 0 sd 3 lw 0 1 1 c 1340 1285 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 1381
     240 1301 m 30 X s [] 0 sd 3 lw 1434 1301 m 30 X s [] 0 sd 3 lw 0 1 1 c 1422 1301 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 1464 1307 m 30 X s [] 0 sd 3 lw 1516 1307 m 30 X s [] 0 sd 3 lw 0 1 1 c 1505 1307 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 1546 1317 m 30 X s
     241 [] 0 sd 3 lw 1599 1317 m 30 X s [] 0 sd 3 lw 0 1 1 c 1587 1317 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 1629 1317 m 29 X s [] 0 sd 3 lw 1681 1317 m 30 X s [] 0 sd 3 lw 0 1 1 c 1670 1317 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 1752 1300 m 11 Y s [] 0 sd 3 lw
     242 1752 1334 m 8 Y s [] 0 sd 3 lw 1711 1322 m 30 X s [] 0 sd 3 lw 1764 1322 m 30 X s [] 0 sd 3 lw 0 1 1 c 1752 1322 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 1835 1281 m 37 Y s [] 0 sd 3 lw 1835 1341 m 25 Y s [] 0 sd 3 lw 1794 1329 m 29 X s [] 0 sd 3 lw 1846
     243 1329 m 30 X s [] 0 sd 3 lw 0 1 1 c 1835 1329 m23 [] 0 sd 3 lw [] 0 sd 3 lw black 1917 1233 m 78 Y s [] 0 sd 3 lw 1917 1334 m 44 Y s [] 0 sd 3 lw 1876 1323 m 30 X s [] 0 sd 3 lw 1929 1323 m 29 X s [] 0 sd 3 lw 0 1 1 c 1917 1323 m23 [] 0 sd 3 lw
     244 [] 0 sd 3 lw black 2000 1187 m 120 Y s [] 0 sd 3 lw 2000 1330 m 57 Y s [] 0 sd 3 lw 1958 1318 m 30 X s [] 0 sd 3 lw 2011 1318 m 30 X s [] 0 sd 3 lw 0 1 1 c 2000 1318 m23 [] 0 sd 3 lw
     245 gsave  1291 590
     246 t 0 r 0 0 m /Helvetica-Bold findfont 44 sf 0 0 m ( = 6 mV\040) show  gr
     247 gsave  1242 573
     248 t 0 r 0 0 m /Helvetica-Bold findfont 32 sf 0 0 m (Thr) show  gr
     249 gsave  1182 590
     250 t 0 r 0 0 m /Helvetica-Bold findfont 44 sf 0 0 m (, D) show  gr
     251 gsave  1162 613
     252 t 0 r 0 0 m /Helvetica-Bold findfont 32 sf 0 0 m (o) show  gr
     253 gsave  1085 590
     254 t 0 r 0 0 m /Helvetica-Bold findfont 44 sf 0 0 m ( = 0) show  gr
     255 gsave  1051 590
     256 t 0 r 0 0 m /Symbol findfont 44 sf 0 0 m (Q) show  gr  1 1 0 c
    173257 gr  gr
    174258showpage
  • trunk/ICRC_01/mccontrib.tex

    r814 r815  
    4444will be finished. The aim of this
    4545detector is the observation of $\gamma$-ray sources in the
    46 enery region above $\approx 10~\mathrm{TeV}$.
    47 The size of the telesope mirros will be around $250~\mathrm{m^2}$.
     46energy region above $\approx 10~\mathrm{GeV}$.
     47The size of the telesope mirrors will be around $250~\mathrm{m^2}$.
    4848The air showers induced by cosmic ray particles (hadrons and gammas)
    4949will be detected with a "classical" camera consisting of 577
     
    5151be recorded by a FADC system running with a frequency of
    5252$f = 333~\mathrm{MHz}$.
    53 The readout of the FADCs by a dedicated trigger system containing
     53The readout of the FADCs will be started
     54by a dedicated trigger system containing
    5455different trigger levels.
    5556
    5657The 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.
     58background from the gamma rays, for which the lowest threshold
     59is aimed.
    5860For a better understanding of the MAGIC telescope and its different
    5961systems (trigger, FADC) a detailed Monte Carlo (MC) study is
    60 unavoidable. Such an study has to take into account the simulation
     62neccessary. Such an study has to take into account the simulation
    6163of air showers, the effect of absorption in the atmosphere, the
    6264behaviour of the PMTs and the response of the trigger and FADC
    63 system.
     65system.
     66 
    6467For a big telescope like MAGIC there is an additional source of
    6568noise, which is the light of the night sky. As a rude assumption
    6669there 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.
     70field of view of the camera.
     71Investigations are neccessary to invent methods which allows to
     72reduce the effect of the light from stars. The methods can be
     73tested before the MAGIC telescope exists by using monte carlo
     74data.
     75
    7076
    7177Here we present the first results of such an investigation.
     
    8187Then the behaviour of the PMTs is simulated and the
    8288response of the trigger and FADC system is generated.
    83 In the followin subsections you find a more precise
     89In the following subsections you find a more precise
    8490description of all the programs.
    8591
     
    95101Gammas where simulated like a point source
    96102whereas 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
     103the given zenith angle.
     104The trigger probality for hadronic showers with
     105a big impact parameter $I$ is not negliable.
     106Therefore we
    100107simulate hadrons with $I < 400~\mathrm{m}$ and gammas
    101108with $I < 200~\mathrm{m}$.
     
    130137close to the telescope position are stored.
    131138
    132 \subsection{mirror simulation}
     139\subsection{atmospheric and mirror simulation}
    133140
    134141The 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.
     142as the input to the mirror simulation.
     143First the absorption in the atmosphere is taken into
     144account.
     145By knowing the height of production and the
     146wavelength of each Cherenkov photen it is possible
     147to calculate the effect of Rayleigh and Mie scattering.
     148The second step is the simulation of the mirror dish.
     149We assume a reflectivity of the mirrors of around 90\%.
     150Each Cherenkov photon hitting one mirror is tracked back
     151to the camera plane of the telescope. This procedure
     152depends on the orientation of the telescope to the
     153shower axis.
    148154All Cherenkov photons reaching the camera plane will be
    149 stored
     155keeped for the next simulation program
    150156
    151157\subsection{camera simulation}
     
    177183a given width.
    178184The amplitude of the response function is randomized
    179 by using the function of figure \ref{fig_ampl}.
    180 By superimpose all photons of one pixel an by taking
    181 the arrival time into account we get the response
    182 of the trigger and FADC system for that pixel (see
    183 also figure \ref{fig_starresp}).
     185by using the distribution of figure \ref{fig_ampl}.
     186By superimposing all photons of one pixel and by taking
     187the arrival time into account the response
     188of the trigger and FADC system for that pixel is generated
     189(see also figure \ref{fig_starresp}).
    184190This is done for all pixels in the camera.
    185191
    186192Then the simulation of the trigger electronic is applied.
    187193We 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.
     194threshold is achieved. In that case a digital output
     195signal of a given length (We use in that study a gate length of 6
     196nsec.)
     197for that pixels.
     198By checking next neighbour conditions (NN) at a given time
     199the first level trigger is simulated.
     200If a given NN condition (Multiplicity, Topology, ...)
     201is fullfilled, a first level trigger signal is generated and
     202the
     203content of the FADC system is written to disk.
    195204%
    196205%
     
    212221the position of an expected gamma ray source is contributing to
    213222the noise in the camera. We developed a program that allows us
    214 to simulate the star light together with the generated shower.
     223to simulate the star light together with the generated showers.
    215224This program takes all stars in the field of view of the camera
    216225around chosen sky region. The light of these stars is track up to
     
    219228get the number of emitted photo electrons per pixel and
    220229time.
     230
    221231These 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%
    222248In figure \ref{fig_starresp} the response of the trigger and the
    223249FADC system can be seen for one pixel with a star of
     
    225251These stars are typical, because there will
    226252be 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
    243254
    244255\section{Results}
     
    277288where T is the trigger probablity. F is perpendicular to
    278289the shower axis. The results for different zenith angle $\Theta$ and
    279 for different trigger settings are shown in figure
     290for different discriminator thresholds are shown in figure
    280291\ref{fig_collarea}.
    281292%
     
    294305%
    295306As bigger the zenith angle the smaller becomes the collection area
    296 for lower energies.
     307for lower energies. As bigger the discriminator threshold is set, as
     308lower is the trigger collection area for low energies.
    297309 
    298310
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