Home

Extensive Air Shower Simulation with CORSIKA: A User`s

1. INTTST ITTAR MCM INTDEC LPIO LETA LHYP LKOS INTSPC LSPEC DIFOFF NDIF TRIGGER NTRIG HISTDS HISTDS 40 the conditions of the interaction test run have to be specified Because of its permanent modification a comprehensive description of the INTTEST option is not available It should be noted that the combinations of allowed parameters for the INTTEST option differ from the standard version without explicitly noting this or checking this during the program run To obtain this program version the INTTEST option has to be selected when extracting the FORTRAN code from the source file 3 5 11 LPM Option The LPM option switches on the Landau Pomeranchuk Migdal effect which is added to EGS4 causing an effective reduction of the pair production and bremsstrahlung cross sections 40 at the highest energies With this option it is possible to include the LPM effect without selecting the THIN option see Sect 3 5 22 46 3 5 12 NEUTRINO Option Muonic and electronic neutrinos and anti neutrinos originate from the decays of the lep tonic decays of K and K7 and the decays of u The neutrino formation is simulated with exact kinematics of all two and three body decays taking into account the polarization of the muons The neutrino trajectories are followed down through the atmosphere disregarding any interaction with the target nuclei of the air The neutrinos are written to the partic
2. 77 4 72 Cherenkov Telescope Data File Name 78 4 13 Wille Data Base File ys 78 4 4 UserName Als d yos roodo rene TE MON SOON 78 AT Host Name em ose Se x REN Og een 79 4 70 Debug eine quu eu ER CR UR EUR RR e bue 79 4 71 Debugging 79 478 FLUKA dor petro n octo Es Sols ice d 79 4 79 GHEISHA Debugging 80 4 80 URQMD Debugging 80 4 81 PYTHIA Printing ee Te Goa G 80 4 82 Cherenkov Debugging 8l 4 83 Interaction Test Target 81 4 54 Interaction Test Desay 4 5 wu ar a ET DB 81 4 85 Interaction Test Spectator Definition 81 4 86 Interaction Test Diffraction Flag 82 4 87 Interaction Test Trigger Condition 82 4 88 Interaction Test Histogram Output 82 4 89 7PIGUQUEDUE an a Ble Ble ROR HRD XS HRD 83 4 90 Plot Axes Dehnilion s e 2 9 os REN ar 83 4 91 Plot Energy Cut Definition 83 4 92 End Of Steering un an Oe e SOROR ee MORE HIA 84 Input Example 85 Coordinate S
3. 70 Format L Default F FEMADD If false no additional information on electromagnetic EM particles is written to particle output file If true additional information on mother and grandmother hadrons of EM particles at the origin of the EM subshower is written to the particle output file Details are similar to those given in Ref 39 for muons This keyword is only available in the EHISTORY option 4 52 Additional Muon Information MUADDI FMUADD Format L Default F FMUADD If false no additional muon information is written to particle output file If true additional information on muons at their origin is written to the particle output file This addi tional muon information consists of 7 data words according to Table 10 page 99 and precedes the corresponding muon particle on particle output file The first data word contains the particle identification 75 or 76 u combined with generation which in this case may differentiate between muons originating from K decay normal generation counter and 7 decay genera tion counter incremented by 50 The 7 data word contains the altitude in cm of the muon birth instead of time see also Table 10 page 99 In combination with the EHISTORY option an extended additional muon information is written to the particle output file Details are given in Ref 39 This keyword is not available in the INTTEST option
4. H sind as X D cos 3 Y D sm 4 Rearth H 5 0 REarth 5 If 0 is small close to shower core then X Y 72 If false the observation level is considered as flat and particle positions X are defined in a Cartesian frame with the origin 0 0 at the core position Particles are tracked only until Z OBSLEV 1 in this Cartesian frame apparent height As a consequence far from the core some particles can be discarded before reaching the ground making a bias in the longitudinal profile To avoid such a problem FCURVOUT false is forbidden by default if the zenith angle is between 85 and 95 The keyword FLATOUT z not FCURVOUT can still be used for backward compatibility These keywords are only available in the CURVED option 4 56 Array Rotation ARRANG ARRANG Format A6 F Default 0 ARRANG Defines a rotation angle in between the detector array x direction and magnetic north direction positive if detector array x direction points to the West Limits are 180 lt ARRANG lt 180 This keyword is not available in the EHISTORY option 4 57 String Detector Configuration DETCFG DETCFG Format A6 F Default 0 DETCFG Gives the geometry configuration of a long vertical string detector as the ratio height diameter Limit is DETCFG gt 0 This keyword is only available in the VOLUMECORR option 4 58 Event Printout MAXPRT MAXPRT
5. These compiler procedures should be used for all needed FORTRAN programs Our experience with machines other than DEC or LINUX are sparse DPMJET option To compile the dpmjet25i f files i 3c 4 5c in dpmjet a pro cedure equivalent to the one for f77 compilers on DEC UNIX machines is recommended 77 c fpe4 check underflow check overflow g3 01 This means Suppress the loading phase generate code to perform runtime checks on subscript continue program after overflow zero divide invalid data or underflow check underflow and overflow at run time produce trace back and debugging information in object file enable local optimizations As the file dpmjet253c f PYTHIA package is extremely large you presumably have to give in advance limit datasize unlimited limit stacksize unlimited to overcome the small default values of many compilers which lead to an error stop during compilation For machines other than DEC UNIX and LINUX there is no experience with the compilation of DPMJET routines EPOS option The compiler procedures of the standard case see begin of this subsection A 1 should be used To compile the epos source files in epos you should use the Make file ka available with EPOS omitting the link step For compiling and linking EPOS you presumably have to give limit datasize unlimited limit stacksize unlimited to overcome the small default values of many c
6. run corsikaread bin sh libtool mode install usr bin install c corsikaread thin run corsikareadthin usr bin install c corsikaread thin run corsikareadthin bin sh libtool mode install usr bin install c plottracks run plottracks usr bin install c plottracks run plottracks make 2 Nothing to be done for install data am make 2 Leaving directory src make 1 Leaving directory src Making install in make 1 Entering directory 7 make 2 Entering directory 7 make install exec hook make 3 Entering directory 7 17 corsika6990Linux_OGSJET_gheisha successfully installed in run You can run CORSIKA in run using for instance corsika6990Linux QGSJET gheisha all inputs output txt make 3 Leaving directory 7 make 2 Nothing to be done for install data am make 2 Leaving directory 7 make 1 Leaving directory 7 Now the installation is finished As written an executable binary file is copied into the run subdirectory where all data files are placed The name of this file is composed by corsika followed by the version number 6990 the system name as given by the uname UNIX com mand an underscore with the selected high energy hadronic interaction model and an under score with the selected low energy hadro
7. F Default 1 D8 DSTLIM Gives the distance in cm a particle would travel with velocity of light downstream the detector before cut away by the time limit An additional security time of 20 usec corre sponding with 6 km is taken into account Limit is DSTLIM gt 0 This keyword is only available in the CURVED option 4 49 Longitudinal Shower Development LONGI LLONG IHSTEP FLGFIT FLONGOUT Format A5 L F 2L Defaults F 20 0 F F LLONGI If true the longitudinal development of particle numbers for gammas EGS4 positrons EGS4 electrons EGS4 positive and negative muons hadrons all charged nuclei and Cherenkov photons CERENKOV is sampled Moreover the longitudinal development of the energy content in the various particle species same order as before but without Cherenkov photons is sampled Additionally the longitudinal development of energy deposit by ionization energy loss and by angular or energy cuts is sampled See also Sect 10 1 page 92 To get the sampling in slant depth instead of the default vertical depth you should use the SLANT option page 45 If false the longitudinal development is not sampled THSTEP Vertical step width rsp slant step width in the SLANT option for sampling of the longitudinal development in g cm The sampling is done in vertical rsp slant depth The altitudes are not depending on the zenith angle of the primary particle except the pr
8. Cambridge University Press Cambridge UK 1992 36 F X Kneizys et al The MODTRAN 2 3 Report and LOWTRAN 7 Model Phillips Lab oratory Hanscom AFB MA 01731 3010 USA 1996 37 M Risse and D Heck Astropart Phys 20 2004 661 38 D Heck Report FZKA 7366 2008 Forschungszentrum Karlsruhe http www ik fzk de heck publications 39 D Heck and R Engel Report FZKA 7495 2009 Forschungszentrum Karlsruhe http www ik fzk de heck publications 40 D Heck and J Knapp Report FZKA 6097 1998 Forschungszentrum Karlsruhe http www ik fzk de heck publications 41 P Homola et al Comp Phys Comm 173 2005 71 42 T Huege REAS 3 00 User s Manual http www ik fzk de huege reas 43 D Heck Report FZKA 7082 2004 Forschungszentrum Karlsruhe http www ik fzk de heck publications 44 D Heck Report FZKA 7254 2006 Forschungszentrum Karlsruhe http www ik fzk de heck publications 45 M Hillas Nucl Phys B Proc Suppl 52B 1997 29 46 M Kobal P Auger Collaboration Astropart Phys 15 2001 259 47 E Andres et al AMANDA Collaboration Astropart Phys 13 2000 1 48 D Heck Report FZKA 6954 2004 Forschungszentrum Karlsruhe http www ik fzk de heck publications F Schr der Diss University Wuppertal 2001 Report WUB DIS 2001 17 2001 Universitit Wuppertal http elpub bib uni wuppertal de edocs dokumente fb08 diss2001 schroeder f080105 pdf
9. Kernforschungszentrum Karlsruhe N N Kalmykov and S S Ostapchenko Yad Fiz 56 1993 105 Phys At Nucl 56 N3 1993 346 N N Kalmykov S S Ostapchenko and A I Pavlov Izv RAN Ser Fiz 58 1994 N12 p 21 N N Kalmykov S S Ostapchenko and A I Pavlov Bull Russ Acad Science Physics 58 1994 1966 N N Kalmykov S S Ostapchenko and A I Pavlov Nucl Phys B Proc Suppl 52B 1997 17 S S Ostapchenko private communications 2001 S S Ostapchenko Nucl Phys B Proc Suppl 151 2006 143 and 147 Phys Rev D74 2006 014026 R S Fletcher T K Gaisser P Lipari and T Stanev Phys Rev D50 1994 5710 J Engel T K Gaisser P Lipari and T Stanev Phys Rev D46 1992 5013 R Engel T K Gaisser P Lipari and T Stanev Proc 26 Int Cosmic Ray Conf Salt Lake City USA 1 1999 415 E J Ahn R Engel T K Gaisser P Lipari and T Stanev Phys Rev D80 2009 094003 R Engel private communications K Werner Phys Rep 232 1993 87 H J Drescher et al Phys Rep 350 2001 93 Werner F M Liu and T Pierog Phys Rev C74 2006 044902 A Fass A Ferrari J Ranft PR Sala Report CERN 2005 10 2005 05 11 SLAC R 773 2005 A Fasso A Ferrari S Roesler Sala Battistoni F Cerutti E Gadioli M V Garzelli F Ballarini O Ottolenghi A Empl and J Ranft Computing in High Energy and Nuclear Physics 2003 Conference CHEP2003 La Jolla CA
10. 100 0 0 00421033 2 6798156 10 Table 29 Parameters of South pole atmosphere for January Lipari 0 6 67 59 0293 1079 00 764170 6 67 13 33 21 5794 1071 90 699910 13 33 20 0 7 14839 1182 00 635650 20 0 100 0 0 0000 1647 10 551010 gt 100 0 0 000190175 59 329575 10 Table 30 Parameters of South pole atmosphere for August Lipari 124 Malarg e Argentina 0 80 150247839 1198 5972 945766 30 80 18 1 6 66194377 1198 8796 681780 12 18 1 345 0 94880452 1419 4152 620224 52 34 5 100 0 4 8966557223 10 730 6380 728157 92 Table 31 Parameters of the average Malarg e Argentina winter atmosphere I 0 83 126 110950 1179 5010 939228 66 8 3 12 9 47 6124452 1172 4883 787969 34 12 9 34 0 1 00758296 1437 4911 620008 53 34 0 2100 0 5 1046180899 1074 761 3281 724585 33 sons i Table 32 Parameters of the average Malarg e Argentina winter atmosphere II 0 59 189 683519 1202 8804 977139 52 5 9 12 0 79 5570480 1148 6275 858087 01 12 0 34 5 0 98914795 1432 0312 614451 60 34 5 100 0 4 87191289 1074 696 42788 730875 73 gt 1000 0 01128292 Table 33 Parameters of the average Malargiie Argentina spring atmosphere 125 0 9 0 136 562242 1175 3347 986169 72 90 146 44 2165390 1180 3694 793171 45 14 6 33 0 1 37778789 1614 5404 60
11. 4 the simple Monte Carlo generator HDPM 5 which is inspired by the Dual Par ton Model and tries to reproduce relevant kinematical distributions being measured the quark gluon string model QGSJET 6 7 the mini jet model SIBYLL 8 9 or VENUS 10 Asa sixth alternative there is added a link to the NEXUS model 11 which combines algorithms of VENUS and QGSJET with new ideas based on H1 and Zeuss data The last model included is EPOS 12 It is based on the NEXUS framework but with important improvement concerning hard interactions and nuclear and high density effect It is the only model available here repro ducing most recent RHIC data The hadronic interaction cross sections at higher energies are adopted according to the used model The low energy hadronic interactions are simulated alternatively with one of the codes FLUKA 13 a very refined model with many details of nuclear effects GHEISHA 14 that is a well approved detector Monte Carlo program in the energy region up to some hundred GeV or UrQMD 15 which describes microscopically the low energetic hadron nucleus collisions The interactions of electrons and photons can be treated either with the EGS4 code 16 follow ing each particle and its reactions explicitly or using the analytic NKG formulae 17 to obtain electron densities at selected locations and the total number of electrons at up to 10 observation levels Further on it is optionally possible to explicitly gen
12. 4 53 Observation Level Definition OBSLEV OBSLEV i Format A6 F Default 110 E2 OBSLEV Observation level 2 above sea level in cm This keyword has to appear once for each level to be defined At maximum up to 10 observation levels are possible Their sequence is arbitrary In the UPWARD option page 48 for upward going primaries the observation level should be chosen preferentially at the top of atmosphere but at minimum above the starting point of the shower The value of OBSLEV has to be selected in a manner that the shower axis crosses the observation level Limits are 0 lt OBSLEV i lt top of atmosphere 59Only one observation level is possible in the CURVED option Up to 20 levels might be specified for the production of histograms in the AUGERHIST option the lowest observation level must be at minimum 1 g cm above sea level 60 For atmospheric models 1 lt MODATM lt 9 limits are 1 E5 lt OBSLEV i lt 112 8E5 71 4 54 Inclined Observation Plane NCLIN XPINCL YPINCL ZPINCL THINCL PHINCL Format SF Defaults 0 0 OBSLEV 1 0 0 XPINCL X coordinate in cm of reference point in inclined observation plane YPINCL Y coordinate in cm of reference point in inclined observation plane ZPINCL Z coordinate in cm of reference point in inclined observation plane THINCL 0 angle in deg of normal vector of inclined observation plane 0 0 poi
13. 49 T H Burnett et al Phys Rev D35 1987 824 129 50 A S Goldhaber Phys Lett B 53 1974 306 51 M Haffke Univers Dortmund Germany private communication 2007 52 http www ngdc noaa gov geomag 53 Gaisser and A M Hillas Proc 157 Int Cosmic Ray Conf Plovdiv Bulgaria 8 1977 353 54 G J Alner et al UA5 Collaboration Phys Rep 154 1987 247 55 E Abe et al CDF Collaboration Phys Rev D41 1990 2330 Phys Rev Lett 61 1988 1819 56 R Harr et al Phys Lett B401 1997 176 57 Handbook of Chemistry and Physics 67 Edition ed R C Weast The Chemical Rubber Co Cleveland USA 1986 F141 58 J Linsley private communication by M Hillas 1988 59 H Ulrich K H Kampert and H O Klages Auger technical note GAP 1998 043 1998 http www auger org admin GAP_notes index html 60 http nssdc gsfc nasa gov space model atmos msise html 61 P Lipari private communication by P Steffen 1998 62 B Keilhauer et al Astropart Phys 22 2004 249 130 Index Preprocessor Options ANAHIST 36 74 103 ATMEXT 37 58 AUGCERLONG 36 37 AUGERHIST 37 74 103 AUGERINFO 38 104 BYTERECL 11 CEFFIC 35 77 CERENKOV 32 75 77 CERWLEN 34 CHARM 38 COMPACT 38 74 102 CURVED 39 54 DPMIET 24 60 114 EHISTORY 40 EPOS 25 60 114 FLUKA 29 115 117 GHEISHA 30 80 IACT 34 78 IACTEXT 34 78 IBMRISC 11 INTCLONG 36 69 103 INTTEST 40 81
14. Contents of word as real numbers R 4 1 particle description encoded as part idx 1000 hadr generation x 10 no of obs level 2 px momentum in x direction in GeV c 3 py momentum in y direction in GeV c 4 pz momentum in z direction in GeV c 5 x position coordinate in cm 6 y position coordinate in cm t time since first interaction or since entrance into atmosphere in nsec for additional muon information z coordinate in cm forn 1 39 if last block is not completely filled trailing zeros added Table 10 Structure of particle data sub block Cherenkov photon data sub block up to 39 bunches 7 words each Contents of word as real numbers R 4 7 x n 1 1 number of Cherenkov photons in bunch in case of output on the particle output file 99 E5 10x NINT number of Cherenkov photons in bunch 1 X position coordinate in cm y position coordinate in cm u direction cosine to x axis v direction cosine to y axis t time since first interaction or since entrance into atmosphere in nsec 7 height of production of bunch in cm for n 1 39 if last block is not completely filled trailing zeros are added Table 11 Structure of Cherenkov photon data sub block The generation counter is set to 0 before the first interaction and augmented by each hadronic interaction or decay The decay of 7 mesons increases this counter by 51 thus the muons and neutrinos
15. LONGI 10 8 dbase File and info File Output To build up a data base as a directory of a shower library which enables a computer aided search for specific shower events the DATnnnnnn dbase file page 78 may be used The content of the DAT nnnnnn dbase file consists of parameter words enclosed within marks followed by the information on the corresponding parameter The list of parameter words and their contents is given in Table 16 page 106 In the AUGERINFO version this file is named 104 DATnnnnnn info and for each parameter new line is started omitting the mark separators It should be noted that some of the parameters listed in Table 16 are present only with the selected options e g for thinning page 46 for external atmospheres page 37 for viewing cone page 49 or for Cherenkov telescopes page 34 105 Content of DAT nnnnnn dbase rsp DATnnnnnn info file Content Format version version number F6 3 versiondate date of version YY YYMMDD 19 modelversion version number of high energy hadronic interaction program F8 3 rundate date of run YY YYMMDD 19 computer computer option 12 3 UNIX LINUX 4 Macintosh curved number indicating CURVED option I2 2 curved O else neutrino number indicating NEUTRINO option I2 cerenkov number indicating CERENKOV option I2 runnumber run number I7 primary particle code of primary particle 15 e_range_l lower end of p
16. THETPR lt 180 For the CURVED option combined with the UPWARD option 2 has to be chosen in a manner excluding the range 90 lt 2 lt 90 The angle 6 90 is spanned between the upward going shower axis and the horizontal detector plane above the shower starting point Further details are given in 44 48 The keyword IMPACT page 56 for skimming horizontal showers overrides THETPR 2 481n the output file the corresponding of each shower is given in the range 7 7 radian 54 4 11 Starting Altitude FIXCH THICKO Format A6 F Default 0 THICKO The starting altitude in g cm mass overburden of the primary particle is set for all showers This choice is not effective if the height of the first interaction is set by FIXHEI gt 0 see Sect 4 13 below With this keyword the development of sub showers starting at the chosen altitude within the atmosphere may be followed The starting altitude must be above the lowest observation level In the UPWARD option with an upward primary particle the starting altitude must be below the observation level page 48 Limit is 0 lt THICKO 4 12 Starting Point of Arrival Timing ISTART IMARGIN Format L Default F TMARGIN Flag indicating the starting point of the arrival time scale If TMARGIN false the first interaction starts the clock If TMARGIN true the entrance into the atmosphere rsp
17. WMAX gives the maximum weight factor which should not be exceeded The core distance up to which the radial thinning at detector level takes place is specified by RMAX Via the keyword page 67 THINH THINRAT WEITRAT or the keyword page 68 THINEM IHINRAT WEITRAT differing thin levels and weight limits can be specified for hadronic or electromagnetic particles overwriting the ratios THINRAT g 5 Etn and WEITRAT WMAX WMAX haar which are set to 1 by default The effect of various thinning levels j on the computing time and the number of particles on MPATAP may be seen from Table 2 which is established with default CORSIKA 43To ensure the surviving of enough particles close to the shower axis RMAX should be chosen not too large In case of a primary energy spectrum ULIMIT gt LLIMIT the value of WMAX is used for the low energy end of the energy interval and slides to higher values according with the sliding primary energy 47 parameters QGSJET option EGS4 activated for vertical proton induced showers of 1015 eV primary energy DEC 3000 600 AXP with 175 MHz with 1 with infinite weight limit and without radial thinning As to each particle an appropriate weight must be attributed the output format described in Sect 10 2 page 94 ff has to be changed to incorpo rate this additional parameter of each particle Consequently MPATAP and MCETAP output
18. a different NUCLEAR BIN file is necessary which is available from CERN or from the author of DPMJET lt johannes ranft cern ch gt 4 the binary files of CORSIKA after compilation e a subdirectory src containing the major part of the source code corsika F and corsika h which is FORTRAN code file with some C preprocessor commands that contains the code of CORSIKA including the EGS4 and model routines It contains also the interfaces to FLUKA GHEISHA UrQMD DPMJET EPOS NEXUS QGSJET SIBYLL and VENUS but without those hadronic interaction codes 5 separate files with pure FORTRAN code of the GHEISHA QGSJETO1c QGSJET II 03 SIBYLL2 1 and VENUS routines gheisha_2002d f qgsjetOlc f qggsjet I1 03 f sibyll2 1 f and venus f 2 separate files with the pure C code of the PRESHOWER and STACEE preshw c and stacee c 2 FORTRAN routines to read the binary CORSIKA particle output files corsikaread f and cor sikaread thin f are compiled the first time CORSIKA is compiled and in stalled in run 2 special C routines needed for compilation timerc c and trap f pe c aroutine plottracks3c f and its include file work inc to visualize shower plots established with the option PLOTSH C routine map2png c to visualize the shower plots established with the option PLOTSH2 e subdirectory urgmd containing the source package of the UrQMD model The CORSIKA code and the files bel
19. covered by CORSIKA feel free to program it Please contact T Pierog or D Heck before doing so If your addition is of general interest it might be worth to take it over into the next official CORSIKA release At the beginning of the corsika h file you find a rather complete list of all global variables used in COMMONS This enables to check the names which you give your variables for conflicts with names already used within CORSIKA The names of the CORSIKA commons start with CR to prevent conflicts with common or subroutine names of linked interaction program packages As the largest fraction of the CORSIKA routines is written in CAPITAL letters you are advised to use lower case characters for your private program extensions This facilitates to distinguish your programming from the official code We advise you to use coconut help dev options configure options to handle your compilation installation processes It is recommended to run coconut without arguments to configure and install CORSIKA Various options are available in coconut for expert use only e Any additional option with trailing will be passed on to con figure directly try e g help e h help Display a help file and stop e b batch No user interaction just take DEFAULT and CACHED configuration e c clean Execute make clean if CORSIKA is already installed once Re move all object files and stop e d d
20. into the pythia subdirectory see Sect 3 5 6 page 38 The COAST and COAST USER LIB routines needed for the ROOTOUT and ROOTRACK version may be downloaded from http www ik fzk de rulrich coast 2 2 2 Example As an example if you have the file corsika 6990 tar gz in the current directory the installation on a LINUX system will look like commands you are giving are underlined tar zxf corsika 6990 tar gz gt cd corsika 6990 coconut Welcome to COCONUT v2 the CORSIKA CONfiguration UTility create an executable of a specific CORSIKA version Please read the documentation for a detailed description of the options and how to use it Try coconut h to get some help about COCONUT Use coconut expert to enable additional configuration steps press Enter to select an option followed by DEFAULT or CACHED 15 Assuming shell one uses setenv FLUPRO flukadirectory 16 lt alfredo ferrari cern ch gt or lt alfredo ferrari mi infn it gt 13 kkkxkxkxkxkxkxkxkxkxkxkkkxkkkxkkkxkkkxkkkxkkkxkkkxkkkxkkkxkkkkkkkkkkkxkkkxkkkkkkkxkkkkxkkkxkkkkkkkkxkkkxkkkxkkkkkx k WARNING Your system does support 64bit binaries Some CORSIKA features are only supported in 32bit mode because of incompatible binary data structures Therefore by default CORSIKA uses the m32 flag to force 32bit mode If you need to overwrite this feature e g to link to a 64bit COAST RO
21. model at a time In principle a combination of NUPRIM with all hadronic interaction models is possible page 116 The CHARM option makes sense only with the interaction models DPMJET or QGSJETOIc with EPOS in preparation as only these interaction models are producing charmed particles explicitely The combination of PRESHOWER with NUPRIM makes no sense as your primary may be either a high energy gamma ray or a neutrino Neither PRESHOWER nor NUPRIM may be combined with STACKIN The ROOTOUT and ROOTRACK options cannot be combined with the COMPACT option The combination of INTTEST with PLOTSH or PLOTSH2 is not reasonable as in the INTTEST option the development of showers is suppressed Also a combination of INTTEST with ANAHIST AUGERHIST CURVED EHISTORY PRESHOWER STACKIN or THIN gives no sense as you are simulating just the first interaction without development of a complete shower A combination with UPWARD makes no sense as in INTTEST anyway all upward going particles are respected The combination of NUPRIM with INTTEST is not supported The combination of FLUKA with INTTEST is not foreseen IACT is only possible with CERENKOV IACT and ATMEXT have been tested only with UNIX computers VOLUMEDET and VOLUMECORR exclude each other as you may use only one detector geometry at a time Similarly INTCLONG and NOCLONG are excluding each other As in the CEFFIC option the atmospheric absorption is treated only in a manner suited for planar
22. when the PLOTSH option is selected The program plottracks reads in the DATnnnnnn track DATnnnnnn track and DATnnnnnn track files specified on the command line by the parameter run nnnnnn integer between and 999999 Then it converts and combines them into 4 PPM images tracknnnnnn em ppm tracknnnnnn mu ppm tracknnnnnn had ppm and tracknnnnnn all ppm of the same resolution as the maps By default the electromagnetic muonic and hadronic maps are taken as the red green and blue channels of the RGB image respectively As with increasing shower energy and decreasing threshold the number of tracks increases drastically you should simulate not more than 1 shower at a time to keep the output on the units 55 56 and 57 at a tolerable size Via the keyword page 83 PLOTSH the PLOTSH option is enabled or disabled This option is not recommended for ordinary shower production because of the large output files to be produced To obtain this program version the PLOTSH option has to be selected when extracting the FORTRAN code from the source file 3 5 15 PLOTSH2 Shower Plot Production Option In the PLOTSH2 option air showers are visualized in a simple way without having to deal with a very large track file With the PLOTSH2 option map files are generated separately for the electromagnetic particles muons and hadrons For each particle species maps are generated in 37977 plottracks3c f o p
23. 13 is a package of routines to follow energetic particles through matter by the Monte Carlo method In combination with CORSIKA only that part is used which describes the low energy hadronic interactions A detailed description of the pro cesses simulated by FLUKA 2011 may be found on the FLUKA web page http www fluka org FLUKA is used within CORSIKA to calculate the inelastic hadron cross sections with the com ponents of air and to perform their interaction and secondary particle production including many details of the de excitation of the target nucleus If you have selected the FLUKA option the Make file will link the FLUKA library with your CORSIKA program pages 115 and 117 To run the FLUKA version an environment variable tells the system where to find the binary data files page 20 needed by the FLUKA routines It should be emphasized that the FLUKA option cannot be combined with the DPMJET option because of several identical subroutine names used within FLUKA and DPMJET 33See footnote page 8 for the usage of the preprocessor option LINUX 34 Assuming csh shell one uses setenv FLUPRO flukadirectory 29 3 2 2 GHEISHA Option GHEISHA Gamma Hadron Electron Interaction SHower code is an interaction package widely used in the detector Monte Carlo program GEANT 28 that has proven its qualities in describing hadronic collisions up to some 100 GeV in many experiments A detailed descrip tion of the physics pr
24. 14 1993 MODATM 8 AT1224 Central European atmosphere for Dec 24 1993 MODATM 9 Atmosphere as read in by keywords ATMB ATMC Layers as in MO 1 8 10 Atmosphere as read in by keywords ATMB ATMLAY uppermost layer also read in MODATM 11 South pole atmosphere for March 31 1997 MSIS 90 E MODATM 12 South pole atmosphere for July 01 1997 MSIS 90 E MODATM 13 South pole atmosphere for Oct 01 1997 MSIS 90 E MODATM 14 South pole atmosphere for Dec 31 1997 MSIS 90 E MODATM 15 South pole atmosphere for January after Lipari MODATM 16 South pole atmosphere for August after Lipari MODATM 17 Malarg e winter atmosphere I after Keilhauer MODATM 18 Malarg e winter atmosphere II after Keilhauer MODATM 19 Malarg e spring atmosphere after Keilhauer MODATM 20 Malarg e summer atmosphere after Keilhauer MODATM 21 Malarg e autumn atmosphere after Keilhauer MODATM 22 U S standard atmosphere as parameterized by Keilhauer The various atmospheric models are described in Appendix D page 120 ff Limits are 0 lt MODATM lt 22 4 17 Atmospheric Parameters A i ATMA AATM1 AATM2 AATM3 AATM4 AATM5 Format A4 AF Defaults 0 0 0 0 for ATMOD 0 Format A4 5F Defaults 0 0 0 0 0 for ATMOD 10 AATMi A parameters for 4 layers of atmospheric model 0 or for 5 layers of atmospheric mode
25. 555305 1222 6562 994186 38 94 919 1144 9069 878153 55 i Ps 1305 5948 636143 04 540 1778 772170 16 om i Table 17 Parameters of the U S standard atmosphere after Linsley 120 Middle Europe 118 1277 1173 9861 154 258 1205 7625 963267 92 0 4191499 1386 7807 614315 5 4094056 1074 555 8935 739059 6 01128292 Table 18 Parameters of the AT115 atmosphere January 15 1993 195 837264 1240 48 933697 50 4128778 1117 85 765229 0 345594007 1210 9 636790 5 46207 10 4 608 2128 733793 8 Table 19 Parameters of the AT223 atmosphere February 23 1993 253 95047 1285 2782 1088310 128 97714 1173 1616 935485 0 353207 1320 4561 635137 5 526876 1074 680 6803 727312 6 0 011229 Table 20 Parameters of the AT511 atmosphere May 11 1993 121 208 12899 1251 474 1032310 120 26179 1173 321 925528 0 31167036 1307 826 645330 wath 5 591489 1074 763 1139 720851 4 001128292 Table 21 Parameters of the AT616 atmosphere June 16 1993 77 875723 1103 3362 932077 214 96818 1226 5761 1109960 0 3721868 1382 6933 630217 5 5309816 10 4 685 6073 726901 3 5 i 1 Table 22 Parameters of the AT822 atmosphere August 22 1993 242 56651 1262 7013 1059360 103 21398 1139 0249 888814 0 3349752 1270 2886 639902 5 527485 10 4 681 4061 727251 8
26. 9 MODATM gt 171 This keyword is only available in the combination of the CURVED option with the UPWARD option 4 15 Stack Input File Name NFILE FILINP Format A64 Defaults FILINP File name to define the name and directory of the input file containing the parameters of secondary particles see Sect 3 5 20 page 45 Lower case characters of FILINP are not converted to capitals Please keep in mind that in FORTRAN an automatic expansion of UNIX names like home is not possible rather you should give the full expanded name of the direc tory ending with a character Limit is FILINP must not begin with a tilde character This keyword is only available in the STACKIN option 56 4 16 Atmospheric Model Selection ATMOD MODATM Format A5 I Default 1 MODATM Gives the number of the atmospheric parameterization MODATM 0 Atmosphere as read in by keywords ATMB ATMC and ATMLAY uppermost layer unchanged MODATM 1 U S standard atmosphere as parameterized by Linsley MODATM 2 AT115 Central European atmosphere for Jan 15 1993 MODATM 3 AT223 Central European atmosphere for Feb 23 1993 MODATM 4 AT511 Central European atmosphere for May 11 1993 MODATM 5 AT616 Central European atmosphere for June 16 1993 MODATM 6 AT822 Central European atmosphere for Aug 22 1993 MODATM 7 AT1014 Central European atmosphere for Oct
27. AUGERINFO option has to be selected when extracting th FORTRAN code from the source file 3 5 6 CHARM Option In the standard CORSIKA program the charmed particles are treated implicitly in the hadronic interaction codes But several codes at present DPMJET and QGSJETOlc produce them in a manner that they can be treated explicitely respecting their transport during their lifetime Be cause of the short lifetimes and the unknown cross sections the fate of the charmed particles always is determined by their decay These decays are treated by the PYTHIA package 19 Therefore in combination with QGSJETOlc the PYTHIA 6 412 package has to be installed in the pythia subdirectory for automatic compilation and linking In combination with DPM the implicit PYTHIA 6 1 package dpmjet253c f is used and needs no extra linking The CHARM option 38 also enables the treatment of the 7 leptons possible interactions bremsstrahlung pair production nuclear interactions of the 7 leptons are respected in a man ner analogously to the ji leptons For the treatment of primary v and 7 neutrinos the CHARM option has to be combined with the NUPRIM option see page 41 For tracing back PYTHIA problems in combination with QGSJETOlc the PYTHIA keyword is available see Sect 4 81 page 80 To obtain this program version the CHARM option has to be selected when extracting the FORTRAN code from the source file Please verify that in combination with QG
28. Format A6 I Default 10 MAXPRT Is the maximum number of events that produce a detailed printout during the sim ulation run Limit is MAXPRT gt 0 73 4 59 Particle Printout ECTMAP ECTMAP Format A6 F Default 1 E4 ECTMAP Defines a cut in the particle y factor or energy in GeV for em particles and neutri nos above which they are printed out on the logical unit MONIOU when passing an observation level 4 60 Output Directory DIRECT DSN Format A6 A64 Defaults anynameupto64characters DSN May be used to define a name of an output directory Lower case characters of DSN are not converted to capitals Do not use capitals with the ANAHIST AUGERHIST or INTTEST options as the HBOOK routines use only lower case characters To suppress the output you might give dev null 9 or use the keyword PAROUT If you want to write into the directory from where you are starting your CORSIKA run you should give DIRECT or DIRECT ablank enclosed in apostrophes or quota tion marks Please keep in mind that in FORTRAN an automatic expansion of UNIX names like home is not possible rather you should give the full expanded name of the directory ending with a character Limit is DSN must not begin with a tilde character 4 61 Table Output PAROUT FPAROUT FTABOUT Format A6 2L Defaults T F FPAROUT If false the particle output onto MPATAP is suppr
29. SCORSIKA USER COMP is not empty then coconut does not set any FORTRAN com piler name or flags If they are not defined by you see A 1 to know the recommended flags configure will give some default value compilation not guaranteed So don t use this option if you don t know exactly what you are doing no support for this Run it a first time to select the options you want to use saved in 1ibdir include config h and then work directly on the src corsika F file FORTRAN preprocessor com mands To compile this modified source without calling configure again use coconut dev make for debugging It s equivalent just to go into the proper subdirectory depending on dev and to type rm compilefile f make This will update the compile file f with your modifications and then compile it When the compilation is successful you can link objects and libraries into run corsika V E R OS _ HIGH _ low by typing coconut install in your corsika 6990 directory When the development phase is over you can use the standard procedure coconut dev 51 Call configure help Where VER is the version number OS is the operating system used for compilation HIGH is the chosen high energy hadronic interaction model and low is the chosen low energy hadronic interaction model 83The coconut compiles and installs all the libraries needed by CORSIKA to be linked with and then creates a binary file in run Then if y
30. USA March 24 28 2003 paper 005 eConf C0303241 2003 arXiv hep ph 0306267 2003 http www fluka org Fesefeldt Report PITHA 85 02 1985 RWTH Aachen 127 15 S A Bass et al Prog Part Nucl Phys 41 1998 225 M Bleicher et al J Phys G Nucl Part Phys 25 1999 1859 http www th physik uni frankfurt de urqmd 16 W R Nelson H Hirayama and D W O Rogers Report SLAC 265 1985 Stanford Lin ear Accelerator Center http www slac stanford edu pubs slacreports slac r 265 html http www irs inms nrc ca inms irs EGS4 get egs4 html 17 A A Lagutin A V Plyasheshnikov and V V Uchaikin Proc 16 Int Cosmic Ray Conf Kyoto Japan 7 1979 18 J N Capdevielle for KASCADE Collaboration Proc 2274 Int Cosmic Ray Conf Dublin Ireland 4 1991 405 18 Corcella et al 0101 2001 010 Marchesini et al Comp Phys Comm 67 1992 465 http hepwww rl ac uk theory seymour herwig 19 T Sj strand S and Skands JHEP 0605 2006 026 http www thep lu se torbjorn pythia html 20 M Ambrosio et al Auger technical note GAP 2003 013 2003 Proc 28 Int Cosmic Ray Conf Tsukuba Japan 2003 595 http wwwl na infn it wsubnucl cosm auger activities html 21 J Knapp D Heck and G Schatz Report FZKA 5828 1996 Forschungszentrum Karlsruhe http www ik fzk de heck publications J Knapp Nucl Phys B Proc Suppl 75A 1999 89
31. and the height h of the form T h 4 1 4 6 In the fifth layer the mass overburden decreases linearly with height T h a5 bs 2 h cs The boundary of the atmosphere in this model is defined at the height where the mass over burden 7 h vanishes which is at h 112 8 km for the U S standard atmosphere Various atmospheres are foreseen U S standard atmosphere parameterized according to J Lins ley 58 7 typical atmospheres as measured above Stuttgart about 60 km away from Karlsruhe at various days of 1993 and transmitted by Deutscher Wetterdienst Offenbach parameterized according to Ref 59 4 South pole atmospheres parameterized by D Chirkin according to the MSIS 90 E model 60 two South pole atmospheres by P Lipari 61 and 5 seasonal dependent atmospheres for the Pierre Auger Observatory experiment at Malarg e Argentina parameterized by B Keilhauer 62 who provided also a new parameterization of the U S standard atmosphere The parameters a b and c are selected in a manner that the function T h is continuous at the layer boundaries and can be differentiated continuously In Tables 17 36 the parameters for the various models are listed Additional atmospheres 36 are available by the keyword ATMOSPHERE page 58 in the ATMEXT option page 37 User specific atmosphere parameters may be read in using the keywords ATMOD ATMA ATMB ATMC and ATMLAY U S Standard Atmosphere 186
32. by default By the preprocessor option INTCLONG the integral mode is selected i e accumulated number of generated Cherenkov photons for each step which needs additional computing time If both kinds of longitudinal distribution are of no interest you may deselect the Cherenkov photon distribution completely by the preprocessor option NOCLONG thus saving computing time The option INTCLONG is effective also with the AUGCERLONG option see Sect 3 5 3 page 37 To obtain these program versions the INTCLONG rsp NOCLONG option has to be selected together with the CERENKOV rsp AUGCERLONG option when extracting the FORTRAN code from the source file 3 47 STACEE Option In the STACEE option the output of the Cherenkov file is generated in a format as used for the STACEE experiment 26 Details on the output data structure may be obtained from the members of the STACEE Collaboration The appropriate C routines are available in the src subdirectory linked after compilation by the Makefile To obtain this program version the STACEE option has to be selected when extracting the FORTRAN code from the source file 3 5 Other Non standard Options 3 5 1 ANAHIST Option The ANAHIST option produces a series of histograms generated with HBOOK routines 24 The histograms are written into the file named datnnnnnn lIhbook page 103 onto the output directory DSN specified by the keyword DIRECT page 74 To suppress the ordinary particle output file th
33. details This CORSIKA GUIDE is an updated version of Ref 23 For citation of CORSIKA in your publications you might use Ref 3 which is available from the CORSIKA www page http www ik fzk de corsika Please do not forget also to make a reference to the hadronic interaction models which you used in your simulations The correct references you find in the bibliography page 127 of this CORSIKA GUIDE and in format in the file references tex see directory doc If you have problems in installing or running the program suggestions to improve the code concerning physics computing or handling please contact Dr T Pierog Dr D Heck Karlsruhe Institute of Technology Karlsruhe Institute of Technology Institut f r Kernphysik Institut f r Kernphysik Hermann von Helmholtz Platz 1 Hermann von Helmholtz Platz 1 D 76344 Eggenstein Leopoldshafen D 76344 Eggenstein Leopoldshafen e mail lt tanguy pierog kit edu gt e mail dieter heck kit edu gt Fax 49 0 721 608 24075 Fax 49 0 721 608 24075 Tel 49 0 721 608 28134 Tel 49 0 721 608 23777 users of CORSIKA are kindly asked not to hand over the program to interested new users but rather to send their name and address to the above addresses By these means new users can be provided with news about the latest program version error corrections and updates Thus problems with outdated versions should be avoided 2 Installation 2 1 CORSIKA Files Th
34. exo orbe ra Par RE 69 Longitudinal Shower Development ooo 69 Muon Multiple Scattering Treatment 70 Additional Electromagnetic Particle Information 70 Additional Muon 71 Observation Level Definition 71 Inclined Observation 72 Observation Level Curvature 72 Array Rolalien Cool poA EORR ee EOS d 73 String Detector 73 Event Pribtolt 2 be ay a Betas 73 Particle Printout a retta een eia Ge eod diio ee 74 Outpt Directory St xe E SCR ee BS RE ES eee Be M 74 Table Output s s MER 4 HON 8 EAR ae 74 Compact OUIpUL v ee UI deg org led 74 Printer Output Unit 2x 2 20 8 SH Eo EEG 75 10 4 64 Data Table Directory Terra 75 4 65 Cherenkov Detector Array Definition 75 4 66 Cherenkov Wavelength 76 4 67 Cherenkov Bunch Size Definition 76 4 68 Cherenkov Output 76 4 69 Cherenkov Quantum 76 4 70 Multiple Use of Cherenkov Events 77 4 71 Cherenkov Telescope Dimensions
35. file Lower case characters of HISTDS are not converted to capitals Do not use capitals as the HBOOK routines use only lower case characters The data file name is extended by a string containing 69For photo nuclear interactions the meaning is 0 multi hadron production and vector meson production mixed 1 no vector meson production only multi hadron production 2 only vector meson production no multi hadron production 82 information about projectile target energy and the type of interaction which has been selected At the end of the data file name hbook is appended such that the total data file name would look like HISTO CORSIKA INTTEST p0014t14e100e3 diffractive hbook for a proton projectile on ni trogen target with a lab energy of 100E3 GeV including diffractive events If you want to write into the directory from where you are starting your CORSIKA run you should give HISTDS or HISTDS ablank enclosed in apostrophes or quota tion marks Please keep in mind that in FORTRAN an automatic expansion of UNIX names like home is not possible rather you should give the full expanded name of the directory ending with a character Limit is HISTDS must not begin with a tilde character This keyword is only available in the INTTEST option 4 89 Plot Output PLOTSH PLOTSH Format A6 L Default F PLOTSH If true the track start and endpoints of the electromagnetic muonic an
36. for the hadron shower 2 for the EGSA part 3 for the simulation of Cherenkov photons only for CERENKOV option 4 for the random offset of Cherenkov telescope systems with respect of their nominal positions only for IACT option and 5 for the HERWIG routines in the NUPRIM option Their activation follows the sequence of occurrence of the keyword lines At minimum 2 seeds must be activated The use of ISEED 2 k gt 0 and especially of ISEED 3 k gt 0 should be avoided as presetting the random number generator by billions of calls needs considerable computing time To get different random sequences it is sufficient to modify ISEED 1 k When the eventio and other separate functions are enabled in the IACT option an external random generator may be used Limit to get independent sequences of random numbers is 1 lt ISEED 1 k lt 900 000 000 4 4 Number of Showers NSHOW NSHOW Format A5 D Default 10 NSHOW Number of showers to be generated in a run Limitis NSHOW gt 1 4 5 Primary Particle Definition PRMPAR PRMPAR 1 Format A6 I Default 14 PRMPAR 1 Particle type of the primary particle See Table 4 page 88 for the particle codes Limits are 1 lt PRMPAR 1 lt 5699 Vector mesons resonances and charmed particles are excluded because of their short life time Primary neutrinos can only be used in the NUPRIM option page 41 Instable nuclei with mass number 5 or 8 may be used only with SIBYLL o
37. int if you select the INTTEST option and create the Make files But it will not run make See Sect 11 page 108 for more details SELECTED 2 FINISH checking whether to enable maintainer specific portions of Makefiles no checking build system type x86_64 suse linux checking host system type x86_64 suse linux checking for a BSD compatible install usr bin install c checking whether build environment is sane yes checking for gawk gawk checking whether make sets MAKE yes checking for pgf77 no 1 HDPM DPMJET EPOS NEXUS QGSJET QGSII SIBYLL or VENUS 20fjuka gheisha or 15 king king king king king king king king king king king king king king for Su for Fortran 77 compiler default output file name a out whether the Fortran 77 compiler works yes whether we are cross compiling no for suffix of executables for suffix of object files o whether we are using the GNU Fortran 77 compiler yes whether g77 accepts g yes Tor pO Cg whether we are using the GNU C compiler yes whether cc accepts g yes for cc option to accept ANSI C none needed for style of include used by make GNU dependency style of cc gcc3 It may take a while check
38. lambda field If thinning is used the particle weight is in the photons field When compiling iact c manually instead of taking advantage of the coconut script or the GNU makefile supplied with the bernlohr package an additional option DIACTEXT is required to have a consistent interface on both sides To obtain this program version the IACTEXT option has to be selected together with the CERENKOV and IACT options when extracting the FORTRAN code from the source file 3 4 5 Cherenkov Light Reduction Option The standard simulation of Cherenkov photons does not regard light absorption within the at mosphere telescope mirror reflectivity or quantum efficiency of the detecting photomultiplier tubes In the CEFFIC option these effects are taken into account at an early stage of the Cheren kov photon simulation thus the computing time is shortened considerably and the requirements for storage of Cherenkov output are reduced additionally Data tables containing information on these three effects as function of photon wavelength are needed in this option depending on the status of the flags specified by the keyword page 76 CERQEF Standard tables for atmospheric absorption atmabs dat mirror reflectivity mirreff dat mea sured for the re coated mirrors of the Whipple telescope Sept 1993 and quantum efficiency quanteff dat measured for Hamatsu R1398HA photo multipliers with UV window and 1 125 tube are supplie
39. of the output see Table 6 page 94 remains unchanged but the blocksize is enlarged to a length of 26208 bytes Now a block has 6552 words each 4 bytes long consisting of 21 sub blocks of 312 words The ends of the sub blocks RUN HEADER see Table 7 page 95 EVENT HEADER see Table 9 page 97 LONGitudinal see Table 12 page 100 EVENT END see Table 13 page 101 and RUN END see Table 14 are filled up with zeros while the data blocks Tables 10 and 11 page 99 contain 8 words for each particle rsp Cherenkov bunch the last one being the weight Again 39 particles are collected within one data sub block 10 3 Compact Output The compact particle output available in the COMPACT option Sect 3 5 7 page 38 is or ganized similar to the normal particle output see Sect 10 2 page 94 ff with the following modifications e The block size of the records has variable length In the block structure Table 6 page 94 the event end blocks are omitted completely 750n UNIX installations using the GNU g77 compiler HP UNIX stations and some other machines the blocks comprise two additional words giving the record length 79 Concerning the weight calculation see Sect 3 5 22 page 46 ff 102 e Only the first event header block has its full length 273 rsp 312 4 byte words and starts with the characters EVTH The headers of subsequent events are shortened and contain only the first 12 parameters of Table 9 page 97 and
40. shower axis points to magnetic North for 90 it points to West see Fig 1 page 86 Limits are 360 lt PHIPR i lt 360 5 4 10 Viewing Cone Specifications VIEWCONE VUECON 1 VUECON 2 Format A8 2F Defaults O 0 VUECON Inner limiting angle of viewing cone in 2 Outer limiting angle of viewing cone in 2 The VIEWCONE option see Sect 3 5 24 page 49 selects the direction of primaries in a circu lar cone around the fixed primary direction THETPR 1 and PHIPR 1 page 53 with the inner opening VUECON 1 and the outer opening VUECON 2 The zenith angular dependence of the selected detector geometry is maintained for flat horizontal rsp spherical detectors see Sect 3 5 25 page 49 Limits 0 lt VUECON 1 VUECON 2 lt 90 The generation of showers with angles be yond the range of the program validity is skipped This keyword is only available in the VIEWCONE option 4 zenith angle limitation is recommended for the standard CORSIKA version because of some approxima tions made in subroutine NKG At 0 gt 70 also the curvature of the Earth s surface must be taken into account For large zenith angles you should use the CURVED option page 39 For the CURVED option the limit is 0 lt THETPR lt 90 for the CURVED option combined with the CERENKOV option the limit is 0 lt THETPR lt 88 For the UPWARD option with upward going primary the limits are 110 lt
41. species They are assumed to be completely stripped and therefore counted with their charge Z in the all charged species 100 1 EVTE statistics for one shower 3 weighted number of photons arriving at observation level s 4 weighted number of electrons arriving at observation level s 5 weighted number of hadrons arriving at observation level s 6 weighted number of muons arriving at observation level s 7 number of weighted particles written to particle output file MPATAP This number includes also Cherenkov bunches if Cherenkov output is directed to MPATAP but excludes additional muon information NKGoupu fshedel 2 1 21 lateral distribution in x direction for 1 level in cm i 1 21 lateral distribution in y direction for 1 level in cm 1 1 21 lateral distribution in xy direction for 1 level in cm 1 1 21 lateral distribution in yx direction for 1 level in cm 2 2 2 2 i 1 21 lateral distribution in x direction for 2 level in cm 1 1 21 lateral distribution in y direction for 2 level in cm 1 1 21 lateral distribution in xy direction for 2 level in cm 1 1 21 lateral distribution in yx direction for 2 level in cm 2 2 i 1 10 electron number in steps of 100 g cm i 1 10 pseudo age in steps of 100 g cm i 1 10 distances for electron distribution in cm 1 1 10 local pseudo age 1 level i 1 10 height of levels for electron numbers in g
42. start with the characters EVHW e The data blocks have variable length trailing zeros are omitted They are headed by a 4 byte integer which defines the length in 4 byte words of the appended data block The maximal length is to 1273 4 byte words rsp 1 312 4 byte words for thinning Therefore a special reading routine for this output is necessary The Cherenkov output is not affected by the COMPACT option but it must be directed to the Cherenkov output file MCETAP page 76 LCERFI true 10 4 inclined binary File Output This file is produced in the ROOTRACK version Sect 3 5 18 page 45 which is needed to define an inclined observation plane by the keyword INCLIN Sect 4 54 page 72 The format and structure is identical to the normal binary output data file as described in Sect 10 2 page 94 besides the fact that all coordinates are given within the inclined plane with the origin at the intersection of the shower axis with the inclined observation plane 10 5 Ihbook File Output The optional datnnnnnn lhbook written to the directory DSN see keyword DIRECT page 74 contains histograms produced by the ANAHIST page 36 and or the AUGERHIST page 37 options Do not use capitals in the DSN directory name as the HBOOK routines tolerate only lower case characters Table 15 gives the numbering of the hbook histograms The histograms with numbers 1000 are produced by ANAHIST while those with numbers above come from the
43. system type is UNIX Using binary mode to transfer files ftp cd pub corsika v690 250 CWD command successful ftp gt mget mget corsika 6990 tar gz y ftp quit 221 You have transferred bytes in 4 files 221 Total traffic for this session was bytes in transfers 221 Thank you for using the FTP service on ftp ik fzk de 221 Goodbye For faster transmission we have compressed the corsika 6990 tar file Before using this file first you have to decompress it by applying the gunzip procedure If you are not successful to fetch files from the subdirectory pub corsika v690 because of permission denied or such file or directory then please try to copy the README file located in the subdirectory pub This file has no limited access and should be read able by you If you have copied this README file successfully please send an e mail to lt tanguy pierog kit edu gt or dieter heck kit edu gt The automatic registration of each ac cess to this file from outside gives a hint what to change to enable your access to the CORSIKA files The files belonging to FLUKA are collected in an object file library This library and the necessary data files are distributed by the FLUKA organization for different computers and compiler versions You find further details on the web page http www fluka org The files belonging to the HERWIG code may be downloaded from the web page http hepwww rl ac uk theory se
44. the geometry completely The zenith angle at the entrance into the atmosphere is calculated with it The angles 2 see keyword THETAP page 53 have no meaning and are overridden The keyword IMPACT may be combined with the keywords FIXHEI page 55 FIXCHI page 55 to start the shower before reaching the minimum altitude of the shower axis For showers with zenith angles gt 90 e g initiated by neutrinos page 41 the starting point of the shower rsp the first interaction must be defined by the keywords FIXHEI page 55 or FIXCHI page 55 in this case the observation level page 71 must be chosen preferentially at the top of the atmosphere but at minimum above the starting point of the shower The shower axis must cross the observation level To obtain the UPWARD program version the UPWARD option has to be selected when extract ing the FORTRAN code from the source file 48 3 524 Viewing Cone Option The VIEWCONE option enables the generation of showers within the viewing cone of e g a Cherenkov telescope Around the fixed incidence angle defined by THETPR 1 and PHIPR 1 page 53 a hollow cone is defined with its tip pointing towards the detector The inner and outer limiting angles of this cone are defined by the keyword VIEWCONE page 54 The zenith angular dependence of the chosen detector geometry see Sect 3 5 25 below is maintained for flat horizontal rsp spherical detectors while the VOLUMECORR option i
45. the energy e The third table gives the energy dissipated within the atmosphere specified for various processes Energy contained within y s falling below energy or angular cut ionization energy loss of e energy contained within e falling below energy or angular cuts ion ization energy loss of energy contained within u falling below energy or angular cuts ionization energy loss of hadrons energy contained within hadrons falling below energy or angular cuts energy taken away by v s and the energy sum for each depth bin For m and falling below the energy or angular cuts 1 4 of the energy 15 attributed to the hadronic energy while 3 4 is attributed to neutrinos For the neutral lt this ratios are 1 2 The last bin of the cut energies reflects the energy content of particles arriving at detector level In this table the rest mass of nucleons and electrons is not counted while the rest mass of the corresponding anti particles which might undergo annihilation is counted twice Energies of unstable hadrons and muons are added up including their rest mass This counting is necessary to respect the target nucleons or electrons involved into the shower development thus enabling a correct energy balancing For writing out the longitudinal tables to DAT nnnnnn long file or as LONG blocks to the particle output DATnnnnnn see the FLONGOUT flag page 69 The control printo
46. they are established in a time consuming procedure some 100 h on a DEC 3000 600 AXP with 175 MHz e The more recent QGSJET II 03 routines need some parameterized data contained within the data files ggsdat II 03 and sectnu 1I 03 QGSJETOIc routines need some pa rameterized data contained within the data files QGSDATO01 and SECTNU They will be generated at the first call within that directory from where you are calling CORSIKA 19 This generation is time consuming 4 days on a 1GHz Pentium LINUX or DEC ALPHA 1000 XP for QGSJET II 03 rsp 30 h on DEC 3000 600 AXP with 175 MHz for QGSJETO1c Later calls will read in these data files ggsdat II 03 and sectnu II 03 rsp OGSDATOI and SECTNU These data files are written and read via logical units 1 and 2 Attention The qgsdat 11 03 file will have a size of zz 131 MB e The STACKIN option needs the parameters type energy momenta of the secondary particles coming from the interaction of an exotic primary in a separate file Its file name is specified by the keyword INFILE page 56 The first line of the file contains for mat free after a leading blank the number of secondaries and the primary energy GeV The following lines contain the current particle number the particle type the energy GeV the longitudinal momentum and the two transverse momenta GeV c in the for mat 215 4 1 15 7 The momenta are relative to the direction of the exotic primary defined by TH
47. 0120 97 33 0 1100 0 5 06583365 10 4 755 56438 725247 87 1365 core Table 34 Parameters of the average Malarg e Argentina summer atmosphere 0 8 0 149 305029 1196 9290 985241 10 8 0 13 0 59 771936 1173 2537 819245 00 13 0 33 5 1 17357181 1502 1837 611220 86 33 5 1100 0 5 03287179 10 4 750 89705 725797 06 51 to Table 35 Parameters of the average Malarg e Argentina autumn atmosphere Keilhauer s U S standard atmosphere 0 7 0 149 801663 1183 6071 954248 34 70 114 57 932486 1143 0425 800005 34 11 4 37 0 0 63631894 1322 9748 629568 93 37 0 1100 0 4 35453690 107 655 67307 737521 77 St 15 Table 36 Parameters of the U S standard atmosphere after Keilhauer 126 References 1 2 3 4 5 6 10 11 12 13 14 T Antoni et al KASCADE Collaboration Nucl Instr Meth 513 2003 490 K H Kampert et al KASCADE Grande Collaboration Nucl Phys B Proc Suppl 122 2003 422 G Navarra et al KASCADE Grande Collaboration Nucl Instr Meth A 518 2004 207 D Heck et al Report FZKA 6019 1998 Forschungszentrum Karlsruhe http www ik fzk de corsika physics_description corsika_phys html J Ranft Phys Rev D51 1995 64 preprint hep ph 991 1213 and hep ph 991 1232 1999 J N Capdevielle et al Report KfK 4998 1992
48. 2 selects code which enables plotting the tracks of the electromagnetic muonic and hadronic particles to demonstrate the development of a shower optically avoiding the large out put files of PLOTSH PRESHOWER selects routines for coupling with a C program package to describe the interac tion of primary gammas with the Earth s magnetic field at EeV energies and to treat the resulting swarm of em particles falling onto the top of atmosphere as one shower ROOTOUT selects routines for writing the particle output in a root file e g for off line analysis of the particle output by root routines COAST package ROOTRACK selects routines for writing the particle output arriving in an inclined observation plane to the DATnnnnnn inclined binary by routines of the COAST USER LIB package It is also necessary for simulating radio emission with REAS 25 SLANT selects a slant depth scale for the longitudinal distributions instead of the vertical depth scale used otherwise STACEE selects C routines to write the Cherenkov output in the format which is in use with the STACEE experiment 26 10 STACKIN selects code to read in the parameters type energy momenta of secondary parti cles resulting from the interaction of an exotic primary WIMP which has been treated off line by a separate program TAULEP selects code for the explicite treatment of the 7 lepton rsp the 7 neutrinos in con nection with the NEUTRINO or NUPRIM option
49. 3 4 7 Slope of Spectrums 22 s 29 oto es EE og Ux e 53 4 8 Zenith Angle Definition uu o9 EG OU eh we Te een 53 49 Azimuth Angle Definition 54 4 10 Viewing Cone Specifications 54 11 Starting i oce erue dere dee derer trete 55 4 12 Starting Point of Arrival Timing 55 413 First Interaction Definition 55 de Skimming INCIDENCE gt 2 5 ae M e IR 56 4 15 Stack Input File Name 56 4 16 Atmospheric Model Selection 57 4 17 Atmospheric Parameters 57 4 18 Atmospheric Parameters 0 58 4 19 Atmospheric Parameters 0 58 4 20 Atmospheric Layer lt 58 iv 4 21 4 22 4 23 4 24 4 25 4 26 4 27 4 28 4 29 4 30 4 31 4 32 4 33 4 34 4 35 4 36 4 37 4 38 4 39 4 40 4 41 4 42 4 43 4 44 4 45 4 46 4 47 4 48 4 49 4 50 4 51 4 52 4 53 4 54 4 55 4 56 4 57 4 58 4 59 4 60 4 61 4 62 4 63 External Tab lated 58 Earth s Magnetic Field 59 Experiment Coordinates for Pre showering 59 DPMJET Selection Flag 60 DPISIG S lection Flag ee T
50. 82 LINUX 8 29 LPM 31 41 MAC 12 NEUTRINO 41 NEXUS 26 62 115 NOCLONG 36 69 103 NUPRIM 41 116 OLDDATE 11 OLDDATE2 11 PLOTSH 42 83 PLOTSH2 23 42 83 PRESHOWER 44 59 116 QGSJET 27 63 QGSJETOLD 28 QGSII 27 63 ROOTOUT 44 ROOTRACK 45 SIBYLL 28 63 SLANT 45 STACEE 36 116 STACKIN 20 45 TAULEP 46 THIN 46 67 102 TIMERC 12 116 UNIX 11 UPWARD 48 URQMD 30 80 115 117 VENUS 28 64 VIEWCONE 49 54 VOLUMECORR 49 VOLUMEDET 49 131 Index Steering Keywords ARRANG 73 ATMA 57 ATMB 58 ATMC 58 ATMLAY 58 ATMOD 57 ATMOSPHERE 58 CDEBUG 81 CERARY 75 CERFIL 76 CERQEF 76 CERSIZ 76 COMOUT 74 CSCAT 77 CURVOUT 72 CWAVLG 76 DATBAS 78 DATDIR 75 DEBUG 79 DETCFG 73 DIFOFF 82 DIRECT 74 DPJSIG 60 DPMJET 60 ECTMAP 74 ECUTS 68 EGSDEB 79 ELMFLG 66 EMADDI 70 EPOPAR 61 EPOS 60 EPOSIG 61 ERANGE 53 ESLOPE 53 EVTNR 51 EXIT 84 FIXCHI 55 FIXHEI 55 FLATOUT 72 FLUDBG 79 GCOORD 59 GHEIDB 80 HADFLG 65 HILOW 65 HISTDS 82 HOST 79 IMPACT 56 INCLIN 72 INFILE 56 INTDEC 81 INTSPC 81 INTTST 81 LONGI 69 MAGNET 59 MAXPRT 73 MUADDI 71 MUMULT 70 NEXPAR 62 NEXSIG 62 NEXUS 62 NSHOW 52 OBSLEV 71 OUTPUT 75 PAROUT 74 PHIP 54 PLAXES 83 PLCUTS 83 PLOTSH 83 PRMPAR 52 PYTHIA 80 QGSJET 63 QGSSIG 63 RADNKG 67 RUNNR 51 SEED 52 SIBSIG 64 SIBYLL 63 STEPFC 66 132 TELESCOPE 78 TELFIL 78 THETAP 53 THIN 67 THINEM 68 THINH 67 TIMLIM 69 TRIGGER 82 TSTART 55 URQMD 80 USER 78 VENPAR 64 VENSIG 64 VEN
51. AR parcha Format A74 Defaults parcha Command line to be read by subroutine aread of program block nexus bas f The possible command lines are described in the NEXUS documentation Use lower case characters Lower case characters of parcha are not converted to capitals Do not use the commands appli cation set nevent run or stop within your input parameters these will cause unpredictable results or crashes Only nexus inix names might be changed by standard users This keyword is only available in the NEXUS option 4 34 NEXSIG Selection Flag NEXSIG FNEXSG 51 typical NEXPAR input looks like NEXPAR fname inics corsika 6990 nexus nexus inics NEXPAR fname iniev corsika 6990 nexus nexus iniev NEXPAR fname inirj corsika 6990 nexus nexus inirj NEXPAR fname corsika 6990 nexus nexus initl NEXPAR fname check corsika 6990 nexus nexus check NEXPAR fname histo corsika 6990 nexus nexus histo for interaction test only NEXPAR fname data corsika 6990 nexus nexus data for debugging only NEXPAR fname copy corsika 6990 nexus nexus copy for debugging only NEXPAR fname log corsika 6990 nexus nexus log for debugging only NEXPAR printcheck screen for debugging only 62 Format L Default T FNEXSG If true the NEXUS high energy hadronic cross sections are used If false the default cross sections as described in Ref 3 are used This keyword is only available in the NEXUS opti
52. AUGERHIST option If both options are selected both series of numbers appear in parallel without interferences Both series of histograms are added up for many showers and normalized correctly before writing them to output The AUGERHIST histograms are produced for up to 20 levels to be specified by the keyword OBSLEV page 71 which are denoted by ii with 01 lt ii lt 20 and for various particle types denoted by jj with 00 lt jj 04 with the meaning 00 gamma 01 electron 02 positron 03 muon 04 hadron 10 6 long File Output The optional file DAT nnnnn long written to the directory DSN keyword DIRECT page 74 contains a table of the longitudinal distribution of various particle numbers arranged in the columns depth y e u u hadrons charged particles nuclei Cherenkov photons In a second table the longitudinal distributions of energy deposit in GeV by various par ticle species are given in columns depth energy cut ionization energy cut 80The Cherenkov photon longitudinal distributions are influenced by selecting the preprocessor options INTC LONG and NOCLONG page 36 see also page 70 and AUGCERLONG page 37 103 histo number dimension content of histograms 1 28 1 dim longitudinal distributions 99 2 dim particle codes vs log10 r 101 331 1 dim ground particle distributions 341 451 2 dim ground particle distributions 999 1 dim density normalization 1011 1 dim la
53. D Heck et al KASCADE Collaboration Proc 27 Int Cos mic Ray Conf Hamburg Germany 2001 233 J Knapp et al Astropart Phys 19 2003 77 D Heck M Risse and J Knapp Nucl Phys B Proc Suppl 122 2003 40 22 D Heck Nucl Phys B Proc Suppl 151 2006 127 23 J Knapp and D Heck Report KfK 5196B 1993 Kernforschungszentrum Karlsruhe for an up to date version see http www ik fzk de corsika usersguide corsika_tech html 24 R Brun D Lienhart HBOOK User s Guide CERN Program Library Y250 1987 25 M Ludwig and T Huege Astropart Phys 34 2011 438 26 Covault et al Proc 27 Int Cosmic Ray Conf Hamburg Germany 2001 2810 27 N N Kalmykov S S Ostapchenko and Alekseeva Proc 26 Int Cosmic Ray Conf Salt Lake City USA 1 1999 419 28 Application Software Group GEANT CERN Program Library 1994 29 R E Cassell and G Bower SLAC private communication 2002 30 R L Ford and W R Nelson Report SLAC 210 1978 Stanford Linear Accelerator Cen ter 128 31 J R Cudell et al PAys Rev D61 2000 034019 32 H Burkhardt S R Kelner and R P Kokoulin Report CERN SL 2002 016 AP 2002 CERN Geneva 33 S Martinez et al Nucl Instr Meth A357 1995 567 34 K Bernl hr internal report MPI Heidelberg 1998 unpublished Astropart Phys 12 2000 255 Astropart Phys 30 2008 149 35 see e g Numerical Recipes W H Press et al
54. ENKOV option and links with compiled iact c routines of the bernlohr package IACTEXT selects code for extended interfacing with the iact c routines of the bernlohr pack age This option is only available in connection with the IACT CERENKOV option INTCLONG selects the longitudinal distribution of Cherenkov photons in longitudinally inte 9 grated form The default gives the generation of photons step so called differential longitudi nal distribution INTCLONG excludes the NOCLONG option This option is only available in connection with the CERENKOV or AUGCERLONG option INTTEST selects special features for the test of the interaction models needs routines of the HBOOK and ZEBRA packages 24 This option is not suited for extensive air shower simu lation LPM selects those EGS4 routines which include the LPM effect but without using the THIN option NEUTRINO selects code by which neutrinos emerging from pion kaon and muon decays are tracked explicitly but without interaction NOCLONG deselects the longitudinal Cherenkov photon distribution NOCLONG excludes the INTCLONG option This option is only available in connection with the CERENKOV or AUGCERLONG option NUPRIM selects the HERWIG code to treat the first interaction of a primary neutrino PLOTSH selects code which enables plotting the tracks of the electromagnetic muonic and hadronic particles to demonstrate the development of a shower optically PLOTSH
55. ETAP page 53 and PHIP page 54 e The VENUS option reads the file VENUSDAT which contains parameterized structure function integrals and is 2051 lines long The file is read via logical unit 14 e The FLUKA option needs various data files from the FLUKA library so you should set an environment variable pointing to the FLUKA library e The URQMD option looks for the existence of the tables dat decay width file If this file exists it is read in otherwise the decay width tables are calculated and this file is created e The ATMEXT option needs tabulated atmosphere input data of the MODTRAN model contained in the atmprofi dat files which are read in by the atmo c routines of the bernlohr package Details are given in the comments at the beginning of atmo c and in the documentation supplied with the bernlohr package e The CEFFIC option reads the atmospheric absorption table atmabs dat photomultiplier quantum efficiency table quanteff dat and or mirror reflectivity table mirreff dat via logical units MCERABS by default 20 MCERQEF by default 21 and MCERMIR by default 22 respectively e Besides these data files CORSIKA needs the input of steering keywords to select the subject and the parameters of the simulation They have to be supplied by the user They are read via logical unit MONIIN MONItor INput by default 5 The format of the steering keywords and their effect is described in detail in Sect 4 page 51 ff Example
56. EUKA Orig crest a SERE RU RC Ge ae at AG 30 2 AGE ISAO DOM hte p S ht o e Sv So aS 3 23 UROMD Option seios grs Electromagnetic Interactions NKG EGS4 Option NKG Treatment 373 5424 N AGE ae ae 24 3 3 2 4 Treatment 52 he a PE Cherenkov Options 3 4 1 Cherenkov Standard Option 3 4 2 Cherenkov Wavelength 3 4 3 Imaging Atmospheric Cherenkov Telescope Option 3 4 4 Imaging Atmospheric Cherenkov Telescope Extension Option 3 4 5 Cherenkov Light Reduction Option 346 INTCLONG and NOCLONG 34 7 Option 52522536584 on Other Non standard Options ANAHIST Option xx E VO 3 5 2 Option with External Atmospheres 3 5 3 AUGCERLONG Option 354 AXUGERHIST ser a a n 3 5 5 AUGERINFO Option iii 9 16 TCHARM 04 vue quw rer Ela 38 3 5 7 COMPACT Output 38 3 5 8 CURVED Atmosphere Option 39 3 3 9 5 ELS TORY 35509 eet e e e fs 40 3 5 10 INTTEST Interaction Test
57. F file contains some explanations the main program with more than 115 subroutines and functions the EGS4 routines the NKG routines the HDPM model routines the interface routines to FLUKA GHEISHA UrQMD DPMJET EPOS NEXUS QGSJET SIBYLL and VENUS the special routines for Cherenkov light generation the routines for generation of Auger oriented histograms and the interaction test routines It is about 68600 lines long The corsika h file length about 4400 lines contains the general common blocks with their explanations These common blocks are included into the source file during preprocessing The C file timerc c contains a date and time routine timerc for those UNIX or LINUX systems where the more modern date system routine is not available The files preshw c and stacee c contain the PRESHOWER C routines and the STACEE C routines The gheisha_2002d f q95sjet 11 03 f qgsjetOlc f sibyll2 1 f and venus f routines are about 18200 12200 7500 8100 and 18000 lines respectively Because of its size the DPMJET code has been divided into 4 portions dpmjet253c f dpmjet 254 f dpmjet255c f and dpmjet256c f with 42400 2300 41900 and 30000 lines each in the dpmjet subdirectory The 30 UrQMD 1 3 cors program files with the 12 include files are collected within the urqmd 1 3_cors tar gz file in urqmd subdirectory The 21 EPOS program files with the 6 include files and the 5 data files are collected within the e
58. IBSIG Selection Flag SIBSIG FSIBSG Format L Default T FSIBSG If true the SIBYLL high energy hadronic cross sections are used If false the default cross sections as described in Ref 3 are used This keyword is only available in the SIBYLL option 4 36 VENUS Selection Flag VENUS FVENUS ISHOO Format A5 L I Defaults T 0 FVENUS If true the VENUS routines are used to treat the high energy hadronic interactions If false routines are used to treat the high energy hadronic interactions ISHOO Determines the amount of debug output for VENUS routines With increasing num ber ISHOO gt 90 the output becomes more and more detailed This output appears on the unit MDEBUG For more information look into the listing of subroutine venini Limits are 0 lt ISHOO lt 98 This keyword is only available in the VENUS option 4 37 VENUS Parameters VENPAR PARCHA 1 PARVAL 1 Format F Defaults 0 PARCHA Name of VENUS parameter to be changed 7 New value of VENUS parameter to be changed A maximum of 2 100 VENUS parameters may be set by the user in arbitrary sequence The available names and their meaning may be taken from the listing of subroutine venini The VENUS parameters should not be changed by standard users This keyword is only available in the VENUS option 4 38 VENSIG Selection Flag VENSIG FVENSG Forma
59. IM version of the corsika_compile file f the HERWIG C INC include file should be available in the subdirectory from which you are calling the compiler to include it into the CORSIKA HERWIG linking routines at the ap propriate places Alternatively you may use the f77 rsp g77 compiler with the option I herwig to indicate the compiler where to find the include file This include file is a simple copy of the HERWIGnn INC file provided with the source code of the HERWIG model In the herwig subdirectory you give the command cp HERWIGnn INC HERWIG C INC Before compiling the HERWIG routines you should e remove erase or comment off the function HWRGEN with entries HWRSET and HWR GET thus using the CORSIKA random generator sequence 5 within the HERWIG rou tines e when using the NUPRIM option together with NEXUS or EPOS Rename the COMMON JET within Herwig The compiler procedures of the standard case see begin of this subsection A 1 should be used for the CORSIKA NUPRIM version as well as for HERWIG C file If you have specified the the PRESHOWER or the STACEE option you need the compilation of the C file timerc c preshw c or stacee c using a command like timerc e rsp cc c preshw c or cc c stacee c For the compilation of the C routines of the bernlohr package see the instructions delivered with the bernlohr package A 2 Linking For linking of most CORSIKA versions t
60. KARLSRUHER INSTITUT F R TECHNOLOGIE KIT Extensive Air Shower Simulation with CORSIKA A User s Guide Version 6 99x from August 8 2011 D Heck and T Pierog Institut f r Kernphysik KIT Universit t des Landes Baden W rttemberg und nationales Forschungszentrum in der Helmholtz Gemeinschaft Copyright Notice Copyright and any other appropriate legal protection of these computer programs and associ ated documentation reserved in all countries of the world These programs or documentation may not be reproduced by any method without prior written consent of Karlsruhe Institute of Tchnology or its delegate The Karlsruhe Institute of Tchnology welcomes comments concerning the CORSIKA code but undertakes no obligation for maintenance of the programs nor responsibility for their correct ness and accepts no liability whatsoever resulting from the use of its programs Trademark notice All trademarks appearing in this CORSIKA GUIDE are acknowledged as such Abstract Extensive Air Shower Simulation with CORSIKA A User s Guide CORSIKA is a detailed simulation program for extensive air showers initiated by high energy cosmic particles The user s guide explains the installation of the code all the necessary input data sets the selection of simulation parameters and the structure of the program outputs Zusammenfassung Simulation ausgedehnter Luftschauer mit CORSIKA Eine Benutzeranleitung CORSIKA ist ein Programm zu
61. LEP option by P Abreu LIP Lisboa is acknowledged 111 112 A Compilation and Linking Using the coconut script it will call make automatically and nothing has to be done But for expert people who want to do their own Make file a description of what has to be done is given in this appendix A 1 Compilation After running coconut asking not to compile at the end of the selection process you get a source file corsika V ER OS HIGH low compilefile f in the src subdirectory This subdirectory is the working directory for the following commands This corsika_compile file f FORTRAN file and the dpmjet251 f eposx f nexus xxx f qgsjet I1 03 f rsp qgs jetOlc f sibyll2 1 f venus f and gheisha_2002d f sources and or the urgmd FORTRAN files have to be compiled before linking them together to obtain an executable module To prevent overwriting of local variables by optimization of some compilers SAVE statements which re place the static option to be used for the previous release have been implemented throughout in the FORTRAN files of corsika_compilefile f gheisha_2002d f dpmjet25i f qgsjet 11 03 f rsp qgsjetOlc f sibyll2 1 f and venus f It is recommended to use the bounds check option for first trials to inhibit uncontrolled array operations outside the allowed index range e For DEC UNIX machines the procedure looks like f77 c check bounds Slat 2 gt 1 err This means Suppress the loading phase gen
62. OCK DATA subprograms Table 1 lists all units together with their default values and the corresponding file names 23 3 Program Options 3 1 High Energy Hadronic Interaction Models 3 1 1 DPMJET Option DPMJET 4 Dual Parton Model with JETs is a program developed to describe high energy hadronic interactions of hadron nucleus and nucleus nucleus collisions using the two compon ent Dual Parton Model with soft chains and multiple mini jets at each elementary interaction For CORSIKA the version DPMJET 2 55 is available For using DPMJET you first have to select the DPMJET option when extracting the FOR TRAN code from the source file The Makefile will automatically compile dpmjet253c f dpmjet254 f dpmjet255c f dpmjet256c f together in a library 2bdpm a and then link it with the compiled gheisha_2002d f code rsp UrQMD library and with your CORSIKA program In your input file you may supply the keyword page 60 DPMJET 0 Setting DPMJET to false F the simple routines are used see also Sect 3 1 3 page 26 If in your calling directory the data set pomtab dat is not yet existent it will be calculated at the first call of subroutine prblm2 of dpm jet256 f which takes 20 min on a DEC 3000 600 AXP with 175 MHz The DPMJET option needs about the same CPU time as the VENUS option NKG enabled EGS4 disabled at primary energies of 10 eV Technically it is possible to use DPMJET up to the highest ener
63. OT use the expert mode coconut expert KKKK You are using the cached configuration from include config h To turn off this you may use the no cache option kkkxkxkxkxkxkxkxkxkxkxkkkxkkkxkkkxkkkxkxkxkxkxkkxkkkxkkkxkkkxkkkkkkkkkkkxkkkxkkkkxkkkxkkkkxkxkkxkxkkkxkkkxkxkkkxx k Which high energy hadronic interaction model do you want to use 1 DPMJET 2 55 2 NEXUS 3 3 QGSJET 01C enlarged commons CACHED 4 OGSJET II 5 SIBYLL 2 1 6 VENUS 4 12 7 EPOS restart make x exit make only one choice possible 3 SELECTED QGSJET Answer the questions to select the options you want to use in CORSIKA see Sect 2 2 1 page 7 and Sect 3 page 24 for details Press Enter to select the options marked by CACHED After each question you can choose to restart the installation at the first question or to stop now x If an option needs some other files the installation program will test if they exist If a problem occurs the installation program w
64. Option 40 LPM Option ek e De 41 3 5 12 NEUTRINO Option 41 3 5 13 NUPRIM Option for Primary Neutrinos 41 3 5 14 PLOTSH Shower Plot Production Option 42 3 5 15 PLOTSH2 Shower Plot Production Option 42 3 5 16 PRESHOWER Option 44 3 5 17 ROOTOUT ODD ui eene to 44 323 18 ROOTRACR Option 55 HUS ee 45 3955 19 SEAN Oplom Vader xr dex Pr PEN a 45 3 5 20 STACKIN 45 39215 TAULEP ODLUBB 5 ectetur etre ette ed dir re Arsch 46 3 3 22 Option for Thinning ceu wen OUR EIUS 4 BASED a 46 3 5 23 UPWARD Option 6 ue ee 9 48 3 5 24 Viewing Cone 40 3 5 25 Volume Detector and Vertical String Geometry Options 49 3 6 Combination of Options 50 Steering of the Simulation 51 Ask R n NUTHDSE s uo uuu Ex eut Een Er EEE DER PIE xe 51 First Event Number um or SEO CR oe ACE E 51 4 3 Random Number Generator Initialization 52 do Number of Shower e des secet tbat EHE AS 32 4 5 Primary Particle Definition 52 4 6 Energy Range I XO RR se EX 5
65. README corsika file inside a subdirectory run to be used to run CORSIKA containing 14 data sets containing the energy dependent cross sections for nucleon nucleus processes NUCNUCCS for electromagnetic interactions 6 sets EGSDAT6_x x for QGSJETO1 QGSDATO01 and SECTNU for QGSJET II sectnu 1I 03 because of its size the ggsdat II 03 file has to be downloaded separately and copied here numerical data to be used by the VENUS routines VENUSDAT cross section ta ble for UrQMD UrQMD VER xs dat and for the DPMJET routines the Glauber tables GLAUBTAR DAT and nuclear data NUCLEAR BIN 3 data sets atmabs dat mirreff dat and quanteff dat to take into account the atmo spheric absorption mirror reflectivity and quantum efficiency of Cherenkov radia tion 6 input examples all inputs nexus inputs and epos inputs to steer the simulation with any model with out thin and stackin with NEXUS or with EPOS epos199 cors tar gz is automatically extracted if needed nexus3 97_cors tar gz is automatically extracted if needed 6This file is in a binary format and is only available for LINUX machines on the CORSIKA ftp server Users of other systems should let the computer recalculate this file at the first run It takes about one day of computing time The NUCLEAR BIN file may be used only with those computers DEC UNIX LINUX applying the IEEE standard for direct access read and write For other computers DEC VA X HP
66. RMIR If true the mirror reflectivity of Cherenkov telescopes is taken into account It needs reading in the mirreff dat file Respecting these effects at an early stage of the Cherenkov photon simulation drastically re duces computing time and storage requirements for Cherenkov photon output For the influence onto the longitudinal distribution of Cherenkov photons see Sect 3 4 5 page 35 and keyword LONGI page 70 This keyword is only available in the CEFFIC option together with the CERENKOV option 4 70 Multiple Use of Cherenkov Events CSCAT ICERML XSCATT YSCATT Format AS I 2F Defaults 1 0 0 ICERML Number of uses of each event XSCATT Maximum scattering of core location in X direction in cm See Sect 3 4 1 page 32 ff YSCATT Maximum scattering of core location in Y direction in cm See Sect 3 4 1 page 32 ff Limits are 0 lt ICERML lt 20 XSCATT YSCATT gt 0 In case of IACT option Cherenkov telescopes ICERML telescope arrays are simulated ran domly see keyword SEED page 52 in the specified area which is a circle of radius XSCATT if YSCATT 0 or within a rectangle of area 2 XSCATT 2 YSCATT This keyword is only available in the CERENKOV option 4 71 Cherenkov Telescope Dimensions TELESCOPE X X 2 R Format A9 4F X Y Z Coordinates of Cherenkov telescope in cm relative to the center of the observation level This keyword adds a new telescope at position X Y 2 with radi
67. S option 50 typical EPOPAR input looks like EPOPAR fname inics corsika 6990 epos epos inics EPOPAR fname iniev corsika 6990 epos epos iniev EPOPAR fname inihy corsika 6990 epos epos inilb EPOPAR fname inirj corsika 6990 epos epos inirj EPOPAR fname initl corsika 6990 epos epos initl EPOPAR fname check corsika 6990 epos epos check EPOPAR fname histo corsika 6990 epos epos histo for interaction test only EPOPAR fname data corsika 6990 epos epos data for debugging only EPOPAR fname copy corsika 6990 epos epos copy for debugging only EPOPAR fname log corsika 6990 epos epos log for debugging only EPOPAR printcheck screen for debugging only 61 4 29 NEXUS Selection Flag NEXUS FNEXUS ISHON Format A5 L I Defaults T 0 FNEXUS If true the NEXUS routines are used to treat the high energy hadronic interactions If false routines are used to treat the high energy hadronic interactions ISHON Determines amount of debug output for the NEXUS routines With increasing number ISHON gt 0 the output becomes more and more detailed This output appears on the unit MDE BUG For more information look into the NEXUS documentation Additional debugging is effec tive by setting print parameters using NEXPAR print This debug output is written to the ifch file see Table 1 page 21 Limits are 0 ISHON lt 9 This keyword is only available in the NEXUS option 4 30 NEXUS Parameters NEXP
68. SJETOlc you have downloaded the PYTHIA 6 412 package from the PYTHIA web page to the pythia subdirectory 3 5 7 COMPACT Output Option The standard output of CORSIKA is not adequate when simulating a large number of showers initiated by primaries of so low energies that only a small percentage of them produces particles arriving at the detector level As most Data blocks of the MPATAP file would be filled up with Zeros a large amount of useless information for the Data blocks and the unnecessary overhead 38 of the Event Header and Event End blocks would be written in this case This is avoided in the COMPACT option which writes out only the Run Header and the full Event Header for the first event For subsequent events only shortened Event Headers the first 12 parameters are written Event End blocks are omitted completely the Run End block is written as usual The Data blocks have a maximal length of 39 particles trailing zeros are suppressed Further details are given in Sect 10 3 page 102 As the NKG parameters are not written out in the COMPACT version the NKG flag keyword ELMFLG page 66 should be disabled The COMPACT option cannot be combined with the ROOTOUT and ROOTRACK option To obtain this program version the COMPACT option has to be selected when extracting the FORTRAN code from the source file 3 5 8 CURVED Atmosphere Option The standard CORSIKA program models the Earth s atmosphere as a flat disc where the densit
69. Soy ew C as 60 EPOS Selection Flag 4 8a au NOSE DER LS XS REUS OL 60 EPOS Parameters lt lt lt gt Det ee o RO cR REOS x 61 EPOSIG Selection Flag 25 Se re aru wa 61 NEXUS 62 NEXUS 5 5 retur dir end do Back diee dein d 62 NEXSI Selection Flag 2 oed oed ete ee xe x REX 62 OOGSIET Selection Flag 2 2 3205 HON a ARROW XE 63 QGSSIG Selection Pag ud ee exe we EHE ex urs 63 SIBYLL 63 SIBSIG Selection Flag sa kur ss ee ee EA 64 VENUS Selection EIQUE qu uo uL oq uo le o dora dao decia dade 64 WEIN US Parameters 4 SE NEBEN nf ed RU 64 VENSIG Selection Has ar 2 wa vx ERE EN dr 64 Interaction Parameters amp 65 Transition Energy between 65 Electromagnetic Interaction Steering 66 Electron Multiple Scattering Length Factor 66 Radius of NKG Lateral Range 67 Thinning 67 Hadronic Thinning 67 Electromagnetic Thinning 68 Enere y one ee eSB AI e ORE de ar ee Br e 68 Time Cut Off es ce eee
70. T page 74 via output unit MTABOUT TABle OUTput by default 46 nnnnnn is the run number specified in the keyword RUNNR page 51 To be activated by the keyword PAROUT page 74 Further details on this file are given in Sect 10 7 page 104 The longitudinal distribution of particle numbers and energy deposits can be written out to the file DAT nnnnnn long onto the output directory DSN keyword DIRECT page 74 via the unit MLONGOUT LONGitudinal OUTput by default 48 nnnnnn is the run number specified in the keyword RUNNR page 51 This output is activated by the FLONGOUT flag see keyword LONGI page 69 Further details on this file are given in Sect 10 6 page 103 Another optional output file contains the compressed information of the Cherenkov pho tons It gets the file name C E Rnnnnnn and is written onto the output directory DSN keyword DIRECT page 74 via output unit MCETAP CErenkov TAPe by default 91 nnnnnn is the run number specified in the keyword RUNNR page 51 Renaming this output to DATnnnnnn txt and redirecting it to the directory specified by the keyword DI RECT is convenient as by the shell commands dir or Is all files belonging to one run are displayed consecu tively which facilitates book keeping 26 read this data set the FORTRAN programs corsikaread f rsp corsikaread thin f placed in the s rc directory may be used 22 e To establish a summary file on the contents of an ai
71. TAULEP excludes the CHARM option THIN selects the thinning mechanism to reduce the computing time for full simulations espe cially for EGS4 and activates the LPM effect UPWARD selects code to treat upward going particles This option treats particles in the up ward direction zenith angle gt 90 VIEWCONE selects the primary direction to come from a cone around a fixed zenith and az imuth angle VOLUMECORR selects the angular dependence of the zenith angle distribution as it is needed for a vertical long string detector e g AMANDA see page 49 The default takes the zenith angle distribution as observed by a horizontal flat detector VOLUMEDET selects the angular dependence of the zenith angle distribution as it will be observed by a volume detector e g Cherenkov telescope see page 49 The default takes the zenith angle distribution as observed by a horizontal flat detector The major part of the program is machine independent due to the restriction to FORTRAN stan dards Nevertheless there are a few points where computer specific adaptations were necessary There are prepared options for PCs and work stations running under UNIX also LINUX and for Apple Macintosh computers The versions are automatically activated for the following options UNIX selects code for calculation on UNIX systems including derivatives like LINUX e g DEC station under ULTRIX ALPHA station under DEC UNIX Tru64 2Thanks to con figu
72. TEPFC 1 0 See also the comments in Sect 4 42 page 66 A detailed discussion on the use of this step length is given in 30 In the standard version treating pair production and bremsstrahlung the EGS4 routines do not regard the Landau Pomeranchuk Migdal LPM effect which should be applied at energies 35These pseudo age parameters should only be used qualitatively For scientific applications you extract better age parameters from a fit to the lateral distribution of the electrons as simulated by the EGS4 option 3l above E gt 10 6 eV The LPM effect is switched on automatically using the THIN option see Sect 4 44 page 67 or the LPM option see Sect 3 5 11 page 41 The files named EGSDAT6_x x replace the files EGSDATS5 x x EGSDAT4_x x EGSDAT3_x x EGSDAT2_x x or EGSDATA used in older CORSIKA versions For the extrapolation to the highest energies the photo nuclear cross section is extrapolated according to Cudell et al 31 published by the Particle Data Group The low energy threshold of these files ranges from 0 05 MeV to 3 MeV They differ from the older data sets by the arrangements of the tables con taining the e branching ratios and Y branching ratios thus giving a more smooth branching ratio for the rare processes of electro nuclear and photo nuclear interactions rsp of u u pair formation 32 A data set with an energy threshold far below ELCUT 4 implies the explicit but unnecessary production of many bremsstr
73. THICKO see above is taken for starting the internal clock Additionally the ionization energy loss deflection within the Earth s magnetic field and the generation of Cherenkov pho tons is enabled for charged hadronic or muonic primaries on their path between entering the atmosphere and the first interaction which otherwise is disabled in the standard version for the CURVED and SLANT options see page 39 rsp 45 For TMARGIN true the height of the first interaction is written negative to element 7 of the event header block This keyword is not available in the CURVED SLANT or STACKIN options TMARGIN is set true by default in the CURVED SLANT and IACT options but it may be overridden in the IACT option 4 13 First Interaction Definition FIXHE FIXHE 15 Format A6 F D Defaults 0 0 FIXHEI Fixes the height in cm of the first interaction of hadronic primaries rsp the start ing altitude for em particles for all showers in a run If FIXHEI 0 the height of the first interaction is varied at random according to the appropriate mean free path In case of unstable hadronic primaries and fixed height the first interaction will not be a decay The fixed height must be above the lowest observation level If FIXHEI gt 0 is set the starting altitude of the primary is not effective see Sect 4 11 above 35 In the CURVED option the keyword FIXHEI cannot be used for em primary particles I
74. Table 23 Parameters of the 1014 atmosphere October 14 1993 195 84842 12104 970276 71 997323 1103 8629 820946 0 3378142 1215 3545 639074 5 48224 1074 629 7611 731776 5 Se 1 3 Table 24 Parameters of the AT1224 atmosphere December 24 1993 122 South pole Altitude km a g cm bi g cm 1 EU 137 656 1130 74 867358 37 9610 1052 05 741208 0 222659 1137 21 633846 0 000616201 442 512 759850 2 3 4 er Table 25 Parameters of South pole atmosphere for March 31 1997 MSIS 90 E bi lem 163 331 1183 70 875221 65 3713 1108 06 753213 0 402903 1424 02 545846 0 000479198 207 595 793043 Sin 1 30 Table 26 Parameters of South pole atmosphere for Jul 01 1997 MSIS 90 E 142 801 1177 19 861745 70 1538 1125 11 765925 1 14855 1304 77 581351 0 000910269 433 823 775155 0 00152236 71005699 10 Table 27 Parameters of South pole atmosphere for Oct 01 1997 MSIS 90 E 123 i 128 601 1139 99 861913 39 5548 1073 82 744955 1 13088 1052 96 675928 0 00264960 492 503 829627 2 3 4 Table 28 Parameters of South pole atmosphere for Dec 31 1997 MSIS 90 E 0 2 67 113 139 1133 10 861730 2 67 5 33 79 0635 1101 20 826340 5 33 8 0 54 3888 1085 00 790950 8 0 100 0 0 0000 1098 00 682800 gt
75. US 64 VIEWCONE 54 133
76. absorption mirror reflectivity and photomultiplier quantum efficiency CEFFIC option see Sect 3 4 5 below Without the CEFFIC option CERSIZ 5 is reasonable as about one photon of such a bunch survives in an off line treatment of these effects By the keyword page 76 CERFIL T the Cherenkov output is directed to the separate Cherenkov output file MCETAP or to the par ticle output file MPATAP In case of a separate output file the Cherenkov output is structured as the particle output file It contains the event header and the event end block and in between the data blocks The data structure of the Cherenkov output data set is given in Table 11 page 99 In the case the Cherenkov bunches are stored together with the other shower particles on the same particle output file a Cherenkov bunch is treated like a particle The definition of an array of Cherenkov detectors serves to reduce the required disk space for Cherenkov shower On the other hand one loses the possibility of using an air shower several times during the analysis with different core locations with respect to the detector Keeping in mind the excessive computation time for Cherenkov showers a possibility is introduced to use Cherenkov showers multiple times with only a tolerable increase of storage space Therefore already during the simulation it is defined how often a single shower should be used and where in the array the core locations should be The core locations for
77. action of the primary energy below which the thinning algorithm becomes active If the fraction is selected in a manner that this energy is below the lowest energy threshold of ELCUT i 1 4 keyword ECUTS page 68 thinning will not become active but the particle output data structure will contain the weight 1 for each particle WMAX Weight limit for thinning If the weight of a particle exceeds WMAX no further thinning is performed RMAX Maximum radius in cm at observation level within which all particles are subject to inner radius thinning Particles are selected with probability r rmaz The weight of sur viving particles is multiplied by the appropriate factor inverse of probability This thinning neither affects the shower development nor the table output nor the histogram output of the ANAHIST or AUGERHIST option rather only the particle output file written onto MPATAP and the Cherenkov output file written onto MCETAB For RMAX lt 0 no radial thinning is applied Limits are ULIMIT EFRCTHN lt 1 101 eV for ULIMIT see keyword ERANGE page 53 0 1 lt WMAX x 1 10 This keyword is only available in the THIN option 4 45 Hadronic Thinning Definition THINH IHINRAT WEITRAI Format A5 2F Defaults 1 1 THINRAT Defines hadronic thinning limit differing from em thinning limit EFRCTHN by the ratio of y 15 Which gives the ratio between the energy of the em particles speci
78. ahlung photons above threshold but below EL CUT 4 resulting in a considerable prolongation of wasted CPU time Therefore CORSIKA automatically selects the EGSDAT6_x x set best suited for the user s specification of the EL CUT 3 and ELCUT 4 thus saving CPU time 3 4 Cherenkov Options 3 4 1 Cherenkov Standard Option The routines treating the Cherenkov radiation have been supplied by the HEGRA Collabora tion 33 and considerably improved by K Bernl hr 34 The Cherenkov light production by electrons positrons muons and charged hadrons is considered in the subroutine cerenk The Cherenkov photons are considered within a wavelength band which may be specified by the lower and upper limits WAVLGL and WAVLGU Atmospheric absorption of the Cheren kov photons is not taken into account by default but might be added by the CEFFIC option see Sect 3 4 5 page 35 Only Cherenkov photons arriving at the lowest observation level are recorded Charged particles create Cherenkov photons at each tracking step when the condition 8 gt 1 n 8 v c and n refractive index is fulfilled The step is subdivided into smaller sub steps such that the number of Cherenkov photons per sub step is less than the fixed number CERSIZ predefined by an input keyword In such a sub step all the photons are sent in a compact bunch along a straight line defined by the emission angle 0c relative to the electron or hadron direction a random value for the angl
79. am calculates a bunch size which is found to be appropriate for the HEGRA array Limit is CERSIZ gt 0 This keyword is only available in the CERENKOV AUGCERLONG and AUGERHIST option 4 68 Cherenkov Output Steering CERFIL LCERFI Format L Default T LCERFI If true Cherenkov output is written to the Cherenkov output file MCETAP If false Cherenkov output is written to the particle output file MPATAP In the IACT option Cherenkov telescopes with LCERFI true the output file name DSN spec ified by keyword DIRECT should be set to dev null 9 to suppress the normal Cherenkov output file as the Cherenkov telescope output will be written to the event io output file LCERFI automatically will be set true in the COMPACT option to prevent a writing of Cher enkov photons to the COMPACT output This keyword is only available in the CERENKOV option 4 69 Cherenkov Quantum Efficiency CEROEF CEROEF CERATA CERMIR 62 The existence of dev null is assumed see footnote of Sect 4 60 63Details on the event io format may be found in the documentation supplied with the bernlohr package 76 Format 6 3L Defaults F E F CERQEF If true quantum efficiency of detector photomultiplier is taken into account It needs reading in the quanteff dat file CERATA If true the atmospheric absorption of Cherenkov photons is taken into account It needs reading in the atmabs dat file CE
80. atmospheres you should not combine the CURVED option with CEFFIC The combination of VOLUMECORR with VIEWCONE is not supported The AUGERHIST option cannot be combined with the CURVED INTTEST PLOTSH or PLOTSH2 options Using the coconut script file see Sect 2 2 2 page 13 conflicting options are indicated and will be avoided automatically 50 4 Steering of the Simulation The simulation of air showers is steered by commands keywords that have to be given on unit MONIIN MONItor INput in the card image format A command consists of a keyword usually up to 6 characters long left shifted upper or lower case characters and one or more arguments in the form KEYWRD arg arg2 sv ATOSS comments The keyword and the arguments must be separated at minimum by one blank The last argu ment may be followed by comments up to column 140 Additional comments may be given on separate lines with the first 6 characters the keyword kept blank with the first character a c or a C followed by a blank or with the first character a In the IACT option page 34 the lines starting with are treated additionally as comment lines Internally all characters includ ing the keywords are converted to upper case characters except the characters following the keywords EPOPAR DATDIR DIRECT HISTDS HOST IACT INFILE NEXPAR TELFIL and USER If you want to specify one of these character arguments by a blank you should
81. atmospheres and for supplying the VIEWCONE option and to D Chirkin Berkeley for contributing the VOLUMECORR option We thank F Schr der Wuppertal for his engagement in developing and testing the CURVED version The authors are obliged to J Wentz Karlsruhe for his pioneering work in coupling the UrQMD model with CORSIKA and for contributing the COMPACT option The C routines for writing Cherenkov output in the STACEE form are contributed by J Hinton Chicago We thank the Auger group Naples C Aramo G Miele O Pisanti L Rosa for developing the NUPRIM option Thanks go to P Homola Krakow who has written the C routines to treat the pre showering of ultra high energetic photons in the Earth s magnetic field We thank A Chou Fermilab to bring our attention to GHEISHA correction patches and R E Cassell and G Bower SLAC to make them available for CORSIKA The programming of the AUGERINFO info file the support by developing the AUGERHIST extensions and the detection of several severe bugs by M Risse Karlsruhe now at Siegen is acknowledged We are indebted to F Schmidt Leeds now at Chicago for the development of the PLOTSH2 option including the visualization program map2png and R Ulrich Karlsruhe now at Penn State for programming the ROOTOUT and ROOTRACK options We thank Kokoulin and A Bogdanov MEPHI Moscow for the more precise treatment of muonic interactions and energy loss The introduction of the TAU
82. billions of calls of sequence 2 I9 seq3seed 1 seed of sequence 3 I9 seq3seed2 number of calls of sequence 3 19 seq3seed3 billions of calls of sequence 3 I9 size size of particle tape output 110 dsn_events data set name of particle tape output A59 dsn_prtout data set name of txt file output A9 tape name name of data tape A10 backup name of backup tape A10 howmanyshowers number of showers to generate 110 host host computer name A20 user user name A20 atmosphere Modtran atmosphere model number I3 refract number indicating use of refractive index I2 viewcon_l inner limiting angle of viewing cone E14 7 viewcon_u outer limiting angle of viewing cone E14 7 telescope 2 coordinates x y z r of telescope 4F11 1 ficscat number and range of scattering in x y 2F10 1 thinning number indicating use of thinning I2 thinnlev_had thinning level hadronic E14 7 thinnlev_em thinning level em E14 7 maxweight_had weight limit hadronic E14 7 maxweight_em weight limit em E14 7 rad_max maximum radius for radial thinning m E14 7 energy_prim primary energy of first shower E14 7 theta_prim primary s 0 of first shower E14 7 phi_prim primary s of first shower E14 7 Table 16 continued Content of D AT nnnnnn dbase rsp DATnnnnnn nfo file 107 11 Hints for Programmers If you need any option addition or other extension which is not yet
83. bins used in the standard case This slant depth scale is more appropriate to investigations of very inclined showers In the SLANT option 43 44 the ionization energy loss deflection within the Earth s magnetic field and the generation of Cherenkov photons is enabled for charged hadronic primaries on their path between entering the atmosphere and the first interaction which is disabled in the standard version without using keyword TSTART page 55 The arrival time refers to the margin of the atmosphere which is indicated by a negative value of element 7 of the event header block page 97 To obtain this program version the SLANT option has to be selected when extracting the FOR TRAN code from the source file 3 5 20 STACKIN Option With the STACKIN option the parameters of secondary particles will be read into the CORSIKA stack Thus interactions of very exotic primaries may be treated off line in a suitable interaction program avoiding a direct coupling of such programs with CORSIKA The air shower gener ated by these resulting secondary particles is simulated in CORSIKA and all options may be combined with STACKIN To characterize the altitude of the first interaction the keyword FIX HEI must be used the shower axis is defined by the angles THETAP and PHIP pages 53 and 42Through the COAST and COAST USER LIB packages which should be installed in the subdirectory defined in the environment variable SCOAST_DIR 45 54 This ext
84. bremsstrahlung pair production nuclear interactions of the 7 leptons are respected in a manner analogously to the j leptons For the treatment of primary v and vz neutrinos the TAULEP or CHARM option has to be combined with the NUPRIM option see page 41 For tracing back PYTHIA problems the PYTHIA keyword is available see Sect 4 81 page 80 To obtain this program version the TAULEP option has to be selected when extracting the FORTRAN code from the source file Please verify that you have downloaded the PYTHIA 6 412 package from the PYTHIA web page to the pythia subdirectory 3 5 22 Option for Thinning For primary energies gt 1019 eV the computing times become excessively long they scale roughly with the primary energy To reduce the times to tolerable durations the so called thin sampling mechanism also named variance reduction 161 is introduced 40 When thinning is active all particles below the adjustable fraction of the primary energy thinning level j E E which emerge from an interaction are exposed to the thinning algorithm Only one of these particles is followed and an appropriate weight is given to it while the other particles below the thinning level are dropped Details on this formalism may be found in Refs 16 40 45 A further improvement 46 to reduce undesired statistical fluctuations of particle densities far from the shower core uses a limitation of the weights Particles emerging fr
85. ccessively by assuming that the non interacting nucleons proceed as one new nucleus NFRAGM 1 This new nucleus may evaporate nucleons or alpha particles with a transverse momentum distribution according to experimental data 49 NFRAGM 2 de fault or with a transverse momentum distribution according to Goldhaber s theory 50 using 0 090 GeV nucleon as the average transverse momentum NFRAGM 3 NFRAGM 4 gives identical fragments as NFRAGM 2 or 3 but without transverse momenta The NFRAGM flag is used also to steer the fragmentation in the various interaction models as described for the HDPM routines EPOS NEXUS and VENUS use the same evaporation model as HDPM with the same meaning of NFRAGM while SIBYLL and QGSJET deliver themselves realistic nuclear fragments with according transverse momenta they are selected by NFRAGM gt 2 In principle DPMJET offers a very detailed nuclear fragmentation model with evaporation But there is no allowance to distribute it Therefore the nuclear evaporation as used for HDPM EPOS NEXUS and VENUS is coupled with DPMJET and the meaning of NFRAGM follows Additionally NFRAGM 5 is used to activate the DPMJET evapo ration module if it exists Limits are 0 lt all flags lt 100 4 40 Transition Energy between Models HILOW HILOELB 65 Format A5 F Default 80 HILOELB Allows to define the transition energy in GeV between high and low energy hadronic inte
86. cm i 1 10 height of levels for electron numbers in cm 1 1 10 distance bins for local pseudo age in cm 1 1 10 local pseudo age 2 level 255 1 1 1 6 parameters of longitudinal distribution of charged particles 262 x per degree of freedom of fit to longitudinal distribution 263 weighted number of photons written to particle output file 264 weighted number of electrons written to particle output file 265 weighted number of hadrons written to particle output file 266 weighted number of muons written to particle output file 267 number of em particles emerging from pre shower 268 273 not used Table 13 Structure of event end sub block 101 Run end sub block once per run Contents of word as real numbers R 4 RUNE run number 3 number of events processed 22273 Table 14 Structure of run end sub block 10 2 1 Version without Thinning The information is stored unformatted in a fixed block structure with a block length of 22932 bytes A block consists of 5733 words each 4 bytes long Each block consists of 21 sub blocks of 273 words These sub blocks can be a RUN HEADER EVENT HEADER DATA BLOCK LONGitudinal EVENT END or a RUN END sub block see Table 6 The contents of the sub blocks are listed in Tables 7 to 14 10 2 2 Thinning Option To take the weight parameter for each particle the data structure of the version without thinning has to be extended for the THIN option The structure
87. coming from 7 decays may be discriminated from those originating in K decays or other reactions 76See keyword TSTART page 55 99 LONG event number particle id particle code or A x 100 Z for nuclei total energy in GeV total number of longitudinal steps x 100 number of longitudinal blocks shower current number m of longitudinal block altitude of first interaction in g cm zenith angle 0 in radian azimuth angle in radian cutoff for hadron kinetic energy in GeV cutoff for muon kinetic energy in GeV cutoff for electron kinetic energy in GeV cutoff for photon energy in GeV vertical rsp slant depth of step 7 in g cm number of y rays at step 7 number of e particles at step 7 number of e particles at step 7 number of particles at step 7 number of u particles at step 7 number of hadronic particles at step 7 number of all charged particles at step 7 number of nuclei at step j number of Cherenkov photons at step 7 for n 1 26 and for 7 longitudinal steps for 1 LONG block 1 j 26 for 274 LONG block 27 j 52 for m LONG block m 1 26 1 j 26 if last block is not completely filled trailing zeros are added Table 12 Structure of longitudinal sub block These type of blocks are written only if LONGI is enabled and FLONGOUT is disabled page 69 77 A gt 1 are not counted with the hadron
88. d S ECT NU are not yet existent they will be calculated at the first call of subroutine ggaini rsp psaini which takes c 4 days 1 GHz Pentium LINUX rsp 30 h for QGSDATOI on a DEC 3000 600 AXP with 175 MHz The resulting qgsdat 11 03 file will have a size of 131 MB The QGSJET option needs about 3 times more qgsjet II 03 rsp the same qgsjetOlc CPU time than as the option NKG enabled EGS4 disabled QGSJET activates also the inelastic hadron nucleus interaction cross sections at higher energies which are supplied in the qgsdat II 03 file read in by the qgsjet II 03 7 rsp the QGSDATO01I file read in by the qgsjetOlc 6 program package The nucleus nucleus cross sections are con tained in the file sectnu 11 03 rsp SECTNU The qgsjet I1 03 cross sections rsp QGSJETOIc 3 Binary type file available for LINUX system on the CORSIKA ftp server for downloading 27 cross sections are selected automatically when the QGSJET option has been used for extract ing the FORTRAN code from the source file In your input file you may supply the keyword page 63 QGSSIG d Setting QGSSIG to false you will use the default cross sections of CORSIKA as described in Ref 3 3 1 6 SIBYLL Option SIBYLL 8 is a program developed to simulate hadronic interactions at extreme high energies based on the QCD mini jet model The actual 9 version is SIBYLL 2 1 For using SIBYLL you first have to select the SIBYLL optio
89. d hadronic component of the shower are given out separately and may be used to plot the shower develop ment This keyword is only available in the PLOTSH and PLOTSH2 option 4 90 Plot Axes Definition PLAXES X X2 Yd Y2 21 22 Format A6 6F Defaults 500000 500000 500000 500000 0 3000000 X1 X2 They denote the X axis range in cm to be plotted in the map Y2 They denote the Y axis range in cm to be plotted in the map 21 22 They denote the Z axis range in cm to be plotted in the map The point of first interaction determines the zero point of the X and Y axes see Fig 1 page 86 Depending on the choice of these parameters the whole shower may be visualized or one can zoom in on interesting regions of the shower Limits are lt X2 lt Y2 71 Z2 This keyword is only available in the PLOTSH2 option 4 91 Plot Energy Cut Definition PLCUTS ELCUTS 1 4 TCUT FBOXCUT 83 Format A6 5F L Defaults 0 3 0 3 0 003 0 003 100000 F ELCUTS 1 4 ELCUTS denote the energy cuts in the same order as those for the keyword ECUTS hadrons muons electrons photons see page 68 TCUT This is an upper bound on the time in ns passed since the first interaction If at the end point of a track the time is above TCUT the track is not plotted This cut allows a visual ization of the shower development FBOXCUT This flag determines whether only track segments inside the
90. d large arrays e g the intermedi ate stack STACKINT needs 30 MB in EPOS NEXUS and VENUS the arrays dimensioned by MXPTL need about 10 MB If the energy range is limited to lt 100 TeV some of those large arrays may be dimensioned smaller thus saving memory On machines with little memory the permanent swapping might significantly contribute to the overall computing time A simplified flow diagram of CORSIKA is given in Appendix B page 118 The sequence of the initializing procedures is given in Appendix C page 119 CORSIKA runs fastest full simulation adopted without THINning when using no EGS4 no DPMJET no EPOS no NEXUS no VENUS no NEUTRINO no Cherenkov light generation For this program version the computing time on a Intel 6600 Core2Duo with 2 4 GHz is 7 3 sec per shower for primary protons of energy 101 eV vertical incidence NKG enabled with one observation level at 110 m a s l and with the hadron and muon energy cut at 0 3 GeV Under the same conditions an iron induced shower consumes z 10 6 sec The computing time scales roughly with the primary energy The full EGS4 option with longitudinal profile is roughly 200x slower than the fastest version mentioned above with ELCUT 3 4 at 3 MeV There is not much experience what the time consumption is for the CERENKOV option but the time consumption will be much higher The use of SIBYLL or QGSJET results in similar computing times as HDPM The use of VENUS needs 8 times mor
91. d with CORSIKA For other installations the user should establish correspond ing tables By early eliminating those Cherenkov photons which are absorbed within the atmosphere not reflected by the mirror or not producing photo electrons within the photomultiplier those sup pressed photons are also not counted in the various forms of the longitudinal distributions see Sect 3 4 6 below As in the CEFFIC option the atmospheric absorption is treated only in a manner suited for planar atmospheres you should not combine the CEFFIC option with CURVED 36The atmabs dat table is composed of 105 wavelength values between 180 and 700 nm in steps of 5 nm one line for each wavelength beginning with the wavelength value nm as integer followed by 51 extinction values starting at sea level up to 50 km height in steps of 1 km The data format is 105 14 5 10F10 3 F10 3 For the same 105 wavelengths the mirreff dat and quanteff dat tables contain reflectivity rsp quantum efficiency values written in the format 8F6 3 Further details may be taken from the comments in the employed subroutine tpdini 35 To obtain this program version the CEFFIC option has to be selected together with the CEREN KOV option when extracting the FORTRAN code from the source file 3 4 6 INTCLONG and NOCLONG Options In the Cherenkov version the longitudinal distribution of photons is given in differential mode i e the number of photons generated within each step
92. data generated with the THIN option differ from those generated in simulations without this option see also Sect 10 2 2 page 102 An optimum choice of the various thinning parameters depends on the information which should be drawn from the simulations To minimize the additional fluctuations caused by the thin sampling algorithm for muonic particle densities at large distances gt 300 m from the shower core which is one of the problems of the Auger experiment a suitable setting 46 of WEITRAT would be WEITRAT 100 while the choice of WMAX is optimized for the primary energy Eo given in GeV and the selected thinning level EFRCTHN for em particles to WMAX EFRCTHN To obtain this program version the THIN option has to be selected when extracting the FOR TRAN code from the source file 3 5 23 UPWARD Option The UPWARD option selects code which treats the upward traveling particles For primary particles the zenith angle is restricted to 0 lt 0 lt 70 and 110 lt 0 lt 180 No additional keyword has to be specified The UPWARD option might be combined with the CURVED option page 39 This enables to start showers with arbitrary zenith angles 0 lt 0 lt 180 and secondary particles with arbitrary zenith angles are followed 44 For showers with skimming incidence zenith angle 90 the minimum altitude of the shower axis above sea level is specified by HIMPACT keyword IMPACT page 56 and defines
93. e amp around this direction As the major part of the Cherenkov light is produced by electrons it makes no sense to sim ulate showers with Cherenkov light production unless using the EGS4 option Therefore the CERENKOV option automatically activates the EGS4 option too The CERENKOV option reduces the step length factor STEPFC to 1 by default page 66 For higher primary energies it is impossible to write all the photon bunches of one shower to the output file Therefore only those bunches are recorded which hit an array at the lowest ob servation level consisting of NCERX x NCERY photon detectors arranged with a grid spacing of DCERX and DCERY cm in x and y direction respectively and with ACERX x ACERY cm area each Each bunch is represented by 7 words which are the number of Cherenkov photons the x and y position coordinates at the observation level direction cosines u and v arrival time 32 and height of production above sea level To obtain this program version the CERENKOV option has to be selected when extracting the FORTRAN code from the source file Via the keyword page 75 CERARY 27 27 1500 1500 100 100 the geometry of your Cherenkov array may be defined A rotation of the Cherenkov array x axis relative to North may be respected by the keyword page 73 ARRANG Q The bunch size may be selected by the keyword page 76 CERSIZ 0 The optimal choice of the bunch size depends on the employment of the atmospheric
94. e CORSIKA 6 9 set is distributed as a gzipped tar file consisting of several files and directo ries a file README giving these short instructions how to proceed an executable shell script file coconut to be used to install CORSIKA a file AUTHORS giving the names of authors a file COPYING giving copyright instructions a file ChangeLog giving the CORSIKA history a file INSTALL giving detailed instructions how to use coconut to install CORSIKA a file NEWS giving latest news about CORSIKA a cCDO NOT RUN CONFIGURE to remind users not to use configure but coconut instead files Makefile am Makefile in acinclude m4 aclocal m4 con f igure in con figure These files and the subdirectory config are needed for the installation and should not be changed unless you know exactly what you are doing subdirectories have a Makefile am and a Make file in which are needed by con figure to create the proper Makefiles a subdirectory bernlohr containing bernlohr package It is a set of C routines for Imaging Atmospheric Cherenkov Telescopes IACT and for use of external atmo spheric profiles in the ATMEXT option several atmospheric profiles atmprofi dat are included together with various auxiliary files This package is provided by K Bernl hr subdirectory coast where to install the COAST package if needed The COAST package is available from http www ik fzk de rulrich coast and con sists of C routi
95. e CORSIKA FLUKA linking routines at the appropriate places Preferentially you use the f77 rsp g77 compiler with the option Iflukadirectory lukapro to indicate the compiler where to find the include files For all steps using the FLUKA package you presumably have to give limit datasize unlimited limit stacksize unlimited to overcome the small default values of many compilers which lead to an error stop during link ing option For compiling the CORSIKA URQMD version of the corsika compilefile f the UrQMD include files boxinc f colltab f comres f coms f inputs f newpart f and options f should be available in the directory from which you are calling the compiler to include them into the CORSIKA URQMD linking routines at the appropriate places Alternatively you may use the f77 rsp g77 compiler with the option I urqmd to indicate the compiler where to find the include files The compiler procedures of the standard case see begin of this subsection A 1 should be used to compile the corsika compilefile f The urgmd1 3_cors tar gz file contains the UrQMD1 3_cors source routines with slight modifi cations to adapt them for the use with CORSIKA To compile these UrQMD source files one 90See footnote at DPMJET compilation 115 uses g make command with the option f GNUmakefile_corsika omitting the link step in the urqmd subdirectory NUPRIM option When compiling the CORSIKA NUPR
96. e CPU time than the fastest version and a combined EGS4 VENUS option is about 20048 208 times slower since the times do not multiply but add The use of DPMJET gives times of the same order of magnitude as the VENUS option EPOS or NEXUS NKG no EGS needs 7 5 times the computing time of VENUS i e about 60 times the computing time of HDPM NKG no EGS FLUKA needs 7 times computing time of GHEISHA UrQMD 40 times that of GHEISHA In case of THINning Sect 3 5 22 page 46 the computing time strongly depends on the energy fraction below which thinning becomes active The interested CORSIKA user may find CPU 90 times for various interaction models and options in Ref 22 The particle output format is described in Sect 10 2 page 94 ff For each particle that pen etrates an observation level 7 words with 4 bytes each are stored on the particle output file Proton showers at 1015 eV deliver at sea level roughly 0 8 MB particle output when calculated with the NKG option Eu gt 0 3 GeV With EGS4 about 30 MB output are written due to the huge amount of photons and electrons that are explicitly stored E gt 0 003 GeV The particle output in the CERENKOV option is additionally increased as the Cherenkov pho tons are stored either separately on the Cherenkov output file or together with the particles on the particle output file While running the interactions produce plenty of secondary particles which are s
97. e a smaller maximum bunch size see keyword CERSIZ page 76 since all photons in a bunch are of the same wavelength and therefore the peak quan tum efficiency rather than the average quantum efficiency determines the maximum acceptable bunch size In combination with the CEFFIC option see Sect 3 4 5 page 35 you should use a maximum bunch size of 1 as usual To obtain this program version the CERWLEN option has to be selected in combination with the CERENKOV option when extracting the FORTRAN code from the source file 3 4 3 Imaging Atmospheric Cherenkov Telescope Option The routines treating the Cherenkov radiation for Imaging Atmospheric Cherenkov Telescopes option have been supplied by Bernl hr 34 The Cherenkov light production by electrons positrons muons and charged hadrons is considered in the subroutine cerenk The positions of the telescopes are defined by the keyword page 77 TELESCOPE 0 0 0 giving the coordinates relative to the center of the lowest observation level see Sect 4 71 page TT The data set name for the telescope specific data output is defined by the keyword page 78 TELFIL filename For further details of the IACT option see Ref 34 the comments at the beginning of the iact c routines and the documentation supplied with the bernlohr package With the IACT option by default the TMARGIN flag keyword TSTART is set to true see Sect 4 12 page 55 but it may be o
98. e function integrals for VENUS NUCLEAR BIN nuclear data for DPMJET and FLUKA error output of FLUKA atmabs dat for atmospheric absorption of Cherenkov light CEFFIC option quanteff dat for photomultiplier quantum efficiency of Cherenkov light CEFFIC option mirreff dat for mirror reflectivity of Cherenkov light CEFFIC option STACKIN input data file EPOS or NEXUS check file not opened EPOS or NEXUS histo file not opened pomtab dat various data for DPMJET DATnnnnnn dbase rsp DATnnnnnn info run summary file for use in an air shower library DATnnnnnn tab table output of y and GLAUBTAR DAT Glauber tables for DPMJET DATnnnnnn long output of longitudinal particle numbers and energy deposit EPOS or NEXUS data file not opened EPOS or NEXUS copy file not opened histogram output file for ANAHIST AUGERHIST vers histogram output file for INTTEST version DATnnnnnn lt spec gt _ lt proj gt map output of PLOTSH2 DATnnnnnn track_em output of PLOTSH em comp D ATnnnnnn track mu output of PLOTSH muon comp D ATnnnnnn track hd output of PLOTSH hadron comp tables dat decay widths tables for UrQMD UrQMD VER xs dat total cross section table for UrQMD C E Rnnnnnn Cherenkov photon output EPOS or NEXUS parameters scratch file Table 1 Logical units for in and output with their default values and file names 21 2 3 2 Output Files There are several streams of CORSIKA output One is control inf
99. e keyword PAROUT page 74 might be used This analysis gives a short overview on various shower properties of the particles arriving at the observation level The histograms are only established for the lowest observation level Radial thinning is not applied to the particles sorted into the histograms Because of its permanent modifications a comprehensive description of the ANAHIST option is not available To obtain this program version the ANAHIST option has to be selected when extracting the FORTRAN code from the source file The HBOOK routines require linking of the CERN li braries with the program they are not supplied with the CORSIKA package 36 3 5 2 ATMEXT Option with External Atmospheres The ATMEXT option allows to use external tabulated atmospheres of the MODTRAN model documented in Ref 36 They are provided together with the bernlohr package as files atm profi dat and read in with special routines written in C Further details may be found in Ref 34 at the beginning of the atmo c routines and in the documentation supplied with the bernlohr package The CURVED option needs the atmospheres in the 5 layer model rather than interpolated from ATMEXT tables Therefore in the CURVED option AATM BATM CATM values are fitted to the tabulated atmospheres and the table interpolation is disabled To obtain this program version the ATMEXT option has to be selected when extracting the FORTRAN code from the source file A linkin
100. each event are chosen with the Sobol quasi random number generator 35 and are stored in the event header Correspondingly the array of Cherenkov detectors is placed several times in the observation plane and store all Cherenkov bunches that hit one of the detectors This possibility is selected by the keyword page 77 CSCAT ICERML XSCATT YSCATT An event is used ICERML times and the core is scattered in the range XSCATT lt 2 lt XSCATT and YSCATT lt Yeore lt YSCATT For the analysis of such CORSIKA events the user has to use the same core locations in the analysis that have been determined during the simulation The output will basically scale with the number of times each event is used but it is still considerably smaller than the output of the complete Cherenkov component would be To obtain this program version the CERENKOV option has to be selected when extracting the FORTRAN code from the source file 33 3 4 2 Cherenkov Wavelength Option In the CERWLEN option the index of refraction is made wavelength dependent As a con sequence photon bunches will carry a specific wavelength Photons of shorter wavelengths with larger index of refraction will result in larger Cherenkov cone opening angles and larger bunch sizes For very fast particles this will generally have a small effect less than 0 03 in the opening angle for example but near the Cherenkov threshold the effect can be larger This option may also require to us
101. eprocessor option SLANT has been selected In the CURVED option the minimum step size has to be selected in a manner that no more than 1875 steps are needed to pass through the complete atmosphere FLGFIT If true and LLONGI also true the longitudinal development of all charged particles number is fitted If false the fit is suppressed 57ELCUT I is used also for neutrinos in the NEUTRINO option In the URQMD option ELCUT 1 should be gt 0 3 GeV 58ELCUT 2 is used also for 7 leptons in the CHARM or TAULEP option 69 FLONGOUT If true and LLONGI also true the longitudinal distributions of particle num bers and energy deposit for the various particle groups are written to the DAT nnnnnn long file see Sect 10 6 page 103 If false and LLONGI true the longitudinal distributions only of the particle numbers for the various particle species are written out to the particle output file DAT nnnnn in extra LONG sub blocks see Sect 10 2 Table 6 page 94 and Table 12 page 100 Limits are 1 lt THSTEP lt 1875 20 lt THSTEP lt 1875 for the SLANT option and horizontal incidence Normally only to the number distribution of all charged particles a function of the Gaisser Hillas type 53 t to Jens tmar t N t Nmaz t P a bt ct Umaz nue to is fitted to describe the dependence on the atmospheric depth and the resulting 6 parameters Nmmax to tmaz a b and c and the x do
102. erate Cherenkov light in the atmosphere to handle electronic and muonic neutrinos and anti neutrinos and to simulate showers with flat incidence Recently the HERWIG 18 interaction routines have been linked 20 with COR 1 SIKA to handle primary neutrinos To shorten the computing times for ultra high energy show ers above 1075 eV the thin sampling option exists by which only a fraction of the secondary particles is followed in the shower development There exists as well a program version that is not suited for air shower simulation but for testing the hadronic interaction models A detailed description of the CORSIKA program frame the used cross sections the hadronic interaction model HDPM the electromagnetic interaction models and the particle decays has been published in Ref 3 For details of the DPMJET EPOS NEXUS QGSJET SIBYLL VENUS FLUKA GHEISHA UrQMD and EGS4 programs see Refs 4 12 11 6 7 8 10 13 14 15 16 However minor modifications were made to these codes to adapt them for simulation of extensive air showers A comparison of the various hadronic interaction models is given in Ref 21 22 Besides the explanation 3 of the physics implemented in CORSIKA this CORSIKA GUIDE is a supplementary description of the technical handling and running of CORSIKA6990 It contains information about the installation of the program the required input data file formats parameter settings outputs and other technical
103. erate code to perform runtime checks on subscript e Procedures for LINUX computers with GNU 77 compilers should be used without optimization and are g77 00 51 2 gt Sl err to ensure correct simulations e Procedures for LINUX hosts with 64bit AMD CPU s with GNU 77 compilers should be used without optimization and are g77 O0 m32 51 2 gt Sl err to ensure correct simulations with the correct data format of the binary output files e Hosts with Portland pgf77 compiler available might use pgf77 c 02 61 2 gt l err which gives a fast and reliable executable on LINUX hosts 55But not using GFORTRAN compiler it will result in unexpected stop 56Do not use the optimization without carefully checking the results There is bad experience with GNU g77 v0 5 24 and egcs 2 91 66 which frequently brings NaN in the particle output file for the x and y coordinates of particles or results in unidentified hang ups within the QGSJET routines Also the g77 optimization causes the DADMUL integration routine to end with an error stop message DBRSGM IFAIL 1 despite the correct programming respecting all FORTRAN standards 113 e Compile procedures for IBM RS6000 are xlf c C O qextnam qmaxmem 1 1 f 2 gt l err e For HP UX processors the compilation procedures look like fort77 c K 1 ppu Dportable 02 Onolimit 1 f 2 gt S l err and the E1 option should also be used in the link step
104. ergy hadron nucleus and nucleus nucleus collisions Also the QGSJET II 03 cross sections are selected SIBYLL selects SIBYLL 2 1 routines for the simulation of high energy hadron nucleus and nucleus nucleus collisions Also the SIBYLL cross sections are selected VENUS selects VENUS routines for the simulation of high energy hadron nucleus and nucleus nucleus collisions Also the VENUS cross sections are selected FLUKA selects the FLUKA 2011 model for the simulation of low energy hadron nucleus collisions Always the appropriate FLUKA cross sections are used This option may be com bined with all high energy interaction models excluding DPMJET 2 55 GHEISHA selects the GHEISHA 2002d routines for the simulation of low energy hadron nucleus collisions Always the appropriate GHEISHA cross sections are used This option may be combined with all high energy interaction models URQMD selects the UrQMD 1 3 cors routines for the simulation of low energy hadron nucleus collisions Always the appropriate UrQMD cross sections are used This option may be com bined with all high energy interaction models The default setting obtained without specifying any option is QGSJET For low energy hadronic interactions the GHEISHA model is taken In addition to these options you may select the following preprocessing options ANAHIST selects code to generate a histogram file datmnnnnn lIhbook for a short analysis of essential properties of the particles ar
105. ernally treated first interaction starts the clock by default the keyword TSTART is disabled The file containing the parameters of the particles has to be specified by the keyword INFILE page 56 and is read in via the logical unit LSTCK by default 23 page 20 The first line is read with free format with a leading blank character and contains the number of secondaries and the primary energy The following lines are read with the format 215 4 1 15 7 containing current particle number particle type see Table 4 page 88 total energy GeV longitudinal momentum GeV c and transverse momenta GeV c The momenta are taken relative to the direction of the shower axis direction of the exotic particle To obtain this program version the STACKIN option has to be selected when extracting the FORTRAN code from the source file 3 5 21 TAULEP Option In the standard CORSIKA program the 7 leptons cannot be treated The TAULEP option 38 as well as the CHARM option enables the treatment of the 7 leptons their decays are treated by the PYTHIA package 19 Therefore except in combination with the DPMJET high energy interaction code the PYTHIA 6 421 package has to be installed in the pythia subdirectory for automatic compilation and linking In combination with DPMJET the implicit PYTHIA 6 115 package is used and needs no extra linking The TAULEP option may be combined with all high energy interaction models All possible interactions
106. essed This might be of advan tage with the CERENKOV option to suppress the particle output file but keeping the Cherenkov output file see Sect 4 68 FTABOUT If true the tabular output of the charged particle development is written out to the file DATnnnnnn tab onto the output directory DSN see Sect 4 60 above 4 62 Compact Output COMOUT COMOUT 61A dummy directory named dev null must be mounted in the system 74 Format A6 F Default T COMOUT If true the particle output is written in COMPACT form see page 38 If false the standard CORSIKA particle output is written This keyword is only available in the COMPACT option 4 63 Printer Output Unit OUTPUT MONNEW Format A6 I Default 6 MONNEW Logical unit of simulation control output on line printer Make sure that your se lection of MONNEW is not conflicting with existing definitions see Table 1 page 21 4 64 Data Table Directory DATDIR DATDIR Format A132 Default DATDIR Can be used to specify a common directory where CORSIKA will try to find all required input data tables except those belonging to FLUKA Lower case characters of DAT DIR are not converted to capitals Limit is DATDIR must not begin with a tilde character 4 65 Cherenkov Detector Array Definition CERARY NCERX NCERY DCERX DCERY ACERX ACERY Format 6 2I 4F Defaults 27 27 1500 1500 100 100 NCERX N
107. ev7 height of 7th observation level E15 7 obslev8 height of 8th observation level E15 7 obslev9 height of 9th observation level E15 7 obslev 104 height of 10th observation level E15 7 hcut energy for hadron cut E14 7 mcut energy for muon cut E14 7 ecut energy for electron cut E14 7 Table 16 Content of DATnnnnnn dbase rsp DAT nnnnnn info file to be continued 106 Content of DATnnnnnn dbase rsp DATnnnnnn info file continued Content Format gcut energy for gamma cut E14 7 theta_l lower end of 0 range E14 7 fitheta ust upper end of 0 range E14 7 phi_l lower end of range E15 7 phi_u upper end of range E15 7 fixhei fixed height of first interaction E14 7 n sttr first target 13 O random air 1 Nitrogen 2 Oxygen 3 Argon fixchi starting altitude of primary particle E14 7 stepfc multiple scattering step length factor E14 7 arrang array rotation angle E15 7 himpact1 lower limit of horizont shower axis skimming incid E14 7 himpact2 upper limit of horizont shower axis skimming incid E14 7 muaddi number indicating use of additional muon information I2 nseg number of used sequences for random generator I2 seqlseedi seed of sequence 1 I9 seqlseed2 number of calls of sequence 1 I9 seqlseed3 billions of calls of sequence 1 I9 seq2seed1 seed of sequence 2 19 seq2seed2 number of calls of sequence 2 19 seq2seed3
108. example other interaction model options may differ slightly The indentation gives the hier archy of subroutines Subroutine names are written in CAPITALS AAMAIN CORSIKA main program START write CORSIKA version and options PAMAF set particle masses and decay times DATAC read keywords from input set OBSLEV atmospheres and layers initialize random generator read NUCNUCCS cross section tables FILOPN open output files and external stack QGSINI initialize QGSJET II OGSET QGSJET II QGSJET II read ggsdat II 03 and sectnu II 03 OGSSIGINI CGHINI initialize GHEISHA EGSIN1 initialize EGS4 EGSIN2 read EGSDAT6_x x calculate physical constants set projectile and target for HSINI HSINI histogram initialization for INTTEST INPRM check input parameters set various parameters magn field Cherenkov MUPINI set u parameters and u cross section tables write RUNHEADER write dbase rsp info file ININKG initialize NKG parameters Clear statistics arrays multiplicity elasticity weight shower loop 119 D Atmospheres The atmosphere adopted consists of N5 O2 and Ar with the volume fractions of 78 1 21 0 and 0 9 57 The density variation of the atmosphere with altitude is modeled by 5 layers In the lower four of them the density follows an exponential dependence on the altitude leading to a relation between the mass overburden T A of the atmosphere
109. f Problems In spite of our care to avoid faults in the physics model and errors in the programming of CORSIKA and in writing this CORSIKA GUIDE you may have problems of technical or physical nature with the code or the results you obtain from it Please report all problems to the address mentioned on page 2 When applying for help in cases of crash it is recommended to transmit the control printout file txt file as it contains the selected preprocessor options as well as it echos the employed input keywords with their parameters Special interest exists in comparisons of CORSIKA simulations with experimental cosmic ray data Suggestions to improve CORSIKA in any respect are welcome you don t use the dev option when running coconut you can follow the same following scheme but us ing Make files located in 6990 11 uname and corsika 6990 1lib uname src for instance corsika 6990 1lib Linux src if you work on a LINUX system instead of just corsika 6990 110 13 Acknowledgments The authors thank to all CORSIKA users who have helped to eliminate errors and to improve the program Special thanks go to the authors of the various hadronic interaction models for their help to get their programs running and for their advice in coupling the programs with CORSIKA We are indebted to K Bernl hr Heidelberg for making available and updating his package of C routines for Cherenkov telescopes and external
110. f are stored in the event end block The longitudinal development of the electromagnetic particles is only sampled if EGSA is selected see ELM FLG If only NKG is activated the fit is applied to the NKG longitudinal distribution which consists of particle numbers from only lt 10 levels If neither EGS4 nor NKG is selected the charged particle distribution contains only muons and charged hadrons In the AUGERHIST option also a Gaisser Hillas type function is fitted to the longitudinal energy deposit if EGS4 is selected In the Cherenkov versions the longitudinal distribution of photons is given in differential mode i e the number of photons generated within each step as default By the preprocessor option INTCLONG the integral mode is selected i e accumulated number of generated Cherenkov photons for each step which needs additional computing time If both kinds of the distribution are of no interest you may deselect the Cherenkov photon distribution completely by the pre processor option NOCLONG thus saving computing time 4 50 Muon Multiple Scattering Treatment MUMULT FMOLI Format L Default T FMOLI If false the muon multiple scattering angle is selected by Gauss approximation If true the muon multiple scattering angle is selected for large steps by Moli re s theory and for small steps by adding many single Coulomb scattering events 4 51 Additional Electromagnetic Particle Information EMADDI FEMADD
111. fied by 54See footnote page 47 67 keyword THIN see above and the energy of the hadronic particles below which the thinning algorithm becomes active for these particle species see also Sect 4 44 above WEITRAT Defines hadronic weight limit differing from em weight limit WMAX by the ratio of weight limit of em particles to weight limit of hadronic particles in case of thin ning see also Sect 4 44 above A simultaneous use of the keyword THINH together with THINEM is not tolerated and will lead to an error stop Limits are ULIMIT EFRCTHN THINRAT lt 1 10 eV for ULIMIT see keyword ERANGE page 53 1 1074 lt WEITRAT lt 1 106 This keyword is only available in the THIN option 4 46 Electromagnetic Thinning Definition THINEM THINRAT WEITRAI Format A6 2F Defaults 1 1 THINRAT Defines em thinning limit differing from hadronic thinning limit EFRCTHN by the ratio of Ethem Ethraa Which gives the ratio between the energy of the em particles and the energy of the hadronic particles specified by keyword THIN see above below which the thinning al gorithm becomes active for these particle species see also Sect 4 44 above WEITRAT Defines em weight limit differing from hadronic weight limit WMAX by the ratio of weight limit of em particles to weight limit of hadronic particles in case of thin ning see also Sect 4 44 above A simultaneous use of the keyword THINEM together with THINH is not t
112. flags NKG EGS4 multiple scattering step length factor outer radius cm of NKG elect distrib magnetic field central Europe uT energy cuts hadr muon elec phot GeV longitud stepsize g cm 2 fit out muon multiple scattering by Moliere additional muon information observation level cm angle between north to array grid max no of printed events printout gamma factor cut directory of particle output Cherenkov detector grid cm Cherenkov wavelength band nm bunch size Cherenkov photons Cherenkov output file scatter Cherenkov events write data base file user name for data base file host name for data base file debug flag log unit delayed debug deg cm The coordinates in CORSIKA are defined with respect to a Cartesian coordinate system with the positive X axis pointing to the magnetic North the positive Y axis to the West and the Z axis upwards The origin is located at sea level This definition is necessary because the Earth s magnetic field is taken into account By default the magnetic field is implemented for the location of Karlsruhe 49 N 8 E as described at the keyword MAGNET page 59 The 85 z axis N y axis west x axis i north Figure 1 Coordinate system in CORSIKA zenith angle 0 of a particle trajectory is measured between the particle momentum vector and the negative Z axis and the azimuthal angle between the positive X axis and the horizontal compone
113. g with the compiled atmo c routines of the bernlohr package is done by the Make file 3 5 3 AUGCERLONG Option With the AUGCERLONG option it is possible to fill the Cherenkov column in the table of the longitudinal particle distribution without full simulation of the Cherenkov radiation Because of an elongation of the CPU time the AUGCERLONG option should only be used if the lon gitudinal Cherenkov distribution is really needed By the INTCLONG option page 36 the integrated instead of the differential longitudinal Cherenkov intensity may be selected The keywords CERSIZ page 76 and CWAVLG page 76 are activated with the AUGCERLONG option To obtain this program version the AUGCERLONG option has to be selected when extracting the FORTRAN code from the source file 3 5 4 AUGERHIST Option The AUGERHIST option produces a series of histograms generated with HBOOK routines 24 The histograms are written into the file named datnnnnnn Ihbook page 103 onto the output directory DSN specified by the keyword DIRECT page 74 As the HBOOK routines use only lower case characters the DSN directory name should not contain capitals These histograms show properties of different particle types at up to 20 horizontal levels to be defined by keyword OBSLEV page 71 They enable to study the longitudinal development of various shower parameters At each defined level a series of histograms is generated e g for radial distances of different par
114. gies DPMJET activates also the inelastic hadron nucleus cross sections at higher energies which are calculated by the subroutine sig Nucleus nucleus cross sections are derived from the DPM JET nucleon nucleon cross sections using the Glauber tables of CORSIKA 3 The DPMJET cross sections are selected automatically when the DPMJET option has been used for extracting the FORTRAN code from the source file In your input file you may supply the keyword page 60 DPJSIG Setting DPJSIG to false F you will use the default cross sections of CORSIKA as described in Ref 3 It should be emphasized that the DPMJET option cannot be combined with the FLUKA option because of several identical common and subroutine names used within DPMJET and FLUKA 27 FORTRAN compiler options described Sect 1 page 114 are used 5Experience shows that because of the complexity and the sparse internal documentation of DPMJET not all possibilities for error stops or crashes are detected and eliminated These errors are difficult to trace back and we are not able to support users in those cases 24 3 1 2 EPOS Option EPOS 12 Energy conserving quantum mechanical multi scattering approach based on Partons Off shell remnants and Splitting parton ladders like NEXUS combines features of the former VENUS 10 and QGSJETOI 6 with extensions enabling a safe extrapolation up to higher energies using the universality hypothesis t
115. h directly transmits the particle output normally di rected to MPATAP to C routines to write an output DAT nnnnnn root file in root for mat e g for root off line analysis of the particle output data without storing the huge particle output data file MPATAP The Cherenkov output file MCETAP is not affected by the ROOTOUT selection The ROOTOUT option cannot be combined with the COMPACT option The appropriate C routines used in the ROOTOUT option are available from the web page http www ik fzk de rulrich coast and must be installed in a subdirectory defined by the environment variable SCOAST_DIR Before the CORSIKA installation COAST must have been compiled and installed first The default COAST ROOTOUT data format is thought for fast and easy off line analysis of CORSIKA data and is NOT a general replacement for CORSIKA binary data files Due to the chosen data structure one shower including all particles and all Cherenkov photons is stored in the computer s memory entirely before it is written to disk This needs a lot of memory for high energy and or high quality showers To obtain this program version the ROOTOUT option has to be selected when extracting the FORTRAN code from the source file and root and COAST must be installed on your system 40Through the COAST package which should be installed in the subdirectory defined in the environment variable SCOAST_DIR 41This option compiles only on LINUX and Mac OSX
116. h to libpng so is not included in the LD LIBRARY PATH variable 43 3 5 16 PRESHOWER Option The PRESHOWER option selects code and C routines 41 to describe the pair production of ultra high energetic Eo gt 1019 eV primary photons and bremsstrahlung interactions of the secondary em particles within the Earth s magnetic field before reaching the top of atmosphere Within the atmosphere the resulting swarm of em particles is treated as one shower To model correctly the field components of the Earth s magnetic dipole field in the outer space additional input is required to specify the location and the time of the experiment The keyword page 59 GCOORD 69 585 35 463 2003 1 0 gives the longitudinal and lateral position of the experiment on the Earth s globe the year the Earth s magnetic field is time dependent a print indicator and a stop indicator for the case no pre showering occurred Details of this input are given in Sect 4 23 With the stop indicator it is possible to skip those events where no pre showering occurred Nevertheless the event header and event end sub blocks are written to MPATAP The appropriate C routines belonging to the PRESHOWER option are available in the src subdirectory compiled and linked by the Make file To obtain this program version the PRESHOWER option has to be selected when extracting the FORTRAN code from the source file 3 5 17 ROOTOUT Option The ROOTOUT option selects code whic
117. he CHARM or TAULEP option Cherenkov photons can not be a primary particle for an air shower simulation 87 Particle Identification Particle 1 51 52 53 54 55 56 57 58 59 60 61 62 63 64 65 66 67 68 69 u 1 74 n ntry 75 add info 76 add info 02 g Table 4 Particle identifications as used in CORSIKA to be continued 88 Particle identifications continued Identification Particle Identification DR N x 100 7 nucleus of Z protons and A Z neutrons 2 lt 59 9900 Cherenkov photons on particle output file Table 4 continued Particle identifications as used in CORSIKA 89 9 Running the CORSIKA Program Depending on the program options CORSIKA needs at minimum 7 MB memory Especially DPMJET EPOS and NEXUS need a huge amount of internal memory Empirical values of required memory for DEC AXP computers are given in Table 5 Using UrQMD instead of GHEISHA needs 8 6 Mbyte additionally Using FLUKA instead of GHEISHA needs about SIBYLL2 1 065 VENUS DPMJET2 55 NEXUS3 97 EPOS Memory 7 6 12 10 21 52 100 2300 Table 5 Required memory for various CORSIKA GHEISHA options DEC ALPHA 100 Mbyte additionally To be able to simulate central collisions of primary 9 Fe nuclei with atmospheric Ar at higher energies some program parts nee
118. ill suggest the solution Just follow what is written 17The bernlohr epos nexus and urqmd packages will be automatically unpacked in their subdirectories 18Trying to use the CERN library when not installed for instance 14 Using the default options on a LINUX system you will get Your final selection to build CORSIKA is options HORIZONTAL QGSJETO1 GHEISHA TIMENEW Configuration is finished How do you want to proceed f Compiling and remove temporary files DEFAULT k Compile and keep extracted CORSIKA source code n Just extract source code Do not compile restart x exit make only one choice possible At this point you should press Enter rsp f If you want to see the code used to compile your CORSIKA program you can answer k but this is not needed by the automatic compila tion Finally the installation program creates proper Makefiles and then runs make install to compile your CORSIKA program Select n only if you want to modify the source code before compiling or if you want to use your former installation tools you prepared for an older version of CORSIKA using a compilefile f This option will preprocess the source code save it in subdirectory src as corsika followed by the version number 6990 an underscore with the selected high energy hadronic interaction model and an underscore with the selected low energy hadronic interaction model and an optional
119. in the DEBUG case also the GHEISHA routines produce debug output This output appears on the unit MDEBUG This keyword is only available in the GHEISHA option 480 URQMD Debugging UROMD FURQMD IUDEBUG Format 5 L I Default 0 FURQMD If true the UrQMD routines are used for the low energy hadronic interactions If false the program will stop IUDEBUG If gt 0 in the DEBUG case also the routines of UrQMD produce some output With increasing value of IUDEBUG this printout becomes more and more detailed This output appears on the unit MDEBUG Limit is 0 lt IUDEBUG lt 3 This keyword is only available in the URQMD option 4 81 PYTHIA Printing PYTHIA IFLGPYW IFLGPYE Format A6 21 Default 0 0 IFLGPYW If set gt 0 the printing of PYTHIA warnings is enabled IFLGPYW gives the number of warnings after which PYTHIA becomes silent see MSTU 26 of Pythia manual 19 IFLGPYE If set gt 0 the printing of PYTHIA errors is enabled IFLGPYE gives the number of warnings after which PYTHIA becomes silent see MSTU 22 of Pythia manual 19 Limits are 0 IFLGPYW 0 lt IFLGPYE This keyword is only available in the DPMJET CHARM and TAULEP options 66The existence of dev null is assumed see footnote of Sect 4 60 80 4 82 Cherenkov Debugging CDEBUG LCERDB Format L Default F LCERDB If false Cherenkov debug output is disabled If true
120. include the blank within apostrophes or quotation marks The sequence of steering keywords is arbitrary The valid keywords the internal argument names their nature character F floating I integer or L logical their default settings their descriptions and their limita tions are listed in the following As CORSIKA is primarily designed to simulate EAS in the energy range 101 eV to some 1070 eV the code contains parameterizations and approximations which are valid only for a limited range of some arguments Leaving the recommended range might cause incorrect results or even end the execution of the program with an error message 41 Run Number RUNNR NRRUN Format A5 D Default 1 NRRUN Run number of this simulation This number is used to form part of the name of the various output files Limit is 0 NRRUN lt 999999 4 2 First Event Number EVTNR SHOWNO Format A5 D Default 1 SHOWNO Event number of first shower The second shower will get number SHOWNO 1 and so on Limit is lt SHOWNO lt 999999 51 4 3 Random Number Generator Initialization SEED ISEED i k i 1 3 Format A4 31 Defaults k 0 0 ISEED 1 k Contains the seed of the random number sequence k ISEED 2 3 k Contain the number of calls N to the generator that are performed for initial ization such that N 2ISEED 2 k 10 ISEED 3 k At present at most k 5 sequences are used Sequence 1
121. ing do not compile binaries just extract CORSIKA compilefile cached no checking to keep the CORSIKA compilefile cached no configure creating config status config status creating Makefile config status creating bernlohr Makefile config status creating dpmjet Makefile config status creating epos Makefile config status creating pythia Makefile config status creating herwig Makefile config status creating nexus Makefile config status creating urqmd Makefile config status creating src Makefile config status creating run Makefile config status creating doc Makefile config status creating lib Makefile config status creating include config h config status executing depfiles commands configure Optional packages not found or deactivated on this system FLUKA COAST ROOT PYTHIA Compile CORSIKA in lib Linux and copy executable in run Making install in src make 1 Entering directory src 16 cc E corsika F DHAVE CONFIG H I include traditional cpp o corsikacompilefile f 477 00 g fbounds check c corsika corsikacompilefile o test f corsikacompilefile f echo corsikacompilefile f if cc DHAVE CONFIG H I I I include g MT trapfpe o MD MP MF deps trapfpe Tpo c o trapfpe o trapfpe c then mv f deps trapfpe Tpo deps trapfpe Po else rm f deps trapfpe Tpo exit 1 fi 477 00 g fbounds check c o corsika qgsjet0lc o te
122. istclean Execute make distclean if CORSIKA is already installed once Remove all files produced by the installation but not the binaries in run and stop e e expert Activate expert mode with additional configuration steps e g force compilation in 64 bit mode e i install Execute make install if CORSIKA is already installed once Compile link and copy binaries into run but configure is not called at all except if it was never done before If Make files are not yet installed configure will be called once m make Execute make all if CORSIKA is already installed once Compile and link but do not copy binaries to run and configure is not called at all no option selection except if it was never done before If Makefiles are not yet installed configure will be called once 108 e no cache Do not use cached configuration e t dist Torunmake dist skips configuration e Configure options Any option can be transfered to configure for more informa tion use h or help but prefix bindir and libdir are already de fined in coconut You should not change this options Values defined in CC CCLAGS SCXX SCXXFLAGS SCPP SCPPFLAGS and SLDFLAGS environment variable are al ways used if defined To use the values defined in F77 and SFFLAGS environment variable in coconut the following environment variable has to be defined setenv CORSIKA USER COMP yes If
123. itionally some parameterized data contained within the data file pomtab dat are read in The latter will be generated at the first call within that directory from where you are calling COR SIKA This calculation needs c 20 min on DEC 3000 600 AXP with 175 MHz Later calls will read in this data file pomtab dat This file is written and read via logical unit 37 and GLAUBTAR DAT is read via unit 47 The binary file VUCLEAR BIN is read from unit 14 and fits only for computers which read data in the direct access mode according with the IEEE conventions DEC UNIX LINUX For other machines DEC VAX HP a different binary file is needed which you may get from CERN or from the author of DPMJET lt johannes ranft cern ch gt e The EPOS routines get user specified parameters from a scratch file via logical unit EPOPRM by default 97 and need some parameterized data contained within the data files epos inics epos iniev epos inilb epos inirj and epos initl If the latter files are not existent or do not fit with the user specified parameters they are established in a time consuming procedure some 100 h on a DEC 3000 600 AXP with 175 MHZ e The NEXUS routines get user specified parameters from a scratch file via logical unit NEXPRM by default 97 and need some parameterized data contained within the data files nerus inics nexus iniev nexus inirj and nexus initl If the latter files are not existent or do not fit with the user specified parameters
124. l 10 For the 577 layer a linear decrease is assumed which in case of ATMOD 0 uses 57 the same parameters as the U S standard atmosphere To be used with ATMOD O or 10 Limit is 0 lt 5 4 18 Atmospheric Parameters B i ATMB BATM BATM2 BATM3 BATM4 Format A4 AF Defaults 0 0 0 0 BATMi B parameters for 4 layers of atmospheric model 0 For the 5 layer a linear de crease is assumed with the same parameters as for the U S standard atmosphere To be used with ATMOD 0 or 10 Limits Z 0 4 19 Atmospheric Parameters C i ATMC 1 2 CATM3 CATM4 CATM5 Format A4 AF Defaults 0 0 0 0 for ATMOD 0 Format A4 5F Defaults 0 0 0 0 0 for ATMOD 10 CATMi C parameters for 4 layers of atmospheric model 0 or for 5 layers of atmospheric model 10 For the 577 layer a linear decrease is assumed which in case of ATMOD 0 uses the same parameters as the U S standard atmosphere To be used with ATMOD 0 or 10 Limits are CATMi gt 0 4 200 Atmospheric Layer Boundaries ATMLAY HLAY2 HLAY3 HLAY4 5 Format AF Defaults 4 D5 10 05 40 05 100 05 HLAYi Layer lower boundaries in cm for the layers of atmospheric model 0 and 10 A value of is adopted for the HLAY1 If not specified the default values of MODATM 1 are used for MODATM 0 and 10 For other models MODATM 0 Z 10 the default value
125. le output file using the particle type numbers 66 to 69 if their energy exceeds the cutoff energy ELCUT 1 To obtain this program version the NEUTRINO option has to be selected when extracting the FORTRAN code from the source file 3 5 13 NUPRIM Option for Primary Neutrinos With this program version showers induced by primary neutrinos can be simulated Possible primary particles are up to now Ve Ve Vu and If combining the NUPRIM option with the CHARM or TAULEP option also the v and the 7 neutrinos can be handled Because of the low cross sections of neutrino induced interactions it is recommended to fix the height of the primary interaction using the keyword FIXHEI page 55 As the first neutrino induced interaction is handled by the HERWIG code 18 a link 20 with the HERWIG rou tines is necessary HERWIG produces besides others secondary particles with charm Those particles can be treated by CORSIKA only if you combine the NUPRIM option with the CHARM option see page 38 Without specifying the CHARM option those charmed sec ondaries decay at the vertex and are not explicitely transported in CORSIKA Specifying the TAULEP option the tau leptons emerging from CC interactions of v or 7 neutrinos are treated explicitely in CORSIKA The interactions of secondary particles coming from the primary neu trino reaction are treated by the selected high energy rsp low energy hadronic interaction model or by NKG EGS4 Sec
126. le to make a UrQMD library liburqmd a from the UrQMD 1 3 cors FORTRAN files and then link it with your CORSIKA program pages 115 and 117 In your input file you may supply the keyword page 80 UROMD 0 Setting the first parameter FURQMD to false F the program will stop 3 3 Electromagnetic Interactions NKG EGS4 Option The NKG and EGS4 options are selected by flags of the input file keyword ELMFLG only A detailed description of the EGS4 program can be found in Ref 16 and the modifications applied to it are published in Ref 3 For using NKG and or EGS4 you have to activate the flags of the keyword page 66 ELMFLG in the input file 30 It must be emphasized that at the highest electron and y energies above 1017 eV the NKG op tion does not contain the Landau Pomeranchuk Migdal effect which is added to EGS4 which may alter the shower development by the decrease of the pair formation and bremsstrahlung cross sections with increasing energy Therefore the analytical NKG treatment deviates more and more from results gained by the EGS4 option For example in a y induced shower 1019 eV energy inclined with 0 60 without PRESHOWER option the maximum of the electron lon gitudinal development simulated by EGS4 is reached deeper in the atmosphere by 100 g cm slant depth than predicted by NKG 3 3 1 NKG Treatment The first flag activates the analytic NKG treatment of the electromagnetic component The l
127. lottracks 42 all three projections x y x z and y z The map files are written onto the directory DSN via the unit 55 and are named DATnnnnnn spec _ lt gt where spec stands for em mu or hd and lt proj gt stands for xy xz yz nnnnnn is the run number specified in the keyword RUNNR see page 51 These map files are basically two dimensional histograms containing the number of tracks in each xy xz yz bin The resolution of the maps is set via the three integer parameters IXRES TYRES and IZRES in the COMMON CRPLOTSH2 The unformatted map files consist of a two word header containing the horizontal and vertical resolution of the respective map file followed by the rows of map values These files are then easily processed further for example by map2png see below To control the plotting the keyword PLAXES followed by 6 parameters see page 83 might be used in the input file PLAXES 955 SES Ou The keyword PLCUTS 02 0 3 02 002 0 003 1 85 see page 83 serves to define energy cuts in the same order as those for the keyword ECUTS hadrons muons electrons photons see page 68 An additional parameter defines an upper bound on the time in ns passed since the first interaction while the final logical determines whether only track segments inside the three dimensional box given by the axis ranges should be plotted Via the keyw
128. ltaneously the electron lateral distribution on ground becomes slightly narrower With STEPFC 10 the CPU time is reduced by a factor of 1 7 relative to the default value A reduction of STEPFC will increase the computing time considerably e g with STEPFC 0 1 by a factor of z 5 Limits are 0 STEPFC lt 10 0 52With the INTTEST option the default value of this border is at 49 GeV rsp 101 GeV depending whether a high or low energy hadronic interaction model should be tested For testing of DPMJET EPOS NEXUS QGSJET and VENUS the default value is set to 49 GeV for SIBYLL to 60 GeV If none of those models is selected the default value is set to 101 GeV to test the models FLUKA GHEISHA or UrQMD 53In the CURVED option the NKG formulas are no longer valid therefore NKG flag is disabled automati cally in this option The NKG flag should be disabled in the COMPACT option as the resulting NKG parameters cannot be written out onto the particle output file 66 4 43 Radius of NKG Lateral Range RADNKG RADNKG Format A6 F Default 200 E2 RADNKG Gives the outer range radius in cm within which the lateral NKG distribution is calculated for 10 radii equidistant in logarithmic scale The inner radius is always kept at 100 cm Limit is RADNKG gt 100 4 44 Thinning Definition THIN EFRCTHN WMAX RMAX Format 4 Defaults 1 E 4 1 E30 0 0 EFRCTHN Factor which defines the energy fr
129. m of the photon with one nucleon 81 Format L Default F LSPEC If true spectators are plotted if false spectators are not plotted in the interaction test This keyword is only available in the INTTEST option 4 86 Interaction Test Diffraction Flag DIFOFF NDIF Format A6 I Default 0 NDIF Allows to select diffractive or non diffractive interactions only 0 diffractive and non diffractive interactions mixed non diffractive interactions only 2 diffractive inter actions only With the QGSJETOlc interaction model NDIF 2 cannot be selected With the EPOS NEXUS and QGSJET II models only NDIF 0 is possible This keyword is only available in the INTTEST option 4 87 Interaction Test Trigger Condition TRIGGER NTRIG Format A7 D Default 0 NTRIG Allows to select various trigger conditions for comparison with experimental data 0 accepts all events 1 accepts only events according to the UA5 experiment 54 trigger 2 accepts only events according to the CDF experiment 55 trigger 3 accepts only events according to the P238 experiment 56 trigger NTRIG 5 0 may be combined only with NDIF 0 This keyword is only available in the INTTEST option 4 88 Interaction Test Histogram Output HISTDS HISTDS Format A120 Defaults HISTO CORSIKA INTTEST HISTDS May be used to specify a name of the histogram output directory and data
130. machines 44 3 5 18 ROOTRACK Option Similar to the ROOTOUT option Sect 3 5 17 the ROOTRACK option selects C4 4 routines which directly transmit the path elements of all tracked particles to ROOT With the routines of the COAST USER LIB package the crossing of a particle track through the inclined observation plane specified by the keyword INCLIN see Sect 4 54 page 72 is calculated and the particle coordinates in the observation plane are written out to the file DATnnnnnn inclined binary see Sect 10 4 page 103 The ROOTRACK option is also necessary for the simulation of radio emission with REAS Radio Emission from Air Showers 25 Further details you find in the REAS manual on the web page of REAS 42 The ROOTRACK option cannot be combined with the COMPACT option The appropriate C routines used in the ROOTRACK option are available from the web pagehttp www ik fzk de rulrich coast and must be installed in a subdirec tory defined by the environment variable SCOAST_DIR Before the CORSIKA installation COAST must have been compiled and installed first To obtain this program version the ROOTRACK option has to be selected when extracting the FORTRAN code from the source file and root and COAST must be installed on your system 3 5 19 SLANT Option With the SLANT option the longitudinal distributions page 69 and Sect 10 6 page 103 are given in slant depth bins along the shower axis instead of vertical depth
131. mer version of CORSIKA and you want to use a corsika_compile file f as before you can optionally save this file during the installation process to compile it yourself The coconut script checks for all options if they can be used on your computer so comments appearing during the installation should be read carefully 2 2 1 Options At present CORSIKA versions may be generated with the following hadronic interaction mod els with their cross section for determining the mean free path between the interactions using the options DPMJET selects DPMJET 2 55 routines for the simulation of high energy hadron nucleus and nucleus nucleus collisions Also the DPMJET cross sections are selected EPOS selects the EPOS routines for the simulation of high energy hadron nucleus and nucleus nucleus collisions Also the EPOS cross sections are selected NEXUS selects the NEXUS 3 97 routines for the simulation of high energy hadron nucleus and nucleus nucleus collisions Also the NEXUS 3 97 cross sections are selected shell terminal a C compiler and FORTRAN compiler are included any UNIX based system 1070 principle any system could be used but only LINUX Mac OSX Dec SunOS have been tested 7 QGSJET selects QGSJETOlc routines for the simulation of high energy hadron nucleus and nucleus nucleus collisions Also the QGSJETOlc cross sections are selected QGSII selects QGSJET II 03 routines for the simulation of high en
132. n the UPWARD option with an upward primary particle the starting altitude must be below the observation level page 48 In the STACKIN option FIXHEI is needed to specify the altitude of the first externally treated interaction NISTTR Fixes the target of the first interaction 1 Nitrogen 2 Oxygen 3 Argon else random selection according to the atmospheric abundances This option is only applicable for high energy hadronic primaries i e primaries with an energy per nucleon of Ej gt HILOW see page 65 Also in the NUPRIM option it may be used In case of unstable hadronic pri maries and predetermined target the first interaction will not be a decay Limits are 0 lt FIXHEI lt border of atmosphere at 112 8E5 cm for atmospheric models 1 lt MODATM lt 9 MODATM gt 17 4 14 Skimming Incidence IMPACT HIMPACT 1 HIMPACT 2 Format A6 2F Default 0 0 HIMPACT 1 Lower value in cm for minimum altitude of horizontal shower axis 2 Upper value in cm for minimum altitude of horizontal shower axis The actual minimum altitude is selected at random out of this interval with uniform distribution Zenith angles given by the keyword THETAP page 53 are overridden by a calculation from the actual minimum altitude See UPWARD option page 48 Limits are OBSLEV 1 lt lt min FIXHEI FIXCHI border of atmosphere at 112 8 5 cm for atmospheric models 1 lt MODATM lt
133. n when extracting the FORTRAN code from the source file The Make file will link the compiled sibyll2 1 f and gheisha_ 2002d f codes rsp FLUKA library or UrQMD library with your CORSIKA program In your input file you may supply the keyword page 63 SIBYLL I 0 Setting SIBYLL to false F the simple HDPM routines are used see also Sect 3 1 3 page 26 The SIBYLL option needs about the same CPU time as the option NKG enabled EGS4 disabled SIBYLL activates also the inelastic hadronic interaction cross sections at higher energies which are supplied with the SIBYLL 8 program package They are based on QCD calculations details are given in 8 SIBYLL also delivers nucleus nucleus cross sections The SIBYLL cross sections are selected automatically when the SIBYLL option has been used for extracting the FORTRAN code from the source file In your input file you may supply the keyword page 64 SIBSIG T Setting SIBSIG to false F you will use the default cross sections of CORSIKA as described in Ref 3 3 17 VENUS Option VENUS 10 Very Energetic NUclear Scattering is a program developed to simulate ultra relativistic heavy ion collisions The actual version is VENUS 4 12 For using VENUS you first have to select the VENUS option when extracting the FORTRAN code from the source file The Make file will link the compiled venus f and gheisha_2002d f codes rsp FLUKA library or UrQMD library with yo
134. nes which might be used in combination with the ROOTOUT and ROOTRACK options a subdirectory doc containing apostscript file CORSIKA PHYSICS ps containing the physics description of COR SIKA Report 6019 The file CORSIKA_PHYSICS pdf contains it in Acrobat format bernlohr 1 44 tar gz is automatically extracted if needed 3COAST cors tar gz is automatically extracted if needed 3 a postscript file CORSIKA_GUIDE69xx ps giving this User s Guide The file COR SIKA_GUIDE69xx pdf contains it in Acrobat format a references tex giving the actual references to CORSIKA and the hadronic interaction models in format to be used in your publications e a subdirectory dpmjet containing source files of the DPMJET II 55 model dpmjet253c f dpmjet254 f dpmjet255c f dpmjet256c f a subdirectory epos containing the source package for the EPOS model a subdirectory herwig where to install HERWIG and containing a README file in a subdirectory include containing the con fig h in file which is needed by configure to do config h The file config h contains all the preprocessor commands needed by CORSIKA a subdirectory 1ib together with a script file libtool are created when compiling COR SIKA The subdirectory contains all object files and libraries a subdirectory nexus containing the source package for the NEXUS model a subdirectory pythia where to install PYTHIA and containing a
135. ng are skipped Limits are 180 lt GLONG lt 180 90 lt GLATI lt 90 1965 lt GRFYEAR lt 2015 This keyword is only available in the PRESHOWER option 4 24 DPMJET Selection Flag DPMJET FDPMJT LEVLDB Format A6 L I Defaults T 0 FDPMST If true the DPMJET routines are used to treat the high energy hadronic interac tions If false the HDPM routines are used to treat the high energy hadronic interactions LEVLDB Gives amount of debug output for the DPMJET code in case of DEBUG With in creasing value up to 8 the debug output becomes more and more detailed This output cannot be redirected and always appears on unit 6 Limits are 0 lt LEVLDB lt 8 This keyword is only available in the DPMJET option 4 25 DPJSIG Selection Flag DPJSIG FDPJSG Format A6 L Default T FDPJSG If true the DPMJET high energy hadronic cross sections are used If false the default cross sections as described in Ref 3 are used This keyword is only available in the DPMJET option 4 26 EPOS Selection Flag EPOS FNEXUS ISHON Format A5 L I Defaults T 0 FNEXUS If true the EPOS routines are used to treat the high energy hadronic interactions If false routines are used to treat the high energy hadronic interactions ISHON Determines amount of debug output for the EPOS routines With increasing number 9The print statements within the PRESHOWER C r
136. nic interaction model and an optional _int if you select the INTTEST option As a consequence you can select different model combinations on different systems without any conflict HDPM DPMJET EPOS NEXUS QGSJET QGSII SIBYLL or VENUS 2fluka gheisha or 23 n case of conflict using different options but with the same models for instance the program will ask you if you want to rename the binary file 18 2 3 Data Files 2 3 1 Input Files To run a simulation one needs to read several input files These are e The Glauber tables to derive nucleon nucleus and nucleus nucleus cross sections from hadron nucleon cross sections are listed in file NUCNUCCS which is 2873 lines long They are read via logical unit NUCNUC NUCleus NUCleus interactions by default 11 e The cross sections and branching ratios for the EGS4 routines are contained in the data files EGSDAT6_x x with a length of 3021 lines each These files differ in the lowest kinetic energy to be followed within a range between 3 MeV x x 3 and 50 keV x x 05 Only one of the sets is selected by the program and connected to the logical unit KMPI by default 12 in a manner appropriate to the lowest energy of em particles specified by the user As the muon nuclear interactions use the routines to treat photonuclear interactions always an EGSDAT6_x x file must be read in e The DPMJET routines need the Glauber tables named GLAUBTAR DAT Add
137. nkov detectors in x direction number of Cherenkov detectors in y direction grid spacing of Cherenkov detectors in x direction in cm 89 grid spacing of Cherenkov detectors in y direction in cm length of each Cherenkov detector in x direction in cm length of each Cherenkov detector in y direction in cm 92 Cherenkov output directed to particle output file 0 or Cherenkov output file 1 Table 9 Structure of event header sub block to be continued EVTH 77 has the following contents if converted to an integer with suitable rounding applied bit 1 CERENKOV option compiled in 2 IACT option compiled in 3 CEFFIC option compiled in 4 ATMEXT option compiled in 5 ATMEXT option used with refraction enabled 6 VOLUMEDET option compiled in 7 CURVED option compiled in see also EVTH 79 9 SLANT option compiled in 11 21 table number for external atmosphere table but limited to 1023 if the number is larger 97 Event header sub block continued Contents of word as real numbers R 4 angle in rad between array x direction and magnetic north flag for additional muon information on particle output file step length factor for multiple scattering step length in EGS4 Cherenkov bandwidth lower end in nm Cherenkov bandwidth upper end in nm number i of uses of each Cherenkov event x coordinate of it core location for scattered events in cm y coordinate of it core location for scattered events in cm SIBYLL interacti
138. nt of the particle momentum vector i e with respect to North proceeding counter clockwise This is shown in Fig 1 Attention This definition disagrees from definitions of other air shower simulation programs and from the conventions of the Auger experiment 86 7 CORSIKA Within CORSIKA uniform units for the various dimensions are used as far as possible But there are deviations at that program parts which are coupled to CORSIKA Table 3 gives an overview on the used units DPMJET CORSIKA GHEISHA SIBYLL EPOS NEXUS QGSJET Quantity VENUS length energy mass time magn field density mass overburden angle wavelength 1 For output files also nsec is used For in and output files also is used 3 In some subroutines also TeV is used Table 3 Units used in CORSIKA and the coupled programs 8 Particles CORSIKA CORSIKA is able to treat the particles that are listed in Table 4 The particle codes have in general been chosen according to the convention in the GEANT detector simulation code 28 Exceptions are vector mesons w and p and resonances and A the n particles which are split in 4 types according to their decays in the HDPM routines the different types of neutrinos to be generated in the NEUTRINO option the nuclei and the Cherenkov photons The codes of the charmed particles correspond with those of DPMJET The particles with codes between 116 and 173 are only available in t
139. nts to the zenith opposite to Fig 1 page 86 and defines a horizontal plane PHINCL angle in deg of normal vector of inclined observation plane coordinates are defined in the standard CORSIKA output coordinate system see Fig 1 page 86 with its origin at the point where the shower axis hits the sea level ATTENTION CORSIKA discards all particles below the height of the lowest standard obser vation level see Sect 4 53 for definition of so as soon as the inclined observation plane drops below the lowest standard horizontal observation level there will be no particles recorded any more Particles on the inclined plane will be stored in a coordinate system within the inclined plane with the origin at the core point where the shower axis intersects the observation level This keyword is only available in the ROOTRACK option 4 55 Observation Level Curvature CURVOUT FCURVOUT Format A7 L Default T FCURVOUT If true the observation level is a sphere following the Earth curvature at an altitude H OBSLEV 1 and X Y in the output file are replaced by X Y which can be used to calculate the angles necessary to obtain X Z in a Cartesian frame defining 0 and the spherical coordinates of the particle as _ XY H atan2 Y X 2 with Rgar n 637131500 cm At the observation level OBSLEV 1 the Cartesian coordinates can be obtained using D
140. nucleus or nucleus nucleus collisions and here the results start to disagree due to the simpler modeling in HDPM If one is interested in differences of air showers induced by different nuclei one probably gets more realistic results by the detailed simulation with other models DPMJET EPOS NEXUS QGSJET SIBYLL VENUS than with the HDPM routines As the HDPM routines are default you have nothing to specify when extracting the FORTRAN code from the source file But the compiled gheisha_2002d f code rsp FLUKA library or UrQMD library will be linked with your CORSIKA program 3 1 4 NEXUS Option neXus 11 NEXt generation of Unified Scattering approach combines features of the former VENUS 10 and QGSJET 6 with extensions enabling a safe extrapolation up to higher en ergies using the universality hypothesis to treat the high energy interactions 11 It handles nucleus nucleus collisions with an up to date theoretical approach The most actual version is NEXUS 3 97 Forusing NEXUS you first have to select the NEXUS option when extracting the FORTRAN code from the source file The Makefile will compile nexus xxx f in the libnexus a library and then link it with the compiled gheisha_2002d f code rsp FLUKA library or UrQMD library and with your CORSIKA program In your input file you may supply the keyword page 62 NEXUS T 0 Setting NEXUS to false F the simple HDPM routines are used see also Sect 3 1 3 above The standard pa
141. numbers and energy deposits may be written to file DAT nnnnnn long The output DATnnnnnn dbase DATnnnnnn nfo is destinated to be used in a data base for examining the content of an air shower library In the ROOTRACK ver sion Sect 3 5 17 page 44 with the keyword INCLIN Sect 4 54 page 72 an output file DATnnnnnn nclined binary is written which is structured as the standard particle output file DATnnnnnn 10 1 Control Printout txt File The simulation run produces a printout txt file unit MONIOU by default standard output that allows to control the simulation and informs about the general run the program version with interaction model the selected options steering keywords physical constants the used atmospheric model and the primary particle about 200 lines For each shower it prints roughly 400 lines containing the random number generator status time at beginning of a shower the primary particle at the place of the first interaction the number of secondaries reaching the observation levels with energies above ECTMAP page 74 the stack statistics internal and external stack usage energy multiplicity and energy elasticity relations interaction statistics for nucleons pions kaons and strange baryons per kinetic energy interval an interaction length statistics for the above particles and a decay statistics for muons summaries of secondaries for each observation level NKG electromagnetic
142. o respect the atmospheric absorption mirror reflectivity and photomul tiplier quantum efficiency of Cherenkov light This option is only available in connection with the CERENKOV option CERENKOV selects code for additional generation of Cherenkov light It needs the simulation with EGS4 CERWLEN selects Cherenkov code including the wavelength dependent generation of Cher enkov photons and respects their wavelength dependent refraction of the atmosphere This option is only available in connection with the CERENKOV option CHARM selects code for the explicite treatment of charmed particles only in connection with interaction codes which produce them and the 7 lepton rsp the 7 neutrinos in connection with the NEUTRINO or NUPRIM option CHARM excludes the TAULEP option COMPACT selects compacted output format for the particle file unit MPATAP which is different from the standard output but better suited for simulations of very large numbers of low energy showers which produce mostly no or only very few particles CURVED selects special code to treat showers with large zenith angles 70 lt 0 lt 90 EHISTORY selects additional code to bring in combination with the MUADDI or EMADDI keyword additional information on the muon and or electron and photon histories to the parti cle output file IACT selects code for simulation of Imaging Atmospheric Cherenkov Telescope arrays This option is only available in connection with the CER
143. o treat the high energy interactions 11 Compared to NEXUS many technical problems have been solved and the screening effects have been sim plified using a more phenomenological approach mainly based on the recent RHIC data In addition high density effects have been included The most actual version is EPOS 1 99 For using EPOS you first have to select the EPOS option when extracting the FORTRAN code from the source file The Make file will compile epos in the libepos a library and then link it with the compiled gheisha_2002d f code rsp FLUKA library or UrQMD library and with your CORSIKA program In your input file you may supply the keyword page 60 EPOS T 0 Setting EPOS to false F the simple HDPM routines are used see also Sect 3 1 3 below The standard parameters for EPOS are set in subroutine aaset of the epos bas xxx f file If in your calling directory the data sets epos inics epos iniev epos inilb epos inirj and epos initl are not existent or not compatible with the selected parameters they will be calculated at the first call of subroutine psainz of epos sem xxx f which takes some 100 h on a DEC 3000 600 AXP with 175 MHz Normally all parameters of EPOS are set by subroutine aaset of the epos bas xxx f file called from subroutine nexini In special cases it may be necessary to overwrite one or more of these parameters or to rename the data files to identify epos inizz files established for different pa rame
144. ocesses covered by GHEISHA may be found in Ref 14 The GHEISHA version is taken as distributed in October 17 1994 with the GEANT package 28 version 3 21 03 by CERN Recently some errors were eliminated using fixes obtained from SLAC 29 and now all variables are used in double precision To discriminate against the uncorrected single precision GHEISHA version it is renamed to gheisha_2002d f GHEISHA is used in CORSIKA to calculate the elastic and inelastic cross sections of hadrons below 80 GeV in air and their interaction and particle production The Make file will link the compiled gheisha_2002d f code with your CORSIKA program if you have selected the GHEISHA option 3 2 3 URQMD Option UrQMD Ultra relativistic Quantum Molecular Dynamics is an interaction package designed to treat low energy hadron nucleus interactions A detailed description of this model may be found in Ref 15 UrQMD 1 3_cors is used in CORSIKA to perform the elastic and inelastic interactions of hadrons below 80 GeV in air The actual linking routines operate with the special UrQMD 1 3 cors version adapted to CORSIKA For using UrQMD you first have to select the URQMD option when extracting the FORTRAN code from the source file For compilation of the compilefile f the UrQMD 1 3 cors include files boxinc f colltab f comres f coms f inputs f newpart f and options f must be avail able So the coconut script will install this files if needed before doing a Makefi
145. olerated and will lead to an error stop Limits are ULIMIT EFRCTHN THINRAT lt 1 1016 eV for ULIMIT see keyword ERANGE page 53 1 1074 lt WEITRAT lt 1 106 This keyword is only available in the THIN option 4 47 Energy Cut Offs ECUTS ELCUT i i 1 4 Format A5 4 Defaults 0 3 0 3 0 003 0 003 ELCUT z The low energy cut off in GeV of the particle kinetic energy may be chosen differently for hadrons without 70 2 1 muons i 2 electrons i 3 and photons including 7 s 4 4 For nuclei ELCUT 1 is applied to the energy per nucleon It is in the responsibility of the user to choose the cut off values in a reasonable way not to 55In the Slowenian thinning 46 an is defined which gives the inverse of WEITRAT There the weight limit 15 defined for em particles and from this the weight limit for hadrons and muons is derived by 56For the INTTEST option Defaults 0 0 0 0 and all limits are ELCUT i gt 0 68 eliminate those parent particles which might decay to secondaries which you are looking for in the investigated problem e g decay of muons to electrons Limits are ELCUT 1 gt 0 05 ELCUT 2 gt 0 01 ELCUT 3 ELCUT 4 gt 0 00005 The value of ELCUT 3 is also taken as threshold value for the NKG calculation In this case an upper limit of ELCUT 3 lt 0 08 is recommended 4 48 Time Cut Off IIMLIM DSTLIM Format
146. om an interaction 46 none 107 107 107 10 7 Time min 98 51 7 2 12 016 particles 413078 58313 11466 2211 419 Table 2 Computing times and number of particles for various thinning levels without application of weight limits and radial thinning which would exceed a specified weight limit are excluded from the thinning algorithm Us ing different weight limits for em particles and hadronic including muonic particles enables a drastic reduction of computing time if the user s interest is focused onto a precise lateral distribution of muons on the expenses of larger fluctuations of the em part A third algorithm to save space on disks reduces the number of particles close to the shower core where anyway the detectors will saturate Particles arriving at the detector level within a selected core distance rmaz are selected at random with a probability prob r rmax and when surviving their weight factor is multiplied with the inverse of this probability irrespective of exceeding the weight limit This radial thinning is not effective for the table output DAT nnnnnn tab see keyword PAROUT page 74 and Sect 10 7 page 104 nor for the datnnnnnn Ihbook file generated in the ANAHIST and or AUGERHIST versions Via the keyword page 67 THIN EFRCTHN WMAX RMAX you may specify the energy fraction EFRCTHN of the primary energy below which the thinning process becomes active Above this energy no thinning will take place
147. ompilers which lead to an error stop during linking Linking is performed e g by 87 GNU 877 compilers the options c C fno automatic finit local zero Wunused m32 Wuninitialized malign double O might be used 55Usage of csh shell is assumed In other shells sh or ksh you should use ulimit d unlimited and ulimit s unlimited 89See footnote at DPMJET compilation page 114 114 f77 corsika compilefile o gheisha_2002d o epos x o o corsika6990 where the compiled EPOS program parts are expected to be available within the subdirectory epos NEXUS option The compiler procedures of the standard case see begin of this subsection A 1 should be used To compile the nexus xxx f source files in 5 you should use the Make file ka available with NEXUS omitting the link step For compiling and linking NEXUS you presumably have to give limit datasize unlimited limit stacksize unlimited to overcome the small default values of many compilers which lead to an error stop during linking Linking is performed e g by f77 corsika compilefile o gheisha 2002d o nexus x o o corsika6990 where the compiled NEXUS program parts are expected to be available within the subdirectory nexus FLUKA option For compiling the CORSIKA FLUKA version of the corsika_compilefile f the FLUKA include files should be available in the subdirectory from which you are calling the compiler to include them into th
148. on 4 32 QGSJET Selection Flag QGSJET FOGS LEVLDO Format A6 L I Defaults T 0 FQGS If true the qgsjet II 03 rsp QGSJETOlc routines are used to treat the high energy hadronic interactions If false the HDPM routines are used to treat the high energy hadronic interactions LEVLDQ Gives amount of debug output for the qgsjet II 03 rsp QGSJETOlc code in case of DEBUG With increasing value up to 4 the debug output becomes more and more detailed This output cannot be redirected and always appears on unit 6 Limits are 0 LEVLDQ lt 4 This keyword is only available in the QGSJET option 4 33 QGSSIG Selection Flag QGSSIG FOGSSG Format L Default T FQGSSG If true the qgsjet II 03 rsp QGSJETO1c high energy hadronic cross sections are used If false the default cross sections as described in Ref 3 are used This keyword is only available in the QGSJET option 4 34 SIBYLL Selection Flag SIBYLL FSIBYL ISDEBUG Format L Default T 0 FSIBYL If true the SIBYLL routines are used to treat the high energy hadronic interactions If false routines are used to treat the high energy hadronic interactions ISDEBUG Debug level with increasing level the SIBYLL 2 1 debug output becomes more and more detailed This output cannot be redirected and always appears on unit 6 This keyword is only available in the SIBYLL option 63 4 35 S
149. on flag 0 2 no SIBYLL 1 vers 1 6 2 vers 2 1 SIBYLL cross section flag 0 2 no SIBYLL 1 vers 1 6 2 vers 2 1 QGSJET interact flag 0 2no QGSJET 1 2QGSJETOLD 2 QGSJETOlc 3 2QGSJET IT QGSJET X sect flag 0 no QGSJET 1 2QGSJETOLD 2 QGSJETOlc 3 2QGSJET IT DPMJET interaction flag 0 2no DPMJET 1 DPMIJET DPMJET cross section flag 0 2no DPMJET 1 DPMJET VENUS NEXUS EPOS cross section flag O neither 1 2 VENUSSIG 2 3 NEXUSSIG 4 EPOSSIG muon multiple scattering flag 1 Moli re 0 Gauss NKG radial distribution range in cm EFRCTHN energy fraction of thinning level hadronic EFRCTHN THINRAT energy fraction of thinning level em particles actual weight limit WMAX for thinning hadronic actual weight limit WMAX WEITRAT for thinning em particles max radius in cm for radial thinning inner angle of viewing cone VIEWCONE in outer angle of viewing cone VIEWCONE in transition energy high energy low energy model in GeV skimming incidence flag 0 standard 1 skimming altitude cm of horizontal shower axis skimming incidence starting height cm flag indicating that explicite charm generation is switched on flag for hadron origin of electromagnetic subshower on particle tape not used flag for observation level curvature CURVOUT 0 flat 1 curved not used Table 9 continued Structure of event header sub block 98 Particle data sub block up to 39 particles 7 words each
150. ondary neutrinos are explicitly generated only if the NEUTRINO option page 41 is selected but they are not treated by HERWIG Initiating a shower with non neutrino primary particles will not call the HERWIG routines 4 Sequence 5 of the CORSIKA random generator is foreseen for HERWIG therefore you should initialize it see Sect 4 3 page 52 For using the NUPRIM version you first have to select the NUPRIM option when extracting the FORTRAN code from the source file The Makefile will compile the HERWIG FORTRAN routines and link them with your CORSIKA program A combination of the NUPRIM option with the INTTEST option is not possible 3 5 14 PLOTSH Shower Plot Production Option In the PLOTSH option the start and end points of each particle track are written to extra files see Table 1 page 21 separate files are used for the electromagnetic muonic and hadronic component Each track is written unformatted as one block consisting of 10 real 4 numbers Particle identification Energy in GeV Xstart Ystart Zstart all in cm Tstart in sec Xend Yend Zend all in cm and Tend in sec In case of THINning the particle Weight is added at the end of each block Plots may be constructed from the content of these files by using the plottracks program The program plottracks3c f available in src converts the particle track maps generated by the PLOTSH option into PPM image files readable by xv plottracks is automatically compiled
151. onging to it can be obtained from Karlsruhe Institute of Technology by anonymous ftp Before access the host name of your computer is checked for authorization If you want to transfer CORSIKA files to your computer system you might pro ceed as follows commands that you have to type are underlined ftp ftp ik fzk de Trying 141252567 185 Connected to ikserv fzk de 220 ftp ik FTP server Version number amp date ready Name ftp ik fzk de username anonymous or ftp 331 Guest login ok send your complete e mail address as password Password your_mail_address 230 PROBLEMS 230 If your FTP client crashes or hangs shortly after login please try 230 using a dash as the first character of your password This will 230 turn off the informational messages that may be confusing your 230 client Administrative contact bekk ik fzk de 5urqmdl 3 cors tar gz is automatically extracted if needed 5 230 230 230 Welcome to ftp ik fzk de the 230 xxxxxx INFOandSOF T Server 230 Forschungszentrum Karlsruhe Institut fuer Kernphysik 230 KASCADE Collaboration Karlsruhe 230 230 230 current directory local time date amp time 230 You are user number out of a possible total of 10 in your domain class 230 All transfers to and from ftp ik fzk de are logged If you don t like this 230 then disconnect now 230 230 Guest login ok access restrictions apply Remote
152. ongitudinal electron numbers and pseudo age parameters are calculated every 100 g cm above the lowest observation level and the lateral electron densities are calculated for a radial grid of 80 points at the two lowest observation levels The inner grid radius is fixed at 100 cm while the outer radius RADNKG in cm is selected by the keyword page 67 RADNKG 200 E2 Also lateral pseudo age parameters are calculated As the NKG formulas do not take into account the curvature of the Earth s surface for the CURVED option the NKG option is suppressed As with the COMPACT option the NKG parameters cannot be written out onto the particle file the NKG flag must be disabled in this case 3 3 2 EGS4 Treatment The second flag of the keyword ELMFLG activates the full Monte Carlo treatment of the elec tromagnetic component by the EGS4 package Both flags may be activated or deactivated inde pendently No special option for extracting the FORTRAN code from the source file is required By selecting the CERENKOV option the EGS4 routines are activated automatically In most applications especially Cherenkov radiation from showers induced by primaries with energies in the GeV range an abbreviated treatment of the multiple scattering of electrons within the EGS4 code is not recommended If you can afford a lower quality of your simulations but no long computing times you may specify an enlarged step length factor STEPFC by the keyword page 66 S
153. ons are selected automati cally when the NEXUS option has been used for extracting the FORTRAN code from the source file In your input file you may supply the keyword page 62 NEXSIG Setting NEXSIG to false F you will use the default cross sections of CORSIKA as described in Ref 3 The nexus inputs in run subdirectory is an example input file to run CORSIKA with NEXUS 3 1 5 QGSJET Option QGSJET 6 7 Quark Gluon String model with JETs is a program developed to describe high energy hadronic interactions using the quasi eikonal Pomeron parameterization for the elastic hadron nucleon scattering amplitude The hadronization process is treated in the quark gluon string model The most actual version is QGSJET II 03 For using QGSJET you first have to select the QGSJET or QGSII options when extracting the FORTRAN code from the source file Without QGSII you will extract the link routines for the older QGSJETOIc program The Makefile will link the compiled qgsjet 11 03 f rsp qgsjetOlc f and gheisha 2002d f codes rsp FLUKA library or UrQMD library with your CORSIKA program The qgsjet 11 03 f package will behave differently compared with the older qgsjetOle f In your input file you may supply the keyword page 63 QGSJET T 0 Setting QGSJET to false F the simple HDPM routines are used see also Sect 3 1 3 page 26 If in your calling directory the data sets ggsdat II 03 and sectnu II 03 rsp QG S D 01 an
154. ord PLOTSH the PLOTSH2 option is enabled or disabled see page 83 This option is not recommended for ordinary shower production To obtain this program version the PLOTSH2 option has to be selected when extracting the FORTRAN code from the source file The C program map2png available in src converts the particle track maps generated by the PLOTSH2 option into PNG image files The only prerequisite needed by the program is libpng which is included in virtually all recent LINUX distributions If this library is not available for your system please use PLOTSH option instead map2png is automatically compiled when the PLOTSH2 option is selected The program map2png reads in the map files specified on the command line via the path to DATnnnnnn and combines them into a single PNG image of the same resolution as the maps By default the electromagnetic muonic and hadronic maps are taken as the red green and blue channels of the RGB image respectively However it is possible to specify other colors to be used for the different particle types The projection to be used as well as whether to use a linear or logarithmic color scale can be specified on the command line To see a list of options simply run map2png without arguments 38Note that on LINUX systems the header and each row are preceded and followed by an additional word 3 90cc Lpath to libpng lpng lm map2png c o map2png The bracketed option is only needed if the pat
155. ormation about the simulation run itself This standard output comes via the logical unit MONIOU MONItor OUtput by default 6 In case of a debugging run very much information is written to the logical unit MDEBUG Monitor for DEBUGging by default 6 Further details on this file are given in Sect 10 1 page 92 The second output stream contains the information about all the particles that reach the observation level It gets the file name DAT nnnnnn and is written onto the output directory DSN keyword DIRECT page 74 via output unit MPATAP PArticle TAPe by default 90 as sequential unformatted FORTRAN file 9 nnnnnn is the run number specified in the keyword RUNNR page 51 This output may be suppressed see key word DIRECT and keyword PAROUT page 74 Further details on this file are given in Sect 10 2 page 94 For the ROOTOUT version with an inclined observation plane a binary data output is written to the file named DAT nnnnnn nclined binary The format is identical to the normal binary output data besides the fact that all coordinates are given within the in clined plane with the origin at the intersection of the shower axis with the inclined ob servation plane Further details on this file are given in Sect 10 4 page 103 Optionally a table of the number of the binned 7 e and u particles might be written out to the file DAT nnnnn tab onto the output directory DSN keyword DIREC
156. ot available in the STACKIN option 4 8 Zenith Angle Definition IHETAP IHETPR 1 THETPR 2 Format A6 2F Defaults O 0 THETPR 1 Low edge of zenith angle range of primary particle in THETPR 2 High edge of zenith angle range of primary particle in The zenith angle is selected at random out of this interval in a manner which respects equal particle fluxes from all solid angle elements of the sky and a registration by a horizontal flat detector arrangement THETPR is the angle of incidence at a horizontal detector THETPR 46Tn the case you use a volume detector sphere or a vertical long string detector instead of a flat horizontal de tector you should respect this by selecting the preprocessor option VOLUMEDET for sphere or VOLUMECORR for vertical long string to get the angular dependence of the shower intensity as observed with such detectors see Sect 3 5 25 page 49 53 0 is vertical If THETPR 1 2 the zenith angle is fixed at this value Limits are 0 lt THETPR lt 70 4 9 Azimuth Angle Definition PHIP PHIPR 1 PHIPR 2 Format A4 2F Defaults O 0 PHIPR 1 Low edge of azimuth angle range of primary particle in PHIPR 2 High edge of azimuth angle range of primary particle in The azimuth angle is selected at random out of this interval If PHIPR 1 PHIPR 2 the azimuth angle is fixed at this value For amp 0 the
157. ou change corsika F doing simply coconut make will produce a corsika executable file in src You can then copy this file into run to use it with all the data files 109 to have binary files with different options If dev is not used any more you will have to type coconut distcleanormake distcleanin corsika 6990 first We strongly recommend to use this scheme instead of the traditional compile file f because it is the easiest way for you and for us if later this modification has to be implemented in the official release of CORSIKA with proper preprocessor commands or if you want to use your modifications with different CORSIKA options If you prefer to work on compile file f anyway you can use the produced Make files to compile it To produce the Make files use dev note the dev option select your options and at the end save the source code and do not compile Then you only have to rename your source file corsika V E R OS HIGH low compilefile f to compile file and then you have to type make in src to compile or make install in your corsika 6990 directory to compile and link to get a binary file In this case you should not use coconut any more because this will not take into account your modifications and even overwrite the compile f ile f Of course if you already used some home made Make files with a former version of CORSIKA you can use it with this compile f ile f 12 In Case o
158. outines write only to the standard output A redirecting of the standard output to a logical unit differing from 6 see keyword OUTPUT page 75 usually will not affect the output of the PRESHOWER C routines 60 ISHON 0 the output becomes more and more detailed This output appears on the unit MDE BUG For more information look into the EPOS documentation Additional debugging is effective by setting print parameters using EPOPAR print This debug output is written to ifch file see Table 1 page 21 Limits are 0 ISHON lt 9 This keyword is only available in the EPOS option 4 27 EPOS Parameters EPOPAR parcha Format A74 Defaults parcha Command line to be read by subroutine aread of program block epos bas xxx f The possible command lines are described in the EPOS documentation Use lower case charac ters Lower case characters of parcha are not converted to capitals Do not use the commands application set nevent run or stop within your input parameters these will cause unpre dictable results or crashes Only epos inivx names might be changed by standard users This keyword is only available in the EPOS option 4 28 EPOSIG Selection Flag EPOSIG FNEXSG Format A6 L Default T FNEXSG If true the EPOS high energy hadronic cross sections are used If false the de fault cross sections as described in Ref 3 are used This keyword is only available in the EPO
159. pos199 cors tar gz file in the epos subdirectory The 21 NEXUS 3 97 program files with the 5 include files and the 4 data files are collected within the nexus3 97 cors tar gz file in the nexus subdirectory The preprocessor option IBMRISC selects the routines date and clock available on IBM RS6000 machines If necessary you might select the option TIMERC or you should adapt subroutine prtime to call the routines of your system for date and time The options BYTERECL OLDDATE OLDDATE2 IBMRISC and TIMERC are only available in connec tion with the UNIX option and can not be selected if it s not adapted to your system 14 Automatically unpacked if selected 12 The load modules of the FLUKA 2011 library routines and the FLUKA data files may be down loaded after being authorized from the official FLUKA web page http www fluka org and properly installed on your machine by setting the envi ronment variable FLUPRO For further information on the FLUKA package you may consult the FLUKA web page or contact A Ferrari The HERWIG routines needed for the NUPRIM version may be downloaded from http hepwww rl ac uk theory seymour herwig and adapted according to the README file in the herwig subdirectory see Sect A 1 page 116 The PYTHIA 6 412 routines 19 needed in connection with QGSJET for the treatment of charmed particles or the 7 leptons and 7 neutrinos may be downloaded from http www thep lu se torbjorn Pythia html
160. r QGSJET for other models the cross sections are not defined This keyword is not available in the STACKIN option 52 4 6 Energy Range ERANGE LLIMIT ULIMIT Format A6 2F Defaults 1 E4 1 E4 LLIMIT Lower limit and ULIMIT Upper limit of the primary particle energy range in GeV The primary energy is selected at random out of this interval If LLIMIT ULIMIT the primary energy is fixed at this value The energies are total energies and include the particle rest mass Limits are LLIMIT gt HILOW by default 80 GeV nucleon for nuclei see page 65 below this limit a simple superposition model is used ULIMIT lt 1 E11 GeV for primary photons and electrons but keep in mind that no LPM effect is included in NKG for primary hadrons and nuclei no upper limit is recommended but the user should take care not to over stretch the selected hadronic interaction model See also Ref 21 It is recommended for HDPM ULIMIT lt 1 10 eV and for VENUS ULIMIT lt 2 107 eV This keyword is not available in the STACKIN option 4 7 Slope of Spectrum ESLOPE PSLOPE Format A6 F Default 0 PSLOPE Exponent y of differential primary energy spectrum The primary energy is taken at random from an exponential energy spectrum of the form dN dEo PSLOPE has no meaning in case of fixed primary energy The energies are total energies and include the particle rest mass This keyword is n
161. r detaillierten Simulation von ausgedehnten Luftschauern die durch hochenergetische kosmische Strahlung ausgel st werden Die vorliegende Anleitung erl utert die Installation des Programms alle n tigen Eingabedateien die Wahl der Simula tionsparameter und die Struktur der Ausgaben des Programms ii Contents 1 Introduction 2 Installation 2 1 2 2 2 9 3 Program Options 3 1 3 2 3 3 3 4 3 5 CORSIKA Filesi gore ar Dre Br br eier Beer Program File Preparation 22 1 ZODUOHS xw sce tv 48 tea Br ne a 22 2 4 Example ec c te CM RIS CORO Cd ee Data Files aa ac A ORA QUEUE CUIR QUU QUEUE a dog Sos npt Files 125 Bok fee 212 2 SDUIpUL BIS ox See dew eei High Energy Hadronic Interaction ILL DPMIETOpHON 5 2225 22 5I 8 S 34 2 EPOS OPON 12 2 aded uer de ure key www ass 3 13 oo rd retrace en rera eu ce SLA NEXUS Options toste ole Tee moyen 91 5 FOGSIET ODUO c coe ker ur dece ar teet dett RT 316 SIBYEL OPTION eot oo PL JET VENUS o s 222094 cw amp CN BUS CN XU HCM S Low Energy Hadronic Interaction Models 321 F
162. r shower library an optional output file containing a run summary is written to DAT nnnnnn dbase on the directory DSN keyword DIRECT page 74 via output unit MDBASE Data BASE by default 45 ac tivated by keyword DATBAS page 78 nnnnnn is the run number specified in the keyword RUNNR page 51 Using the AUGERINFO option the name of this file will be DATnnnnnn info and the formats are adapted to the requirements of the Auger experiment Further details on this file are given in Sect 10 8 page 104 e The PLOTSH files contain all tracking steps for each particle with start and end point to produce demonstration plots of the development of showers They are written onto the directory DSN via the units 55 file DAT nnnnnn track for em particles 56 file DATnnnnnn track_mu for muons and 57 file DAT nnnnnn track_hd for hadrons see Sect 3 5 14 page 42 nnnnnn is the run number specified in the keyword RUNNR page 51 e The PLOTSH2 map files are basically two dimensional histograms containing the num ber of tracks in each xy xz yz bin Details are given in Sect 3 5 15 page 42 The map files are named DATnnnnnn lt spec gt _ lt proj gt map where lt spec gt stands for em mu or hd and lt proj gt stands for xy xz yz They are written onto the direc tory DSN via the unit 55 nnnnnn 1s the run number specified in the keyword RUNNR page 51 e The inte
163. raction model Limits depend on the used interaction model for most high energy hadronic interaction models the low energy limit is in the range of 80 GeV for SIBYLL 60 GeV while most low energy models enable a limit as high as several 100 GeV 4 41 Electromagnetic Interaction Steering Flags ELMFLG FNKG FEGS Format A6 2L Defaults T F FNKG If true the NKG option is switched on for calculating the electromagnetic sub cascades analytically For the electron kinetic energy threshold the value of ELCUT 3 is taken keyword ECUTS page 68 If false NKG option is disabled FEGS If true the EGS4 option is selected to calculate all interactions of e e and photons in the atmosphere explicitly The second random number sequence should be initialized for use in the EGS4 part Otherwise the default initialization is taken If false the EGS4 option is disabled In the CERENKOV option this flag is obsolete as EGS4 is selected automatically The two options may be selected or disabled independently at the same time 4 42 Electron Multiple Scattering Length Factor STEPFC STEPFC Format A6 F Default 1 STEPFC Factor by which the multiple scattering length for electrons and positrons in EGS4 simulations is elongated relative to the value given in 16 A detailed discussion on the use of the step length is given in 30 An enlargement of this factor may be tolerated to reduce computing time but simu
164. raction test option INTTEST generates histograms their data are written to the file with the name defined by keyword HISTDS page 82 via the output unit LUNPLT Logical UNit for PLoT by default 52 e The ANAHIST and the AUGERHIST options generate histograms their data are written to the file named datnnnnnn Ihbook via the output logical unit 53 nnnnnn is the run number specified in the keyword RUNNR page 51 Further details on this file are given in Sect 10 5 page 103 During the calculation the program uses a temporary data set scratch file as an external particle stack if the internal one is over full This data set is connected to unit MEXST EXternal STack by default 96 The names of EPOS data files epos inics epos iniev epos inilb epos inirj and epos initl may be changed using the keyword EPOPAR page 61 The parameters given in the keyword EPOPAR are written to a scratch file connected to unit NEXPRM by default 97 This file is read by the EPOS routines when initializing EPOS Similarly the names of NEXUS data files nexus inics nexus iniev nexus inirj and nexus initl may be changed using the keyword NEXPAR page 62 The parameters given in the keyword NEXPAR are written to a scratch file connected to unit NEXPRM neXus PaRaMeters by default 97 This file is read by the NEXUS routines when initializing NEXUS Some values of the in and output units may be redefined by changing their values in the corre sponding BL
165. radian 13 number of different random number sequences max 10 11 4 3x integer seed of sequence i 12 4 3 x i number of offset random calls mod 10 of sequence i 13 4 3 x i number of offset random calls 109 of sequence i 44 run number 45 date of begin run yymmdd 46 version of program 47 number of observation levels slope of energy spectrum lower limit of energy range in GeV upper limit of energy range in GeV cutoff for hadrons kinetic energy in GeV cutoff for muons kinetic energy in GeV cutoff for electrons kinetic energy in GeV cutoff for photons energy in GeV NFLAIN NFLDIF NFLPIO NFLPIF NFLCHE NFRAGM Table 8 Structure of event header sub block to be continued 96 Event header sub block continued Contents of word as real numbers R 4 x component of Earth s magnetic field in z component of Earth s magnetic field in wT 73 flag for activating EGS4 74 flag for activating NKG low energy hadr model flag 1 GHEISHA 2 UrQMD 3 FLUKA 76 high energy hadr model flag 0 HDPM 1 VENUS 2 SIBYLL 3 QGSJET 4 DPMIET 5 NEXUS 6 EPOS 77 CERENKOV flag 4 78 NEUTRINO flag 79 CURVED flag O standard 2 CURVED computer flag 3 UNIX 4 Macintosh lower edge of 0 interval in upper edge of 0 interval in lower edge of interval in upper edge of interval in 85 Cherenkov bunch size in the case of Cherenkov calculations number of Chere
166. rameters for NEXUS are set in subroutine aaset of the nexus bas f file If in your calling directory the data sets nexus inics nexus inicsei nexus inidi nexus iniev nexus inigrv nexus inirj nexus inirjei and nexus initl are not existent or not compatible with the selected parameters they will be calculated at the first call of subroutine psainz of nexus sem f which takes some 10 h on a DEC 3000 600 AXP with 175 MHz Normally all parameters of NEXUS are set by subroutine aaset of the nexus bas f file called from subroutine nexini In special cases it may be necessary to overwrite one or more of these parameters or to rename the data files to identify nexus inizz files established for different pa rameter sets This is performed using the keyword NEXPAR in the input file see footnote to keyword NEXPAR Sect 4 30 page 62 aaaaaaaaaa is a mand line as described in the NEXUS documentation These aaaaaaaaaa commands are written 30The FORTRAN compiler options described in Sect A 1 page 115 are used 26 onto the file connected with the logical unit NEXPRM by default 97 and read by subroutine aread of the nexus bas f file The NEXUS option needs roughly 7 5 times more CPU time than the VENUS option Eo 1015 eV NKG enabled EGS4 disabled NEXUS activates also the inelastic hadron nucleus interaction cross sections at higher energies They are calculated by the subroutine nexsig The NEXUS cross secti
167. re coconut checks your machine configuration and sets the proper options 13Some UNIX machines HP RS6000 and installations with GNU 877 compiler e g LINUX need the record length parameter RECL used in the OPEN statement for the external stack MEXST in bytes instead of 4 byte words This holds also for DEC UNIX running the f77 compiler with the option assume bytrecl For easy adaptation the additional preprocessor option is available to enlarge the RECL parameter by a factor 4 Most UNIX systems offer a system routine date_and_time which overcomes the millenary border In systems without this internal routine the preprocessor option OLDDATE selects an older routine for date and time The similar option OLDDATE2 selects an alternative needed for PGF77 environment on LINUX platforms IN2P3 Computing Center at Lyon or HP UX machines with the 1 option of the fort77 compiler This selection is attainable only by giving coconut e expert mode of coconut 11 MAC selects code for calculation on a former 68k APPLE Macintosh Within the corsika F file the optional code for the various versions to be unpacked by the preprocessor is marked by fif _ flag else dendif blocks If you are using a sequential computer other than the ones listed here you should try to adapt the UNIX or perhaps MAC version to your machine as this is most straight forward to understand In the src subdirectory the corsika
168. rimary energy range E14 7 fe range 0 upper end of primary energy range E14 7 slope slope of primary energy spectrum E15 7 nkg number indicating use of NKG option I2 flegsit number indicating use of EGS4 option I2 model high energy hadr int model OZHDPM 1 VENUS 2 SIBYLL 3 QGSJET 4 DPMIJET 5 NEXUS EPOS I2 gheisha low energy hadr model 12 GHEISHA 2 UrQMD 3 FLUKA I2 isobar low energy hadr model 1 GHEISHA 2 UrQMD 3 FLUKA I2 model crossect high energy hadr model and cross sections 0 HDPM 11 VENUS 22 SIBYLL 33 QGSJET 44 DPMJET 55 NEXUS 66 EPOS 12 hadflag 1 number indicating NFLAIN I2 hadflag2 number indicating NFLDIF 12 hadflag3 number indicating NFLPIO 12 hadflag4 number indicating NFLPIF 12 hadflag5 number indicating NFLCHE 12 hadflag6 number indicating NFRAGM 12 longi number indicating use of longitudinal sampling 12 longistep step width for longitudinal sampling E14 7 magnetx horizontal component of Earth s magnetic field E15 7 magnetz vertical component of Earth s magnetic field E15 7 nobslev number of observation levels I3 obslev 1 height of highest observation level E15 7 obslev2 height of 2nd observation level E15 7 obslev3 height of 3rd observation level E15 7 obslev4 height of 4th observation level E15 7 obslev5 height of 5th observation level E15 7 obslev6 height of 6th observation level E15 7 obsl
169. ritten to the file DATnnnnnn dbase rsp DATnnnnnn nfo in the AUGERINFO option onto the output directory DSN keyword DI RECT page 74 This file may be used to build a data base for examining the content of an air shower library page 104 This keyword is only available in the UNIX options 4 74 User Name USER USER Format A4 A20 Defaults USER A user name is read in to be written to the DATnnnnnn dbase file Lower case characters of USER are not converted to capitals 64Details on the event io format may be found in the documentation supplied with the bernlohr package 65 The existence of dev null is assumed see footnote of Sect 4 60 78 4 75 Host Name HOST HOST Format A4 A20 Defaults HOST A host name is read in to be written to the DATnnnnnn dbase file Lower case characters of HOST are not converted to capitals 4 76 Debugging DEBUG DEBUG MDEBUG DEBDEL NDEBDL Format A5 L I L I Defaults F MONIOU 100000 DEBUG If false debugging is disabled If true additional output for debugging purposes is given on logical unit MDEBUG MDEBUG Logical unit where to write debugging information Make sure that your selection of MDEBUG is not conflicting with existing definitions see Table 1 page 21 DEBDEL If true the debugging printouts are activated after NDEBDL particles above the ECTMAP energy have been printed If fal
170. riving at ground as it is usually performed for the showers simulated at Lyon for the Auger experiment This option needs linking with the CERN library to get the routines of the HBOOK and ZEBRA packages 24 ATMEXT selects code for treatment of the atmosphere according to MODTRAN model for var ious atmospheres by tabulated values ATMEXT is recommended with the CERENKOV option for careful treatment of refractive index This option links with compiled atmo c fileopen c and straux c routines of the bernlohr package AUGCERLONG selects code to fill the Cherenkov column in the table giving the longitudinal particle distribution 11 As there exist several FLUKA libraries suited for different computers the preprocessor option LINUX will be automatically selected if you have a LINUX system for a correct extraction of the code to be coupled with the LINUX variants of the FLUKA libraries AUGERHIST selects code to generate a histogram datnnnnnn lhbook containing vari ous histograms of different particle types at up to 20 vertical atmospheric depths to follow the development of shower properties which are of interest for the Auger experiment Cherenkov and fluorescence photon production This option needs the THIN option and linking with the CERN library to get the routines of the HBOOK and ZEBRA packages 24 AUGERINFO selects code which writes a file named DAT nnnnnn info instead of DAT nnnnnn dbase file CEFFIC selects code t
171. rst interaction which is disabled in the standard version without using keyword TSTART page 55 The arrival time refers to the start at the margin of the atmosphere which is indicated by a negative value of element 7 of the event header block page 97 The NKG formulas do not take into account the curvature of the Earth s surface Therefore the NKG output is suppressed in the CURVED option The combination of the CURVED option with the UPWARD option is described in Sect 3 5 23 page 48 As in the CEFFIC option the atmospheric absorption is treated only in a manner suited for planar atmospheres you should not combine the CURVED option with CEFFIC The CURVED option needs the atmospheres in the 5 layer model rather than interpolated from 39 ATMEXT tables Therefore in the CURVED option AATM BATM CATM values are fitted to the tabulated atmospheres and the table interpolation is disabled To obtain this program version the CURVED option has to be selected when extracting the FORTRAN code from the source file 3 5 9 EHISTORY Option With this option additional information on the prehistory of muons and electromagnetic EM particles is given out to the particle output file This extended additional information is activated for the muons by the keyword MUADDI see page 71 For EM particles it is activated with the keyword EMADDI see page 70 The precursor hadrons grandmother and mother of the particles at ground are specified wi
172. rtical component of the Earth s magnetic field in uT downwards The default values represent the magnetic field for the Karlsruhe location The values of other locations may be obtained from the program G eomag which is available on line in the world wide web 52 The value H of Geomag corresponds with our BX the value Z with our BZ For orientation see also Fig 1 page 86 Limits are BX BZ 5 0 4 23 Experiment Coordinates for Pre showering GCOORD GLONG GLATI GRFYEAR IPREPR IPRSTP Format 2I Defaults 69 585 35 463 2003 1 0 GLONG Gives the geographical longitude in West length is negative of the experiment GLATI Gives the geographical latitude in South latitude is negative of the experiment GRFYEAR Gives the year of the experiment the magnetic field is varying with time These coordinates are used to calculate the magnetic dipole field of the Earth s globe above the atmo sphere of the experiment s position in the case of a pre shower induced by ultra high energetic primary photons The default values give the position coordinates of the southern Pierre Auger Observatory at Malarg e Argentina for the year 2003 59 IPREPR Print indicator IPREPR lt 0 disables pre shower printing IPREPR 1 prints de tails of pre shower in case of MAXPRT page 73 or DEBUG page 79 IPREPR gt 2 always prints details of pre shower IPRSTP If IPRSTP Z 0 events without pre showeri
173. rvation levels This is what has to be analyzed for detailed energy spectra and distributions These files are written to the directory DSN as defined by keyword DIRECT page 74 as sequential unformatted FORTRAN files They may be read by the programs corsikaread f rsp corsikaread thin f The particle output file and the Cherenkov photon output file are structured as shown in Table 6 with the sub blocks as given in Tables 7 to 14 All quantities are written as single precision real numbers Block structure RUN HEADER nrun EVENT HEADER 1 DATABLOCK DATABLOCK LONG 1 1 LONG 1 n EVENT END 1 EVENT HEADER 2 DATABLOCK DATABLOCK LONG 2 1 LONG 2 n EVENT END 2 EVENT HEADER nevt DATABLOCK DATABLOCK LONG nevt 1 LONG nevt n EVENT END nevt RUN END nrun Table 6 Block structure of the particle and Cherenkov photon output files The LONG blocks eventually occur only in the particle output file 94 Run header sub block once per run Contents of word as real numbers R 4 1 2 run number 3 date of begin run 4 version of program 5 number of observation levels maximum 10 5 7 height of observation level i in cm slope of energy spectrum lower limit of energy range upper limit of energy range 19 flag for EGS4 treatment of em component 20 flag for NKG treatment of em component 2 kin energy cutoff for hadrons in GeV 22 kin energy cu
174. s are given on page 85 and in the file inputs All these files are placed in the run subdirectory where the program can be run Using the DATDIR keyword see page 75 the data input files may be placed in an arbitrary directory with exception of FLUKA data files and the steering input file with the keywords 24 Assuming csh shell one uses setenv FLUPRO flukadirectory 20 File name and file LUNOUT KMPI NBERTP LUNERR MCERABS MCERQEF MCERMIR LSTCK amp ifch ifhi IUNIT MDBASE MTABOUT MLONGOUT ifdt ifcp LUNHST LUNPLT MCETAP NEXPRM 0500 input steering keywords simulation control output on line printer debug output if DEBUG it selected NUCNUCCS nucleus nucleus cross sections DATnnnnnn particle output and simulation results external particle stack scratch file epos inics various tables for EPOS epos iniev various tables for EPOS epos inilb various tables for EPOS epos inirj various tables for EPOS epos initl various tables for EPOS nexus inics various tables for NEXUS nexus iniev various tables for NEXUS nexus inirj various tables for NEXUS nexus initl various tables for NEXUS qgsdat II 03 rsp OGSDATOT various tables for qgsjet II 03 rsp QGSJETOlc sectnu IT 03 SECTNU nucleus nucleus cross sections for qgsjet II 03 rsp QGSJETOIc control output of FLUKA EGSDAT x x EGS4 cross sections VENUSDAT structur
175. s correspond with the selected model MODATM Should only be used with ATMOD 0 or 10 Limits are 0 lt HLAYi 4 21 External Tabulated Atmosphere ATMOSPHERE IATMOX FREFRX 58 Format A10 I L Defaults 0 F IATMOX Use MODTRAN 36 atmospheric model IATMOX i in terms of density and refractive index instead of CORSIKA built in model This requires a file named atmprofi MODTRAN model atmospheres supplied with the bernlohr package include tropical i 1 mid latitude summer 2 mid latitude winter 3 sub arctic summer 4 sub arctic winter 5 and U S standard atmosphere 1976 6 Additionally for the MAGIC Cherenkov telescope on La Palma the summer 7 and winter 8 atmospheres 51 are supplied The atmosphere 9 gives the winter atmosphere at the South pole User supplied models are possible i gt 9 FREFRX If true the atmospheric refraction for Cherenkov photons is taken into account for plane parallel atmosphere if false refraction is ignored The value of this second argument is ignored if the CERENKOV option is not selected This keyword is only available in the ATMEXT option and needs linking with the compiled atmo c routines of the bernlohr package 4 22 Earth s Magnetic Field MAGNET BX BZ Format A6 2F Defaults 20 40 43 23 BX Is the horizontal component of the Earth s magnetic field in uT to the x direction of the detector North and BZ Is the ve
176. s not supported Showers originating from those portions of the cone which exceed the allowed range of COR SIKA are not simulated rather they are skipped and a new angle is selected at random out of the range of the cone To obtain this program version the VIEWCONE option has to be selected when extracting the FORTRAN code from the source file 3 5 25 Volume Detector and Vertical String Geometry Options With this options it is possible to select at random the zenith angle in a manner which respects the geometrical acceptance of the detector The default primary intensity distribution goes with the zenith angle 0 like I x sin cos The sin term respects the solid angle element of the sky while the cos term takes the geometri cal efficiency of a flat horizontal detector into account This allows to use each shower several times with the shower axis intersecting the detector array with equal distribution in x and y at random The area to be covered by randomly scattering the shower axis is independent from the zenith angle and extends horizontally Using the VOLUMEDET option the primary intensity distribution goes with the zenith angle like I x sind respecting only the solid angle elements of the sky This is appropriate for detectors of approx imated spherical geometry e g atmospheric Cherenkov telescopes To use a shower several times you might scatter it on an area which has fixed extensions in a plane perpendicular to the
177. se delayed debugging is disabled This feature helps to trace run time errors that have occurred in long simulation runs NDEBDL See DEBDEL 4 77 Debugging EGS EGSDEB JCLOCK Format A6 I Default 2147483647 JCLOCK Counter for delayed start of EGS4 debugging After activation of debug by DEBUG or by NDEBDL see Sect 4 76 above each pass of subroutine electr or photon is counted If the counter exceeds JCLOCK the debug statements within the EGS4 portion are activated This output appears on the unit MDEBUG 4 78 FLUKA Printing FLUDBG FFLUDB Format L Default F FFLUDB If true the two files DAT nnnnnn flout for additional information on the param eters used FLUKA DAT nnnnnn flerr on possible FLUKA error messages are written onto the output directory DSN keyword DIRECT page 74 If by the keyword DIRECT the directory dev null has been specified the two files are opened within the directory from 79 where the job has been started If false in the LINUX option the two files are written to fort 1lrsp fort 15 and may be redirected at runtime to dev null using shell commands like setenv FORT 11 dev null setenv FORT 15 dev null Without the LINUX option the files are opened directly to the directory dev null 66 This keyword is only available in the FLUKA option 4 79 GHEISHA Debugging GHEIDB GHEISDB Format L Default F GHEISDB If true
178. shower axis Using the VOLUMECORR option the primary intensity distribution is a more complicated function of the zenith angle which respects the geometry of a long vertical string detector e g AMANDA experiment 47 and other neutrino telescopes with a ratio of l d length diameter of the sensitive volume The functional form of the zenith angle distribution becomes I x d 2 sind cosh A m l d sin 45Selecting in the CURVED version the zenith angle 0 at random one should keep in mind that for the default version the probability vanishes at 0 90 If the zenith angle range is specified as 01 lt 0 lt 05 with 01 lt 90 and 90 lt 05 the zenith angle is selected at random from MIN 81 180 05 lt 0 lt 01 180 05 49 The d ratio defining the DETector ConFiGuration has to be read in using the keyword DETCFG page 73 The VOLUMECORR option cannot be combined with the VIEWCONE option To obtain these program versions the VOLUMEDET rsp VOLUMECORR option has to be selected when extracting the FORTRAN code from the source file 3 6 Combination of Options In principle most options may be combined Do not combine FLUKA with the present version DPMJET 2 55 because of severe clashes caused by duplicate names of COMMONS and sub routines DPMJET EPOS NEXUS QGSJET and SIBYLL are tested only with UNIX work stations You can not select more than one high energy and one low energy hadronic interaction
179. shower information and the longitudinal shower development The NKG output keyword ELMFLG page 66 comprises a table on the longitudinal develop ment of the electromagnetic shower component giving every 100 g cm the number of electrons and the longitudinal pseudo age parameter For the lateral electron distribution the densities in electrons cm are calculated on a grid of 80 points 8 directions separated by 45 with 10 distances between 1 m and RADNKG page 67 for each direction and the lateral pseudo ages for those various distances are determined The lateral distribution is calculated only for the lowest two observation levels For the longitudinal development keyword LONGI page 69 three tables are generated 70Renaming the standard log output to DATnnnnnn txt and redirecting it to the directory specified by the keyword DIRECT page 74 is convenient page 93 as by the shell commands dir or Is l all files belonging to one run are displayed consecutively which facilitates book keeping 715 footnote page 31 97 e The first one gives the particle numbers of y e e u hadrons all charged nuclei and Cherenkov photons as function of atmospheric depth e The second one reflects the energy content within the various particle species y 7 hadrons charged particles and the energy sum as function of atmospheric depth For all particle species the particle rest mass is included within
180. sika6990 0GS II urq13 to include the o files of UrQMD which are stored into the subdirectory urqmd ob j urqcors by GNU make compilation procedure No other libraries are normally required If you have specified the TIMERC the PRESHOWER or the STACEE option you need the linking of the compiled C file timer c o rsp preshw o or stacee o For linking the compiled C routines of the bernlohr package see the instructions delivered with the bernlohr package 92Be aware that the FLUKA LINUX version and the runtime library are fitting together 117 B Flow Diagram START initialization read steering cards amp data write general run information lt output file initialize shower primary energy amp angle height of first interaction coordinate correction write general shower information determine transport range transport to next interaction observation level traversed choice of interaction type energy amp angle cuts perform interaction electromagnetic interaction A hadronic interaction inter decay mediate stack various models take next particle write end of shower print shower information write end of run print run information END Figure 2 Simplified flow diagram of CORSIKA 118 C Sequence of Initializations The sequence of initializations is shown for the QGSJET option INTTEST option in brackets as
181. st f qgsjetOlc f echo ggsjetOlc f g77 O0 g fbounds check c o corsika gheisha 2002d o test f gheisha 2002d f echo gheisha 2002d f bin sh libtool mode link g77 g fbounds check o corsika corsika corsikacompilefile o trapfpe o corsika qgsjet0lc o corsika gheisha2002d o L lib Linux mkdir libs 977 g fbounds check corsika corsika corsikacompilefile o trapfpe o corsika qgsjet0lc o corsika gheisha 2002d o L lib Linux g77 g fbounds check c o corsikaread o corsikaread f bin sh libtool mode link g77 g fbounds check o corsikaread corsikaread o g77 g fbounds check o corsikaread corsikaread o g77 g fbounds check c o corsikaread_thin o corsikaread thin f bin sh libtool mode link g77 g fbounds check o corsikaread thin corsikaread thin o g77 g fbounds check o corsikaread thin corsikaread thin o g77 g fbounds check c o plottracks3c o plottracks3c f bin sh libtool mode link g77 g fbounds check o plottracks plottracks3c o g77 g fbounds check o plottracks plottracks3c o make 2 Entering directory src test Il meee apse Cusfurfvorzfrunt bin sh libtool mode install usr bin install c corsika run corsika usr bin install c corsika run corsika bin sh libtool mode install usr bin install c corsikaread run corsikaread usr bin install c corsikaread
182. t L Default T FVENSG If true the VENUS high energy hadronic cross sections are used If false the default cross sections as described in Ref 3 are used This keyword is only available in the VENUS option 64 4 39 Interaction Parameters amp Fragmentation HADFLG NFLAIN NFLDIF NFLPIO NFLPIF NFLCHE NFRAGM Format 6I Defaults 0 0 0 0 0 2 Steering flags of the high energy hadronic interaction model HDPM and of the projectile nu cleus fragmentation of all hadronic interaction models NFLAIN The number of interactions of a projectile in a target nucleus may fluctuate NFLAIN 0 or is calculated as an average value NFLAIN 5 0 NFLDIF No diffractive interactions are allowed in case of more than 1 interaction in the target NFLDIF 0 or diffractive interactions are possible NFLDIF 5 0 NFLPIO The rapidity distribution of 7 is taken different from that of charged pions as indi cated by collider data NFLPIO 0 or is taken as for charged pions NFLPIO 5 0 NFLPIF The number of 7 fluctuates in the same way as the number of charged pions NFLPIF 0 or fluctuates independently as parameterized from collider data NFLPIF 5 0 NFLCHE Charge exchange reactions for the proj and target particles are allowed NFLCHE 0 or inhibited NFLCHE 5 0 NFRAGM A primary nucleus fragments at the first interaction completely into free nucleons NFRAGM 0 or su
183. ter sets This is performed using the keyword EPOPAR aaaaaaaaaa in the input file see footnote to keyword EPOPAR Sect 4 27 page 61 aaaaaaaaaa is a com mand line as described in the EPOS documentation These aaaaaaaaaa commands are written onto the file connected with the logical unit NEXPRM by default 97 and read by subroutine aread of the epos bas xxx f file The EPOS option needs roughly 7 5 times more CPU time than the VENUS option Ey 10 eV NKG enabled EGS4 disabled EPOS activates also the inelastic hadron nucleus interaction cross sections at higher energies They are calculated by the subroutine nexsig The EPOS cross sections are selected automati cally when the EPOS option has been used for extracting the FORTRAN code from the source file In your input file you may supply the keyword page 61 EPOSIG Setting EPOSIG to false F you will use the default cross sections of CORSIKA as described in Ref 3 The epos inputs in run subdirectory is an example input file to run CORSIKA with EPOS 29The FORTRAN compiler options described in Sect A 1 page 114 are used 25 3 1 35 HDPM Routines HDPM is a set of routines to simulate high energy hadronic interactions These routines are fast and adjusted to experimental data where available Proton proton interactions simulated with HDPM and other models agree fairly well with each other see Ref 21 Experimental data are however rare for high energy nucleon
184. teral particle distributions 201110 1 dim Cherenkov photons vs emission angle 3011jj 1 dim energy spectra 4014 1 dim deposited energy vs distance 411 1 dim releasable energy vs distance Table 15 Histogram numbering of the datnnnnnn lhbook file ionization u energy cut hadron ionization hadron energy cut neutrino sum of all For both tables the binning is in vertical depth in g cm as specified by the keyword LONGI rsp slant depth in g cm if the SLANT option page 45 has been selected This table output is activated by the keyword LONGI page 69 10 7 tab File Output The optional file DAT nnnnnn tab written to the directory DSN keyword DIRECT page 74 contains information on the particles arriving at the lowest detector level Activation is done by the keyword PAROUT page 74 There are 3 tables containing separately the number of y and particles binned into energy 40 bins ranging from 100 keV to 10 TeV in logarithmic steps time delay relative to a spherical shower front 30 bins ranging from 10 nsec to 10 usec in logarithmic steps and core distance 20 bins ranging from 50 m to 5 km in logarithmic steps Additionally a fourth table is written containing the longitudinal development of y et e W hadrons and charged particles see Sect 10 1 page 92 in steps as defined by keyword LONGI page 69 This fourth table output is activated by the parameter LLONGI of keyword
185. th the penetrated matter between start and end of grand mother s track the position of mother s birth and the momenta of grandmother and mother at that point The generation counter of the mother particle is also given which might be com pared to the generation counter of the muon thus indicating additional decays between mother particle and the muon which otherwise are not given Further details are described in 39 3 5 10 INTTEST Interaction Test Option With this option the interaction model routines can be tested which are used to describe the hadronic collisions Only the first interactions are simulated and no air showers are developed Various projectiles Keyword PRMPAR and targets keyword INTTST may be selected The result of the test is a series of histograms generated with the HBOOK routines 24 and written to the unit HISTDS The histograms show properties of the secondary particles produced in the first interaction e g distributions of transverse momenta of squared transverse momenta of longitudinal momenta of Feynman x distributions of rapidity and pseudo rapidity distribu tions and various particle multiplicity distributions To obtain this program version the INTTEST option has to be selected when extracting the FORTRAN code from the source file The HBOOK routines require linking of the CERN li braries with the program they are not supplied with the CORSIKA package Via the keywords with their parameters page 81 82
186. the Cherenkov routines pro duce debug output This output appears on the unit MDEBUG This keyword is only available in the CERENKOV option 4 83 Interaction Test Target Definition INTTST ITTAR MCM Format A6 2D Defaults 0 0 ITTAR Defines the target for the interaction test option proton 2 neutron 9 Beryl lium 12 Carbon 14 Nitrogen 16 Oxygen 40 Argon 99 air Defines the reference system for which the interaction products are plotted 1 rest system of 1 target nucleon and 1 projectile nucleon 2 laboratory system 3 rest system of all secondary particles but not the spectators This keyword is only available in the INTTEST option VEN ES 4 84 Interaction Test Decay INTDEC LPIO LETA LHYP LKOS Format A6 AL Defaults T T T T LPIO If true the particles decay before gathering them in the interaction test LETA If true the 7 particles decay before gathering them in the interaction test LHYP If true all hyperons decay before gathering them in the interaction test LKOS If true the K particles decay before gathering them in the interaction test This keyword is only available in the INTTEST option 4 85 Interaction Test Spectator Definition INTSPC LSPEC 67For the DPMJET high energy model and ITTAR lt 14 the Glauber data file glaubint glb has to be used instead of the glaubtar glb file 68 n photo nuclear interactions the cm syste
187. three dimensional box given by the axis ranges should be plotted If true all track segments whose endpoints both fall outside this box are not plotted This keyword is only available in the PLOTSH2 option 4 92 End of Steering EXIT Format A4 This keyword ends the keyword input 84 5 Input Example The keyword input file for a CORSIKA run including QGSJET and CERENKOV options may look like the following list UNNR VTNR 1 100400 100401 0 0 100402 100403 0 0 10 5626 2 00 4 4 zd O 180 200 E2 20 4 2 29 43 23 015 015 UADDI OBS ECTMAP DIREC CERARY CWAVLG CERSIZ CERFIL CSCAT DATBAS USER HOST EV 1 ARRANG 1 AXPRT 1 1 82 home user corsika run 10 8 1200 1500 80 300 450 Da F 5 1000 d you your host 1000 DEBUG EXI F 6 F 999999999 6 Coordinate System 50 number of run no of first shower event seed for hadronic part seed for EGS4 part seed for Cherenkov part no of showers to simulate primary particle code iron energy range of primary GeV slope of energy spectrum range zenith angle deg range azimuth angle deg OGSJET for high energy amp debug level OGSJET cross sections enabled HDPM interact flags amp fragmentation flag elmag interaction
188. ticle species for the energy deposit by different particle species as function of distance from the shower axis for energy spectra as function of distance and much more Examples are given in Ref 37 For histograms relating to the emission of Cherenkov radiation the bunch size and wavelength band has to be specified using the keywords CERSIZ page 76 and CWAVLG page 76 Only particles arriving at the lowest observation level are directed to the particle output file page 94 and or the table output file keyword PAROUT page 74 and or binned into the ANAHIST histograms 37 Because of its permanent modifications a comprehensive description of the AUGERHIST op tion is not available The AUGERHIST option works only in combination with the THIN option To obtain this program version the AUGERHIST option has to be selected when extracting the FORTRAN code from the source file The HBOOK routines require linking of the CERN libraries with the program they are not supplied with the CORSIKA package 3 5 5 AUGERINFO Option The AUGERINFO option produces an output file named DATnnnnnn info replacing the DATnnnnnn dbase file when activated by the DATBAS keyword page 78 The output format of the info file differs from that of the dbase file to enable the automatic production of a data base for the Auger experiment showing the content of the CORSIKA shower library at the IN2P3 computing center Lyon To obtain this program version the
189. toff for muons in GeV 23 kin energy cutoff for electrons in GeV 24 energy cutoff for photons in GeV lx physical constants and interaction flags 1 50 75 XPINCL X displacement of inclined observation plane 76 YPINCL Y displacement of inclined observation plane 77 ZPINCL Z displacement of inclined observation plane 78 THINCL angle of normal vector of inclined observation plane 79 PHINCL angle of normal vector of inclined observation plane 79 2 0 i 1 15 no longer used 94 i CKAG i 1 40 134 1 5 139 2 CSTRBA 2 2 1 11 150 0 1 97 no longer used 248 XSCATT scatter range in x direction for Cherenkov 249 YSCATT scatter range in y direction for Cherenkov HLAY 1 5 1 5 BATM 1 5 i 1 5 NFLAIN NFLDIF 272 NFLPIO 100x NFLPIF 273 NFLCHE 100xNFRAGM Table 7 Structure of the run header sub block 95 Event header sub block once per event Contents of word as real numbers R 4 EVTH event number total energy in GeV starting altitude in g cm 6 number of first target if fixed 7 coordinate height of first interaction in cm negative if tracking starts at margin of atmosphere see TSTART 8 px momentum in x direction in GeV c 9 py momentum in y direction in GeV c 10 pz momentum in z direction in GeV c pz is positive for downward going particles zenith angle 0 in radian azimuth angle in
190. tored in an intermediate stack which is foreseen for 200000 particles After completing an interaction all particles in case of THINning only a fraction of them are moved to the internal stack The size of this internal stack 15 large enough to keep 680 in case of thinning 624 particles If the size of the internal stack is full 680 624 particles are temporarily added to the external stack If the internal stack is empty 340 312 particles are re read from the external stack Only half of the internal stack is read back to avoid a permanent shifting of data from and to the internal stack if it is just full and the number of secondaries oscillates with a small amplitude around 680 624 69These energy cuts correspond with the sensitivities of the KASCADE array detectors 91 10 Outputs There are two major output files produced by a simulation run The control printout txt file allows to survey the simulation run The particle output file is written to the data file DATnnnnnn with nnnnnn being the run number specified in the keyword RUNNR page 51 This file becomes very large when simulating showers in great detail EGS4 low thresh olds In the CERENKOV version an additional file C E Rnnnnnn might be written Op tionally a tabular output y e and u particles at ground and longitudinal development of charged particles is written out to the file DAT nnnnnn tab Further on the longitudinal dis tributions of particle
191. umber of Cherenkov detectors in X direction NCERY Number of Cherenkov detectors in Y direction DCERX Grid spacing in cm of Cherenkov detectors in X direction The DCERX value has no relevance in case of NCERX 1 DCERY Grid spacing in cm of Cherenkov detectors in Y direction The DCERY value has no relevance in case of NCERY 1 ACERX Length in cm of each Cherenkov detector in X direction ACERY Length in cm of each Cherenkov detector in Y direction The altitude of this array is at the lowest observation level For the definition of the X and Y directions see Fig 1 page 86 and keyword ARRANG page 73 Limits are NCERX NCERY gt 1 DCERX DCERY ACERX ACERY gt 1 This keyword is only available in the CERENKOV option but not in the IACT option for Cher enkov telescopes 75 4 66 Cherenkov Wavelength Band CWAVLG WAVLGL WAVLGU Format A6 2F Defaults 300 450 WAVLGL Lower limit in nm of the wavelength band for Cherenkov radiation production WAVLGU Upper limit in nm of the wavelength band for Cherenkov radiation production Limits are 100 lt WAVLGL lt WAVLGU lt 700 This keyword is only available in the CERENKOV AUGCERLONG and AUGERHIST option 4 67 Cherenkov Bunch Size Definition CERSIZ CERSIZ Format A6 F Default 0 CERSIZ Defines the maximal bunch size of Cherenkov photons that are treated together If set to 0 by the subroutine getbus the progr
192. ur CORSIKA program In your input file you may supply the keyword page 64 32Omitting the default QGSJETOLD selection uses hadron air cross sections increased by 3 to take into account the individual nuclear radii of 14N and 160 as stated in Ref 27 28 VENUS T 0 Setting VENUS to false F the simple HDPM routines are used see also Sect 3 1 3 page 26 Normally all parameters for VENUS are supplied by the routine venini In special cases it may be necessary to overwrite one or more of these parameters specified by its name PARCHA and its new value PARVAL This is performed using the keyword page 64 VENPAR PARCHA PARVAL in the input file page 64 The VENUS option needs roughly 15 times more CPU time than the HDPM option NKG enabled EGS4 disabled VENUS activates also the inelastic hadron nucleus interaction cross sections at higher energies which are calculated by the subroutine vensig Nucleus nucleus cross sections are derived from the VENUS nucleon nucleon cross sections using the Glauber tables of CORSIKA 3 The VENUS cross sections are selected automatically when the VENUS option has been used for extracting the FORTRAN code from the source file In your input file you may supply the keyword page 64 VENSIG Setting VENSIG to false you will use the default cross sections of CORSIKA as described in Ref 3 3 2 Low Energy Hadronic Interaction Models 32 1 FLUKA Option FLUKA FLUctuating KAscade
193. us R within which the telescope is fully contained At least one telescope has to be specified For the definition of the X and Y directions see Fig 1 page 86 and keyword ARRANG page 73 Limits are 0 lt R 1 lt number of telescopes lt 1000 This keyword is only available in the CERENKOV option together with the IACT option for Cherenkov telescopes 77 4 72 Cherenkov Telescope Data File Name TELFIL TELFNM Format A100 The telescope specific data are to be written to a file named TELFNM in event io format Lower case characters of TELFNM are not converted to capitals If this file exists and is write enabled new data are appended After ending the run the file will be set read only to avoid accidental overwriting The file name dev nu11 65 suppresses the output file If you want to write into the directory from where you are starting your CORSIKA run you should give TELFIL or TELFIL ablank enclosed in apostrophes or quota tion marks Please keep in mind that in FORTRAN an automatic expansion of UNIX names like home is not possible rather you should give the full expanded name of the directory ending with a character This keyword is only available in the CERENKOV option together with the IACT option for Cherenkov telescopes 4 73 Write Data Base File DATBAS FDBASE Format L Default F FDBASE If true all essential run parameters are w
194. ut contains as well all kinds of warnings and error messages System errors may be redirected in UNIX systems to the standard output txt file by the amp character following immediately the gt character as given in the example corsika inputs gt amp home user corsika run DATnnnnnn txt assuming that all output should go to the directory home user corsika run as given in the ex ample on page 85 Users are advised to check this printout carefully for any indications of problems during the run time and keeping it together with the particle output for later consulta tion When errors occur the DEBUG option may help in localizing the bug This option entails a very detailed printout of the simulation process that easily fills large disks when enabled for many showers these informations are printed per event For low energy primaries and high statistics this printout per event may not be necessary and can be suppressed by selecting a maximum number of showers to be printed keyword MAXPRT page 73 At the end of each run a short run summary is printed with similar tables as for single showers but averaged over all showers of the actual run 72The usage of the korne shell is assumed 73For the naming of standard output see the footnotes page 22 and 92 93 10 2 Normal Particle Output The particle and Cherenkov photon output files contain the information about the simulation run and about all particles reaching obse
195. verridden This affects the x and y coordinates of the Cherenkov photons arriving at the observation level if the altitude of the first interaction is fixed by the keyword FIXHEI see Sect 4 13 page 55 To obtain this program version the IACT option has to be selected together with the CERENK OV option when extracting the FORTRAN code from the source file The Make file will com pile the needed C files of the bernlohr package in the libbern a library and then link it with your CORSIKA program 3 4 4 Imaging Atmospheric Cherenkov Telescope Extension Option With the IACTEXT option the interface to the telout function iact c routines is extended by parameters describing the emitting particle This extended information is stored as an additional 34 photon bunch after the normal one with mass charge energy and emission time replacing the cx cy photons and zem fields respectively and are identified by a wavelength of 9999 The compact output format is disabled for making that possible In addition all particles arriving at the observation level are included in the event io format output file in a photon bunch like block identified by array and detector numbers 999 The x y cx cy and ct ime fields keep the normal sense with coordinates directions and time counted in the detection level reference frame The particle momentum is filled into the zem field negative for upward moving particles and the particle ID is filled into the
196. y of the air decreases with the height The shower calculations and tracking are using Cartesian coordinates In a flat atmosphere the thickness increases with 1 0 This is a good ap proximation for inclined showers if their zenith angles are below 70 Above this value the differences between a flat and a curved atmosphere become more and more important At 90 eventually the thickness of the flat atmosphere becomes infinite whereas the correct thickness is 37000 g cm Within the CURVED atmosphere option for large zenith angles above 70 the Earth s atmo sphere is no longer assumed to be completely flat as in the standard version for smaller zenith angles Rather the atmosphere is replaced by a sliding plane atmosphere Each times the horizontal displacement of a particle exceeds a limit of 6 to 20 km dependent on altitude a transition to a new locally plane atmosphere is performed By these means the advantages of the simpler transport formulas within a planar atmosphere are combined with the faster simulation speed by avoiding the lengthy and more complicated treatment by using a true spherical sys tem Because of technical reasons only one observation level may be specified in the CURVED option In the CURVED option the ionization energy loss deflection within the Earth s magnetic field and the generation of Cherenkov photons is enabled for charged hadronic primaries on their path between entering the atmosphere and the fi
197. y range 3 x 10 4 to 1 x 10 eV and after its upgrade to KASCADE Grande 2 it is reaching 10 eV The CORSIKA program 3 allows to simulate interactions and decays of nuclei hadrons muons electrons and photons in the atmosphere up to energies of some 1079 eV It gives type energy location direction and arrival times of all secondary particles that are created in an air shower and pass a selected observation level CORSIKA is a complete set of standard FORTRAN routines It uses no additional program libraries for the simulation of air showers Therefore it runs on almost every computer where FORTRAN is available The CORSIKA program consists basically of 4 parts The first part is a general program frame handling the in and output performing decay of unstable particles and tracking of the particles taking into account ionization energy loss and deflection by multiple scattering and the Earth s magnetic field The second part treats the hadronic interactions of nuclei and hadrons with the air nuclei at higher energies The third part simulates the hadronic interactions at lower energies and the fourth part describes transport and interaction of electrons positrons and photons CORSIKA contains several models for the latter three program parts that may be activated optionally with varying precision of the simulation and consumption of CPU time High energy hadronic interactions may be treated by one of the models The Dual Parton Model DPMJET
198. ymour herwig 6 2 20 Program File Preparation By unpacking the corsika 6990 tar file with the command tar xvf corsika 6990 tar the file structure of CORSIKA will be established To install CORSIKA you type coconut no argument and answer the questions it s done The main source file is corsika F with all common blocks in cor s ka h It s a FORTRAN source file with some C preprocessor commands which allows optional compilation of some part of the code It uses standard Make file and compiler options and therefore doesn t require any special software to be installed on your machine Using the shell script coconut the user can interactively select the specific CORSIKA version for his application and compile it to get directly ready to run executable binary files in the run subdirectory Computer dependent options and Make files are prepared automatically by the shell script configure called by coconut The configure is a standard portable shell script used together with make by GNU packages to be installed but con figure should NOT be used directly to get a proper installation of CORSIKA The coconut shell script has been designed to get a user friendly machine dependent installation so that binary files can be compiled in parallel from the same source directory but on different systems in a large computer farm for instance All object files and libraries are hidden in a 1ib subdirectory If you already used a for
199. ypically a procedure is used assuming QGSJET is employed like 477 corsika_compilefile o gheisha 2002d o qgsjet II 03 o trapfpe o m32 o corsika For linking the large packages of FLUKA UrOMD DPMJET EPOS HERWIG NEXUS and VENUS you presumably have to give limit datasize unlimited 915 footnote at DPMJET compilation page 114 116 limit stacksize unlimited to overcome the small default values of many compilers which lead to an error stop during link ing If the pg 77 compiler has been used for compilation you should also use pgf77 for linking pgf77 corsika compilefile o gheisha 2002d o qgsjet II 03 0 o corsika For linking FLUKA versions the FLUKA library has to be included in the link step g77 corsika compilefile o qgsjet II 03 0 trapfpe o Lflukadirectory 1 lukahp m32 o corsika For linking FLUKA with pg 77 you should use the option 9g771ibs in the link step to ensure that the runtime library of 977 is available as it is needed for running the FLUKA routines In the run step of FLUKA versions the environment variable FLUPRO has to be set setenv FLUPRO flukadirectory which is necessary to link the data files which will be read in by the FLUKA package Addi tionally the stacksize and datasize limits have to be overcome also in the run step Linking of URQMD versions is performed easiest e g for DEC UNIX by 77 corsika compilefile o qgsjet II 03 0 urqmd obj urqcors o trapfpe o m32 o cor
200. ystem 85 Units in CORSIKA 87 Particles in CORSIKA 87 Running the CORSIKA Program 90 Outputs 92 10 1 Control Printout txt File 92 10 2 Norm l Particle Output 2 RE Eq SL 94 10 2 1 Version without Thinning 102 vi 10 22 Thinning Option 43 9 4e Vw er erde 10 3 Compact Output 4 2 24 6 4 PE 4 10 4 inelined binary File Output uv 10 5 lhbook File Output 10 6 long File Output 5 ouk RR RR ERG RE 10 7 lab File Output gt 4 BSR ORE BARRA ARIS epu 10 8 dbase File and info File Output 11 Hints for Programmers 12 In Case of Problems 13 Acknowledgments A Compilation and Linking Compilation gt s 62923593923 AL Jmkmg twr ER USES B Flow Diagram C Sequence of Initializations D Atmospheres Bibliography vli 110 111 113 113 116 118 119 120 127 viii 1 Introduction CORSIKA COsmic Ray SImulations for KAscade is a detailed Monte Carlo program to study the evolution and properties of extensive air showers in the atmosphere It was developed to perform simulations for the KASCADE experiment 1 at Karlsruhe in Germany This exper iment measured the elemental composition of the primary cosmic radiation in the energ

Extensive Air Shower Simulation with CORSIKA: A User`s

Contents

Download Pdf Manuals

Related Search

Related Contents