Voilà un rayon cosmique! (Look, a cosmic ray!)

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1 CORSIKA

2 Voilà un rayon cosmique! (Look, a cosmic ray!)

3 CORSIKA COsmic Ray SImulations for KAscade

4 D. Heck

5 Why do we need Corsika? %!

6 Auger vs. IceCube High Multiplicity Large Area No Shielding Low Multiplicity Large Volume Ice Shielding

7 CR 106 ev to ~1020 ev ~E 2.7 ~E 3.1 ~E 2.7 IceCube After T. Gaisser, ICHEP02 [GeV]

8 Muons IceCube

9 CORSIKA >UCR >MMC >Photonics NuSim >DOM Simulation 10km center:1950m below surface 800m 1600m

10 CR Primary p/nucleus CORSIKA (CR shower simulation) air Hadronic Interaction pion/kaon lepton/neutrino gamma

11 CR Primary p/nucleus air Handled by main CORSIKA! pion/kaon lepton/neutrino gamma

12 Hadronic Interactions CORSIKA compile options 80GeV, K DPMJET NEXUS QGSJET QGSJET II SIBYLL VENUS EPOS FLUKA GHEISHA QMD Low E High E

13 Production Asymmetry u d p + N(n) anti Forward p s N(n) +

14 100% + u d s % anti Forward

15 Muon Parents K! + ± KL K ±

16 Pions (ud) E( )>400GeV DSLOPE= 1

17 Kaons (us) +

18 Atmospheric Neutrino Fluxes T. Gaisser, hep ph/

19 SIBYLL (good)

20 QGSJET (bad) K + +

21 Good / Bad: Energy

22 Good / Bad: Zenith Angle Needs full detector simulation!

23 MINOS R. Birdsall, UW Madison

24 general IceCube

25 Run Seed Had. Sim Output

26 ATMOD and OBSLEV 13 = South Pole, October

27 CR Composition

28

29 RANPRI 2 DSLOPE= 1: 1.71 DSLOPE limit! CORSIKA Poly Gonato

30 Protons, Helium and Iron ERANGE 600 Cutoff at tens of PeV SPRIC Option

31 Speed SIBYLL QGSJET here: DSLOPE= 1.45, Eprim>600GeV, E >273GeV 3.128Hz 3.025Hz DPMJET QGSJET II EPOS 0.102Hz 0.093Hz 0.042Hz DSLOPE=0: Most Events DSLOPE= 1.45(max): Best Spectrum

32 DSLOPE= 1.45 ECUTS 273. Most Muons from Iron Inverted after weighting!

33 Composition/High E Studies One Primary Type Specified PL Index Primary Type (here:p) RANPRI 0 ESLOPE 2.72 PRIMPAR 14 Add them together separately Work in Progress

34 Normalization Primary Particle Flux: FLUXSUM = per meter2 second sr Depends on: [Emin, Emax] DSLOPE Composition NSHOW*Nfiles wev=eprim DSLOPE Individual event *F*10 3*DSLOPE TeV >GeV *10 /Nprim 4 m2 >cm2

35 IceSim tray.addmodule("i3corsikaweightmodule","corsikaweight")( ("nevents", ), # number of showers generated in CORSIKA ("spectrumtype",2), # the RANPRI parameter in CORSIKA steering file (Hoerandel spectrum) ("cylinderlength",1400*i3units.meter), # the generation cylinder length as in LENGTH=1400 above ("cylinderradius",700*i3units.meter), # the generation cylinder radius as in RADIUS=700 above ("fluxsum", ), # the energy integrated spectrum calculated by CORSIKA ("energyprimarymin",600.*i3units.gev), # the minimum energy as from ERANGE in CORSIKA steering file ("energyprimarymax", *i3units.gev), # the maximum energy as from ERANGE in CORSIKA steering file ) FLUXSUM +Volume =Rate!

36 Shower Size 100m

37 Multiplicity >1000 /event ( 1/min)

38 Energy Spectrum = + mult+ CR+1= 3.5 dn /de =(dn /de )0*dN /decr* (dncr/decr)decr Monoenergetic Primary Multiplicity Power Law: cx

39 QED Slope: 2.5 1/h 1/d

40 Spectral Variations Dense air (vertical, summer): short mean free path, more reinteractions, less energetic muons Thin air (horizontal, winter): long mean free path, fewer reinteractions, more energetic muons

41 F2K Header: Muon Event # 17, Run 100 Primary: 1496GeV Proton, 12.4 End Event Secondary: 279GeV

42 UCR in IceSim $I3_SRC/examples simulation/resources/examples/ucrgenerator.py module: ucr icetray tray.addmodule("i3generatorucr","generator")( ("EventsToIssue",nevents), ("UCROpts",ucropts)) executable UCROpts = /home/berghaus/offline/build/bin/ucr icetray ucr F2K file /net/local/icecube/i3tools/rhel4 x86_64/test data/icesim corsika/f2k gz oms over=1 SHOWERS= FLUXSUM= LENGTH=1200 RADIUS=600 DEPTH=1945 HEIGHT=2834 EARTHR=6.4e6 DCORR=35 cutfe=400. curved=4 cutth=85 tr=2

43 UCR out=[name] change output file to NAME tr=[num] output only events with # of tracks >= NUM -over=[..] oversample by this number, default is 1 r = randomize randomize shower core xy locations c = curved same for curved Earth's surface curved=[1 4] different curved surface treatment: 1: only downgoing primaries (th from 0 to 90 deg.) 2: only upgoing primaries (th from 90 to 180 deg.) 3: decide at random, either goes up or down 4: oversample x2 each event with th > cutth phi = r phi also randomize azimuth angle cutth=[degrees] value used for curved=4 EARTHR=[radius] of the Earth [m] LENGTH=[length] of the detector [m] RADIUS=[radius] of the detector [m] DEPTH=[depth] of the detector center [m] HEIGHT=[altitude] of the ice surface [m] DCORR=[correction] depth correction (35 m) [m] trigw=[time in ms] assign event times and combine events that are within trigw ms of each other r mpri remove primaries r musr remove user blocks -oms output only muons ohm leave only muon with highest energy per event msn leave only muon and neutrinos, delete others cmt=[file] append comments contained in the file run=[number] set the run number FLUXSUM=[CORSIKA's value] per meter2 second sr SHOWERS=[number] of showers generated by CORSIKA rr remove possible previous xy randomization rr=[depth] and set the previous value of DEPTH test [num] [theta] [phi] test xy randomization -cutfe=[gev] -corr angle-dependent cutoff energy for muons enforce f2k compliance Options: ucr icetray ucr h

44 Threshold Energy vertical top (70 ) top (85 ) bottom (85 )

45 Angle dependent Energy Cutoff before ucr horizon after ucr horizon

46 Prompt CR Primary: Spectral Index 2.7 (below knee) Non prompt: Decay probability before reinteraction Lepton Spectral Index 3.7 Prompt: No reinteraction Lepton Spectral Index 2.7

47

48 Motivation Diffuse Flux Atmospheric Flux J. Hodges, UW Madison

49

50 Hadronic Interactions Charm? 80GeV FLUKA GHEISHA QMD DPMJET (2.55) NEXUS QGSJET QGSJET II SIBYLL VENUS EPOS DMPJET Low E High E

51 New DPMJET in CORSIKA 1 Multiplicity! 10 18

52 Prompt Neutrinos

53 Good Luck

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