C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS NEMO software Carla Distefano for the NEMO Collaboration KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS The simulations performed by the NEMO Collaboration are carried out using the OPNEMO and ANTARES software. By the end of 2002, ANTARES software modified for a km3 detector by D. Zaborov was installed in Catania In parallel: development of simulation software OPNEMO with new track and energy reconstruction algorithms (work mainly conducted in Rome) The NEMO Software

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Using the ANTARES software several issues important for the km3 detector feasibility and performance were addressed: - Dependence on environmental parameters (depth, optical background, optical proprieties …) (see talk by R. Coniglione) - Dependence on detector structures (towers, strings, lattice ….) and geometries (distance between towers, storeys, PMT orientation …) (see talk by R. Coniglione) - Effect of directional-sensitive optical modules (see talk by K. Fratini) - Detection of the Moon Shadow (this talk) -Detector sensitivity for diffuse and point sources (see tomorrow talk by C.D.) NEMO Simulations

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS The ANTARES Software Detector generator gendet Geomety file Gentra Genneu Muon tracks km3 modk40 Hits on PMs Hits on PMs + back hits reco Reconstructed tracks Muon Generator or Neutrino Generator Light simulator and propagator Track reconstructor Background and electronics simulator code I/O

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Simulated NEMO-km 3 detector Simulated Detector Geometry: square array of 81 NEMO towers 140 m between each tower 18 floors for each tower vertical distance 40 m storey length 20 m 4 PMTs for each storey 5832 PMTs Depth = 3500 m (Capo Passero site) PMT location and orientation (  PMT =10”) DETECTOR LAY-OUT The ANTARES code gentra v1r2 has been used to generate the detector geometry file.

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS The ANTARES Software Detector generator gendet Geomety file Gentra Genneu Muon tracks km3 modk40 Hits on PMs Hits on PMs + back hits reco Reconstructed tracks Muon Generator or Neutrino Generator Light simulator and propagator Track reconstructor Background and electronics simulator code I/O

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Muon tracking and light generation The same package (codes gen and hit) has been used to generate new photon tables simulating the absorption length profile measured in the Capo Passero site by the NEMO and ANTARES Collaborations. Light scattering has been simulated according to the –partic model, with L b ~50 nm (see the ANTARES documentation). The ANTARES simulation package km3 v2r1 is used to simulate the passage of muons inside the detector and to generate the PMT hits

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS The ANTARES Software Detector generator gendet Geomety file Gentra Genneu Muon tracks km3 modk40 Hits on PMs Hits on PMs + back hits reco Reconstructed tracks Muon Generator or Neutrino Generator Light simulator and propagator Track reconstructor Background and electronics simulator code I/O

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Optical background was measured in Capo 3000 m depth. Data are consistent with 30 kHz background on 10”PMT at 0.5 s.p.e. Optical background in Capo Passero The ANTARES code modk40 v4r8 is used to add optical background hits and to simulate the electronics. ** gain randomisation (0-off, 1-on) GAIN 1 ** K40 frequency (Hz) and time offset (ns) FK ** raw hit production from SPE integration with 2 ARS, 25 nsec integration, 250 nsec ** dead time chosing the last number negative, the 'hit' tag can be suppressed from output RAWH

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS The ANTARES Software Detector generator gendet Geomety file Gentra Genneu Muon tracks km3 modk40 Hits on PMs Hits on PMs + back hits reco Reconstructed tracks Muon Generator or Neutrino Generator Light simulator and propagator Track reconstructor Background and electronics simulator code I/O

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Main modifications by Zaborov for a km3 Reco V4r3 modified by Zaborov (AartStrategy) Causality filter respect to the hit with the highest charge (|dt|<dr/v light + 20ns) AND (||dt|-dr/c|<500ns) Hit selection for prefit-> at least 3 hits with charge > 2.5 p.e. Some parameters in include files has been changed in order to take into account the high number of PMTs, clusters,strings…

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Main modifications by LNS in RECO Recov4r4km3 (LNS version) Same as v4r3km3 (Zaborov version) with: Some internal conditions in AartStrategy.cc have been relaxed If(mest_hits[0].size() <15) continue; modified into If(mest_hits[0].size() <6) continue; If(ndof<5) continue; modified into If(ndof<1) continue; Hit selection for prefit-> at least 3 hits with charge higher than 2.5 p.e. or in concidence (at least two hits with Dt<20ns in a LCM) Modifications for gcc3.X Recov4r5km3 Same as v4r4km3 with: Hit selection for prefit-> at least 3 hits with charge higher than 2.5 p.e. or in concidence (at least three hits with Dt<20ns+dr/v light in a LCM)

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Comparison between different RECO versions Nemo detector (5832 PMT 81 Towers 140m distant) 20kHz background Median vs E  A eff  vs E    vs E   v4r3km3 (Zaborov Version)  v4r4km3 (LNS version with coinc)  v4r4km3 (LNS version with coinc)+quality cuts

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS log 10 E  (GeV) Main modification by LNS Recov4r6km3: Starting from v4r6 ANTARES version we applied the same modifications of v4r4km3 version Documentation for v4r6 improvements in antares.in2p3.fr/users/stolar/internal/recoco  v4r6km3  v4r4km3 (LNS version with coinc) Nemo detector (5832 PMT 81 Towers 140m distant) 35kHz background ratio Aeff (v4r6km3) /Aeff (v4r4km3) quality cuts reconstruction

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Detection of the Moon shadow

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Detection of the Moon shadow The detection of the deficit (The Moon Shadow) and of its position in the sky provides a measurement of: the detector angular resolution; the detector absolute orientation. The Moon is opaque to Cosmic Rays and thus causes a deficit in the CRs and therefore in the atmospheric muon flux reaching the detector. This approach has been already adopted in several cosmic ray detectors as MACRO, SOUDAN, MILAGRO….

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Simulation of the Moon shadow: OkadaMoon code The code OkadaMoon (C++ gcc3.X): calculates the Moon position in the sky at a given time and transforms the Moon astronomical coordinates in the detector frame; generates the muons in a circular window around the Moon position with radius R=10°; simulates the lack of atmospheric muons in correspondence to the Moon disk; weights the muons to the Okada parameterization but any other parameterizations could be easily implemented. L. Ferrari, Diploma Thesis Moon below the Horizon

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Observation of the Moon shadow (simulation normalized to 1 year of data taking) k= 659 ± 8 deg -2  = 0.19 ± 0.02 deg Event Selection*: N hit min = 20  cut = -7.6 S 1year =5.5 Minimum time needed for observation: Moon rest frame Moon disk Event density * Events selection criteria will be discussed tomorrow.

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Estimate of the detector angular resolution  = 0.19 ± 0.02 deg Event Selection: N hit min = 20  cut = -7.6 S 1year =5.5 median angle of selected events: estimated angular resolution:  = 0.22 deg Reconstructed Selected

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Study of the telescope absolute pointing We introduce a rotation  around the Z axis to simulate a possible systematic error in the absolute azimuthal orientation of tracks. (1 year of data taking) for   0.2  (expected accuracy), the shadow is still observable at the Moon position; for   0.2  (pessimistic case), systematic errors could be corrected; the presence of possible systematic errors in the absolute zenithal orientation is still under analysis. Moon rest frame

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Moon shadow: CORSIKA-Music muon generation Corsika ( has been modified to simulate the Moon Shadow: We implemented the calculation of Moon position in the sky; We restricted the generation of primaries in a circular window around the Moon position with radius R=10°; The lack of primaries in correspondence to the Moon disk is simulated; The produced muons are propagated up to the detector using the MUSIC code (Antonioli et al, 1997). Study of the effect of multi-muons events in the detection of the Moon Shadow  a full simulation of atmospheric muons.

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS  Primary ions -> p, He, N, Mg, Fe  Primary energy -> TeV/nucleon  Primary zenith angles –> 0°  85°  Energy threshold for muons at sea level -> 0.5 TeV for ions between 0° and 60° and 1 TeV for ions between 60° and 85°  Slope primary spectrum  E -2  Isotropic angular primary distribution CORSIKA input  Corsika version: CORSIKA version 6.2 ( + Sheffield modifications to get output files in the ANTARES format + modifications to simulate the Moon Shadow  Hadronic interaction model -> QGSJET and GHEISHA  “curved” version for horizontal showers and “flat” for vertical showers Simulation input

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS Cosmic Ray Primary Spectrum The generated events are weighed to the Cosmic Ray Primary Spectra provided by J.R. Horandel Astr. Phys. 19 (2003) 193. Total numbers of Generated Primaries: Muons reaching the detector can: Reconstructed Events: Present statistics

C.Distefano KM3NET ‘Physics and Simulation (WP2)’ Oct 24 – 25, 2006 LNS CORSIKA-Music generation: preliminary results Corsika + Music Events statistics too poor: preliminary results Okada Event Selection: N hit min = 20  cut = -7.6 Fit results:  = 0.19 ± 0.02 deg k= 659 ± 8 deg -2 Event Selection: N hit min = 26  cut = -7.1 Fit results:  = 0.26 ± 0.04 deg k= 230 ± 2 deg -2 PRELIMINARY