1. Tuesday 30 October 2007 09:00 Introduction (30') Paschal Coyle (CPPM) 09:30 Lepton and cherenkov light propagation with mmc&photonics (30') Claudio Kopper (Univ.Erlangen) 10:00 Status of the KM3Tray software framework (30') Ralf Auer ((Univ. Erlangen)) 10:30 break (30') 11:00 Design studies for the KM3NeT neutrino Telescope in Erlangen (30') Rezo Shanidze (Erlangen) 11:30 Simulations of hexagon geometries using NESSY (30') Damien Dornic (CPPM) 13:00 lunch (1h00') 14:00 status of simulations using direction sensitive PMs (30') Mauro Taiuti (Genova) 14:30 New filtering and reconstruction techniques for KM3NeT (30') Apostolos Tsirigotis (HOU) 15:30 break (30') 16:00 Simulation of extended sources: SNR RXJ1713.7-3946 (30') Carla Distefano (LNS-INFN) Wednesday 31 October 2007 09:30 KM3 geometries with the Antares software (30') Rosa Coniglione (LNS-INFN) 10:00 Simulation of ring geometries using SIRENE (30') Paul Koojiman (Nikhef) 10:30 break (30') 11:00 UHE neutrinos (15') Jean-Pierre Ernenwein (Mulhouse) 11:15 A status report on simulations using GEANT at Demokritos (15') Petros Rapidis (Demokritos) 11:30 General discussion (1h30') 13:00 lunch (1h00') 14:00 More discussion-if necessary! (1h00) AGENDA (http://km3net.in2p3.fr) Manage password: wp20710

2. Pending Issues Physics Priority –< 1 TeV:Dark matter –1-100 TeV:HESS sources, GRBs –>1 PeV:Diffuse flux, GZK, AGN Evaluation of NEMO geometry Evaluate effect of energy measurement on sensitivity Rejection of downgoing atmospheric muons Cost Model Reconstruction of electron and tau neutrinos energy resolution, direction resolution Specification of front end? Time resolution, dynamic range, 2 track separation, 1 vs 2 photon separation, dead time….

3. More Issues Standard simulation/analysis framework ANTARES/NEMO soft (KM3, geasim….) NESSY-mathematica SIRENE/MMC+PHOTONICS KM3TRAY KM3NET internal notes For us For reference in CDR CDR writing framework Word, latex, something else? Extrapolation of Auger observations Manpower

4. WP2 and the CDR Major contributions to writing of: Physics Case Detection techniques Optimisation studies Physics performance CDR Workshop: Monday morning (10-13h)Parallel session Wedsnesday morning (1h30)Plenary session This meeting: status of ongoing work choice of reference effective area/resolution plan for documents allocation of writing tasks

5. Contributions Source modelling: INFN, CEA, DUBLIN Atmospheric muons: INFN Galactic (CR) neutrinos: INFN, UK, CEA Galactic (HESS) sources: Erlangen, IN2P3, CEA, INFN Dark matter: INFN, Erlangen, IN2P3, UK, FOM Diffuse flux:INFN, Erlangen Extragalactic pt sourceUK, IN2P3 GRBs:Erlangen, FOM UHE:UHA-GRPHE, APC Neutrino flux generator: INFN software: FOM, IN2P3, Erlangen Multi-PMT geometry: FOM Directional PMT:INFN simulation of triggerINFN, FOM, Demo, HOU, Erlangen, IN2P3 Reconstruction algorithms: Erlangen,INFN, IN2P3, HOU, FOM, CEA Time,position calibration: UK, Valencia, Erlangen, INFN Absolute positioning : INFN(moon), HOU(surface array) Optimisation of design:ALL physics and analysis software calibration

6. Plan of WP2 CDR Documents Part 1: Physics of KM3NET Part 2: Detection technique Part 3: Geometry Optimisation studies Part 4: Physics performance

7. Part 1: Physics of KM3NET Introduction Galactic sources Aharonian –SNRs, PWN –Compact binary systems –Galactic centre diffuse emissionJouvenot –No conterparts –Hidden sources Extragalactic sources –Diffuse fluxSpurio –AGNsWhite –GRBsPetronovic –GZK, top-downErenwein, Kouchner Neutrino Flavour ratios ? Dark matter annihilation Motz Magnetic monopoles Popa Other physics –Cosmic raysLyons? –Neutrino oscillationsBrunner –Lorentz invariance, quantum gravity etc.? New phenomenon Aharonian, coyle

8. Part 2: Detection techniques Introduction Neutrino interactions The Cherenkov effect Backgrounds –Atmospheric muons –Atmospheric neutrinos –40K –Bioluminescence Effective area Angular resolution Energy resolution Observable sky –Cf. ICECUBE –Match to HESS, Auger Markou, coyle

9. Part 3: Optimisation studies Simulation Software –AntaresBrunner –NESSYDornic –SIRENE/KM3TRAYPresanora, Auer Track finding and reconstruction Cost model Katz Photodetection studies –10’’ PMT –20’’ PMT –Multi-small PMTs –Hybrid PMs –Direction sensitive PMsTauiti Geometry Optimisation –Hexagonal/cuboid –Cluster –Ring/Square –NemoSapienza –reference effective area& angular resolution Effect of site parameters –Absorption length, scattering, depthConglione Beyond 1KM3 Absolute pointing calibration –Moon shadowDistefano –Surface arrayTsirigotis Carr, shandize, Sapienza, coyle

10. Part 4: Physics Performance Introduction –Methods for discovery/limit settingShanidze –MRF, MDF Galactic sources Kappes? –SNRs, PWN –Compact binary systemsDistefano –Galactic centre diffuse emissionJouvenot Extragalactic sources –Diffuse fluxSpurio –AGNsWhite –GRBsPetronovic –GZK, top-downErenwein, Kouchner Neutrino Flavour ratios? ? Dark matter annihilation Motz Magnetic monopoles Popa Other physics? –Cosmic raysLyon? –Neutrino oscillationsBrunner? New phenomenon Shanidze, Coyle

11. Nikhef NWO Investment Proposal 2007

12. Nikhef NWO Investment Proposal 2007

13. Agenda Amsterdam Monday 10h00-13h00Parallel session Cost model softwareUli Katz SNR Gilles Maurin Galactic diffuse emission Fabrice Jouvenot WB boundAndrew Taylor Neutrino from SNRStefano Gabici … Weds (1h30)Plenary session Physics F. Aharonian Detector OptimisationP. Coyle

14. The Ball Park Construction costs~?/km3 Meuros Angular resolution~0.1 degrees above 100 TeV Effective surface area>2 km 2 above 100 TeV Number of structures:~80-150 Number of PMs:~5000-10000 Distance between structures90-130m Distance between storeys15-40m first storey height~100m Total height500-1000m Number of PMs per storey3-6 Timing precision~3ns (TTS+dispersion+electronics+positioning) (Assumes PMs not dominant cost)