KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 1 INFN in WP2 Marco Circella on behalf of the collaboration Bari Bologna Napoli LNS, Catania Pisa Roma

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 2 Layout  Participants and contact persons  Present activities (relevant to WP2) of the INFN groups  Interest of INFN groups in WP2 activities

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 3 Participants (and contact persons)  Bari: Roberto Bellotti, Francesco Cafagna, Marco Circella, Rosario Megna, Teresa Montaruli  Bologna: Marco Bazzotti, Giada Carminati, Annarita Margiotta, Maurizio Spurio  LNS: Rosa Coniglione, Carla Di Stefano, Emilio Migneco, Piera Sapienza  Napoli: Gianfranca De Rosa  Pisa: Ersilio Castorina, Vincenzo Cavasinni, C. Evoli, Dario Grasso, Luca Maccione, Antonio Marinelli  Roma: Tommaso Chiarusi, Giulia De Bonis, Fabrizio Lucarelli

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 4 Current activities (ANTARES & NEMO)  Neutrino sources: Bari, Catania, Pisa  Neutrino generators: Bari  Atmospheric muons, muon propagation: Bari, Bologna, LNS  Non-standard physics: Bologna, Pisa  Tracking and event viewer: Bologna, LNS, Roma  ANTARES offline physics filter and event processor: Bologna  NEMO time calibration: Bari  Apparatus simulation and physics performance (angular resolution, source sensitivity, etc.): Bari, Bologna, LNS, Roma

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 5 Software tools  ANTARES software  ANTARES software adapted to a KM3 apparatus  NEMO software (+ specific codes)

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 6 Proposed activity in WP2 (I)  Define benchmark neutrino fluxes: Bari, Pisa, Roma It requires: Source modelling Flux parameterization Neutrino generators

KM3NeT kickoff meeting, Erlangen 11 April 2006 M. Circella, INFN contribution to WP2 7 Neutrinos from pointlike sources Complement to gamma-astronomy; sensitive to sources opaque to photons; distinguish hadronic and leptonic interactions; study of very dense sources; hints of dark matter existence; cosmic ray origin (from SNR?); study of measurability by: AMANDA, ICECUBE, ANTARES, NEMO, NESTOR, Km3 … Theoretical-phenomenological activity in Pisa: High energy neutrinos generated by pointlike and diffuse galactic sources V. Cavasinni, D. Grasso, L. Maccione, C. Evoli (Dipartimento di fisica, Scuola Normale Superiore, I.N.F.N. Pisa) (Contributed slide from Pisa -1)

KM3NeT kickoff meeting, Erlangen 11 April 2006 M. Circella, INFN contribution to WP2 8 Activities: Expected neutrinos from near or embedded in GMC SNR (astro-ph/ ) Hypothesis: - Shock wave accelerate protons and nucleat at energies > 1 PeV. Relationship between neutrinos and gamma rays: Gamma rays from π 0 decays - Neutrinos from π ± e K ± decays - Take into account neutrino-oscillations Estimate also neutrinos from neutron decays; neutrons from: - Photodisintegration of nuclei on UV photons; - Hadronic interactions (main contribution). Under investigations: neutrinos from Galactic Centre Near future : Other gamma rays sources (HESS, MAGIC…) new sources (high density regions, OB stars) …..… (Contributed slide from Pisa -2)

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 9 NeutrinoFlux: Motivation  “multi purpose” tool: can be used as root macro and linked into an executable  An updated neutrino flux generator to be used to generate inputs for detector simulation chains. (Contributed slide from Bari - 1)

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 10 NeutrinoFlux: General  At the moment it is possible to generate:  Atmospheric: 3 Conventional and 11 prompt models  Astrophysical: 7 models for emission from AGNs, 8 models for emission from GRBs and 3 models of upper bound  We are working to implement a more general class able to parse any directory and load the fluxes stored in formatted files. (Contributed slide from Bari - 2)

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 11 A new calculation (Fluka based) of atmospheric neutrino and muon fluxes  Extension of the previous calculation up to 10 6 GeV/nucleon  Focus on prompt neutrino tagging coming from the decay of short-lived heavy quark  Irreducible background for neutrino telescopes  Study of charm production cross section at high energy  New primary spectrum (Contributed slide from Bari – 3)

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 12 Proposed activity in WP2 (II)  Atmospheric muons: Bari, Bologna, LNS It requires: Estimate of muon flux Propagation of muons Parameterized simulation

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 13 Proposed activity in WP2 (III)  Apparatus simulation: Bari, Bologna, LNS, Roma It requires: Geometry reconfiguration Instrumental response Site characteristics control

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 14 Proposed activity in WP2 (IV)  Event reconstruction and classification: Bari, Bologna, LNS, Roma It requires: Tracking Triggering Background rejection Particle classification

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 15 Proposed activity in WP2 (V)  Apparatus performance (related to cost and site choices): Bari, Bologna, LNS, Napoli, Roma Key issues: Site (depth and optical background) Apparatus architecture

M. Circella, INFN contribution to WP2 The NEMO lay-out Characteristics of the simulated km 3 detector Square array m, 300 m, … tower spaced Tower characteristics: - total height 830 m - instrumented 680 m - number of bars 18 - number of PMTs per bar 4 - number of towers 81 - number of PMTs bar length 20 m - bar vertical distance 40 m - PMT 10’’ 40m 20m (Contributed slide from LNS - 1)

M. Circella, INFN contribution to WP2 “Trigger” for reconstruction 2/2 at least 2/4 The reconstruction procedure is based on a maximum likelihood method all the hits with amplitude < 0.5 p.e. are rejected a causality filter with respect to the highest amplitude hit is applied a linear prefit is applied on a sub-set of hits that passed the following conditions (they are part of a local coincidence) OR (hit amplitude >2.5 p.e.) Local coincidences = hit with 20ns+  t(L) difference in time in different PMT Local coincidences at least3/4 (Contributed slide from LNS - 2)

M. Circella, INFN contribution to WP2 Effective muon area vs background rates Even with local coincidence “trigger” (3/4) a stronger and stronger effective area reduction is observed with increasing background rates The best “trigger” for each rate value is applied 35 kHz - 2/4 local coinc.  60 kHz – 3/4 local coinc.  120 kHz – 3/4 local coinc (Contributed slide from LNS - 3)

M. Circella, INFN contribution to WP2 Effects of abs abs 440 nm abs 440 nm At muon energy lower than 3TeV effective areas larger by (more than) 20% A eff (70m)/A eff (50m) vs E  A eff ( abs 70m)/A eff ( abs 50 m) A eff vs E  - 20 kHz (Contributed slide from LNS - 4)

M. Circella, INFN contribution to WP2 The architectural comparison Compromise between performance and technical feasibility Performance-> Angular resolution and effective areas for  up-going muons (E   10 2  10 8 GeV) in the whole angular range Studied architectures with  about 100 structures  about OM  tower height <1000m (Contributed slide from LNS - 5)

M. Circella, INFN contribution to WP2 The geometries 40m 20m 5832 PMT 81 strings String height 680 m (18floors/string) V= 0.88 km 3 String-dh_140_20NEMO_140String-d_125_ PMT 100 strings String height 912 m (58 PMT/string) V= 1.15 km PMT 81 towers String height 680 m (18floors/tower) V= 0.88 km 3 (Contributed slide from LNS - 6)

M. Circella, INFN contribution to WP2 The effective neutrino areas vs E NEMO_140 string-d_125_16  string-dh_140_20 35 kHz background – abs Up-going neutrinos (Contributed slide from LNS - 7)

Angular resolution vs  Up-going neutrinos E 10 2  10 3 GeVE 10 3  10 4 GeV Vertical Horizontal The “string” detectors show a wore angular resolution for near vertical muons Q. Cut applied NEMO_140 string-d_125_16  string-dh_140_20 (Contributed slide from LNS - 8)

M. Circella, INFN contribution to WP2 Determination of the angular resolution (Simulated time 1 year) 100 days needed to observe a 3  effect Observation of the Moon shadowing effect on the flux of atmospheric muons Determination of the angular resolution (Contributed slide from LNS - 9)

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 25 Proposed activity in WP2 (VI)  Time calibration issues: Bari Key issues: Accuracy requirements Spacing of calibration units

KM3NeT kickoff meeting, Erlangen 11 April 2006M. Circella, INFN contribution to WP2 26 That’s all for the moment… Thank you for your attention!