1 / 14

AGENDA (km3net2p3.fr)

AGENDA (http://km3net.in2p3.fr). Manage password: wp20710. 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

hova
Download Presentation

AGENDA (km3net2p3.fr)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. 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 source UK, 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 trigger INFN, 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. Aharonian, coyle Part 1: Physics of KM3NET • Introduction • Galactic sources Aharonian • SNRs, PWN • Compact binary systems • Galactic centre diffuse emission Jouvenot • No conterparts • Hidden sources • Extragalactic sources • Diffuse flux Spurio • AGNs White • GRBs Petronovic • GZK, top-down Erenwein, Kouchner • Neutrino Flavour ratios ? • Dark matter annihilation Motz • Magnetic monopoles Popa • Other physics • Cosmic rays Lyons? • Neutrino oscillations Brunner • Lorentz invariance, quantum gravity etc. ? • New phenomenon

  8. Markou, coyle 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

  9. Carr, shandize, Sapienza, coyle Part 3: Optimisation studies • Simulation Software • Antares Brunner • NESSY Dornic • SIRENE/KM3TRAY Presanora, Auer • Track finding and reconstruction • Cost model Katz • Photodetection studies • 10’’ PMT • 20’’ PMT • Multi-small PMTs • Hybrid PMs • Direction sensitive PMs Tauiti • Geometry Optimisation • Hexagonal/cuboid • Cluster • Ring/Square • Nemo Sapienza • reference effective area& angular resolution • Effect of site parameters • Absorption length, scattering , depth Conglione • Beyond 1KM3 • Absolute pointing calibration • Moon shadow Distefano • Surface array Tsirigotis

  10. Shanidze, Coyle Part 4: Physics Performance • Introduction • Methods for discovery/limit setting Shanidze • MRF, MDF • Galactic sources Kappes? • SNRs, PWN • Compact binary systems Distefano • Galactic centre diffuse emission Jouvenot • Extragalactic sources • Diffuse flux Spurio • AGNs White • GRBs Petronovic • GZK, top-down Erenwein, Kouchner • Neutrino Flavour ratios? ? • Dark matter annihilation Motz • Magnetic monopoles Popa • Other physics? • Cosmic rays Lyon? • Neutrino oscillations Brunner? • New phenomenon

  11. Nikhef NWO Investment Proposal 2007

  12. Nikhef NWO Investment Proposal 2007

  13. Agenda Amsterdam Monday 10h00-13h00 Parallel session • Cost model software Uli Katz • SNR Gilles Maurin • Galactic diffuse emission Fabrice Jouvenot • WB bound Andrew Taylor • Neutrino from SNR Stefano Gabici • … Weds (1h30) Plenary session • Physics F. Aharonian • Detector Optimisation P. Coyle

  14. The Ball Park Construction costs ~?/km3 Meuros Angular resolution ~0.1 degrees above 100 TeV Effective surface area >2 km2 above 100 TeV Number of structures: ~80-150 Number of PMs: ~5000-10000 Distance between structures 90-130m Distance between storeys 15-40m first storey height ~100m Total height 500-1000m Number of PMs per storey 3-6 Timing precision ~3ns (TTS+dispersion+electronics+positioning) (Assumes PMs not dominant cost)

More Related