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KM3NeT: A Next Generation Neutrino Telescope in the Mediterranean Sea

Alexander Kappes University Erlangen-Nuremberg For the KM3NeT Consortium 6 th International Workshop on New Worlds in Astroparticle Physics 6. – 8. September 2007, Faro Portugal. KM3NeT: A Next Generation Neutrino Telescope in the Mediterranean Sea. Outline of Talk. Physics case

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KM3NeT: A Next Generation Neutrino Telescope in the Mediterranean Sea

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  1. Alexander Kappes University Erlangen-Nuremberg For the KM3NeT Consortium 6th International Workshop on New Worlds in Astroparticle Physics 6. – 8. September 2007, Faro Portugal KM3NeT: A Next Generation Neutrino Telescope in the Mediterranean Sea

  2. Alexander Kappes, U-Erlangen Outline of Talk Physics case Towards a km3 detector The KM3NeT Design Study How does it go on?

  3. Alexander Kappes, U-Erlangen Potential Cosmic Neutrino Sources Galactic: Pulsar Wind Nebula Supernova Remnants Microquasars RX J1713.7-3946HESS Extra-Galactic: Active Galactic Nuclei Gamma Ray Bursts (GRB970228, BeppoSax)

  4. Alexander Kappes, U-Erlangen Directional Sensitivity of Neutrino Telescopes Muons fromnmfor identification of individual sources (angular resolution) Muons can penetrate several km of water if Em > 1 TeV⇒huge background from atmospheric m Sensitivity for upward sources largely reduced needs either very high energies or short transients (e.g., GRBs) downward horizon upward

  5. Alexander Kappes, U-Erlangen Why a Neutrino Telescope in the Mediterranean ? Observed sky region in galactic coordinates assuming efficiency onlyfor downwardhemisphere. Mediterranean site: >75% visibility >25% visibility → We need Northern  telescopes to cover the Galactic Plane

  6. Alexander Kappes, U-Erlangen n Flux Predictions from g-Ray Measurements Example: Vela X (PWN) measured-ray flux (H.E.S.S.) mean atm. flux(Volkova, 1980, Sov.J.Nucl.Phys., 31(6), 784) 1  error bands include sys. errors (20% normalization, 10% index & cut-off) expected neutrino flux –in reach for KM3NeT A. Kappes et al., ApJ 656:870, 2007 (astro-ph/0607286) All calculations show that we need km3-scale detectors

  7. Alexander Kappes, U-Erlangen The KM3NeT Project Currently consisting of 37 institutes from 10 European countries(Cyprus, France, Germany, Greece, Ireland, Italy, Netherlands, Romania, Spain, UK) Includes expertise from all pilot projects (ANTARES, NEMO, NESTOR) Objectives: build and operate a km3-scale next generation water Cherenkov neutrino telescope build and maintain a deep sea research infrastructurefor oceanographic sciences:(Oceanology, Marine Biology, Environmental Sciences, Geology and Geophysics)

  8. Alexander Kappes, U-Erlangen The KM3NeT Vision KM3NeT will be a multidisciplinary research infrastructure: Deep-sea access for marine sciences. Data will be publicly available; KM3NeT will be a pan-European project but non European institutes are highly welcome! 10 European countries already involved; Substantial funding already now from national agencies; KM3NeT on ESFRI roadmap. KM3NeT will be constructed in time to take dataconcurrently with IceCube. KM3NeT will be extendable.

  9. Alexander Kappes, U-Erlangen The KM3NeT Design Study Supported by the European Union in FP6 with 9 M€, tot. volume ~20 M€. Major Objectives: Started on Feb. 1, 2006; will run for 3 years. Conceptual Design Report by end 2007 (workshop Nov. 2007); Technical Design Report by Spring 2009; Detector target specifications: Effective volume ≥ 1 km3 0.1˚ angular resolution for muons (E ≥ 10 TeV) Energy threshold few 100 GeV (~100 GeV when pointing) Sensitivity to all neutrino flavors Field of view close to 4 p for high energies

  10. Alexander Kappes, U-Erlangen Some Key Questions Maximize physics output for given budget: Which architecture to use?(strings vs. towers vs. new design) How to get the data to shore?(optical vs. electric, electronics off-shore or on-shore) How to calibrate the detector?(separate calibration and detection units?) Design of photo-detection units?(large vs. several small PMs, directionality, ...) Deployment technology?(dry vs. wet by ROV/AUV vs. wet from surface) And finally: path to site decision.

  11. Alexander Kappes, U-Erlangen Production model (example) Configuration: 10000 optical modules 250 detector units 25 calibration units 3 years for construction (2010-2013) 15 / day 10 / month 1 / month ~ 5 assembly sites are needed 10 detector units / 400 OMs per month to be deployed !

  12. Alexander Kappes, U-Erlangen KM3NeT Phases Design study: 2006-2009 Technical Design Report Preparatory phase: 2008-2010(invited for negotiations) Political convergence Commitment for construction of funding agencies/ministries Governance and legal structure System prototype Tendering procedures Construction phase: 2010-2013 Build a 1 km3 detector

  13. Alexander Kappes, U-Erlangen Summary and Outlook Compelling scientific arguments for neutrino astronomy andthe construction of large neutrino telescopes It is essential to complement IceCube with a km3-scale neutrino telescope in Northern Hemisphere Joint effort of ANTARES, NEMO and NESTOR to realize such a detector in the Mediterranean Sea EU funded KM3NeT Design Study (2006–2009) is well on its way CDR workshop in November Technical Design Report early 2009 Start of “Prepatory Phase” expected early 2008 (until 2010)

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