1. Status report Els de Wolf Annual Meeting 2011, Nikhef

2. 180m - 130m 860m 320 towers 20 storeys/tower 12800 DOMs 2 Artist’s impression Volume: 6 – 4 km 3

3. Cosmic neutrino sources Galactic sources – SuperNova Remnants – Pulsar Wind Nebulae – Micro Quasars Extra Galactic Sources – Active Galactic Nuclei – Gamma Ray Bursts Cosmogenic (GZK) neutrinos Dark Matter annihillation 3

4. KM3NeT sensitivity to E -2 flux Sensitivity (90% C.L.) for E -2 point sources after 1 year. (declination) 308 towers; 180 m distance; instrumented volume ~ 6 km 3 4

5. Optimization of sensitivity For fixed number of € one can optimize sensitivity for different sources This depends on photocathode density eV 5

6. KM3NeT Science Focus Geographical location in Northern Hemisphere – Field of view includes Galactic centre Optical properties of deep-sea water – Excellent angular resolution Envisaged budget 220 ‒ 250 M€ – Large effective neutrino area Observe Supernova remnants in our Galaxy 6

7. Example source RXJ1713 Q.Yuan et al, Astrop. Phys. 35(2011)33, arXiv 1010.1901v2 Using hadronic model 7 Gamma ray flux can be interpreted with leptonic models (IC) or with hadronic models Detection of neutrinos: smoking gun of identifying acceleration sources of the Galactic CRs

8. RXJ1713 in KM3NeT E [GeV] events /year Triggered events *) Neutrinos from RXJ1713 *) TDR detector: 2 blocks of 157 towers; 180 m between towers 8 Optimization background reduction  towers closer together and/or longer bar length Atmospheric neutrinos [deg -2 ] About 1 event/month from RXJ1713

9. Discovery potential factor 1.5 ‒ 2 improvement compared to TDR design 9 *) 5σ discovery: probability that an upward fluctuation of background is larger than the expectation value of the signal, is < 2.8 x 10 -7 ; typical error +/- 1 year *)

10. Include other sources Un-binned likelihood method (~20%) – morphology of source – inclusion of energy estimate Reconstruction – use of directionality of DOMs – looking few degrees above horizon (upto ~20%) Anticipated improvements 10 Good prospects for a 5 σ discovery in 5 year

11. KM3NeT Digital Optical Module 31 x 3” PMTs Light concentrator ring → “free” larger tube Calibration instrumentation inside compass, tiltmeter acoustic piezo Nano (led) beacon All electronics inside Radius [mm] 11

12. PMTs for KM3NeT 4 manufacturers – ETEL (delivered 50; plus 50 within 2 weeks) – Hamamatsu (delivered 50) – MELZ (prototype expected soon) – Zhan Chuang Photonics (prototype expected mid 2012) All 4 consider production rate for KM3NeT feasible High Q.E. (>32%@380nm;>22%@470nm) ETEL tubes tested at Nikhef/KVI ETEL 12

13. Heat conductor Read Out Electronics Nanobeacon Foam core Octopus board Inside the DOM 13 Central Logic board with FPGA and TDCs DC/DC convertor

14. Communication network 14 Shore station Primary Junction Box Secondary Junction Boxes Detection Units Optical Fanout Module Single optical channel between shore and each DOM Complex electronics on-shore

15. Mechanical structure 15 6m Rope Spiralized e/o cable Cable connection to DOM

16. In-situ validations in 2012 Multi-PMT module in ANTARES instrumentation line – Measurements of singles and coincidence rates using ANTARES readout KM3NeT DOM in ANTARES instrumentation line – Long term bench mark of KM3NeT DOM readout via ANTARES backbone Prototype KM3NeT tower at Capo Passero site (Possibly) Mechanical KM3NeT tower at Pylos site Planning dependent on availability of vessels and ROVs 16

17. Smaller building blocks Better strategy for deployment Does not compromise sensitivity flux Allows for a networked detector Sensitivity flux for RXJ1713 17

18. Reviews NWO roadmap proposal – KM3NeT headquarters in Amsterdam – Temperature array inside neutrino telescope (NIOZ) – Referees positive – Site visit in January 2012 KM3NeT external Scientific Standing Committee – Review of scientific priorities and technology choices – Meeting in March and November 2011 at Nikhef – Report expected February 2012 18

19. After the preparatory phase FP7 Preparatory Phase will end March 2012 Current total funding for construction ~60 M€ – Need to spend before 2015 Coordination of orders/tendering starting 2012 – Need legal structure  ERIC (no VAT) – MoU is in preparation – Management team to be formed Aim for production: first DOM assembly line in 2012 19

20. Summary Galactic sources are within reach Good prospects for a 5σ discovery in 5 years Technical solutions are (near to being) verified Networked remotely operated detector Legal framework is imminent Funds allow for start of construction 20

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22. Fermi-LAT 22 Mixed spectrum need neutrinos??

23. Example source RXJ1713 Assumed neutrino spectrum Radius=0.65  E -2 23

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26. Performance E [GeV] PP Angle [degrees] Effective area [m 2 ] Trigger *) Angular resolution *) muon neutrino ABCABC )* TDR detector: 2x 157 towers; distance 180 m 26

27. Other physics Other galactic sources Extra-galactic sources Gamma-ray bursts Fermi bubbles Diffuse fluxes Cosmic rays Magnetic monopoles Nuclearites Dark matter...