1. KM3NeT status Neutrino telescope in the Mediterranean Sea Dorothea Samtleben, NIKHEF Jamboree December 2012

2. 180m - 130m 860m 640 strings 20 storeys/string 12800 DOMs 2 Artist’s impression Volume: 6 – 4 km 3 Height almost 8 times Utrecht dom- toren (112 m x 7.7)

3. Outline Formal developments Science focus Hardware developments Simulations New ideas at low energies: ORCA Outlook

4. People at Nikhef Scientific staff: Aart Heijboer, Maarten de Jong, Paul Kooijman, DS, Jos Steijger, Els de Wolf Engineering: Hans Band, Edward Berbee, Ad Berkien, Rene de Boer, Herman Boer Rookhuizen, Deepak Gaianana, Mesfin Gebyehu, Vladimir Gromov, Eric Heine (retired), Jelle Hogenbirk (retired), Mar van der Hoek (consultancy), Peter Jansweijer, Gerard Kieft, Hans Kok, Jan Koopstra, Auke Korporaal, Boudewijn van der Kroon, Sander Mos, Henk Peek, Oscar van Petten, Erno Roeland, Jan Willem Schmelling, Paul Timmer, Patrick Werneke Students involved in hardware testing: Tino Michael, Dimitris Palioselitis, Maria Tselengidou, Erwin Visser

5. Establishing the project Official ending of KM3NeT preparatory phase (FP7) in February 2012 Successful proposal to stay on Netherlands’ Roadmap for Large-Scale Research Facilities -> Moving some of the funds to establish KM3NeT headquarters at Nikhef Agreement on baseline technology: Multi-PMT optical module (= Nikhef design) String (= Dutch design) Operation of modular blocks at several sites being considered: The advantage of additional funding and human resources resulting from adopting a multi-site solution significantly outweighs any financial or scientific advantage from adopting a single site solution

6. Establishing the project Funds available for 1/5 of full detector (phase I) => Preparing for full detector (phase II) Formation of collaboration: - MoU almost done - new management structures are being set up KM3NeT Collaboration meeting scheduled 29-31 January,2013

7. Facilities of the KM3NeT Research Infrastructure 7

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

9. Science focus Observation of Galactic Neutrino sources RXJ1713, Vela-X, … Fermi Bubbles First KM3NeT paper accepted for publication in Astrophysical Journal „Detection Potential of the KM3NeT Detector for High-Energy Neutrinos from the Fermi Bubbles“ Observation in gamma-rays Hard E -2 spectrum of  rays, origin unknown No fully consistent models available explaining radiation from leptonic processes Possibly cosmic ray population from star forming region in the Galactic center  Hadronic processes responsible  Pion decays create neutrino flux Detection/Flux limit can distinguish models

10. …….. 5σ C.L. 50% prob.3σ C.L. 50% prob.

11. Photomultipliers Two companies with established prototypes Hamamatsu: 200 PMTs from prototype series delivered August-December 2012 Testing at Nikhef, Erlangen, Catania ET Enterprises Ltd: 100 PMTs from prototype series delivered Larger diameter PMT under development Testing at Nikhef, Erlangen Orders for 1000s of PMTs starting next year New Chinese PMT manufacturer (HZC): Planned delivery of a few PMTs in December 2012 utilizing Photonis expertise Maarten de Jong & Els de Wolf visiting right now Opportunity for new partners in KM3NeT Price per photocathode better than for large (Antares-like) 10 inch PMTs

12. PPM-DOM integration 12

13. Integration in ANTARES IL12 Time calibration 13

14. Ready for installation in ANTARES Thanks to: ANTARES, CPPM, ECAP, ISS, Nestor, Nikhef, LNS, Saclay, Valencia 14

15. 15 Central Logic Board (CLB) Rx_mac2buf 2 nd CPU LM32 MEM I2CUART Fifo 31 TDCs TDC0 Managemen t & Control Data Control Wishbone shared bus (32 bits) RxPacket Buffer 64KB IP/UDP Packet Buffer Stream Selector (IPMUX) Rx_buf2data RxPort 1 RxPort 2 RxPort_m Managemen t & Config. Tx_pkt2mac Tx_data2buf TxPort 1 TxPort 2 TxPort_m Flags Rx Stream Select TxPacket Buffer 32KB Flags Tx Stream Select 31 PMTs UTC time & Clock (PPS, 125 MHz) Pause Frame ADC Managemen t & Control Hydrophone State Machine Fifo TDC3 0 Fifo Nano Beacon GPIO Debug LEDs I2C Debug RS232 TempCompassTilt Point to Point interconnection Xilinx Kintex-7

16. 16 Basic White Rabbit Synchronization Test Setup Based on SPEC Board Based on Kintex Ev. Board SoftPLL Hardware DIO http://www.ohwr.org/projects/fmc-dio-5chttla/wiki Extra info on SPEC-to-SPEC test setup: http://www.ohwr.org/projects/wr-cores/wiki/Spec-to-spec Our goal Kintex-to-Kintex test setup! FMC Connector

17. ASIC development for PMT base Both ASICs have been successfully tested, orders for 10,000 being prepared

18. Vertical Electro-Optical Cable - carries optical fibres and copper wire bundle - oil-Filled cable with break-out boxes In-situ tests - November 2012: mechanical test @ 5000 m depth + stand-alone cables - Planned April 2013: several tests @ 1000 m depth + Integration in string-DU + Using LOM launching vehicle VEOC backbone

19. Assembly of VEOC

20. Recovery from 5000 m depth RV Pelagia 1 Nov, 2012 NIOZ involvement

21. Data from loggers 5000 m 3 o at 5000 m Temperature depth pressure attenuation loss Conform calculations -4.7 dB (?) Unexpected loss explained by use of SMF28 in containers i.s.o. Bendbright ; SMF28 fibre got stuck in narrow container. Depth effect < 1 dB 7 hours

22. DU-deployment tests with LOM Launching vehicle (NIOZ design) First two weeks April, 2013 Off-shore Spanish coast (Motril) RV Pelagia of NIOZ Test programme defined Aiming at 10 deployments/recoveries 22

23. events / year number of linesnumber of floors Building block = smallest detector with optimal efficiency Modular installation possible: blocks can be installed without loss in science reach at different sites scaling factor Simulations: Optimizing the configuration

24. Track Reconstruction Different algorithms under development, used for evaluating physics potential At Nikhef development of reconstruction based on scanning approach: Scan all directions with linear prefit Follow up with likelihood fit of most promising candidates Approach also under investigation on Antares data, first Antares data reprocessing underway with implementation of this scheme Implementation on Multi-PMT DOMs exploiting background suppression usingdirectionality and correlations of the PMTs

25. RXJ 1713 ‒ Supernova remnants as “origin of cosmic rays” ‒ KM3NeT can make 5 (3) sigma discovery in 5 (2.5) years E [GeV] Probability Angle [degrees] Area [m 2 ] Effective neutrino area Angular resolution muon neutrino 3 Vela X Performance

26. Possibly new science option New results this year in neutrino experiments: Mixing angle  13 not zero (2 independent measurements announced spring this year) => opens possibility of large CP violation in neutrino sector interpretation of measurements depend on the neutrino mass hierarchy Can Neutrino Telescopes contribute? Sensitivity at low energies (1-20GeV) needed IceCube -> Deepcore -> PINGU (Precision IceCube Next Generation Upgrade) New initiative from KM3NeT: ORCA (Oscillation Research with Cosmics in the Abyss

27. Mass hierarchy Oscillation measurements determined mass differences, but different ordering Possible, named ‚Normal Hierarchy‘ (NH) and ‚Inverted Hierarchy‘ (IH) But be careful in the conventions you use! Mass differences and nomenclature of NH/IH are ambiguous:

28. Neutrino oscillations Propagation of neutrinos and antineutrinos in matter different (MSW effect) Electron-neutrinos can interact with electrons via t-channel W-exchange For electron-antineutrinos s-channel W-exchange enters with opposite sign Effective mass differences shifted due to MSW effect, different impact on normal and inverted hierarchy Mixing between flavour and mass eigenstates

29. Oscillation probabilities Parameter uncertainties determine width of bands Different zenith angles (top: straight upwards, bottom: zenith 127 degrees)

30. Assuming energy resolution of 20% 15 hits in detector

31. 2 km Vertical distances on a string: 40m 150 m Vertical distances on a string: 6m 1 possible modular building block 154 Strings, ~1/4 full phase II KM3NeT configuration Possible phase-I configuration for ORCA

32. 50 Strings in KM3NeT configuration (black) in comparison with possible ORCA configuration (red) 1400 m

33. Conclusion and Outlook Formal establishment of collaboration in sight Dedicated Nikhef workforce successful to move critical hardware developments forward United developments with European partners on single technology (strings with Multi- PMT DOMs) and multiple sites Excellent prospects for the detection of neutrinos from Fermi Bubbles and Galactic Sources Potentially neutrino mass hierarchy could be measurable with restructuring configuration of phase I to a dense structure DECISION NEEDED WITHIN A YEAR Work underway on the ‚Global Neutrino Telescope Network‘ aiming to embed KM3NeT together with other neutrino telescopes in an overall structure to bond and strengthen community also towards the funding agencies