Spyros Tzamarias School of Science and Technology Hellenic Open University

1. Spyros Tzamarias School of Science and Technology Hellenic Open University Neutrino Telescopy after the new developments in Particle and Astroparticle Physics

2. Sky viewof a MediterraneanUnderSea Neutrino Telescope FOV for up-going neutrinos shown From Mediterranean 24h per day visibility up to declination d~-50° >25% >75% • KM3NeT coverage of most of the sky (87%) including the Galactic Centre

3. KM3NeT consortium consists of 40 European institutes, including those in Antares, Nemo and Nestor, from 10 countries (Cyprus, France, Germany, Greece, Ireland, Italy, The Netherlands, Rumania, Spain, U.K) • KM3NeT is included in the ESFRI and ASPERA roadmaps • KM3NeT Design Study (2006-2009) defined telescope design and outlined main technological options • Approved and funded under the 6° EU Frame Program • Conceptual Design Report published in 2008 http://www.km3net.org/public.php • Technical Design Report (TDR) completed => outline technology options for the construction, deployment and maintenance of a deep sea neutrino telescope http://www.km3net.org/KM3NeT-TDR.pdf • KM3NeT Preparatory Phase (2008-2012) defines final design, production planes for the detector elements and infrastructure features. Prototype validationis under way. Legal, governance and funding aspects are also under study. • Scientific Standing Committee: External Scientific Evaluation • Approved and funded by EU under the 7° EU Frame Program

4. General KM3NeT lay-out Detection Units Primary Junction box Secondary Junction boxes Electro-optical cable OpticalModule (OM) = pressureresistant/tight spherecointainingphoto-multpliers Detection Unit (DU) = mechanicalstructureholding OMs, enviromentalsensors, electronics,… DU is the building block of the telescope

5. Design Study TDR - Detection Unit and OpticalModuleConcepts Flexible tower with horizontal bars equipped with large PMT OMs Slender string Vertical sequence of multi-PMT OMs • Preparatory Phase =>Convergence i.e. DU=Flexible tower, OM=Multi-PMT • Prototype and validation activities crucial for final choice • GOLDEN ROOL: Maximize the Discovery Potential 5 TwodifferentoptionsforOMs and Dusreported in TDR

6. DOMBAR Prototype–Storey - Bar Frame Rope Storage Rope & Cable Storage Mechanical Cable Connection 6 m Optical Module Mechanical Interface 2 DOM + 1 BAR = 1 DOMBAR 20 DOMBARS = DOMTOWER The Vertical String Structure IS NOT ROOLED OUT

7. Fermi LAT Observation – Fermi Bubbles - • Large extension (50°lat. 40° long.) • no spatial variation in the g spectrum From Meng Su, Tracy R. Slatyer, Douglas P. Finkbeiner Astrophys.J.724:1044-1082,2010

8. From M. Crocker and F. Haronian Phys. Rev. Lett. 106 (2011) 101102 “We show below that a cosmic ray population can explain these structures” ……… “…Finally, we predict that there should be a region of extended, TeV g radiation surrounding the Galactic nucleus on similar size scales to the GeV bubbles with an intensity up to E-2 Fg(TeV) ~10-9 TeV cm-1 s-1 sr-1which should make an interesting target for future g-ray studies. Likewise, the region is a promising source for future, Northern Hemiphere, km3-volume neutrino telescope: we estimate (assuming a g=2.0 proton spectrum cut-off 1 PeV)…. The expected neutrino flux for one bubble is E-2 Fn(TeV) ~ 10-6GeV cm-1 s-1 sr-1 * 0.34 sr / 2.5 ~ 1.3 10-7GeV cm-1 s-1 From g spectrum to n spectrum Single bubble solid angle Gamma flux

9. Rosa Coniglione Neutrino generation homogeneous in a circular region around fixed points North d = -15° RA = 243° R =19° South d = -44° RA = 298° R =19° one block of 154 DU

10. In Meng Su et al. bubbles are due to relativistic CR electrons that produce gamma through IC process

11. Galactic Candidate n Sources – SNRs - RXJ1713-39.43 IF hadronicmechanisms=>nspectrumcan becalculatedfromVHE gspectrum( solidredlineVissani) Observation at 5s withinabout 5ys withKM3NeT Hess RXJ1713-39.43 OriginofCosmicRays SNR paradigm, VHE gbutno conclusive evidenceaboutCR acceleration RXJ1713-39.43 and Vela JR best candidates

15. Gamma Ray Bursts

17. The spatial distribution of the photosensitive area is a critical parameter that affects the discovery potential of the telescope NIM A 626-627 (2011) S188-S190

18. Environmental Parameters & Early Discovery Driven Scenario doi:10.1016/j.nima.2010.09.040 |

19. Detector Geometrical Layout 154 Towers or 77 Towers Each Tower consists of 20 bars, 6m in length and 40m apart One MultiPMT OM at each end of the bar. 29% QE Detectors Footprint

20. (θ, φ) z Use WISELY the whole Experimental Information (θm, φm) ψ • Reconstruction Resolution on a track by track basis • Energy Estimation x y

21. Eν<10 TeV 100TeV<Eν<1 PeV 10TeV<Eν<100 TeV 1PeV<Eν

22. A Neutrino Telescope CAN Measure Energy NIM A 626-627 (2011) S185-S187

23. 0.5<cos(θ)<0.55 Reconstructed Energy (log of GeV)

24. N=0 N=4 N=6 N=8

25. Discovery Potential (50% Discovery Probability) preliminary 3σ This Method: 1.2x 10-9 E-2 flux for 50% discovery This Method without Energy: 1.6x10-9 Binned method: >2.4x10-9 4σ This Method: 1.6x 10-9 This Method without Energy: 2.6x10-9

26. Atmospheric γ=2 γ=1.8 (re-weighted)) Log(E/GeV)

27. 15 Signal Events on Top of Background 24 Signal Events on Top of Background Signal Events Signal Events Spectral Index Spectral Index

28. Spectral Index estimation accuracy Signal events on top of Background

29. Final Remarks • We gain a factor of 2 in discovery potential by using more of the information offered by the data ! We can make it better… • The Design of KM3 is not finished yet Optimize the layout for fast discovery Galactic Extended Sources GRBs, AGN, GKZ Dark Matter? UHE Atmospheric Showers ?