ANTARES, KM3NeT, ORCA: Astronomy (and not only) in. the Abyss

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1 trino Telescopes: w and the Next ade ANTARES, KM3NeT, ORCA: Astronomy (and not only) in ulti-tev and Beyond eudon, 30 Nov 2015 the Abyss Véronique Van Elewyck (APC & Université Paris Diderot) Paschal Coyle 1 Centre de Physique des Particules de Marseille

2 Neutrinos From MeV to PeV Small cross-sections: Need very large detectors for highest energies KM3NET-ARCA ICECUBE 41 m KM3NeT-ORCA PINGU ANTARES SuperK 2

3 Neutrino telescopes: science scope Low Energy 3 GeV < E < 100 GeV Medium Energy 10 GeV < E < 1 TeV High Energy E > 1 TeV ν Oscillations ν Mass hierarchy Exotic particle physics Monopoles, nuclearites, Dark matter search from extra-terrestrial sources Origin and production mechanism of HE CR oceanography, biology, geology, glacierology 3

4 The CR-Gamma-Neutrino Connection e : : =1:2:0 source e : : =1:1:1 Earth 4

5 Neutrinos and Multi-Messenger Astronomy Cosmic Rays Subject to deflection by magnetic fields Horizon limited by GZK cutoff Large time delay w.r.t. optical signals Photons leptonic and hadronic processes-> confusion Absorbed at high energies and large distances Neutrinos Unambiguous signature of hadronic acceleration Not deflected by magnetic fields or absorbed by dust Horizon not limited by interaction with CMB/IR Escape from region of high matter density -> identify the cosmic ray sources Time correlated with EM signals Full sky 24/24, 7/7 5

6 Event Topologies Track-like Muon track from CC muon neutrinos Angular resolution 0.5 /0.1 for ice/water Track-like contains both a cascade and one track de/dx resolution factor 2-3 Not to scale Shower-like CC electron/tau and NC all flavour 80% of all nu interactions Angular resolution 10 /1 at 100 TeV for ice/water Energy resolution ~ 10% No track is identified

7 Reducing Atmos Muon and Atmos nu Backgrounds log (dn/de) p, a p Downgoing atmos muons: Select upgoing Go deep Energy cut Spatial clustering Time clustering Coinc. with EM signals Veto outer layers Atmospheric neutrinos: Select upgoing Go deep Energy cuts Spatial clustering Time clustering Coinc. with EM signals Veto assoc. muon (outer layers) Go shallow ν μ atm E -3,7 ν μ cosm E -2 Energy cut ~ TeV Energy

8 Current Neutrino Telescopes NT 200+ Antares IceCube South Pole Lake Baikal 1/2000 km3 228 PMTs Mediterranean ~ 43 o North Mediterranean Sea 1/100 km3 885 PMTs South Pole glacier 1 km PMTs Larger, sparser 8

9 ANTARES Completed 2008 Depth 2475m 12 lines, ~70m spacing 25 storeys per line 3x10 inch PMTs per storey Decomissioning m 60-70m 9

10 IceCube 10

11 IceCube Diffuse Flux Signal 4 year HESE analysis ICRC events 5.7 sigma Ethreshold: 60 TeV Best fit spectral index: Unfolded upgoing muon spectrum TEVPA yr data 5.9 sigma Ethreshold: 200 TeV Best fit spectral index:

12 ANTARES Diffuse flux Expected: 9.5 ± 2.5 bkgd 5.0 ± 1.1 IC flux Observed: 12 events 1.75 excess Consistent with bkgd Consistent with IC

13 Flux Characteristics 90% CL contours Results of IC tracks(6yr) and IC combined not compatible at > 3.6σ level Indication of spectral break (different energy thresholds)?? Indication of galactic and extra-galactic contributions (different hemispheres)??

14 Flavour Ratios 14

15 Origin of Astrophysical Neutrinos? Cascade resolution mainly Southern hemisphere Muon resolution only Northern hemisphere p=2.5% in gal. plane scan within ± 7.5 gal. latitude Indications of Galactic and extra-galactic contributions??

16 No Point Source Found Cascade resolution <4 30% improvement adding cascades

17 ANTARES: Some Galactic Searches IC hot spot Galactic plane: molecular clouds Fermi Bubbles No signifcant cluster found within 20 of IC hotspot Exclude more than 2 HESE events for index=2.5 Expected: 12 Observed: excess

18 Multi-Messenger Program The Multi-messenger Program 18 GeV-TeVγ-rays Fermi / HESS CTA UHECR Auger HE neutrinos Optic / X-ray TAROT, ROTSE / Swift, ZADKO Gravitational Waves Virgo / Ligo ANTARES events needed for 5 sigma

19 GRBs? Fermi-LAT Blazars? The Multi-messenger Program 19

20 Indirect Searches for Dark Matter Indirect search for Dark Matter 20 Relic WIMPs gravitationally trapped via elastic collisions (Sun, Earth, Galactic Center) Earth <E > ~ M /3 ANTARES

21 Baikal: Gigaton Volume Detector 21

22 > 100 TeV IceCube-Gen2

23 KM3NeT KM3NeT is a distributed research infrastructure with 3 main science topics: - The origin of cosmic neutrinos (high energy) - Measurement of fundamental neutrino properties (low energy) - Deep Sea Observatory - Oceanography, bioacoustics, bioluminescence, seismology Single Collaboration Single Technology Low-Energy (ORCA) High-Energy (ARCA) ARCA- Astroparticle Research with Cosmics in the Abyss ORCA- Oscillation Research with Cosmics in the Abyss

24 3NeT/ ARCA and KM3NeT/ ORCA KM3NeT Building Block (115 strings) y [m] ~36m/9m ~700m/200m ~90m/20m he layout of KM3NeT: strings with 18 DOMs each instrument a large volume of sea water. ARCA x [m] ORCA Location Italy France String distance (m) DOM spacing (m) 36 9 Volume (MTon) 500*2 3.8 ARCA OR Location Italy Fra String dist. [m] DOM spacing [m]

25 Phased Implementation Phase Blocks Primary deliverables Proof of feasibility and first science results (6 ORCA strings/ 24 ARCA strings) ARCA 1 ORCA Study of neutrino signal reported by IceCube; All flavor neutrino astronomy Neutrino mass hierarchy Neutrino astronomy including Galactic sources 25

26 KM3NeT Design String Digital Optical Module Launcher Vehicle x 3 PMTs LED & acoustic piezo inside Uniform angular coverage Directional information Photon counting Background rejection Low ageing Low drag ~ 600 or 200 m Rapid deployment Compact Autonomous unfurling Recoverable 26

27 KM3NeT Digital Optical Module x 3 PMTs Reflective rings around PMTs (+27% light detection, JINST 8 (2013) T03006) PMTs supported by plastic structure produced by 3D-printing Electronics components attached to cooling mushroom One single penetrator for connection to vertical cable Optical fibre data transmission DWDM with 80 wavelengths Gb/s readout FPGA readout 1 ns time stamp Time over threshold Modified White Rabbit time synchronisation Calibration: piezo-acoustic sensor, compass + tiltmeter, nano-led beacon Low power (7W per DOM)

28 KM3NeT Prototypes Rate [Hz] Rate [mhz] 1) Optical Module deployed at Antares, April 2013 (2500 m) Eur. Phys. J. C (2014) 74:3056 Multiplicity 2) Mini string deployed at Capo Passero, May 2014 (3500 m) m) arxiv: Accepted by Eur. Phys. J. C cos(q) 28

29 KM3NeT-Italy KM3NeT Picture Gallery KM3NeT-France

30 KM3NET: Diffuse Flux IC Diffuse flux KRAg Model radially dependent diffusion coefficient for Galactic cosmic rays Muon only muon cascade Angular resolution Energy resolution 300% 5% 30

31 KM3NET: Point Sources Galactic sources in reach 100% hadronic Significant discovery potential for extragalactic sources KM3NeT STAC, : ARCA LoI (U. Katz) 31

32 The Neutrino Mass Hierarchy P (νx νμ) Prime discriminator for theory models Origin of neutrino mass and flavour Help measuring the CP phase Absolute mass scale Nature (Dirac vs Majorana) Core-Collapse Supernovae Physics Normal Inverted 1 P(νμ νμ) for θ=130º IH NH 0.5 νμ νe normal Eν [GeV] 32

33 ORCA/PINGU: Neutrino Mass Hierarchy Determination 3 sigma determination of neutrino mass hierarchy in 3/4 years Widths indicate main uncertainty LBNE/NOVA: δcp JUNO: σe ( %) ORCA/PINGU/INO: θ 23 Other projections assume worst case parameters (1 st oct) ORCA ORCA timeline, assumes start construction 2017 for 3 years LBNE from LBNE-doc-8087-V10 PINGU from MANTS 2015 Others Blennow 33

34 Summary Neutrinos unique and unexplored messengers from the cosmos More than 20 years of difficult and pioneering efforts to open a window on the neutrino Universe: Biakal, ANTARES, Amanda/IceCube IceCube have observed a diffuse signal of cosmic neutrinos, at a level at the top end of theoretical expectations Much speculation on the origin of these neutrinos Galactic vs extragalactic? Flavour ratios? Spectral breaks? Diffuse vs point source? Tau neutrinos? Dark matter Planned upgrades of the Northern hemipshere teescopes (GVD, KM3NeT) will be online early 2020s Optimal view of the Galaxy Water medium provides improved angular resolution for muons and cascades Complementary energy ranges Towards end of 2020s, GEN2 completed with *10 volume optimised for PeV neutrinos Low energy extensions (ORCA/PINGU) provide fast and (relatively) cheap determination of the neutrino mass hierarchy and other neutrino properties Exciting times ahead! 34

35 KM3NeT Technical Design Report KM3NeT Timeline Figure 10-1: Overall time schedule of the KM3NeT project. Deliverable of EU-funded Design Study. 35

36 Water vs Ice: OM-hit probability 36 Probability to have at least one detected photon (KM3NeT OM) 10m 20m 10m 20m 30m 40m 30m 40m 50m 70m 50m 70m 36

37

38 Dq [deg] ARCA: Cascade Resolutions Energy e E R /E T Dq Direction KM3NeT/ARCA Preliminary KM3NeT/ARCA Preliminary E R /E T 1 sigma 90% E [GeV] E [GeV] 5% <2 38

39 Results (cut-and-count) 1 year Cascade analysis Muon analysis KM3NeT STAC, : ARCA LoI (U. Katz) 39

40 Neutrinos from CR interaction in the Galactic Ridge? Neronov et al. arxiv: , 4 Dec 2014 Gaggero et al. arxiv: ANTARES 90% CL (1500 days) KM3NeT ARCA sensitivity (1500 days) The KRAγ model adopts a radial dependent diffusion coefficient which turns into a spectral hardening toward the GC region.

41 KM3NeT Collaboration 12 Countries 42 Institutes 225 Scientists High-Energy (ARCA)

42 Cost of ORCA (115 Strings) Factor 4 cost reduction cf ANTARES item quantity unit cost (k ) total cost (k ) MEOC nodes +deployment string+il+deployment readout but with phase 1 we have 1 MEOC, 1 node, 6 strings MEOC reuse ANTARES MEOC cable (400k to relocate) ant meoc node strings Based on actual Phase-1 costs Anticipate 20% reduction in PMT costs and benefit from economy of scale Many ideas for further cost reduction: PowerSea connectors, 20 DOMs in string, 5 nodes,.

43 Point-source search with cascades Results are rather preliminary Important: Provides cascade event sample for source candidates Closes visibility gap KM3NeT STAC, : ARCA LoI (U. Katz) 43

44 ORCA Measurement of neutrino mass hierarchy 1 building block 200 m 44

45 DOM Prototype on ANTARES April 2013: First DOM installed on ANTARES instrumented line (KM3NeT-Fr) 40 K decay provides: - intra-dom time calibration - absolute PMT efficiencies g g (coincidence rate ~5 Hz on neighbouring PMTs) 40 K e - (β decay) Up to 150 Cherenkov photons per decay; stable 40 K concentration 40 Ca Eur. Phys. J. C (2014) 74:3056 (Δt=20 ns) 45

46 KM3NeT Capo Passero Smooth operation and data taking since May 2014 DOM3 DOM2 DOM1

47 Mainly p=2.5% in gal plane scan within ± 7.5 gal latitude > 100 TeV

48 > 100 TeV

49 Earth and Sea Sciences Deep Ocean Cabled Observatories Workshophttps://indico.cern.ch/conferenceDisplay.py?ovw=True&confId= Connected 30 Oct 2010 Secondary Junction Box O2, CTD, P WALLY crawler Seismograph Turbidity BioCam Currentmeter Instrumentation module 49

50 AC power transmission Daisy chain of 4 strings 50