Latest Results from the ANTARES and KM3NeT Neutrino Telescopes

Transcription

1 Latest Results from the ANTARES and KM3NeT Neutrino Telescopes Lake Louise Winter Institute 2014 Tino Michael on behalf of the ANTARES and KM3NeT Collaborations National Institute for Subatomic Physics, Amsterdam Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

2 The ANTARES Collaboration 8 countries 31 institutes 150 Collaborators Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

3 The ANTARES Collaboration 8 countries 31 institutes 150 Collaborators Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

4 The Detector Location off the coast of Toulon, France connected via 40 km electro-optical cable Ù Astropart. Phys. 13 (2000) (Background light) Ù Astropart. Phys. 19 (2003) (Bio-fouling) Ù Astropart. Phys. 23 (2005) (Light transmission) Ù Astropart. Phys. 35 (2012) (Group velocity of light) Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

5 ANTARES on-site Shifting Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

6 ANTARES on-site Shifting

7 ANTARES on-site Shifting

8 ANTARES on-site Shifting

9 ANTARES on-site Shifting Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

10 The ANTARES Detector complete since Lines, 885 PMTs + IL 2500 m below sea surface 0.01 km 3 instrumented volume 0.5 ns time resolution < cm acoustic positioning NIM A 656 (2011) AMADEUS hosted on L12 and IL Acoustic neutrino detection NIM A (2011) KM3NeT prototype DOM hosted on IL Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

11 Muon Track Reconstruction 3 atmospheric muons per second maximum likelihood fit based on hit time residual PDFs cut on direction and fit quality parameter Λ 4 atmospheric neutrinos per day 1 m 2 effective area at E νµ = 30 TeV median angular resolution visibility: 3/4 of the sky, most of galactic plane including galactic centre ApJ. 760:53 (2012) Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

12 Neutrino Point Source Search data (1340 days) 5516 neutrino candidates (angular error estimate < 1 for 90 %) no significant excess same most significant cluster from last analysis ( data) with 6 additional events: p-value: 2.1 % (2.3σ) compatible with background hypothesis Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

13 Neutrino Point Source Search: Limits s -1 ] -2 [GeV cm 90%CL ν φ 2 E -4 ANTARES sensitivity (1339 days) ANTARES (1339 days) MACRO (2300 days) Super-K (2623 days) AMANDA-II (1387 days) -5 IceCube ( days) IceCube sensitivity ( days) δ [ ] dedicated studies for extended sources (RXJ1713, Vela X) limits most stringent limits for a large part of the southern sky in TeV region expect further improvement including showers (work in progress) arxiv: Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

14 GRB searches Search for neutrino events in coincidence with observed GRB analysis of 296 long GRBs from information from FERMI/SWIFT/GCN GRB simulations of expected neutrino fluence: Astrop.Phys. 20 (2004) 429 (Guetta) ApJ 721 (20) 630 (NeuCosmA) grey: first ANTARES limit (40 GRBs) JCAP 03 (2013) 006 black: IceCube IC40+59 (215 GRBs) -2 [GeV cm F ν E 2 ] ANTARES 2007 ANTARES NeuCosmA ANTARES Guetta IC E [GeV] -13 s -1 sr -1 ] -2 [GeV cm Φ ν 2 E no event found within window from GRB A&A 559, A9 (2013) Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

15 Atmospheric Muon Spectrum data set two different energy estimators: de/dx as evaluated from total collected charge de/dx ρ = NHits Q i ε( x) 1 L µ( x) Combined likelihood for hit / no-hit for all OMs L (E µ) = 1 N OM Li (E µ) N OM s -1 sr -1 cm -2 ] 2.5 dn/de [GeV 3.5 E 1 ANTARES Unfolding AMANDA-II Unfolding IceCube40 Unfolding Bartol flux Bartol uncertainty atmospheric neutrino energy spectrum by unfolding measured spectrum; averaged in zenith band -1 Bartol + Martin flux Bartol + Enberg flux log (E /GeV) ν Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

16 Search for diffuse, cosmic ν µ Flux -1 ] -5 search with data (855 days): energy estimator based on de/dx negligible muon contamination: < 0.4 % sensitivity: E 2 Φ = GeVcm 2 s 1 sr 1 s -1 sr -2 Φ [GeV cm 2 E Amanda II ANTARES IceCube 59 IceCube 40 MACRO MPR/2 τ n γ < 1 Baikal NT-200 ν x/3 PRELIMINARY WB/2, evolution WB/2, no evolution -9 unblinded results: E 2 Φ 90% = GeVcm 2 s 1 sr for 45 TeV < E < PeV Energy [GeV] N obs = 8, N bkg = 8.4, N sig = 2.3 Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

17 Summary largest neutrino telescope in northern hemisphere competitive physics results extensive multi-messenger program Astropart. Phys. 35 (2012) 530 (TAToO) JCAP06(2013)008 (Gravitational Waves) proves the feasibility of a deep sea Cherenkov detector and paves the way for KM3NeT Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

18 The KM3NeT Detector 40 institutes 180 members large overlap with ANTARES Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

19 The KM3NeT Detector Location Located at 3 different sites in the deep Mediterranean Sea: KM3NeT-France (Toulon) KM3NeT-Italy (Capo Passero) KMNeT-Greece (Pylos) Tino Michael (Nikhef) 2500 m 3400 m 4500 m Ù TDR [ISBN ] (20) Results from ANTARES & KM3NeT / 24

20 The KM3NeT Detector Layout France inter-node link MEOC 1 node node MEOC 2 power via Main Electro-Optical Cable short distances - AC, long distances - DC 3 nodes per MEOC node node 20 strings per node 4 strings in series 120 strings in total node node inter-string spacing: 0 m Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

21 The KM3NeT Detection Unit 18 storeys (one OM each), 36 m distance, 0 m anchor first storey held by 2 pre-stretched Dyneema ropes DOMs connected via electro-optical cable 1 fibre + 2 copper wires breakout box with fuses at each storey DWDM with 80 wavelengths GB/s readout all data to shore policy Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

22 String Deployment Launcher of Optical Modules (LOM) string wound up for self-unfurling compact deploy multiple strings per cruise LOM recover- and reusable successful demonstration of deployment concept some issues with penetrators understood and fixed Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

23 String Deployment Launcher of Optical Modules (LOM) string wound up for self-unfurling compact deploy multiple strings per cruise LOM recover- and reusable successful demonstration of deployment concept some issues with penetrators understood and fixed Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

24 String Deployment Launcher of Optical Modules (LOM) string wound up for self-unfurling compact deploy multiple strings per cruise LOM recover- and reusable successful demonstration of deployment concept some issues with penetrators understood and fixed Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

25 String Deployment Launcher of Optical Modules (LOM) string wound up for self-unfurling compact deploy multiple strings per cruise LOM recover- and reusable successful demonstration of deployment concept some issues with penetrators understood and fixed Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

26 The KM3NeT multipmt DOM 17 glass sphere 31 3 PMTs, 5 rings á 6 PMTs DOM equivalent to 3 ANTARES OMs (cheaper) but only one penetrator per floor (less risky) low power consumption (< W per DOM) covers almost whole solid angle directional information background reduction from PC segmentation Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

27 The pre-production Optical Module PPM-DOM multipmt DOM deployed with ANTARES Instrumentation Line on 16. April 13 mounted on 1st floor of IL (0 m above seabed) regular data taking since then (about 50 h 3.4 TB) Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

28 The pre-production Optical Module PPM-DOM multipmt DOM deployed with ANTARES Instrumentation Line on 16. April 13 mounted on 1st floor of IL (0 m above seabed) regular data taking since then (about 50 h 3.4 TB) Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

29 inter-dom Time Calibration Hits / ns (T29 T30) / ns sea water contains radioactive 40 K decay with with emission of 1.33 MeV electron up to 150 Cherenkov photons per decay coincidences on neighbouring PMTs for time calibration Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

30 inter-dom Time Calibration PMTs / (0.5 ns) before Calibration after Calibration sea water contains radioactive 40 K decay with with emission of 1.33 MeV electron up to 150 Cherenkov photons per decay coincidences on neighbouring PMTs for time calibration T / ns Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

31 Rate of different Coincidence Levels Rate / Hz Data 41h 29min Simulation Muons Simulation 40 K Combinatorial Background Coincidence Level: # of Hits within 20 ns Combinatorial Background: estimate for coincidences caused by multiple single hits derived from average PMT rate in data publication in preparation Coincidence Level Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

32 Hit Count according to PMT Zenith Hits / PMT 5000 Data 41h 29min Simulation Muons Coincidence Level > 7 clear asymmetry towards upwards looking PMTs drops due to LCM shadowing we can see the LCM directional information from single storey ϑ PMT Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

33 Hit Count according to PMT Zenith Hits / PMT 5000 Data 41h 29min Simulation Muons Coincidence Level > 7 clear asymmetry towards upwards looking PMTs drops due to LCM shadowing we can see the LCM directional information from single storey ϑ PMT Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

34 Hit Count according to PMT Zenith Hits / PMT 5000 Data 41h 29min Simulation Muons Coincidence Level > 7 clear asymmetry towards upwards looking PMTs drops due to LCM shadowing we can see the LCM directional information from single storey ϑ PMT Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

35 160m 72m 36m 36m 15m Next Step: pre-production Detection Unit PPM-DU CONFIGURATION OF THE PPM DU Buoy: 4x syntactic foam modular buoy (+1300N) DOM 3 (ETEL PMTs) 40m branch VEOC DOM 2 (ETEL PMTs) 40m branch VEOC DOM 1 (Hamamatsu PMTs) 2x40m branch VEOC prototype string with 3 additional multipmt DOMs in assembly DOMs equipped with PMTs from different manufacturers to be deployed upcomming spring at Italian site Mechanical ropes Anchor including base container and 0m jumper Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

36 Summary when completed, KM3NeT largest neutrino detector on earth will be a distributed, networked research infrastructure all choises made: sites, multipmt DOMs, DWDM, strings PPM-DOM operating well and results are very encuraging PPM-DU in final assembly to be deployed soon 1st full sized string to be deployed end of 2014 phase 1 funding secured KM3NeT is going to happen 600 PMTs already arrived beeing tested at Nikhef, Amsterdam and ECAP, Erlangen additional PMTs have been ordered, cables and PMT bases are being produced Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

37 Backup Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

38 Detector Size Study Use estimated neutrino flux from HESS gamma measurement of SNR RXJ1713 spectrum with high energy cutoff horizontal spacing: 0 m vertical spacing: 36 m DOMs/string: 18 strings: 115 no efficiency loss in splitting up detector almost no overhead from different sites (several main cables have to be used anyway) profit from regional fundings associated sciences benefit Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

39 currents of up to 30 cm/s observed typically around 5 cm/s mostly homogeneous over detector volume deviation from vertical at top about 150 m at 30 cm/s critical current 45 cm/s (anchor starts to move) Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24

40 T between different PMT pairs 3 3 Hits / ns 70 Hits / ns (T15 T21) / ns (T6 T21) / ns Hits / ns Hits / ns (T17 T21) / ns (T1 T21) / ns Tino Michael (Nikhef) Results from ANTARES & KM3NeT / 24