S. E. Tzamarias. Neutrino Telescopy and Extensive Air Showers

Transcription

1 S. E. Tzamarias Neutrino Telescopy and Extensive Air Showers

2 Observation Techniques γ ray bursts nebula Cosmic Ray Showers

3 The Origin of Cosmic Rays Cosmic Accelerators

4 KANGAROO multi-wavelength spectrum TeV γ-rays of hadronic origin?

5 H.E.S.S. RXJ1713 Index 2.84±0.15±0.20 preliminary H.E.S.S.: full remnant CANGAROO: hotspot Index 2.2±0.07±0.1 Spectrum Hadronic Mechanism 1.no cut-off in the HE tail of HESS Spectrum 2. signal from the direction of molecular clouds

6 Chandra observed Sgr A* and Sgr A East on September 21, 1999, with the Advanced CCD Imaging Spectrometer (ACIS).

7 by the Adaptive Optics (AO) NAOS-CONICA (NACO) instrument on the 8.2-m VLT YEPUN telescope at the ESO Paranal Observatory 50mas 2 light days

8 Neutrinos would verify the hadronic acceleration scenario

9 Neutrino Sources Active Galactic Nuclei Cataclysmic Phenomena Diffused fluxes Dark Matter of the Universe p + γ CMB π +. Ε > ev flux*e 2 < 10-7 GeVcm -2 s -1 sr -1 Relics of the Grand Unification Era THE UNEXPECTED Point sources Background Environmental noise atmospheric muons atmospheric neutrinos

10 The Neutrino Telescope world map First Generation: E μ >1Gev A eff. ~ m 2 Second Generation: E μ > 5-100Gev A eff. ~0.1-1km 2

11 First Generation Neutrino Telescopes Skyplot of Reconstructed Neutrino Induced Events cosθ>0 SuperKamiokande (A. L. Stachyra, 2002) cosθ<0 MACRO (M. Ambrosio et al, 2001)

12 Second Generation Neutrino Telescopes Steffen-ICRC2003 Baical Neutrino Telescope Neutrino Induced Cascades B. Lubsandorzhier- RICH2002 V. Balkanov et al

13 Second Generation Neutrino Telescopes AMANDA

14 spase-amanda SPASE air shower arrays 1 km calibration of AMANDA angular resolution and pointing! resolution Amanda-B10 ~ km results in ~ 3 for upward moving muons (Amanda-II: ~ 2 ) C. Spiering- VLVNT Workshop

15 NESTOR Second Generation Neutrino Telescopes reweighting Blind fit Okada model I o dn α = 4.7 ± I = (9.0 ± 0.7) 10 cm s sr α o dω dt ds = Icosθ o α

16 Edgar V. Bugaev, et al, Physics Review D58, (1998). α = 4.7 ± 0.5( stat) ± 0.2( syst) I = ± ( stat) ± ( syst)cm s sr o

17 ANTARES Operation and Results..

18 NEMO - Towards the km3 neutrino telescope R&D phase ( ) Site selection and characterization Several sites close to the italian coasts have been studied. A site close to Capo Passero (Sicily) at 3500 m with optimal characteristics has been identified for the installation R&D activities Development of specific ASICS for the underwater front end electronics Large area hybrid photomultipliers Development of deep sea instrumentation Feasibility study for the km3 detector All the critical components and the deployment procedures have been examined A preliminary project for a km3 detector has been developed Phase 1: Advanced R&D and prototyping ( ) Realization of a detector subsystem including all critical components The system will be installed off Catania at the Underwater Test Site of the LNS

19 Summary of KM3NeT physics goals Search for astrophysical point sources Smoking gun for identification of hadronic accelerators and investigation of acceleration mechanisms; Neutrino part of multi-messenger observations to correlate radiative and hadronic processes; Study of transient sources (e.g. Gamma Ray Bursts); Unique chance to study neutrinos from galactic disk. Measurement of the diffuse neutrino flux Information on cosmological source densities/distributions; Search for Big Bang relics. Dark Matter Search for neutrinos from WIMP annihilations. Particle physics & cosmology Magnetic monopoles, topological defects, Z bursts, nuclearites,

20 Design Study Target Values Detection principle: water Cherenkov Location in Europe: in the Mediterranean Sea Detection view: maximal angular acceptance for all possible detectable neutrino signals including down-going neutrinos at VHE Angular resolution: close to the intrinsic resolution (<~0.1 degrees for muons with E ν >~ 10 TeV) Detection volume: 1 km 3, expandable Lower energy threshold: a few 100 GeV for upward going neutrinos with possibility to go lower for ν from known point sources Energy reconstruction: within factor of 2 for muon events Reaction types: all neutrino flavours Duty cycle: close to 100% Operational lifetime: >= 10 years But these parameters need optimisation!

21 Technical Design of the ν Telescope Cost-effectiveness: <~ 200 MEuro per km 3 Architecture: strings vs. rigid towers vs. flexible towers vs. new solutions Photo detectors Mechanical solutions Readout: electronics, data acquisition, data transport Calibration and slow control Cables and connectors: dry vs. wet Simulations: design optimisation and assessment; impact of environmental conditions Construction of the telescope within 5 years after end of the Design Study Detailed assembly procedures Distributed production lines Evaluation of logistics needs Quality control and assurance model

22 Installation and Maintenance Deployment: fast procedures; parallelisation of operations Shore infrastructure: supply units; on-shore computing; internet connection Maintenance: flexible, low-cost access to sea-operation equipment; rapid recovery procedures; cost-effective repair options Exploitation Model facility exploited in multi-user and interdisciplinary environment Reconstructed data will be made available to the whole community Observation of specific objects with increased sensitivity will be offered (dedicated adjustment of filter algorithms) Close relation to space-based observatories will be established (alerts for GRBs, Supernovae etc.) Plug-and-play solutions for detectors of associated sciences

23 Operation Model Maintenance centre for detector components (closely related to seaoperation base) Computer facilities allowing for external operation and control Data storage and distribution (relation to GRID?) Software development and maintenance,in particular for on-line filter Funding and Governance Invite and coordinate world-wide participation Explore national, European and regional funding sources Assess and study models for contractual structures Address legal questions related to the international structure and in particular to a possible detector deployment in international waters

24 a parenthesis

25 Events Generator Atmospheric Muon Generation Extensive Air Showers Neutrino Interactions (use of Pythia) Neutrino (all flavors) Induced Events Atmospheric Neutrinos Cosmic Neutrinos (Several Models) Production of Secondaries, transportation, energy loss Probability of a ν μ to cross Earth Example: Earth Absorption Nadir Angle Example: ν e interacting inside a grid-like detector A. Tsirigotis

26 Monte Carlo Development : Simulation Technique Cherenkov photon emission A new, very efficient, general purpose, Cherenkov simulation algorithm Stage 1:Define PMT clusters according to the detector geometry Stage 2: Use the Clusters for the Cherenkov photon production Define 2 points inside the detector, p1 & p2 For all PMTs Which point is closer? p1 p2 Add PMT to group1 find the center f mass m1 of group1 Add PMT to group2 find the center of mass m2 of group2 is m1=p1 and m2=p2 yes converge no The simulation strategy is applicable and efficient for any detector architecture without any extra optimization A. Tsirigotis

27 Monte Carlo Development : Simulation of the Detector Response (GEANT4) EM Shower Parameterization Parameterization of EM Shower Number of Cherenkov Photons Emitted (~shower energy) Angular profile of emitted photons Longitudal profile of shower Angular Distribution of Cherenkov Photons General purpose: Simulation of (any) PMT Response Simulation of electronic functions A. Tsirigotis

28 Simulation Example 1 TeV Vertically incident muon K 40 Noise Hits Signal Hits (Hit amplitudes > 2p.e.s) A. Tsirigotis

29 Event Rate (khz) Track Reconstruction Algorithms 180 kbyte/event Efficiency Direct Walk Filter Χ 2 time fit deposited charge based likelihood ratio criteria Kalman Filter (novel application in this area) Cut to the number of active triplets Clustering of candidate tracks Current Studies PMT orientation and photon directionality nested vs uniform architecture for ~1TeV muons fast triggers and filtering algorithms detector calibration using EAS Computer Kalman Power Filter (novel application in this area) Computer Farm with 15 computers (15 double xeons ) Cut to the number of active triplets 1TeV muons Angular deviation (degrees) 1TeV muons We are currently installing 64 more computers (64 double opterons) 350 Gflops Angular deviation (degrees)

30 H.O.U., Univ. Athens, Univ. Patras, INP DEMOKRITOS, NTUA t 1 t 2 Ethernet t 3 A. Leisos

31 ALTA --A Collaboration between local area highschools and the University of Alberta in the area of cosmic ray research U. of Alberta, Athabasca U., UBC, (Northeastern U, Boston). ~30 Schools Involved 7(9) FULL Detector systems operating with data being recorded.

32 Eurocosmics

33 A Station Scintillator GPS ~20 m Scintillator Scintillator Scintillator TCP/IP PC A. Leisos

34 Prototype Construction 10 x 12 cm tiles 80 tiles ~ 0.96 m 2 12 WLS fibers per row Single PMT read out A. Leisos

35 DAQ 4 PMT Signal Inputs Trigger Ouput USB Port HPTDC 32 channels (LR) 8 Channels (HR) 25ps (HR) to 800 ps (LR) accuracy Self Calibrating 25ps accuracy TDC GPS Input A. Leisos

36 Monte Carlo Studies Time Delay (ns) curvature Distance from core (mm) Vertical Proton Showers ( GeV) Single Station Performance Θ rec -Θ true thickness A. Leisos

37 The General Idea Resolution in determining a possible Angular Offset (degrees)-10 day operation Examples of a 3-Station Performance Crude (plane approximation) Analysis Resolution per reconstructed track (degrees) Threshold Charge (pes) Angular offset Efficiency Resolution Position Vertical Proton Showers ( GeV)

38 HELYCON HELLENIC LYCEUM COSMIC OBSERVATORIES NETWORK ev ev ev 2km A. Leisos

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40 Diffuse ν Flux: Models, Limits and Sensitivities Amanda, Baikal Amanda,Antares, Baikal, Nestor RICE AUGER ν τ AGASA RICE GLUE Anita km 3 Auger + new technologies C. Spiering, J. Phys. G 29 (2003) 843

41 Possible Origin of the Extremely Energetic Cosmic Rays Decays of particles produced by topological defects or relic particles Z decays due to UHE neutrino interactions on relic ν s UHECR photopion production on CMB Or Experimental Systematic Error

42 EHECR-Puzzle: Better understanding of experimental errors (better energy and directional Resolution) Hybrid Approach: Independent EAS-observation techniques Shower-by by-shower in one Experiment More events Much larger Experiment

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45 KASCADE-Grande / LOPEZ

46 O N S E NW SW DAM NE SE scintillator antenna CODALEMA Observatoire de Paris-Meudon Meudon,, Station de Nançay ay - INSU L1 L0 L2 130 m 130 m A. Bellétoile toile, Rencontres de Moriond 2005

47 AUGER + Radio 4 km 1EeV air shower If LOPES R&D successful add radio detectors to AUGER radio beam vertical ev air shower center +100m +250m data:allan and Prah 1mV/m/Mhz A. Horneffer et al., SPIE

48 Radio Detection in Media G.A. Askaryan JETP 14 (1962) 441 Excess negative charge of an electron-photon shower and its coherent radio emission Saltzberg et al., PRL 86 (2001) 2802 d c L c Confirme effect by accelerator measurements in silica sand Coherence condition: d c 10cm < λ radio 300 MHz λ= 100 cm Signal power ~ E 2 ~ N p 2

49 Radio Cherenkov Detectors astro-ph/ , 3500 hours livetime ν Rice Anita ANITA-LIGHT: 18 days at float altitude, 1.25 revolutions. Data recovered in Feb 04 Initial scan of data reveals no obvious ν signal

50 Radio Cherenkov Detectors GLUE

51 Radio Cherenkov Detectors FORTE: Scientific program in lightning & related atmospheric discharges MHz range ~4 M triggers recorded 9/97-12/99 P. Gorham et al., astro-ph/ v3 05/2004

52 Salt dome: RF loss similar to ice at -40 C but 2.5 times more dense build radio detector array Meeting at SLAC Feb/05 : SalSA Collaboration born U-Hawaii,UCLA, SLAC, Phase 1: look for right location deploy test strings in a few holes study attenuation, noise etc in-situ 1 Depth (km) Rolf Nahnhauer Moriond 2005 Halite (rock salt) L a (<1GHz) > 500 m w.e. Depth to >10km Diameter: 3-8 km V eff ~ km 3 w.e. No known background >2p steradians possible 2.5 km 3 array with 225 m spacing 12 2 =144 strings, 12 3 =1728 antenna nodes 12 antennas per node, dual polarization ~300 km 3 sr at 1 EeV threshold ev, few 100s antennas hit at 1 EeV, >1000 hits at 10 EeV Rate: claim at least 10 events per year from rock-bottom minimal GZK predictions

53 Acoustic Detection λ abs (sound) λ abs (radio) (1000m) G.A. Askaryan, At. Energ., vol.3, no.8, (1957) p.152 Askar yan, Dolgoshein, Kalinovsky, NIM 164(1979) 267 Learned, Phys.Rew. D 19(1979) 3293 Beam test with 200 MeV protons Sulak et al. NIM 161(1979) 203 SAUND (7km 2 ) Frequency khz Signal power ~ E 2 J. Vandenbroucke et al.,astro-ph/

54 + Acoustic 1000 hydrophone array for Mediterranean 3 hydrophones per cluster ( sensor distance : 50 m ) 300 m grid spacing red line red cube : incident neutrino (7.2*10 19 ev) : deposited energy of ν - interaction yellow points : hydrophones L. Thompson U. Katz, ApPEC Workshop 2003 green cubes : signal hits

55 Monte Carlo Studies Examples of a Multi-Station Performance (Crude Analysis) Station Configuration Not need for position holding Resolution in determining a possible Angular Offset (degrees)-10 day operation Vertical Proton Showers ( GeV) Number of stations

56 Water Tank in the Pampa Communication antenna GPS antenna Electronics enclosure 40 MHz FADC, local triggers, 10 Watts Solar Panel Battery box three 9 PMTs Plastic tank with 12 tons of water