Outline UHE Neutrino Astronomy

Transcription

1 Outline UHE Neutrino Astronomy Shigeru Yoshida Chiba University HE emission What it can tell Theoretical Bound of fluxes Extremely High-Energy generation Cosmic detection the current status IceCube : reachable to EHE universe Charged particle astronomy? Physics motivation TeV sources! cosmic rays origin and acceleration of cosmic rays understand cosmic cataclysms find new kind of objects? neutrino properties (τ, cross sections..) dark matter (neutralino annihilation) tests of relativitiy... search for big bang relics... effects of extra dimension etc.... Active Galaxies: Jets 20 TeV gamma rays Higher energies obscured by IR light black hole radiation enveloping black hole VLA image of Cygnus A 1

2 You cannot expect too many! p γ (p,n) π 2γ µ TeVEGRET observations!! e Cosmic Ray observations! Synchrotron cooling You cannot expect too high energies Theoretical bounds atmospheric µ DUMAND test string FREJUS MACRO NT-200 opaque for neutrons MPR neutrons can escape Suppressed by Synchrotron Cooling W&B EHE(Extremely HE) Synchrotron cooling of µ Production sites with low B Intergalactic space!! GZK Production Z-burst Topological DefectsSuper heavy Massive particles Mannheim, Protheroe and Rachen (2000) Waxman, Bahcall (1999) derived from known limits on extragalactic protons + γ-ray flux GZK Neutrino Production p E = ev γ π + μ+ e + n γ p E ~ 0.8 x ev GZK fluxes (EeV~ZeV!) K 411 photons cm Gamma Beam Energy (GeV) Cross Section (mb) x cm 2 γ+ p Δ(1232) π o p or π + n Conventional Mechanism of EHE neutrinos!! Yoshida and Teshima 1993 Yoshida, Dai, Jui, Sommers

3 Parameters involved in calculation. Predicted fluxes. (Diego González-Díaz, Ricardo Vázquez, Enrique Zas 2003) Parameters Orientative order of magnitude CR and fluxes for different models γ spectral injection index m activity evolution index z max Ω M H o B z of formation of sources density of matter Hubble constant intergalactic magnetic field η L ρ L η o ρ o local enhancement E max maximum acceleration energy in source [1-3] [3-5] [1-4] [0.2-1] [50-80 KmsMpc] [B 1nG] [?] [E max > ev] (Diego González-Díaz, Ricardo Vázquez, Enrique Zas 2003) Z-bursts Concept It is the standard particle physics p, π+,π-.π 0.. CRs extending to superehes! Z-burst constraints (Yoshida, Sigl, Lee 1998) (Yoshida, Sigl, Lee 1998) 3

4 EHE Neutrino Fluxes Where the source of (Extremely)-high energy? Present bound My $100 goes to GZK My $1 goes to GRB (E)HE generation needs target photons! resonance in the photopion production E p E γ ~ 0.25 Γ2 [GeV 2 ] Cross Section (mb) γ+ p Δ(1232) π o p or π + n Gamma Beam Energy (GeV) Γ ~ 300, E γ ~ MeV Γ ~ 300, E γ ~ ev E p ~ ev ~ 10 PeV E p > ev ~ 1 ZeV E γ ~ ev?? Proton-synchrotron model (Totani 1998) Energy limit! 4

5 Kyoto 2003 (Highly biased) conclusion Cosmic neutrinos come from. GRBs Cosmic detection E ~ PeV + GZK + GRBs(p-synch) E > EeV Neutrino Telescopes ANTARES, IceCube etc. All diffusivebackground fluxes How to build a detector Infrequently, a cosmic neutrino is captured in the ice, i.e. the neutrino interacts with an ice nucleus cosmic ray In the crash a muon (or electron, or tau) is produced Earth Cherenkov muon light cone µ interaction Detector Detector The muon radiates blue light in its wake Optical sensors capture (and map) the light Optical Cherenkov Neutrino Telescope Projects ANTARES La-Seyne-sur-Mer, France neutrino ANTARES Deployment Sites BAIKAL Russia Thetys Marseille La Seyne sur Mer Toulon Existing Cable Marseille-Corsica NEMO Catania, Italy DUMAND Hawaii (cancelled 1995) NESTOR Pylos, Greece Demonstrator Line Nov Jun N, 5 17 E Depth 1200 m New Cable (2001) La Seyne-ANTARES ANTARES 0.1km2 Site N, 6 10 E Depth 2400 m IceCube, South Pole, Antarctica ~ 40 deployments and recoveries of test lines for site exploration 0.1 km2 Detector with 900 Optical Modules, deployment

6 ANTARES Layout Laser calibration at the CPPM dark room 12 lines 25 storeys line 3 PMT storey 14.5 m Optical beacon 350 m t2 t1 t3 Cylinder Junction box Optical fibres 100 m 40 km to shore ~60-75 m Laser Readout cables Optical Splitter IceTop AMANDA II Detector AMANDA IceCube South Pole Amundsen-Scott Station South Pole Skiway 80 Strings 4800 PMT Instrumented volume: 1 km3 (1 Gt) IceCube is designed 1400 m to detect neutrinos of all flavors at energies from 107 ev (SN) to 1020 ev Optical module 2400 m m IceTop IceTop 160 tanks frozen-water tanks 2 OMs tank First year deployment (Jan 2005) 4 IceCube strings (240 OMs) 8 IceTop Tanks (16 OMs) Who are we? Bartol BartolResearch ResearchInst, Inst,Univ UnivofofDelaware, Delaware, Univ. Univ.ofofAlabama, Alabama, Pennsylvania State University, Clark-Atlanta University, Pennsylvania State University, Clark-Atlanta University, University Univ. UniversityofofWisconsin-Madison, Wisconsin-Madison, Univ.ofofMaryland, Maryland, University IAS, UniversityofofWisconsin-River Wisconsin-RiverFalls, Falls, IAS,Princeton, Princeton, LBNL, Berkeley, University of Kansas, LBNL, Berkeley, University of Kansas, UC Southern UCBerkeley, Berkeley, SouthernUniv. Univ.and anda&m A&MCollege, College,Baton BatonRouge Rouge UC UCIrvine, Irvine, IceCube Chiba ChibaUniversity, University,Japan Japan AMANDA University of Canterbury, University of Canterbury, Christchurch, Christchurch,New NewZealand Zealand IceCube 80 strings 60 OMsstring 17 m vertical spacing 125 m between strings IceTop Tank deployed in Hamamatsu R-7081 Université Libre de Bruxelles, Belgium Université Libre de Bruxelles, Belgium Vrije VrijeUniversiteit UniversiteitBrussel, Brussel,Belgium Belgium Université de Mons-Hainaut, Belgium Université de Mons-Hainaut, Belgium Universität Mainz, Germany Universität Mainz, Germany DESY-Zeuthen, Germany DESY-Zeuthen, Germany Universität Wuppertal, Germany Universität Wuppertal, Germany Uppsala Universitet, Sweden Uppsala Universitet, Sweden Stockholm Stockholmuniversitet, universitet,sweden Sweden Kalmar Universitet, Sweden Kalmar Universitet, Sweden Imperial College, London, UK Imperial College, London, UK University of Oxford, UK University of Oxford, UK Utrecht University, Utrecht, NL Utrecht University, Utrecht, NL 6

7 Color displays: LE Primary Channels Size displays: ADC Size scaling: Lin <4 <9 <13 <17 <22 <26 <31 <35 <40 <44 <49 <53 <58 <62 <67 <71 No external geometry file is opened. Detector: amanda-b-10, 19 strings, 680 modules Data file: he_deff.f2k Displaying data event from run 336 Recorded yrdy: seconds past midnight. Before cuts: 264 hits, 264 OMs After cuts : 264 hits, 264 OMs The highest energy event (~200 TeV) TeV) Detection of e,µ, τ O(km) long muon tracks Electromagnetic and hadronic cascades Color displays: LE 15 m Size displays: ADC ~5m Size scaling: Lin <4 <9 <13 <17 <22 <26 <31 <35 <40 <44 <49 <53 <58 <62 <67 <71 No external geometry file is opened. Detector: amanda-b-10, 19 strings, 680 modules Data file: he_deff.f2k Displaying data event from run 336 Recorded yrdy: seconds past midnight. Before cuts: 264 hits, 264 OMs After cuts : 264 hits, 264 OMs direction determination by cherenkov light timing Excess of cosmic neutrinos? Not yet... talk HE for now use number of hit channels as energy variable... preliminary (2000 data) 10 2 experiment background MC -2 E signal MC (e) 10 talk HE Point source search in AMANDA II Search for excess events in sky bins for up-going tracks cascades (2000 data) events 197 d 0.2 muon neutrinos (1997 B10-data) accepted by PRL Primary Channels m events observed above horizon 3% non-neutrino background for θ > 5 cuts optimized in each declination band PRE LI MI N ARY above horizon: mostly atmospheric s AGN with 10-5 E-2 GeV-1 cm-2 s-1 sr-1 1 below horizon:mostly fake events sky subdivided into 300 bins (~7 x7 ) log10(erecogev) cuts determined by MC blind analyses! no clustering observed - no evidence for extraterrestrial neutrinos... Grid Search Results Low state: Mrk 421 sensitivity (AMANDA) can be compared to our best upper limit (sensitivity shown here) about factor 2 Fit of the measured spectrum from HEGRA (Low) Allowed range for the emitted flux AMANDA sensitivity 2002 IceCube sensitivity Correction for extragalactic γ absorption : TeV γ-ray spectra are modified by red-shift dependent absorption by intergalactic IR-UV background O.C.De Jager & F.W.Stecker, Astrophy.J. 566 (2002),

8 Theoretical bounds and future DUMAND test string GIGA-ton detector!! atmospheric µ FREJUS MACRO NT-200 AMANDA-97 AMANDA-00 AMANDA-II opaque for neutrons MPR neutrons can escape NT-200+ W&B IceCube Mannheim, Protheroe and Rachen (2000) Waxman, Bahcall (1999) derived from known limits on extragalactic protons + γ-ray flux ev ev ev How (E)HE events look like EHE MC Event examples 300 PeV taus ev ev ev EHE (EeV or even higher) Neutrino Events Arriving Extremely Horizontally Needs Detailed Estimation Limited Solid Angle Window (σρna) -1 ~ 600 (σ10-32 cm 2 ) -1 (ρ2.6g cm -3 ) -1 [km] Involving the interactions generating electromagnetichadron cascades Energy loss profile in UHEEHE By JULIeT Stochastic Loss Initiating high energy Cascades! µn µx e + e - 8

9 MC Truth Incoming e µ τ eγ µ τ π e Products µ τ µ τ π eγ Cascades Pairdecay Bremss Pair Bremss Pair Pair PhotoNucl. Pair Pair PhotoNucl. Cascades Muon(Neutrinos) from µ τ Nadir Angle Tau(Neutrinos) from µ τ Suppression By τ decay GZK IceCube depth Upward-going Downward going!! Down-going events dominate Atmospheric µ is attenuated faster Up 11000m Down 2800 m 1400 m Atmospheric muon! a major backgrond But so steep spectrum EHE events! Downward Signal(GZK) Vs Atm µ 1.4km e+ e - lepton γ Very Preliminary noise Ice 1km γ γ π ± signal Rock 1km e+ e - lepton Upward MC Truth 9

10 First Guess Signal(GZK) Vs Atm µ We MEASURE energy deposit in km 3 Very Preliminary dedx~βe E~ XbE # of Hit We MEASURE energy deposit in km 3 Flux as a function of energy deposit in km 3 dedx~βe E~ XbE dedx~βe E~ XβE R<300m 300m <R<500m 500m <R<600m 600m <R<700m 700m <R Energy Reco algorithm under development Intensity of EHE µ and τ GZK m=4 Zmax=4 Down Up Down m=7 Zmax=5Down Atm µ [cm -2 sec -1 ] Iµ(E>10PeV) Iµ(E>10PeV) Energy Deposit Iτ(E>10PeV) Iτ(E>10PeV) Energy Deposit RATE [yrkm 2 ] IceCube EHE Sensitivity 90% C.L. for 10 year observation S.Yoshida, R.Ishibashi, H.Miyamoto, PRD (2004) RESCEU

11 IceCube : The Present status detection by EAS HiResAuger etc Yoshida et al ApJ (1997) ~10 strings will be being deployed now! ~ IceCube Charged Particle Astronomy? E>>10 EeV θ ~ a few deg Event cluster > 40 EeV 29 th ICRC Pune No significant excess: AGASA s triplet Pch ~0.28 (Westerhoff, this conference) AGASA triplet story 29 th ICRC Pune 29 th ICRC Pune BL Lac Correlation: New Claim Most recent claim by Gorbunov is based on published HiRes data. It uses a 10 EeV threshold, so it is a new claim. Magnitude Redshift 6cm Radio Flux # Obj. CR Sample # CRs Bin Size # Pairs Prob HiRes stereo event Catalog: Veron (9 th Ed.) BL Lacs z > 0.1 or m < 18 S6cm > 0.17 Jy unknown Catalog: Veron (10 th Ed.) BL Lacs correlated with EGRET sources no cut no cut no cut AGASA >48 EeV < 10-4 Yakutsk >24 EeV HiRes > 24 EeV AGASA >48 EeV Yakutsk >24 EeV HiRes > 24 EeV Catalog: Veron (10 th Ed.) BL Lacs m < 18 no cut no cut 156 AGASA > 40 EeV HiRes > 40 EeV One event added BUT below 40 EeV!! (Westerhoff, this conference) Catalog: Veron (10 th HiRes > 10 EeV Ed.) BL Lacs m < 18 no cut no cut Gorbunov et al., JETP Lett. 80 (2004) 145. (Finley, this conference) 11

12 Future Outlook (of UHECR) Auger: 7 x AGASA by 30 th ICRC HiRes: <2 years STEREO data to be analyzed. ~70% more statistics independent dataset for testing the BL Lac New observatory in the Northern sky Telescope Array EHE gamma rayneutrino search EAS detector, IceCube, Rice, ANITA etc. 29 th ICRC Pune Summary and outlook HE cosmic neutrinos come from GZK (100PeV 100 EeV) $100 GRB (PeV) GRB-P-synch $10 Neutrino observatory IceCube provides DATA 0.1 x IceCube ~2006! Strong capability of EHE search Charged Particle Astronomy (Cluster, BLLac E>10 EeV) wait for HiRes data for real test 本講演の収録原稿は来年 1 月まで待ってください 12