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High Energy Neutrino Astronomy: 

High Energy Neutrino Astronomy Christian Spiering DESY Zeuthen TAUP 2001

Predictions and Bounds: 

Predictions and Bounds

Classes of Models: 

log(E2  Flux) log(E/GeV) TeV PeV EeV 3 6 9 pp core AGN p blazar jet Top-Bottom model GRB (W&B) Various recent models for transient sources Classes of Models

Bounds to diffuse fluxes: WB: 

Bounds to diffuse fluxes: WB Waxman & Bahcall, 1999  sources optically thin to primary cosmic rays  fix the spectral index to 2  normalize to cosmic rays at 1019 -1020 eV atmospheric flux bound without evolution bound with evolution * * moderately dependent on cosmology

Bounds to diffuse fluxes: MPR: 

Bounds to diffuse fluxes: MPR Mannheim, Protheroe, Rachen, 2000  do not assume a specific CR spectrum, use available upper limit on extragalactic proton contribution  allow also for optically thick sources (no neutrons escape)

MPR limit for optically thin sources : 

MPR limit for optically thin sources source spectra of neutrons Qn(En)  En-1 exp(-En / Emax) cosmic ray spectrum after propagation through Universe neutrino spectrum after propagation through Universe red: limit without GZK shift blue: renormaliztion after GZK shift

More bounds ....: 

More bounds .... E-2 , one source type E-1 exp (-E/Emax ) optically thick optically thin with evolution without evolution generic blazar EGRET blazar BL Lac Bound construction parallels that for optically thin sources. Energy dependent opacities. Averaging over luminosity functions and z-distributions of EGRET blazars and BL Lac objects.

Diffuse Fluxes: Predictions and Limits: 

Diffuse Fluxes: Predictions and Limits Mannheim & Learned, 2000 Macro Baikal IceCube Amanda

Hidden Sources: 

Hidden Sources Young SN shells, binary submerged in red giant, coooned MBH, ... Pre-AGN (prior to formation of massive black hole) Berezinsky & Dokuchaev, 2000 Collision & destruction o normal stars in a contracting central cluster Massive gas envelope NS & BH survive, further contraction and collisions Repeating fireballs, particle acceleration in rarified cavity

Hidden sources (2): 

Interactions in envelope HE neutrinos Muon events per source with E > 1 TeV, in 1 km2 detector: N ~ 70 (assuming Lp = 1048 erg s-1 and distance = 103 Mpc) Duration of pre-AGN hidden source phase ~ 10 years Average number of galaxies just in hidden source phase: ~ 10-100 Hidden sources (2)

GRB: 

Alvarez-Muniz, Halzen, Hooper, 2000 z = 1  z distribution expect up to  = 300  thousands of  events/yrkm2 Also multiple events from -faint-bursts ! GRB “Reference” model: Waxman & Bahcall, 1997   emission from protons accelerated at internal & external shocks in fireball,  ~ 300  normalization to CR  E2  dN/dE ~ 310-9 cm-2 s-1 sr-1 GeV between 100 TeV and 10 PeV

GRB: 

GRB Meszaros & Waxman, 2001 Core collapse of massive stars  relativistic fireball jet may either penetrate stellar envelope or may be choked N ~ 0.2 (E /1053 erg) km-2 for z =1 (E 5 TeV)  103 events correlated with -bursts + more from -dark bursts Paolis et al., 2001 Shock-accelerated protons from GRB interact with external protons in dense cloud  neutrinos with few GeV to ~ 1 PeV  single GRB at z=1 yields 0.1-1 event per km2 (E > 1 TeV)

Cannon Ball Model of GRB (Dar, De Rujula, Plaga): 

Cannon Ball Model of GRB (Dar, De Rujula, Plaga)

Neutrinos from Microquasars: 

Neutrinos from Microquasars Waxman, Loeb, 2001  Accreting stellar-mass BH or neutron star ejecting jets  Radio outbursts with L ~ 1043 erg   of order 1-10  Shock acceleration in electron proton plasma  Neutrino burst of several hours, preceding radio outburst 1-100 TeV neutrinos from proton–X-ray interactions N (1km2) ~ 10-2  -1 3 (for distance 10 kpc)  8 for source along line of sight  several neutrino events per outburst

Experiments under ground: 

Experiments under ground

Slide16: 

MACRO  Limit on flux from point sources  Limit on diffuse flux  Limit on neutrino emission from GRB Since 1989: 1356 upward going 

Slide17: 

MACRO point source search MACRO sky-map in equatorial coordinates 90% c.l. upper limits for 42 selected sources (red dots)

MACRO: limit on diffuse E-2 flux: 

Selection of HE neutrinos: timing cut (upward) energy deposition in scintillators E2  < 4.5 10-6 cm -2 s -1 sr –1 GeV MACRO: limit on diffuse E-2 flux

MACRO: Neutrinos from GRB: 

MACRO: Neutrinos from GRB Search for space-time correlation With 2527 BATSE GRB between 1991 and 1999 Flux < 0.8 x 10-9 cm-2 per average burst about 10 times above optimistic predictions (Paolis et al., Halzen & Hooper), about 100 times above Waxman & Bahcall)

Superkamiokande: 

1761 upward going muons (through-going and stopping) from 1264 live days (April 96-May 00) 1200 m2 acceptance area Superkamiokande

Super-K: point source search: 

Super-K: point source search

Upward muons underground: 

Upward muons underground Super-Kamiokande 2.0 k events MACRO 1.4 k events Baksan 1.0 k events IMB + K-II + KGF + Soudan + ... ~ 1.5 k events (?)  ~ 6000 events sets scale for underwater/ice experiments

Experiments under water: 

Experiments under water

Lake Baikal, NT-200: The Site: 

Lake Baikal, NT-200: The Site

NT-200: the detector: 

pair of 37 cm Quasar PMTs NT-200: the detector

Lake Baikal: atmospheric neutrinos: 

„Gold plated“ neutrino event, 4-string stage (1996) NT-200: zenith angle distribution 234 days in 1998/99 19 hits Lake Baikal: atmospheric neutrinos

Upper limit on diffuse flux of HE e: 

 Request upward moving light front (like from e.m. shower below detector)  Then cut on # hits Vertex distribution for E-2 e Blue dots: time cut Red squares: # hit > 45  E2 < 1.9 10-6 cm-2 s-1 sr-1 GeV Upper limit on diffuse flux of HE e

NT-214: 

Reach upper limit in   E2  3.5 10-7 cm-2 s-1 sr-1 GeV ! 0.1 1 10 100 1000 PeV NT-214

The Mediterranean Projects: 

The Mediterranean Projects

NESTOR: 

NESTOR First Mediterranean project (founded 1991) Site: Pylos (Greece), 3800m depth towers of 12 titanium floors each supporting 12 PMTs

Nestor Tower: 

Nestor Tower

Deployment plans: 

Deployment plans Schedule: 2001: re-lay cable to site and deploy 2 floors 2003: full tower

ANTARES: 

ANTARES

Site, History, Schedule: 

Demonstrator Site 42°59 N, 5°17 E Depth 1200 m ANTARES Site 42°50 N, 6°10 E Depth 2400 m Demonstrator Line: 8 OMs Nov 1999 - June 2000 Existing cable Marseille-Corsica New Cable (2001) La Seyne-ANTARES Marseille Toulon La Seyne sur Mer 0.05 km2 Detector: 900 OMs , Deploy 2002- 2004 Site, History, Schedule

The Detector: 

The Detector

ANTARES Performance: 

ANTARES Performance Very good angular accuracy below 3 TeV angular error is dominated by kinematics, above 3 TeV by recon- struction error (~ 0.4°) Effective area: ~ 10 000 m2 at 1 TeV ~ 50 000 m2 at 100 TeV E/E ~ 3 (1-10 TeV) 2 (> 10 TeV)

View of Sky: Complementary to AMANDA: 

Fraction of time sky visible View of Sky: Complementary to AMANDA

NEMO: 

NEMO

Nemo-2: 

Nemo-2

Nemo3: 

Nemo3

Experiments under ice: 

Experiments under ice

AMANDA: 

AMANDA Location: Geographic South Pole Amanda –II: 677 PMTs at 19 strings

AMANDA: Atmospheric neutrinos: 

AMANDA: Atmospheric neutrinos ~ 300 neutrinos from 130 days in 1997 (Amanda-B10) Systematic still error ~ 50% (prediction atm.  ~ 30%, experiment ~ 40% (ice properties, OM sensitivity)

AMANDA: limit on diffuse flux: 

AMANDA: limit on diffuse flux E2 F < 0.9 10-6 GeV-1 cm-2 s-1 sr-1 „AGN“ with 10-5 E-2 GeV-1 cm-2 s-1 sr-1 Full: Experiment Dots: Atmos. Search for excess of high energy neutrinos Optimize analysis for HE neutrinos Use number of hit PMT as energy estimator. Place cut according to Feldman- Cousins (using only MC)

Search for point sources: 

Search for point sources Optimize analysis on HE neutrinos and good angular resolution Accept large background contribution Systematic uncertainties

Other limits from AMANDA and BAIKAL: 

Other limits from AMANDA and BAIKAL AMANDA, 78 BATSE bursts in 1997 WIMPs from center of Earth Relativistic Magnetic Monopoles Baikal

AMANDA-II: 

AMANDA-II Trigger Level After BG rejection up horizon A-II B-10 dramatically increased acceptance towards horizon Nearly horizontal event (experiment)

Physics Reach of AMANDA-II: 

Physics Reach of AMANDA-II Mk-501 Search for  from TeV  sources Milagrito all-sky search sets limit at > 1 TeV: 7-30  10-7 m-2 s-1, ( E-2.5) Amanda probes similar flux if/ > 1 Sensitivity to diffuse flux E2 F ~ 5 10-8 GeV cm-2 s-1 sr-1

AMANDA-II and EeV search: 

AMANDA-II and EeV search Transmission of Earth for Neutrinos as a function of zenith angle and energy  Earth opaque above a few PeV PeV acceptance around horizon EeV acceptance above horizon Downward- background at high energies is small.

AMANDA-II and EeV search: 

AMANDA-II and EeV search Look for bright tracks passing inside and outside array Background rejection “straightforward” Total energy and “energy flow” variables SPASE vetoes large DW at relevant ECR Calibration possible using in-situ N2 laser Equivalent to 200 TeV cascade in energy Improve sensitivity above 10-100 PeV to E2 F ~ 2 10-8 GeV cm-2 s-1 sr-1 Sensitive to some trans-GZK models !

Slide51: 

80 strings, each with 60 PMTs AMANDA-II SPASE South Pole IceCube

Slide52: 

IceCube: Search for diffuse -fluxes “AGN” dN/dE = 10-7 ·E-2 cm-2 sec-1 GeV-1  2.300 events / year Atm. neutrinos (after quality cuts):  130.000 events / year Atmospheric AGN Sensitivity after 3 years: E2 dN/dE (in cm-2 sec-1 GeV) 2.7 · 10-9 (limit expectation) 8.0 · 10-9 (5 detectable flux) (assuming a model with low prompt neutrinop flux and galactic neutrinos as „signal“)

Slide53: 

IceCube: Point Source Search Angular resolution: Expect improvement at high energies from WLS & use of waveform information Sensitivity of IceCube after 3 years of operation (average for zenith angles > 90º): dN/dE ~ 3.5 · 10 -9 · E-2 cm-2 sec-1 GeV-1 Improve limit by a factor of 2 ? Within predictions of many recent models (1-100 TeV)

Energy spectra: 

Energy spectra Diffuse search Point source search Colored: standard reconstruction and cuts against fake events Black: ultimate Nhit cuts to get the lowest limit

Slide55: 

IceCube: Neutrinos from Gamma Ray Bursts Only 200 GRB needed to detect/rule out WB99 flux Test signal: 1000 GRB a la Waxman/Bahcall 1999 Expected no. of events: 11 upgoing muon events Expected background: 0.05 events Sensitivity (1000 bursts): 0.2  dN/dE (Waxman/Bahcall 99)

The high energy frontier: 

The high energy frontier

Acoustic Detection : 

Acoustic Detection Improve S/N : many hydrophones (close to each other as well as at several strings) Maximum of emission at ~ MHz

Renewed efforts along acoustic method for GZK neutrino detection: 

Renewed efforts along acoustic method for GZK neutrino detection AUTEC: US Navy array in Atlantic: existing sonar array for submarine detection Russia: AGAM antennas near Kamchatka: existing sonar array for submarine detection Russia: MG-10M antennas: withdrawn sonar array for submarine detection Greece: SADCO Mediterannean, NESTOR site, 3 strings with hydrophones Baikal : first signals from air showers? Sea-based Acoustical Detector of Cosmic Objects

RICERadio Ice Cherenkov Experiment (1): 

RICE Radio Ice Cherenkov Experiment (1) 20 receivers + transmitters Triggers:  4 RICE   1 RICE + Amanda A  1 RICE + SPASE firn layer (to 120 m depth) UHE NEUTRINO     DIRECTION 300 METER DEPTH

RICERadio Ice Cherenkov Experiment (2): 

RICE Radio Ice Cherenkov Experiment (2) 90% C.L. Upper Limits 10 TeV 1 PeV 100 PeV Neutrino Energy D.Besson, 2000 (preliminary) Flux dN/d(lnE) ~ 10-6 cm-2 sr-1 yr-1

Horizontal or upward air showers at EeV: 

Horizontal or upward air showers at EeV for E  1018 - 1020 eV: mass = 1-20 Giga-tons sensitivity  3·10-7 GeV·cm-2·s-1·sr-1 Horizontal showers in AUGER AGASA 2001: < 10-5 GeV·cm-2·s-1·sr-1

GLUE (1): 

GLUE (1)  E2·dN/dE < 10-4 GeV·cm-2·s-1·sr-1 Lunar Radio Emissions from Inter- actions of  and CR with > 1019 eV  1 nsec moon Earth Gorham et al. (1999), 30 hr NASA Goldstone 70 m antenna + DSS 34 m antenna at 1020 eV Goldstone Lunar Ultra-high energy neutrino Experiment Effective target volume ~ antenna beam (0.3°)  10 m layer  105 km3

GLUE (2): 

GLUE (2) method is going to challenge topological defect models ! Limited by live time. Only a small portion of antenna time devoted to one project

Outlook: 

Outlook

Slide65: 

 Amanda and Baikal challenge model predictions, Amanda is below “soft” theoretical bound  Soon: 10 - 20.000 m2 arrays in Mediterranean  Amanda-II (Antares, Nestor): discovery potential  IceCube and km3-underwater array will come to the limits of discovery potential for diffuse sources below EeV. Main focus: point sources, transient sources.  Acoustic and radio in ice still (or again) alive  Trans-GZK events revived interest in EeV physics  Promising limits from AGASA, GLUE. Further improvement by AUGER, EUSO, OWL, ..  “Signal” at TAUP-2003 ?