high energy neutrino astronomy christian spiering desy zeuthen taup 2001
TRANSCRIPT
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High Energy Neutrino Astronomy
Christian SpieringDESY Zeuthen
TAUP 2001
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Predictions and Bounds
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log(E2 Flux)
log(E/GeV)TeV PeV EeV
3 6 9
pp core AGN p blazar jetTop-Bottom model
GRB (W&B)
Various recentmodels for transient sources
Classes of Models
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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
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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)
atmospheric flux
W & B
MPR
optically thick for neutrons
optically thin
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MPR limit for optically thin sources
109
1012
Emax=106
3 1013
3 1010
3 107
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 shiftblue: renormaliztion after GZK shift
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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.
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1 pp core AGN (Nellen)2 p core AGN Stecker & Salomon)3 p „maximum model“ (Mannheim et al.)4 p blazar jets (Mannh)5 p AGN (Rachen & Biermann)6 pp AGN (Mannheim)7 GRB (Waxman & Bahcall)8 TD (Sigl)
Diffuse Fluxes: Predictions and Limits
Mannheim & Learned,2000
MacroBaikal
IceCube
Amanda
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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 starsin a contracting central cluster Massive gas
envelope
NS & BH survive, furthercontraction and collisions
Repeating fireballs,particle acceleration inrarified cavity
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Interactions in envelopeHE 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)
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Alvarez-Muniz, Halzen, Hooper, 2000
z = 1 z distribution expect up to = 300 thousands of events/yrkm2
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 ~ 310-9 cm-2 s-1 sr-1 GeV between 100 TeV and 10 PeV
100 300 1000
-faint,high flux
Low flux,high energy
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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)
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GRB (quasi-thermal) from 0 decay
neutrinos
Cannon Balls
SN shell
242
2
10
10)0(
zEkmd
dnin
CB
‘s extremely forward collimated - the stronger the higher their energy
Cannon Ball Model of GRB
(Dar, De Rujula, Plaga)
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Neutrinos from MicroquasarsWaxman, 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
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Experiments under ground
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MACRO
Limit on flux from point sources
Limit on diffuse flux
Limit on neutrino emission from GRB
Since 1989:1356 upward going
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MACRO point source searchMACRO sky-map in equatorial coordinates
90% c.l. upper limits for 42 selected sources (red dots)
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Selection of HE neutrinos:1. timing cut (upward)2. energy deposition in scintillators Rate of survived
events in 5.8 yr
ATMMC 1.1±0.5stat
AGNMC 0.54±0.03stat
DATA 2
E2
< 4.5 10-6 cm -2 s -1 sr –1
GeV
MACRO: limit on diffuse E-2 flux
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MACRO: Neutrinos from GRB
Search for space-time correlationWith 2527 BATSE GRB between1991 and 1999
Flux < 0.8 x 10-9 cm-2
per average burst
about 10 times above optimisticpredictions (Paolis et al., Halzen & Hooper), about 100 times above Waxman & Bahcall)
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1761 upward going muons(through-going and stopping)from 1264 live days (April 96-May 00)
1200 m2 acceptance area
Superkamiokande
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Super-K: point source search
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Upward muons undergroundSuper-Kamiokande 2.0 k eventsMACRO 1.4 k eventsBaksan 1.0 k events
IMB + K-II + KGF + Soudan + ... ~ 1.5 k events (?)
~ 6000 events sets scale for underwater/ice experiments
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Experiments under water
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3600 m
1366 m
Lake Baikal, NT-200: The Site
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pair of 37 cm Quasar PMTs
NT-200: the detector
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„Gold plated“ neutrino event, 4-string stage (1996)
NT-200: zenith angledistribution 234 days in 1998/99
19 hits
Lake Baikal: atmospheric neutrinos
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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 cutRed squares: # hit > 45
E2 < 1.9 10-6 cm-2 s-1 sr-1 GeV
Upper limit on diffuse flux of HE e
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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
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The Mediterranean Projects
Antares
Nestor Nemo test site
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NESTOR
First Mediterranean project (founded 1991) Site: Pylos (Greece), 3800m depth
towers of 12 titanium floors each supporting 12 PMTs
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Nestor Tower
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Deployment plans
Schedule:
2001:re-lay cable to siteand deploy 2 floors
2003:full tower
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ANTARES
-2400m
40 km
Submarine cable
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Demonstrator Site 42°59 N, 5°17 E Depth 1200 m
ANTARES Site42°50 N, 6°10 E Depth 2400 m
Demonstrator Line: 8 OMs Nov 1999 - June 2000
Existing cableMarseille-Corsica
New Cable (2001)La Seyne-ANTARES
Marseille
ToulonLa Seyne sur Mer
0.05 km2 Detector: 900 OMs , Deploy 2002- 2004
Site, History, Schedule
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The Detector
2500m2500m
300m300mactiveactive
Electro-opticElectro-opticsubmarine cablesubmarine cable ~40km~40km
Junction boxJunction box
Readout cablesReadout cables
Shore stationShore station
anchoranchor
floatfloat
Electronics containersElectronics containers
~60m~60mCompass,Compass,tilt metertilt meter
hydrophonehydrophone
Optical moduleOptical module
Acoustic beaconAcoustic beacon
~100m
10 strings12 m between storeys
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ANTARES Performance
Very good angular accuracybelow 3 TeV angular error is dominatedby 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)
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ANTARESNorthern Hemisphere
AMANDASouthern Hemisphere
Galactic Centre seen 80% of time
Galactic Centre not visible
Fraction of time sky visible
View of Sky: Complementary to AMANDA
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NEMO
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Nemo-2
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Nemo3
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Experiments under ice
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AMANDA
Location:Geographic South Pole
Amanda –II:677 PMTs at 19 strings
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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)
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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)
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Search for point sources
Optimize analysis on HE neutrinos and good angular resolution
Accept large background contribution
Systematic uncertainties
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Other limits from AMANDA and BAIKAL
AMANDA, 78 BATSE bursts in 1997
WIMPs from center of Earth
RelativisticMagnetic MonopolesBaikal
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AMANDA-II
TriggerLevel
After BGrejection
up horizon
A-II
B-10
dramatically increased acceptancetowards horizon
Nearly horizontal event
(experiment)
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Physics Reach of AMANDA-II
0
50
100
150
200
-1 -0.8 -0.6 -0.4 -0.2 0
Aef
f [
x10
3 m
2]
Cos(theta)
E = 10 TeV
Am-II Trigger
Am-II Point Cuts
Am-B10 Point Cuts
Am-II GRB Cuts
10-10
10-8
10-6
10-4
102 103 104 105 106
E2 (d
N/d
E )
[G
eVcm
-2s
-1]
E(GeV)
AMANDA-II (3 yr)
AMANDA-B10 ('97)
IceCube3C273
Crab
AGN Core
Mk501 (=)
Atm.
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
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AMANDA-II and EeV searchTransmission 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 athigh energies is small.
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AMANDA-II and EeV search
10-4
10-3
10-2
10-1
100
101
102
-1 -0.5 0 0.5 1
cos()
AGN (Protheroe)GZK*100
• 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 !
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80 strings,each with 60 PMTs
AMANDA-II
SPASE
South Pole
IceCube
02468
1012141618
s3/4 s4/5 s5/6 s6/7 s7/8 s8/9
Number ofstrings
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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“)
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IceCube: Point Source Search
0.25
0.5
0.75
1
1.25
1.5
1.75
2
2.25
2.5
0 -1 -0.9 -0.8 -0.7 -0.6 -0.5 -0.4 -0.3 -0.2 -0.1 0
muon energy 0.1 to 1.0 TeVmuon energy 1.0 to 10.0 TeVmuon energy 10.0 to 100.0 TeV
cos(zenith angle)
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 predictionsof many recent models
(1-100 TeV)
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Energy spectra
Diffuse search
Point source search
Colored: standard reconstruction and cuts against fake eventsBlack: ultimate Nhit cuts to get the lowest limit
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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)
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The high energy frontier
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Acoustic Detection
10 m
hydrophones
Improve S/N : many hydrophones (close to each other as well as at several strings)
Maximum of emission at ~ MHz
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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
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RICERadio 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
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RICERadio 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
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Horizontal or upward air showers at EeV
el.-magn.cascade
from e
hardmuons
from CR
for E 1018 - 1020 eV:
mass = 1-20 Giga-tonssensitivity 3·10-7 GeV·cm-2·s-1·sr-
1
Horizontal showers in AUGER
500 km
60 °
Horizontal showers seen by EUSO / OWL
E > 1019 GeV
Area upto 106 km2
Mass upto 10Tera-tons
AGASA 2001: < 10-5 GeV·cm-2·s-1·sr-1
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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 Goldstone70 m antenna + DSS 34 m antenna
at 1020 eV
Goldstone LunarUltra-high energyneutrino Experiment
Effective target volume~ antenna beam (0.3°) 10 m layer
105 km3
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GLUE (2)
method is going to challengetopological defect models !
Limited by live time. Only a small portionof antenna time devoted to one project
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Outlook
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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 ?