ultra - high energy neutrino astronomy ultra - high energy neutrino astronomy dmitrysemikoz ucla,...
TRANSCRIPT
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Ultra - High Energy Neutrino Ultra - High Energy Neutrino AstronomyAstronomy
Dmitry Dmitry
SemikozSemikozUCLA, Los Angeles UCLA, Los Angeles
in collaboration with in collaboration with
F.Aharonian, A.Dighe, O.Kalashev, F.Aharonian, A.Dighe, O.Kalashev, M.Kachelriess, V.Kuzmin, A.Neronov, M.Kachelriess, V.Kuzmin, A.Neronov,
G.Raffelt, G.Sigl , M.Tortola and G.Raffelt, G.Sigl , M.Tortola and R.TomasR.Tomas
Ultra High Energy \\ Cosmic Rays
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Fermilab February 9, 2004
Overview: Introduction: high energy neutrinos Experimental detection of high energy
neutrinos:Under/ground/water/iceHorizontal air showersRadio detection Acoustic signals from neutrinos
Neutrinos from UHECR protons Neutrinos from AGN
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Fermilab February 9, 2004
Most probable neutrino sources Neutrinos from Galactic SN Neutrinos in exotic UHECR models Conclusion
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Fermilab February 9, 2004
INTRODUCTION
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Fermilab February 9, 2004
Extragalactic neutrino flux? Sanduleak –69 Sanduleak –69 202 202
Large Magellanic Cloud Large Magellanic Cloud Distance 50 kpcDistance 50 kpc (160.000 light years)(160.000 light years)
Tarantula NebulaTarantula Nebula
Supernova 1987A Supernova 1987A 23 February 198723 February 1987
Georg
Raff
elt
, M
ax-P
lan
ck-I
nst
itu
t fü
r Ph
ysi
k (M
ün
chen
)
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Fermilab February 9, 2004
Neutrino Signal from SN 1987A Kamiokande (Japan)Kamiokande (Japan) Water Cherenkov detectorWater Cherenkov detector Clock uncertainty Clock uncertainty 1 min1 min
Kamiokande (Japan)Kamiokande (Japan) Water Cherenkov detectorWater Cherenkov detector Clock uncertainty Clock uncertainty 1 min1 min
Irvine-Michigan-BrookhavenIrvine-Michigan-Brookhaven (USA)(USA) Water Cherenkov detectorWater Cherenkov detector Clock uncertainty Clock uncertainty 50 ms50 ms
Irvine-Michigan-BrookhavenIrvine-Michigan-Brookhaven (USA)(USA) Water Cherenkov detectorWater Cherenkov detector Clock uncertainty Clock uncertainty 50 ms50 ms
Baksan Scintillator TelescopeBaksan Scintillator Telescope (Soviet Union)(Soviet Union) Clock uncertainty +2/-54 sClock uncertainty +2/-54 s
Baksan Scintillator TelescopeBaksan Scintillator Telescope (Soviet Union)(Soviet Union) Clock uncertainty +2/-54 sClock uncertainty +2/-54 s
Within clock uncertainties,Within clock uncertainties, signals are contemporaneoussignals are contemporaneous Within clock uncertainties,Within clock uncertainties, signals are contemporaneoussignals are contemporaneous
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Fermilab February 9, 2004
Atmospheric 's in AMANDA-II neural network energy reconstruction regularized unfolding
spectrum up to 100 TeV compatible with Frejus data
In future, spectrum will be usedto study excess due to cosmic ‘s
PRELIMINARY
1 TeV
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Fermilab February 9, 2004
Why UHE neutrinos can exist?
Protons are attractive candidates to be accelerated in astrophysical objects up to highest energies E~1020 eV.
Neutrinos can be produced by protons in P+P pions or P+pions reactions inside of astrophysical objects or in intergalactic space.
Neutrinos can be produced directly in decays of heavy particles. Same particles can be responsible for UHECR events above GZK cutoff.
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Fermilab February 9, 2004
Pion production
ee
...
'
i
b
i
b
PP
NN
p
n
20
eepn
Conclusion: proton, photon and neutrino fluxes are connected in well-defined way. If we know one of them we can predict other ones: tottot EE ~
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Fermilab February 9, 2004
High energy neutrino
experiments
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Fermilab February 9, 2004
Neutrino – nucleon cross section
Proton density
np~ 1024/cm3
Distance R~104km Cross section
N=1/(Rnp)~10-33cm2
This happens at energy E~1015 eV.
~E0.4
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Fermilab February 9, 2004
Experimental detection of E<1017eV neutrinos
Neutrinos coming from above are secondary from cosmic rays
Neutrino coming from below are mixture of atmospheric neutrinos and HE neutrinos from space
Earth is not transparent for neutrinos E>1015eV
Experiments: MACRO, Baikal, AMANDA
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Fermilab February 9, 2004
Experimental detection of UHE (E>1017eV) neutrinos
Neutrinos are not primary UHECR
Horizontal or up-going air showers – easy way to detect neutrinos
Experiments: Fly’s Eye, AGASA, HiRes
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Fermilab February 9, 2004
Radio detection
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Fermilab February 9, 2004
e + n p + e-
e- ... cascade
relativist. pancake ~ 1cm thick, ~10cm
each particle emits Cherenkov radiation
C signal is resultant of overlapping Cherenkov cones
for >> 10 cm (radio) coherence
C-signal ~ E2
nsec
negative charge is sweeped into developing shower, which acquiresa negative net chargeQnet ~ 0.25 Ecascade (GeV).
Threshold > 1016 eVExperiments:
GLUE, RICE, FORTE
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Fermilab February 9, 2004
Acoustic detection
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Fermilab February 9, 2004
d
R
Particle cascade ionization heat pressure wave
P
t
s
Attenuation length of sea water at 15-30 kHz: a few km(light: a few tens of meters)
→ given a large initial signal, huge detection volumes can be achieved.
Threshold > 1016 eV
Maximum of emission at ~ 20 kHz
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Fermilab February 9, 2004
Renewed efforts along acoustic method for GZK neutrino detection
Greece: SADCO Mediterannean, NESTOR site, 3 strings with hydrophones
Russia: AGAM antennas near Kamchatka:existing sonar array for submarine detection
Russia: MG-10M antennas: withdrawn sonar array for submarine detection
AUTEC: US Navy array in Atlantic:existing sonar array for submarine detection
Antares: R&D for acoustic detection
IceCube: R&D for acoustic detection
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Fermilab February 9, 2004
Present limits on neutrino flux
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Fermilab February 9, 2004
MACRO
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Fermilab February 9, 2004
FORTE
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Fermilab February 9, 2004
4-string stage (1996)
First underwater telescopeFirst neutrinos underwater
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Fermilab February 9, 2004
AMANDA-II
depth AMANDA
Super-K
DUMANDAmanda-II:677 PMTsat 19 strings
(1996-2000)
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Fermilab February 9, 2004
AGASA
AGASA covers an area of about 100 km2 and consists of 111 detectors on the ground (surface detectors) and 27 detectors under absorbers (muon detectors). Each surface detector is placed with a nearest-neighbor separation of about 1 km.
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Fermilab February 9, 2004
High Resolution Fly’s Eye: HiRes
HiRes 1 and HiRes 2 sit on two small mountains in western Utah, with a separation of 13 km.
HiRes 1 has 21 three meter diameter mirrors which are arranged to view the sky between elevations of 3 and 16 degrees over the full azimuth range;
HiRes 2 has 42 mirrors which image the sky between elevations of 3 and 30 degrees over 360 degrees of azimuth.
At the focus of each mirror is a camera composed of 256 40-mm diameter hexagonal photomultiplier tubes, each tube viewing a 1 degree diameter section of the sky.
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Fermilab February 9, 2004
GLUE Goldstone Lunar Ultra-high Energy Neutrino Experiment
E2·dN/dE < 105 eV·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
Effective target volume~ antenna beam (0.3°) 10 m layer
105 km3
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Fermilab February 9, 2004
RICE Radio Ice Cherenkov Experiment
firn layer (to 120 m depth)
UHE NEUTRINO DIRECTION
300 METER DEPTH
E 2 · dN/dE < 10-4 GeV · cm-2 · s-1 · sr-1
20 receivers + transmitters
at 1017 eV
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Fermilab February 9, 2004
Future limits on neutrino flux
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Fermilab February 9, 2004
Mediterranean Projects
4100m
2400m
3400mANTARESNEMO NESTOR
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Fermilab February 9, 2004
NEMO 1999 - 2001 Site selection and R&D
2002 - 2004 Prototyping at Catania Test Site 2005 - ? Construction of km3 Detector
ANTARES 1996 - 2000 R&D, Site Evaluation 2000 Demonstrator line 2001 Start Construction
September 2002 Deploy prototype line December 2004 10 (14?) line detector complete 2005 - ? Construction of km3 Detector
NESTOR 1991 - 2000 R & D, Site Evaluation Summer 2002 Deployment 2 floors Winter 2003 Recovery & re-deployment with 4 floors Autumn 2003 Full Tower deployment 2004 Add 3 DUMAND strings around tower 2005 - ? Deployment of 7 NESTOR towers
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Fermilab February 9, 2004
Baikal km3 project: Gigaton Volume Detector GVD
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Fermilab February 9, 2004
IceCube
1400 m
2400 m
AMANDA
South Pole
IceTop
- 80 Strings- 4800 PMT - Instrumented
volume: 1 km3
- Installation: 2004-2010
~ 80.000 atm. per year
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Fermilab February 9, 2004
Pierre Auger observatory
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Fermilab February 9, 2004
Telescope Array
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Fermilab February 9, 2004
MOUNT
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Fermilab February 9, 2004
OWL/EUSO
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Fermilab February 9, 2004
ANITA Antarctic
Impulsive
Transient
Array
Flight in 2006
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Fermilab February 9, 2004
Natural Salt Domes
Potential PeV-EeV Neutrino Detectors
SalSA Salt Dome Shower Array
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Fermilab February 9, 2004
Renewed efforts along acoustic method for GZK neutrino detection
Greece: SADCO Mediterannean, NESTOR site, 3 strings with hydrophones
Russia: AGAM antennas near Kamchatka:existing sonar array for submarine detection
Russia: MG-10M antennas: withdrawn sonar array for submarine detection
AUTEC: US Navy array in Atlantic:existing sonar array for submarine detection
Antares: R&D for acoustic detection
IceCube: R&D for acoustic detection
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Fermilab February 9, 2004
RICE AGASA
Amanda, Baikal2002
2007
AUGER
Anita
AABN
2012
km3
EUSO,OWLAuger
Salsa
GLUE
2004
RICE
Amanda II
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Fermilab February 9, 2004
Neutrinos from UHECR protons
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Fermilab February 9, 2004
Why neutrinos from UHE protons?
All experiments agree (up to factor 2) on UHECR flux below cutoff. All experiments see events above cutoff!
Majority of the air-showers are hadronic-like
Simplest solution for energies 5x1018 eV < E < 5x1019 eV: protons from uniformly distributed sources like AGNs.
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Fermilab February 9, 2004
Active galactic nuclei can accelerate heavy nuclei/protons
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Fermilab February 9, 2004
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Fermilab February 9, 2004
Photo-pion production
ee
iNN '
p
n
20
eepn
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Fermilab February 9, 2004
Parameters which define diffuse neutrino flux
Proton spectrum from one source:
Distribution of sources:
Cosmological parameters:
E
AEF )(
maxmin EEE
3)1( mzD maxmin zzz
0H vac
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Fermilab February 9, 2004
Theoretical predictions of neutrino fluxes
WB bound: 1/E2 protons; distribution of sources – AGN; analytical calculation of one point near 1019 eV.
MPR bound: 1/E protons; distribution of sources – AGN; numerical calculation for dependence on Emax
The ray bound: EGRET
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Fermilab February 9, 2004
The high energy gamma ray detector on the Compton Gamma Ray Observatory (20 MeV - ~20 GeV)
EGRET: diffuse gamma-ray flux
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Fermilab February 9, 2004
Detection of neutrino fluxes: today
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Fermilab February 9, 2004
Future detection of neutrinos from UHECR protons
AGN,1/E
Old sources1/E^2
/ EUSO
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Fermilab February 9, 2004
Neutrinos from Active galactic
nuclei
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Fermilab February 9, 2004
Active Galactic Nuclei (AGN)
Active galaxies produce vast amounts of energy from a very compact central volume.
Prevailing idea: powered by accretion onto super-massive black holes (106 - 1010 solar masses). Different phenomenology primarily due to the orientation with respect to us.
Models include energetic (multi-TeV), highly-collimated, relativistic particle jets. High energy -rays emitted within a few degrees of jet axis. Mechanisms are speculative; -rays offer a direct probe.
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Fermilab February 9, 2004
Neutrinos from AGN core
/ EUSO
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Fermilab February 9, 2004
Photon background in core Energy scale
E= 0.1 – 10 eV Time variability
few days or
R = 1016cm Model: hot thermal
radiation.
T=1 eVT=10 eV
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Fermilab February 9, 2004
Photo-pion production
ee
iNN '
p
n
20
eepn
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Fermilab February 9, 2004
Neutrino spectrum for various proton spectra and backgrounds
1/E
1/E2
T=10 eV
1/E2
T=1 eV
E~1018eV
Atm.flux
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Fermilab February 9, 2004
Most probable neutrino sources
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Fermilab February 9, 2004
Optics: SDSS. Most powerful objects are AGNs
500 sq deg of the sky, 14 million objects, spectra for 50,000 galaxies and 5,000 quasars.
Distance record-holder
>13,000 quasars (26 of the 30 most distant known)
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Fermilab February 9, 2004
Low energy radiation from AGN is collimated
Typical gamma-factor is
Radiation is collimated in 1/ angle ~ 5o in forward direction.
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Fermilab February 9, 2004
EGRET 3rd Catalog: 271 sources
Most of identified MeV-GeV sources are blazars
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Fermilab February 9, 2004
Which sources ?
Blazars (angle – energy correlation)
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Fermilab February 9, 2004
High energy photons from pion decay cascade down in GeV region
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Fermilab February 9, 2004
EGRET 3rd Catalog: 271 sources
Only 22 sources from 66 are GeV - loud
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Fermilab February 9, 2004
Which sources ?
Blazars (angle – energy correlation) Blazars should be GeV loud (conservative model)
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Fermilab February 9, 2004
Which sources ?
Blazars (angle – energy correlation) Blazars should be GeV loud (conservative model) ‘Optical depth’ for protons should be large:
pnR
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Fermilab February 9, 2004
Bound on blazars which can be a neutrino sources
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Fermilab February 9, 2004
TeV blazars does not obey last condition
Indeed, in order TeV blazars be a neutrino sources:
pnR nR
p= 6x10-28cm2 while = 6.65 x 10-25cm2
CONTRADICTION!!!
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Fermilab February 9, 2004
Which sources ?
Blazars (angle – energy correlation) Blazars should be GeV loud (conservative model)
Optical depth for protons should be large:
pnR No 100 - kpc scale jet detected (model-dependent)
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Fermilab February 9, 2004
Neutrino production in AGN
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Fermilab February 9, 2004
Collimation of neutrino flux in compare to GeV flux
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Fermilab February 9, 2004
Neutrinos from Galactic
Supernova
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Fermilab February 9, 2004
Prompt neutrino signal in 1-50 MeV energies.Prompt neutrino signal in 1-50 MeV energies.
1-10 sec after SN burst/Strong signal in each optical 1-10 sec after SN burst/Strong signal in each optical
module / SN 1987A signalmodule / SN 1987A signal
Prompt neutrino signal in 1-50 MeV energies.Prompt neutrino signal in 1-50 MeV energies.
1-10 sec after SN burst/Strong signal in each optical 1-10 sec after SN burst/Strong signal in each optical
module / SN 1987A signalmodule / SN 1987A signal
50-200 events with E> 1TeV in 10-12 hours after burst. 50-200 events with E> 1TeV in 10-12 hours after burst. Shock front reached surface and became colisionless.Shock front reached surface and became colisionless. Duration t ~ 1 hour / Waxman & Loeb 2001Duration t ~ 1 hour / Waxman & Loeb 2001
50-200 events with E> 1TeV in 10-12 hours after burst. 50-200 events with E> 1TeV in 10-12 hours after burst. Shock front reached surface and became colisionless.Shock front reached surface and became colisionless. Duration t ~ 1 hour / Waxman & Loeb 2001Duration t ~ 1 hour / Waxman & Loeb 2001
SN shock interact with pre-SN wind and interstelar SN shock interact with pre-SN wind and interstelar medium. 1000-10000 events with E>1 TeV in km^3 medium. 1000-10000 events with E>1 TeV in km^3 detectordetectorFrom 10 days till 1 year /Berezinsky & Ptuskin 1989From 10 days till 1 year /Berezinsky & Ptuskin 1989
SN shock interact with pre-SN wind and interstelar SN shock interact with pre-SN wind and interstelar medium. 1000-10000 events with E>1 TeV in km^3 medium. 1000-10000 events with E>1 TeV in km^3 detectordetectorFrom 10 days till 1 year /Berezinsky & Ptuskin 1989From 10 days till 1 year /Berezinsky & Ptuskin 1989
Possible neutrino signals from Galactic SN in km^3 detector
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Fermilab February 9, 2004
Supernova MonitorAmanda-II
Amanda-B10
IceCube0 5 10 sec
Count rates
B10: 60% of Galaxy
A-II:95% of Galaxy
IceCube:up to LMC
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Fermilab February 9, 2004
Pointing to Galactic SN
AMANDA II will see 5-20 events with E> 1TeV. For angular resolution 2o of each event. Pointing to SN direction is possible with resolution ~0.5o
For ANTARES pointing is up to 0.1o . Compare to SuperKamiokande 8o now and 3.5o
with gadolinium. HyperKamiokande ~0.6o
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Fermilab February 9, 2004
Detection of Galactic SN from wrong side by km^3 detector
Atmospheric muons 5*1010/year or
300/hour/(1o)2
Signal 200 events, besides energy cut 1 TeV. Angular resolution 0.8o for each event or less
then 0.1o for SN signal !!!
(A.Digle, M.Kachelriess, G.Raffelt, D.S. and R.Tomas, hep-ph/0307050)
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Fermilab February 9, 2004
Neutrinos from exotic UHECR
models
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Fermilab February 9, 2004
Z-burst mechanism(T.Weiler, 1982)
Resonance energy E = 4 1021 (1 eV/m) eV
Works only if
meV
Mean free path of neutrino is
L = 150 000 Mpc >> Luniv
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Fermilab February 9, 2004
Cross sections for neutrino interactions with
relict background and
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Fermilab February 9, 2004
Pure neutrino sources
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Fermilab February 9, 2004
Sources of both and
Kalashev, Kuzmin, D.S. and Sigl, hep-ph/0112351
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Fermilab February 9, 2004
Gelmini-Kusenko model: X->
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Fermilab February 9, 2004
FORTE and WMAP practically exclude Z-burst model
D.S. and G.Sigl, hep-ph/0309328
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Fermilab February 9, 2004
Top-down models
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Fermilab February 9, 2004
New hadrons (Kachelriess, D.S. and Tortola, hep-ph/0302161)
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Fermilab February 9, 2004
Diffuse neutrino flux
Flux is unavoidably high due to
Shape depends on distribution of background photons and on proton spectrum
S
p
S
pUHE E
EFF
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Fermilab February 9, 2004
Conclusions Sensitivity of the neutrino telescopes will be
increased in 102-3 times during next 10 years. Now they just on the border of theoretically interesting region.
Secondary neutrino flux from UHECR protons can be detected by future UHECR experiments.
Neutrino flux from AGN’s can be detected by under-water/ice neutrino telescopes. GeV-loud blazars with high optical depth for protons are good candidates for neutrino sources.
Galactic SN can be detected with neutrinos at low and high energies.
Some of exotic UHECR models will be ruled out or confirmed in near future by neutrino data.
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Fermilab February 9, 2004
References:
Diffuse neutrino flux. O.Kalashev, V.Kuzmin, D.S. and G.Sigl, hep-ph/0205050; D.S. and G.Sigl, hep-ph/0309328
Extragalactic neutrino sources. A.Neronov & D.S., hep-ph/0208248
AGN jet model. A.Neronov, D.S., F.Aharonian and O.Kalashev, astro-ph/0201410
Z-burst model. O.Kalashev, V.Kuzmin, D.S. and G.Sigl, hep-ph/0112351
New hadrons as UHECR. M.Kachelriess, D.S. and M.Tortola, hep-ph/0302161
SN pointing with low and high energy neutrinos. R.Tomas, D.S., G.Raffelt, M.Kachelriess and A.Dighe, hep-ph/0307050