Kyoto 2005
Kyoto 2005

OutlineUHE Neutrino Astronomy
Shigeru Yoshida
Chiba University
http://www.ppl.phys.chiba-u.jp/~syoshida/HE ν emission – What it can tell
Theoretical Bound of ν fluxes
Extremely High-Energy ν generation
Cosmic ν detection – the current status
IceCube : reachable to EHE ν universe
Charged particle astronomy?

Physics motivation
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/ TeV sources!
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cosmic
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/
rays
/
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/
/
/

ν

 origin and acceleration of cosmic rays
 understand cosmic cataclysms
 find new kind of objects?
 neutrino properties (ντ , 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 holeradiationenveloping
black hole

VLA image of Cygnus A

1

You cannot expect too many ν!
pγ(p,n) π2γ

TeV/EGRET
observations !!

µνeννCosmic Ray
observations!

Synchrotron
cooling
You cannot expect too high energies

Theoretical bounds
EHE(Extremely HE) ν
DUMAND test string
FREJUS

MACRO

opaque for neutronss
atmo

NT-200MPR
MPR

neutrons can escape

c
pheri

Suppressed by
W&B
Synchrotron Cooling
W&B

Synchrotron cooling of µ …
Production sites with low B
Intergalactic space!!

νµ•GZK Production•Z-burst•Topological Defects/Super heavy Massive particles

Mannheim, Protheroe and Rachen (2000) – Waxman, Bahcall (1999)
 derived from known limits on extragalactic protons + γ-ray flux

Kyoto 2005

GZK Neutrino Productionpγ π＋

E = 10 20 eV

n

ν e＋

μ＋

γ

ν

GZK ν fluxes (EeV~ZeV!)p
E ~ 0.8 x 10 20 eV

2.725 K411 photons / cm3

Cross Section (mb)

0.6 x 10-27 cm2
0.1

γ+ p→Δ（1232）→ πo p or π+ n

0.01
Gamma Beam Energy (GeV)

Conventional Mechanism of EHE neutrinos!!

Yoshida and Teshima 1993
Yoshida, Dai, Jui, Sommers 1997

Kyoto 2005

2

Parameters involved in calculation. Predicted fluxes.

Parameters

Orientative order of magnitudeγ

spectral injection index

[1-3]

m

activity evolution index[3-5]

zmax z of formation of sources

[1-4]

ΩM

density of matter[0.2-1]

Ho

Hubble constant[50-80 Km/s/Mpc]

Bintergalactic magnetic field

[B≤
≤1nG]

ηLρL/ηoρo local enhancement[?]

Emax maximum acceleration energy in source[E max >4 1020 eV](Diego González-Díaz, Ricardo Vázquez, Enrique Zas 2003)

CR and ν fluxes for different models(Diego González-Díaz, Ricardo Vázquez, Enrique Zas 2003)

Kyoto 2005

Z-bursts Concept

Kyoto 2005

It is the “standard” particle physics

ννp, π+,π-.π0..

CRs extending tosuperEHEs!

(Yoshida, Sigl, Lee 1998)

Kyoto 2005

Z-burst constraints(Yoshida, Sigl, Lee 1998)

3

EHE Neutrino Fluxes

Where the source of(Extremely)-high energy ν?
My $100 goes to GZKPresent bound

My $1 goes to GRB(E)HE ν generation needs
target photons!
∆resonance inthe photopion production

Ep Eγ ~ 0.25 Γ2 [GeV2]

Cross Section (mb)

Kyoto 2005

0.1

γ+ p→Δ（1232）→ πo p or π+ n

0.01
Gamma Beam Energy (GeV)Γ ~ 300, Eγ~ MeV

Ep ~ 10 16 eV ~ 10 PeV

Γ ~ 300, Eγ~ eV

Ep > 10 20 eV ~ 1 ZeV

Eγ~ eV ??

Proton-synchrotron model(Totani 1998)

Energy limit!

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Kyoto 2003

(Highly biased)conclusion ☺
Cosmic neutrinos come from …….

GRBs

Cosmic ν detectionEνν ~ PeV+GZK + GRBs(p-synch)Eνν > EeV
Neutrino Telescopes – ANTARES,
IceCube etc.

All “diffusive/background” fluxes

How to build a ν
cosmic ray
detector•Infrequently, a cosmic neutrino is
captured in the ice, i.e. the neutrino
interacts with an ice nucleus•In the crash a muon (or electron,or tau) is produced

Earth

ν
ν

Cherenkov
muonlight coneµinteraction

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
RussiaThetysMarseille

La Seyne
sur Mer

ToulonExisting Cable
Marseille-Corsica

NEMO
Catania, Italy

DUMAND
Hawaii(cancelled 1995)

NESTOR
Pylos, Greece

Demonstrator Line
Nov 1999- Jun 2000
42°59 N, 5°17 E
Depth 1200 m

New Cable (2001)
La Seyne-ANTARESANTARES 0.1km2 Site
42°50 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 2002- 2004

5

ANTARES Layout

Laser calibration at the
CPPM dark room

• 12 lines• 25 storeys / line
• 3 PMT / storey

14.5 m
Opticalbeacon

350 m

t2

t1

t3

CylinderJunctionbox

Opticalfibres

100 m
40 km toshore

~60-75 m

Laser

Readout cables

Optical Splitter

IceTop

AMANDA II Detector

AMANDA

IceCubeSouth PoleAmundsen-Scott Station South Pole

Skiway80 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) to1020 eV
Opticalmodule2400 m1996-2000

1200 m

IceTopIceTop
160 tanksfrozen-water tanks
2 OMs / tankFirst year deployment (Jan 2005)
4 IceCube strings (240 OMs)
8 IceTop Tanks (16 OMs)

Who are we ?
BartolBartolResearch
ResearchInst,
Inst,Univ
UnivofofDelaware,
Delaware,USA
USA Univ.
Univ.ofofAlabama,
Alabama,USA
USA
Pennsylvania State University, USA
Clark-Atlanta University, USA
Pennsylvania State University, USA
Clark-Atlanta University, USA
University
Univ.
UniversityofofWisconsin-Madison,
Wisconsin-Madison,USA
USA
Univ.ofofMaryland,
Maryland,USA
USA
University
IAS,
UniversityofofWisconsin-River
Wisconsin-RiverFalls,
Falls,USA
USA
IAS,Princeton,
Princeton,USA
USA
LBNL, Berkeley, USA
University of Kansas, USA
LBNL, Berkeley, USA
University of Kansas, USA
UCSouthern
UCBerkeley,
Berkeley,USA
USA
SouthernUniv.
Univ.and
andA&M
A&MCollege,
College,Baton
BatonRouge
Rouge
UC
UCIrvine,
Irvine,USA
USA

IceCube

Chiba
ChibaUniversity,
University,JapanJapan
AMANDA

University of Canterbury,
University of Canterbury,
Christchurch,
Christchurch,New
NewZealand
Zealand

IceCube80 strings
60 OMs/string
17 m vertical spacing
125 m between strings

IceTop Tank deployed in 2004
10” 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
SwedenKalmar Universitet, Sweden
Kalmar Universitet, Sweden
Imperial College, London, UK
Imperial College, London, UK
UniversityofOxford,UK
University of Oxford, UK
Utrecht University, Utrecht, NL
Utrecht University, Utrecht, NL

6

Color displays: LE
Primary Channels
2370
13
2501
23
2631
40
2762
38
2893
34
3023
28
3154
21
3285
19
3415
11
3546
9
3677
6
3807
9
3938
4
4069
5
4199 24330 2Size 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 1425281 from run 336
Recorded yr/dy: 2000/170
59857.5405130 seconds past midnight.
Before cuts: 264 hits, 264 OMs
After cuts : 264 hits, 264 OMs

The highest energy event (~200 TeV)
TeV)

Detection of νe ,νµ , ντO(km) long muon tracks

Electromagnetic and hadronic cascades
Color displays: LE≈ 15 m

23
40
38
34
28
21
19
11
9
6
9
4
5
2
2

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 1425281 from run 336
Recorded yr/dy: 2000/170
59857.5405130 seconds past midnight.
Before cuts: 264 hits, 264 OMs
After cuts : 264 hits, 264 OMs

direction determinationby cherenkov light timing

Excess of cosmic
neutrinos? Not yet ...

talk HE 2.3-4.. for now use number of hit channels as energy variable ...
preliminary (2000 data)

102experiment
background MC-2

E signal MC (νe)

10talk HE 2.3-5

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
13

300 m

2370
2501
2631
2762
2893
3023
3154
3285
3415
3546
3677
3807
3938
4069
4199
4330

 697 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 ν‘s„AGN“ with 10-5 E-2
GeV-1 cm-2 s-1 sr-1

1

below horizon:mostly fake events-110

 sky subdivided into 300 bins (~7°x7°)
4

4.5

5

5.5
6
6.5
log10(Ereco/GeV)

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 ourbest upper limit(sensitivity shown here)

2000-01

Fit of the measured
spectrum from HEGRA(Low)
Allowed range for theemitted flux
AMANDA sensitivity

2002

about factor 2

IceCube sensitivity

Correction for extragalactic γ absorption¶:
TeV γ-ray spectra aremodified by red-shiftdependent absorption
by intergalactic IR-UV
background¶O.C.De Jager & F.W.Stecker, Astrophy.J. 566 (2002), 738-743

17

7

Theoretical bounds andfuture

GIGA-ton detector!!

DUMAND test string
FREJUS

MACRO

opaque for neutronss
atmo

NT-200AMANDA-97

cpheri

AMANDA-00

MPR
MPR

neutrons can escapeNT-200+

AMANDA-II

νµ

W&B
W&B

IceCubeMannheim, Protheroe and Rachen (2000) – Waxman, Bahcall (1999)
 derived from known limits on extragalactic protons + γ-ray flux

1015 eV

1016 eV1017 eV

EHE MC Event examples
300 PeV taus

How (E)HE events look like
1018 eV1019 eV1020 eV

EHE (EeV or even higher) Neutrino Events
Arriving Extremely Horizontally

Energy loss profile in UHE/EHE
By JULIeT• Needs Detailed Estimation• Limited Solid Angle Window(σρNA)-1 ~ 600 (σ/10-32cm2) -1(ρ/2.6g cm-3) -1 [km]Stochastic Loss
Initiating high energy
Cascades!

Involving the interactions generating
electromagnetic/hadron cascadesµNµX e+e-Kyoto 2005

8

Products

νe

νe

νµ

ντ

µ

e/γ

τ

Weak

π
Weak

Muon(Neutrinos) from νµ ντ

Tau(Neutrinos) from νµ ντNadir Angle
Weak

IncomingνµWeak
Suppression
Weak

Weak

Pair/decay
Pair
BremssPair

PhotoNucl.

Decay
Pair

Pair

PhotoNucl.

ντe/γ

By τ decay

Cascades

µ

Decay

Decay
Weak

Decay

Decay

Decay
Weak

τ

Pair
Bremss
Decay

Decay

Cascadesπ

Kyoto 2005

Down-going events dominate…

GZK spectrum @ IceCube depth
Upward-going

Atmospheric µ is attenuated faster…

Downward going!!

11000mUp

Down

2800 m
1400 mAtmospheric muon! – a major backgrond
But so steep spectrum
Kyoto 2005

Kyoto 2005

EHE events!

νSignal(GZK) Vs Atm µ

Downward

Very Preliminary

leptone +e －

γ

noise

γ

Ice

１ｋｍ

Rock

ν
１ｋｍ

e +e －

γπ±

leptonMC Truth

１．４ｋｍ

signalUpward ν

MC Truth9

Signal(GZK) Vs Atm µ

We MEASURE energy
deposit in km3
dE/dX~βE∆E~∆XbE

First Guess

Very Preliminary# of Hit

We MEASURE energy
deposit in km3

Flux as a function ofenergy deposit in km3

dE/dX~βE

dE/dX~βE∆E~∆XbE∆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[cm-2 sec-1]
Iτ(E>10PeV)

RATE[/yr/km2]

Down

5.90 10-19 5.97 10-19

0.37

Up

3.91 10-20 6.63 10-20

0.03

GZK m=4Iµ(E>10PeV)

Zmax=4Iµ(E>10PeV)

Iτ(E>10PeV)

Energy Deposit

Energy Deposit

Down

4.75 10-19 3.28 10-19

0.25

m=7
Zmax=5Down

7.21 10-17

37.9

Atm µ

1.74 10-19

4.83 10-17

IceCube EHE ν Sensitivity
90% C.L. for 10 year observation
S.Yoshida, R.Ishibashi, H.Miyamoto, PRD 69 103004 (2004)

0.05

RESCEU 2003

10

IceCube : The Present status

ν detection by EAS
HiRes/Auger etc

Yoshida et al ApJ (1997)~10 strings will be being deployed now!

~ IceCube

29th ICRC Pune

Charged Particle
Astronomy?

Event cluster > 40 EeV

E>>10 EeV  ∆ θ ~ a few deg

No significant excess: AGASA’s triplet Pch ~0.28(Westerhoff, this conference)

29th ICRC Pune

AGASA triplet story

29th 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.

th

Catalog: Veron (9 Ed.) BL Lacs

#
CRs

Bin
Size

#
Pairs

Prob.

AGASA >48 EeV
Yakutsk >24 EeV

65

2.5°°

8

< 10-4

CR Sample

22

HiRes stereo event

6060
60°
°

m < 18z > 0.1 or
unknown

S6cm > 0.17 JythCatalog: Veron (10 Ed.) BL Lacs
correlated with EGRET sources
no cutno cut

HiRes > 24 EeV

66

2.5°°

0

1.00

AGASA >48 EeV
Yakutsk >24 EeV

65

2.9°°

8

10-4

HiRes > 24 EeV

66

2.9°°

1

.70

AGASA > 40 EeV

57

2.5°°

12

.02

HiRes > 40 EeV

27

2.5°°

2

.78

HiRes > 10 EeV

271

0.8°°

10

10-3

14

no cutthCatalog: Veron (10 Ed.) BL Lacs156
m < 18

180
°
180
°

170
°
170
°

One event added – BUT below 40 EeV!!

no cutno cutthCatalog: Veron (10 Ed.) BL Lacs156
m < 18no cutno cutGorbunov et al., JETP Lett. 80 (2004) 145.

(Westerhoff, this conference)(Finley, this conference)11

29th ICRC Pune

Future Outlook (of UHECR)
Auger: 7 x AGASA by 30th 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 ray/Neutrino search
EAS detector, IceCube, Rice, ANITA etc.

Kyoto 2005

Summary and outlook
HE cosmic neutrinos come fromGZK (100PeV – 100 EeV) $100
GRB (PeV) GRB-P-synch $10

Neutrino observatory IceCube provides DATA
0.1 x IceCube ~2006!
Strong capability of EHE ν search
Charged Particle Astronomy (Cluster, BLLac E>10 EeV)
wait for 2004-5 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。

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