Kyoto 2005

UHE Neutrino Astronomy
Shigeru Yoshida
Chiba University
http://www.ppl.phys.chiba-u.jp/~syoshida/Kyoto 2005

OutlineHE 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?

////// TeV sources!
///
cosmic//rays//////

νPhysics motivation
 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. ...

black holeradiationenveloping
black hole

You cannot expect too many ν!
pγ(p,n) π
2γ

TeV/EGRET
observations !!

µνeννCosmic Ray
observations!

Synchrotron
cooling
You cannot expect too high energies

Theoretical bounds
DUMAND test string
FREJUS

MACRO

opaque for neutronsatmo

NT-200MPRMPRneutrons can escaperic ν µsphe

Suppressed byW&B
Synchrotron Cooling
W&B

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

EHE(Extremely HE) ν
Synchrotron cooling of µ …
Production sites with low B
Intergalactic space!!
•GZK Production•Z-burst•Topological Defects/Super heavy Massive particles

Kyoto 2005

GZK Neutrino Productionp
E = 10 20 eV＋γπν e＋＋μγ

νpn

E ~ 0.8 x 10 20 eV

2.725 K411 photons / cm3

Cross Section (mb)

0.6 x 10-27 cm20.1γ+ p→Δ（1232）→ πo p or π+ n

0.01
Gamma Beam Energy (GeV)

Conventional Mechanism of EHE neutrinos!!

GZK ν fluxes (EeV~ZeV!)

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

Kyoto 2005

Parameters involved in calculation. Predicted fluxes.

Parameters

Orientative order of magnitudeγ

spectral injection index[1-3]

mactivity 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)

Kyoto 2005

(Diego González-Díaz, Ricardo Vázquez, Enrique Zas 2003)

CR and ν fluxes for different models

Kyoto 2005

Z-bursts Concept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)

Kyoto 2005

EHE Neutrino Fluxes

Present boundWhere the source of(Extremely)-high energy ν?
My $100 goes to GZKMy $1 goes to GRB∆resonance inthe photopion production

Ep Eγ ~ 0.25 Γ2 [GeV2]

Cross Section (mb)

(E)HE ν generation needs
target photons!
0.1

γ+ p→Δ（1232）→ πo p or π+ n0.01
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!

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

GRBsEν
ν ~ PeV+GZK + GRBs(p-synch)Eνν > EeVAll “diffusive/background” fluxes

Kyoto 2003

Cosmic ν detection

Neutrino Telescopes – ANTARES,
IceCube etc.

How to build a ν
cosmic raydetector
Earthν
νµDetector

•Infrequently, a cosmic neutrino iscaptured in the ice, i.e. the neutrino
interacts with an ice nucleus•In the crash a muon (or electron,or tau) is produced
Cherenkov
muonlight cone

Detector•The muon radiates blue light in its wake
•Optical sensors capture (and map) the lightinteractionneutrino

Optical Cherenkov
Neutrino Telescope Projects
ANTARES
La-Seyne-sur-Mer, France

NEMO
Catania, Italy

BAIKAL
RussiaDUMAND
Hawaii(cancelled 1995)

NESTOR
Pylos, Greece

IceCube, South Pole, Antarctica

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

14.5 m350 m

Junctionbox
100 m
40 km toshore~60-75 m
Readout cables

AMANDA II Detector
Amundsen-Scott Station South Pole

Opticalmodule
1996-2000

IceTop

IceCube

AMANDASouth Pole
Skiway80 Strings
4800 PMT
Instrumented
volume: 1 km3 (1 Gt)
IceCube is designed 1400 m
to detect neutrinos ofall flavors at energies
from 107 eV (SN) to1020 eV2400 m1200 mIceTopIceTop
160 tanksfrozen-water tanks
2 OMs / tankFirst year deployment (Jan 2005)
4 IceCube strings (240 OMs)
8 IceTop Tanks (16 OMs)

IceCube
AMANDA

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

IceTop Tank deployed in 2004
10” Hamamatsu R-7081

Who are we ?
BartolBartolResearch
ResearchInst,
Inst,Univ
UnivofofDelaware,
Delaware,USA
USA Univ.
Univ.ofofAlabama,
Alabama,USAUSAPennsylvania
StateUniversity,
USA
Clark-Atlanta
University,
Pennsylvania State University, USA
Clark-Atlanta University,USA
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
ofKansas,
LBNL, Berkeley, USA
University of Kansas,USA
USA
UC
Southern
UCBerkeley,
Berkeley,USA
USA
SouthernUniv.
Univ.andandA&M
A&MCollege,
College,Baton
BatonRouge
Rouge
UC
Irvine,USA
UC Irvine, USA
Chiba
ChibaUniversity,
University,JapanJapan

University
UniversityofofCanterbury,Canterbury,
Christchurch,
Christchurch,New
NewZealand
Zealand

Université
UniversitéLibre
LibrededeBruxelles,
Bruxelles,Belgium
Belgium
Vrije
Universiteit
Brussel,Belgium
Vrije Universiteit Brussel, Belgium
Université
UniversitédedeMons-Hainaut,Mons-Hainaut,Belgium
Belgium
Universität
Mainz,
Germany
Universität Mainz, Germany
DESY-Zeuthen,
DESY-Zeuthen,Germany
Germany
Universität
UniversitätWuppertal,
Wuppertal,Germany
Germany

UppsalaUppsalaUniversitet,
Universitet,Sweden
SwedenStockholm
universitet,
Stockholm universitet,Sweden
SwedenKalmarKalmarUniversitet,
Universitet,Sweden
SwedenImperial
ImperialCollege,
College,London,London,UKUK
UniversityofOxford,
UK
University of Oxford, UK
Utrecht
UtrechtUniversity,University,Utrecht,
Utrecht,NLNL

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

Electromagnetic and hadronic cascades≈ 15 mdirection determinationby cherenkov light timing~5m

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

Primary Channels
1323
40
38
34
28
21
19
11

The highest energy event (~200 TeV)
TeV)

96
94
52
2

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 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

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 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

300 m

Color displays: LE
Primary Channels
2370
132501232631402762382893343023283154213285
193415113546
93677
63807
93938
44069
54199 24330 2

Excess of cosmic
neutrinos? Not yet ...

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

events / 197 d / 0.2

muon neutrinos (1997 B10-data)
accepted by PRL

102experiment
background MC-2

E signal MC (νe)

10

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

1-1

10
4

4.5

5

cuts determined by MC – blind analyses !

5.5
6
6.5log10(Ereco/GeV)

talk HE 2.3-5

Point source search inAMANDA II
Search for excess events in sky bins for up-going tracks
 697 events observed above horizon
 3% non-neutrino background for θ >5°
 cuts optimized in each declination bandPRELIMINA
RY

above horizon: mostly atmospheric ν‘sbelow horizon:mostly fake events

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

no clustering observed - no evidence for extraterrestrial neutrinos ...

Grid Search Results
2000-012002

17

Low state:

Mrk 421 sensitivity (AMANDA)

can be compared to ourbest upper limit(sensitivity shown here)
Fit of the measured
spectrum from HEGRA(Low)
Allowed range for theemitted flux
AMANDA sensitivity

about factor 2IceCube 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

Theoretical bounds andfuture
DUMAND test string
FREJUS

MACRO

opaque for neutronsatmo

NT-200AMANDA-97

ric ν µsphe

AMANDA-00
AMANDA-II

MPR
MPR

neutrons can escapeNT-200+

W&B
W&B

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

GIGA-ton detector!!

1015 eV

1016 eV1017 eVHow (E)HE events look like
1018 eV1019 eV1020 eVEHE MC Event examples
300 PeV taus

EHE (EeV or even higher) Neutrino Events
Arriving Extremely Horizontally• Needs Detailed Estimation• Limited Solid Angle Window(σρNA)-1 ~ 600 (σ/10-32cm2) -1(ρ/2.6g cm-3) -1 [km]Involving the interactions generating
electromagnetic/hadron cascadesµNµX e+e-Kyoto 2005

Energy loss profile in UHE/EHE
By JULIeT

Stochastic Loss
Initiating high energy
Cascades!

Products

νeνeνµντe/γ

Weake/γ

τππ
Weak

ντµτ

WeakνµIncomingµWeak

Weak

Weak

Pair

PhotoNucl.

Cascades

Decay

Decay
Weak

Decay

Decay

Pair/decay
Pair
Bremss
Decay
Weak

Pair
Bremss
Decay

Decay
Pair

Decay

Pair

PhotoNucl.
CascadesGZK spectrum @ IceCube depth
Upward-going

Downward going!!

Atmospheric muon! – a major backgrond
But so steep spectrum
Kyoto 2005

Down-going events dominate…
Atmospheric µ is attenuated faster…
11000mUp

Down

2800 m
1400 mKyoto 2005

EHE events!

νDownward１．４ｋｍlepton
e +e －γγ

Ice１ｋｍRockν１ｋｍe +e －γπ±

leptonUpward νSignal(GZK) Vs Atm µVery Preliminary

MC Truthnoisesignal

MC TruthSignal(GZK) Vs Atm µFirst Guess

Very Preliminary# of Hit

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

We MEASURE energy
deposit in km3
dE/dX~βE∆E~∆XbE
R<300m
300m <R<500m
500m <R<600m
600m <R<700m
700m <R

Energy Reco algorithm
under development

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

IceCube : The Present status~10 strings will be being deployed now!

ν detection by EAS
HiRes/Auger etc

Yoshida et al ApJ (1997)~ IceCubeCharged Particle
Astronomy?
E>>10 EeV  ∆ θ ~ a few deg

29th ICRC Pune

Event cluster > 40 EeV

No significant excess: AGASA’s triplet Pch ~0.28(Westerhoff, this conference)29th ICRC Pune

AGASA triplet story

HiRes stereo event

606060°°

180°
180°

170°
170°

One event added – BUT below 40 EeV!!
(Westerhoff, this conference)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.
#CRsBinSize#PairsProb.

AGASA >48 EeV
Yakutsk >24 EeV

652.5°°

8< 10-4

HiRes > 24 EeV

662.5°°

01.00

AGASA >48 EeV
Yakutsk >24 EeV

652.9°°

810-4

no cut

HiRes > 24 EeV

662.9°°

1.70

Catalog: Veron (10th Ed.) BL Lacs

AGASA > 40 EeV

572.5°°

12.02

HiRes > 40 EeV

272.5°°2.78

HiRes > 10 EeV

2710.8°°1010-3Magnitude

Redshift

6cm Radio Flux

#Obj.

Catalog: Veron (9th Ed.) BL Lacs

CR Sample22
m < 18z > 0.1 orunknown

S6cm > 0.17 Jy

Catalog: Veron (10th Ed.) BL Lacs
correlated with EGRET sources
no cutno cut14156
m < 18no cutno cutthCatalog: Veron (10 Ed.) BL Lacs156
m < 18no cutno cutGorbunov et al., JETP Lett. 80 (2004) 145.

(Finley, this conference)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 $10Neutrino 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。