The current statusof the neutrino telescopeexperiments

K. Mase, Chiba Univ.

2008.06.27 22nd Neutrino seminar

K. Mase■ The neutrino astronomy
Want to open the neutrino astronomy

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 AGNs GRBs Cosmic ray origin

 Dark Matter particle physics

 GZK neutrinos
 Supernova
2008.06.27 22nd Neutrino seminar Exiotic(monopole, Q-ball, etc…)
K. Mase■ Neutrinos should be there…
The source of cosmic rays will be the neutrino source.

p  n   

Waxman-Bahcall limit・c 2 dN CRE 2    Z t H
E CR84
dE CR
ε: fraction of energy going to neutrinos

If ε=1, WB limitE2   2 108 GeV cm2 s1sr 1Baikal
AMANDA IIWB limit

Full IceCube 1 yr (expect)

The sensitivity of 1 km3 size detector

 is lower than WB limit.

2008.06.27 22nd Neutrino seminar

K. Mase■ But, where?
Where are cosmic rays generated?
→ we don't know yet(We know where electrons are accelerated)→ Neutrinos can tag it.

Konopelko et al., ApJ 597(2003) 851
Mkn421
Note: if there is a photo-pion production,roughly same amount neutrinos andgammas are generated.
Even more if we consider gamma-ray
absorption.
The flux (>1TeV) can be 10-11(cm-2s-1)
and detectable with 1 km 3 detector.
(A. Aharonian et al., MNRAS 387,3, 1206-1214, 2008)

Fitted with SSC model

2008.06.27 22nd Neutrino seminar

K. Mase The detection
method2008.06.27 22nd Neutrino seminar@NeutrinoK. 2008
Mase…Dumand

Optical Neutrino Telescopes
Nemo

Lake Baikal
Antares

Nestor

KM3Net2008.06.27 22nd Neutrino seminar

AMANDA /IceCube
K. MaseNT-200■ Baikal deployed in lake Baikal
 Long history
 1.4 km depth
 1980: R&D started
 1993: NT-36 (36 PMTs with 3 strings)

 1998: NT-200 completed (192 OMs (14.6''PMT), 8 strings ~105 m3)

J. Carr @ Neutrino 2008 2005: NT-200+ (NT-200 + 3 outer strings)
completed 2006/7: R&D of Gigaton VolumeDetector(GVD)

GVD

 2008: a prototype of GVD installed (testingnew PMTs and 250M SPS FADC)

91-100 strings with 12-16 OMs
Δlog(E)~0.1, Δθ<5 deg.
2008.06.27 22nd Neutrino seminar

K. Mase■ NESTOR (Neutrino Extended Submarine
Telescope with Oceanographic Research)

J. Carr @ Neutrino 2008

15'' PMT→ Going to KM3NeT and NuBE NESTOR (GRB search)
2008.06.27 22nd Neutrino seminar

K. Mase■ ANTARES (Astronomy with a Neutrino
Telescope and Abyss environmental RESearch) deployed in the Mediterranean sea
 2.5 km depth
 1996-2000: R&D
 2001: The deployment started
 The construction completed (2008/5/30)(12 lines ~ 107 m3)

 3x25x12=900 OMs (10'' PMT) 300-1100 MHz ARS
 technology proven. (although 12% of thedetectors had problems, but can be fixed.)

15m

 ready for KM3NeT

350m

70m
2008.06.27 22nd Neutrino seminar

K. Mase■ ANTARES[astro-ph] 0805.2545v2

J. Carr @ Neutrino2008

25m

Good angular resolution

J. Carr @ Neutrino 2008

500m

2008.06.27 22nd Neutrino seminar

K. Mase■ NEMO (NEutrino Mediterranean Observatory) R&D for 1 km3 detector
 deployed in the Mediterranean sea
 phase1: 2003-2007 @ LNS test site (2 kmdepth)
A mini-tower (300 m) deployed Dec. 2006

(4 floor, 16 OMs, 10'' PMT)

J. Carr @ Neutrino 2008

 Some problems with the buoy phase2: 2006-2009 @ Capo Passero site
(3.5 km depth) A full tower (750 m, 16 floor) under construction (plan to be completedat beginning of 2009)2008.06.27 22nd Neutrino seminar

K. MaseThe AMANDA Detector
AMANDA

677 OMs on 19 strings (~107m3)
Hamamatsu 8” PMT inglass pressure vessel
Several readout systems(electrical, fiber-optic)DAQ electronics on surface

top view
200 m

Deployed in stages:
AMANDA-II
complete in 2000
Optical Module

2008.06.27 22nd Neutrino seminar

K. Mase■ The IceCube experiment to detect VHE neutrinos from astrophysicalsources deployed in the Antarctica glacier~1 km

 >70 strings

IceTop >4200 photo-multiplier tubes (PMTs)
 Detector volume: 〜1km3
 ATWD 300MHz, effectively 16 bits
 3 different gains (x16, x2, x0.25)
 10 bits FADC for long duration pulse

AMANDA-II

IceCube Neutrino energy of above 100 GeV isdetectable.

 40 strings are deployed so far, and taking
data as the biggest neutrino detector.
 full detector @2009/10

DOM

HV board

Mu metal cageFlasher board

Delay board

Main board

10 inch PMT
2008.06.27 22nd Neutrino seminar

Optical gel

〜1 km

1km3
K. Mase■ Particle identification

Particle identification possible from the topology
2008.06.27 22nd Neutrino seminar

K. Mase■ Bright event
IC-40

Estimated energy: 866 PeV(by IceTop (preliminary))In-ice detector also give theconsistent energy

2008.06.27 22nd Neutrino seminar

K. Mase KM3NeT
European community is proposing to build 1 km3 volume detector in
Mediterranean sea.
Mostly from ANTARES, NESTOR and NEMO.
• Design Study (2006-2009):
aims at developing a cost-effective designfor the construction of a 1 km 3 neutrino
telescope• Preparatory Phase (2008-2010):
preparing for the construction by defining
the legal, financial ad governance issues
as well as the production plans of thetelescope components(from E.Migneco@Neutrino2008)2010: IceCube complete

Design goal
 Life time 10 years without major maintenance, construction anddeployment < 4 years Angular resolution 0.1 deg
 Substantially better sensitivity than IceCube(from E. Migneco@Neutrino2008)

See more the KM3NeT conceptual design report→ http://www.km3net.org/CDR/CDR-KM3NeT.pdf
2008.06.27 22nd Neutrino seminar

K. Mase■ Point source search by AMANDA II
Unfortunately, no signal so far…

Search circle: 2.25-3.75 deg.

Angular resolution: 1.5-2.5 deg.

Search for clustering in northern hemisphere• compare significance of local fluctuation toatmospheric expectations

2000-2006

Random events

Preliminaryδ=90º6595 events

Max Significanceδ=54º, α=11.4h
3.38ζ

3 yr max significance
3.73ζ → 1.5ζ

2000-2004

24h0h02008.06.27 22nd Neutrino seminar1234

5 yr max significance3.74ζ → 2.8ζ

5SignificanceK. Mase■ Point source search by IceCube
IC-9
233 ν in 137 days
Consistent with atmospheric νNo signal

IC-22~5000 ν in 250 days
Resolution 1.5 deg.

2000-2004
5 times better sensitivity than IC-9
(Better than AMANDA 5 years!)
Soon to open the blinded box
Diffuse result is also coming
Scrambled in right ascension2008.06.27 22nd Neutrino seminar

K. Mase■ Point source sensitivityPreliminary
Random events
IC-9

ANTARES 1yr (expect)
AMANDA (7yr) IC-22 (expect)

2000-2004
KM3NeT 1yr (expect)

2008.06.27 22nd Neutrino seminar

Full IceCube 1yr (expect)

K. Mase■ Diffuse neutrinos
Even though we can’t resolve signals from each source, we canintegral signals in all sky and should see some excess.

2000-2004

BaikalAMANDA IIANTARES 1 yr (expect)

Full IceCube 1 yr (expect)

But, no excess so far
2008.06.27 22nd Neutrino seminar

K. Mase■ The cosmogenic neutrinosp 2.7K     X     e   's "guaranteed source" ee2008.06.27 22nd Neutrino seminar

K. Mase WIMP Search
10

Neutralino scatters and loses energy
Becomes trapped in gravity well
Annihilates to pairs of SM particles
SM particles decay producing n10 + 10  W +W-

W

AMANDA 2003
(sys. not included)

10 + 10  l+l-, qq, W +W-, Z0Z0
10 + 10  H01,2 H03, Z0H01,2, W +H-, W-H+

2008.06.27 22nd Neutrino seminar

K. Mase■ IceCube Deep Core

Extend IceCube sensitivity to neutrinos withenergies below a few hundred GeV
 Replacement for AMANDA Six strings with 60
high-QE PMTs each (HAMAMATSU
super bialkali)
 Use very clear ice at bottom of IceCube



Already budgeted2008.06.27 22nd Neutrino seminar

Measured at Chiba Univ.

K. Mase■ SN Neutrino Search
AMANDA

Bursts of low-energy (MeV) neutrinos
from core collapse supernovae

e+ p  n + e+

The produced positron is emitted almost isotropicallyDetection via rate increase of the dark noise rate

Count rates

30 kpcIceCube- AMANDA sees 90% of the galaxy- IceCube will see out to the LMC(Large Magellanic Cloud, ~50 kpc)

Simulation(IceCube)

O(10cm) long tracks

0510sec

Record noise rate in 500 ms (~6x105 event/bin,stat. err. very small)No pointing, no energy
2008.06.27 22nd Neutrino seminar

SNEWS (SuperNova Early Warning System)
is a collaborative effort among Super-K, SNO,LVD, KamLAND, AMANDA, BooNE andgravitational wave experiments
K. Mase Radio detectors
 1962: Askaryan predicted coherent radioemission from excess negative charge in an
EM shower (~20% due to mainly Comptonscattering)Askaryan effect 2001: confirmed at SLAC
Saltzberg& Gorham et al. PRL 2001

 several experiments to detect EHECRsusing Askaryan effect:• Parkes 64 m dish

• RICE• GLUE• 64m Kalyazin telescope• FORTE• ANITA2008.06.27 22nd Neutrino seminar

Gorham et al. PRD 2003

K. Mase■ ANITA (Antarctic Impulsive Transient Antenna)
 detect radio wave from showers using Askaryaneffect view: 1.5 M km2 ! (Tokyo-Hakata: 880km)

 sensitive: 0.2-1.2 GHz
 2003-4: ANITA-lite (2 hones)

 2006-7: full ANITA
35 days, 3.5 orbits, good data: ~10 days
 2008-9: ANITA 2x5 event rate (by mainly lowering the threshold)2008.06.27 22nd Neutrino seminar

K. Mase2008.06.27 22nd Neutrino seminar

K. Mase2008.06.27 22nd Neutrino seminar

K. Mase2008.06.27 22nd Neutrino seminar

K. Mase■ ANITA sensitivity

preliminary

2008.06.27 22nd Neutrino seminar

K. Mase■ AURA (Askaryan Uunder ice Radio Array)surfacejunctionbox

 3 DRMs (digital radio module) deployed(2006-7) in ice at IceCube site

Countinghouse broad dipole antena centered at 400 MHz
 The R&D is in progress

A signal candidate

Digital radio module
Toantenna

Toantenna

2008.06.27 22nd Neutrino seminar

K. Mase Acoustic Detectors
A pressure wave is generated instantaneous following a sudden deposition ofenergy in the medium (neglecting absorption: O(10 km) at 10 kHz )2008.06.27 22nd Neutrino seminar

K. MaseSPATAS detector

 Acoustic Detectors (cont'd) There are many R&D for the use
ice• SPATAS (@ IceCube)• SAUND• ACORNE• AMADEUS (@ ANTARES)• NEMO-OnDE (@ NEMO)• @Baikal measuring the midium property and noise.
 effort to reconstruct events
Measured noise by SAUND

2008.06.27 22nd Neutrino seminar

Measured event by ACORNE

K. Mase■ Hybrid Detector
Hybrid IceCube+Radio+Acoustic (IRA) ~100 km3 effective volume at
GZK energies
 ~100 strings on 1 km spacinggrid

2008.06.27 22nd Neutrino seminar

K. Mase■ How Kifune plot will be for VHE neutrinos?
Logscale

VHE neutrinos?

“Kifune plot” ©Rene Ong 2002
2008.06.27 22nd Neutrino seminar

K. Mase■ Summary
 Very high energy neutrinos should be generated
where the cosmic rays are generated.
 One neutrino source will open the astronomy.
 A 1 km3 detector can possibly detect it. (reachingthe WB limit) A detector having a larger effective volume is morefeasible to detect. The efforts are being made forsuch detectors.
Who will open it?

2008.06.27 22nd Neutrino seminar

K. Mase