UHE Neutrino Astronomy Summary on International UHE Neutrino

at Beijing

Zhen Cao IHEP, Beijing, China

Annual Conference of Chinese HE-Phys. SocietyGuilin, Oct., 2006

Outline

• Motivation and the workshop

• Searches for UHE neutrino with Existing Experiments

• Status of Constructing Neutrino Projects

• Updates on UHE Neutrino Related Physics

• Outlook

Motivation & the Workshop

• Taipei2002 workshop successfully discussed UHE neutrino detection using a mountain as a neutrino converter and C-telescope array to detector neutrino induced air showers

• Enormous progresses in experiment, detector R/D and theory since then

• A new Workshop was held in IHEP, Beijing, April 23rd to 26th

• About 50 people from US, France, Italy, Span, Taiwan and Mainland China attended the workshop

• About 40 experimentalists and 10 theoreticians showed up

Search for UHE Neutrino

• AUGER Experiment at Argentina

(south hemisphere)• HiRes Experiment at Utah, US

(north hemisphere)

How to: horizontal & low altitude events

Experiment: aperture>10000km2

E >1EeV

905 surface detector stations deployed

Three fluorescence buildings complete each with 6 telescopes

AUGER: March 2006 ~ 1000 stations

Fluorescence Detector Building at Los Leones

M. Roth et al., Karlsruhe

FD search

Event 767138

= 87.6 = -134.9E ~ 30 EeV/dof =1.7NTanks = 37

SD search

Falltime vs Risetime (2 cuts)S ≥ 15 VEM & r ≥ 500 m

θ ≥ 70 deg.

θ ≤ 45 deg.

Neutrino candidates should have θ ≥ 70 deg and should show up here.

No events up to now!

For E>1 EeV

• Both Auger and HiRes have not seen any neutrino event yet

• More focused analyses are going on

AMANDAII results @ lowerenergiesHow to:

C. Spiering

Constructing Neutrino Projects

• IceCube

• ANITA

• Antares

• Nemo

• CRTNT

• Nutel

• No report from NT200+, Nestor and Ashra

Second Generation Neutrino Telescopes

Eμ> 5-100Gev Aeff.~0.1-1km2

AMANDA - IceCube

BAIKAL

NESTOR

NEMO

ANTARES

IceCube

R/D Neutrino Telescopes

Eμ> 200Tev Aeff.>60km2

NuTel

ASHRA

CRTNT

ANITA

ANITA ANITA (ANtarctic Impulsive Transient Antenna)(ANtarctic Impulsive Transient Antenna)

Each flight ~15 days –

or more

32 quad-ridged horn antennas, dual-polarization, with 10± cant

Downgoing - not seen by payloadUpcoming – absorbed in the earth

! ANITA sees “skimmers”.

Anita-liteAnita-lite• Two independent analyses

modeled time dependent pulse on measured noise

• Designed cuts to select Askaryan-like events– # cycles in a waveform

– Integrated power

– Time coincidence between channels

– Reduce noise with cross-correlation analysis

• Both analyses find analysis efficiency ~50%• ANITA-lite strongly constrains

Z-burst models

ES&S baseline (min)Kalashev, et al., saturate all bounds (max)

Stanford Linear Accelerator Calibration• ANITA is going to SLAC for 2 weeks of beam time in End Station A

during June 2006– Full-up system calibration with actual Askaryan impulses from Ice– Uses one of SLAC’s largest experiment halls (End Station A)

250’x200’ w/ 50’ crane– Build 1.6 x 1.6 x 5 m ice cube by stacking blocks, “zamboni” each

surface before stacking, refrigerate• Will provide amplitude, phase, polarization, temporal, and spectral

calibration of the antenna array, including all structure• Excellent opportunity to calibrate the simulation• Payload will be shipped to Antarctica from California after the SLAC test

© F. Montanet

• 12 lines• 25 storeys / line• 3 PMTs / storey• 900 PMTs

~70 m

100 m

350 m14.5 m

Submarine links

JunctionBox

40 km toshore

Anchor/line socket

a storey

2500m depth

ANTARES Line 1

14 Febuary 2006

The first muon!

This is the first

muon recorded with

this first Antares

line and

reconstructed

Next steps and future

• Completion of the Antares detector– 12 full lines + an instrumented line by the end

of 2007– Line assembly in parallel in two labs

The NEMO Phase 1The NEMO Collaboration is undergoing the Phase 1 of the project, installing a fully equipped

deep-sea facility to test prototypes and develop new technologies for the km3 detector.

Shore laboratory at port of Catania

e.o. cable from shore

TSS Frame

To be completed in 2006

Junction Box

NEMO mini-tower(4 floors)

Deployed on Jan 2005

underwater e.o. cable

Underwater test site: 25 km E offshore Catania at 2000 m depth

Realizaton of a system hosting all key elements for the km3 detector:

Mechanical structures; Optical and environmental sensors; Electronics; Data

transmission system; Power distribution system; Acoustic positioning system;Time

calibration system

Sea operations January 2005

The NEMO Phase 1: the underwater station

TSS Frame

Junction Box

NEMO mini-tower(4 floors, 16 OM)

300

m

Mini-Tower compacted

Mini-Tower unfurled

15 m

Al alloy

Buoy

e.o. connections

Neutrino Telescopes status

AMANDAICECUBE

Mediterraneankm3

BAIKAL

DUMAND

Pylos

La Seyne

Capo Passero

DUMAND R&D - finished

BAIKAL, AMANDA - taking data

ANTARES, NEMO, NESTOR - under construction / first data

ICECUBE, Mediterranean km3 - next generation

There are strong scientific motivations that

suggest to install two neutrino telescopes in

opposite hemispheres :

• Full sky coverage

• The Universe is not isotropic at z<<1

• Observation of transient phenomena

• Galactic Center only observable from

Northern Hemisphere

Towards the Mediterranean km3Electro-optical cable: construction anddeployment

Data transmission system

Underwaterconnections

Detector:design and constructiondeployment and recovery

Power transmission system

Electronics

Power Distribution

Acoustic positioning•DS KM3NeT funded (9 M€) for 3 years (started in Feb 2006)DS KM3NeT funded (9 M€) for 3 years (started in Feb 2006)

•Antares, Nemo, Nestor join their effortsAntares, Nemo, Nestor join their efforts

CRTNT Experiment Status

• Site selection is done• Two prototype telescopes are

on the way to YBJ for testing• Full scale experiment (16

telescopes): 2008

How to detect with a mountain

PC104

±LV

RCP

Telescope control: remote control & monitoring of door open/close, LV & HV turn on/off

32 FADC （ 10bit) 8 APGA

Camera: 4x4 sub-cluster & BP DAQ

data bus PC104(linux)

Single Channel Trigger• sky noise background: 40 photon/μsec/m2

• single channel trigger: signal/noise ratio>4σ• 320 ns running widow• 3 histories of 6μsec per event stored

Opening/closing doors

Balikun vs. Wheeler Peak

Mt. Balikun, Xinjiang, China

Mt. Wheeler Peak, Nevada, USA

宇宙线中微子望远镜（ CRTNT ）实验

16 台望远镜组成四个阵列探测超高能中微子站址：新疆哈密北 130KM 巴里坤山视场：南纬 35~49 度 X64 度水平方位角能量范围： >100TeV( 中微子 ), >0.1EeV( 宇宙线 )

普通宇宙线簇射

中微子引起的空气簇射

新物理相关的空气簇射

F C

> 6 triggered pixels per telescope per event

Examples: triggered τ & CR event

Nutel Status: • NuTel is an experiment dedicated to Earth

skimming / mountaing watching• The PeV cosmic rate is ~ 1 event/year• The cost is low: O(1) million US dollars to build it• Very good project for training students• However, lack of funding support in last two years• Ceased collaboration with ASHRA last year• Look for new funding support from university this

spring, if succeed will start the optics this summer• Schedule: prototype deployment in ~2007-2008

for initial observation

Schematics of electronics

Trigger

Hamamatsu8x8 MPMT

16-channelspreamplifier

DAQ

PMT Preamp.

32 – channels Data Collection Module in cPCI

10 bit x40 MHzADC

FADC

bufferRAM

Triggerdaisychain

cycleRAM

Signal-sharing plate

2 m cable

HV powersupply

Front-end electronics Inside cPCI (PXI) chassis

4 preamplifier boards and signal- sharing plate are connected to one MAPMT

Holes for mechanical purposesin future

Sensitivity Summary

Defined as reachable upper limit of fluxAssume F(En) = F0 En-2

Assume no signal in 2 years of observationFeldman-Cousin method for upper limits: 2.44 signal events CRTNT

Updates on Physics

• Traditional Physics Topics– Diffusive flux from AGN, GRB and GZK

• Progresses on Galactic Sources• 近距离河内脉冲星对超高能中微子的贡献，仅次于

AGN的贡献，成为北半球观测站的重要观测目标！ L.Zhang (2006)• SWIFT: near-by (Z<0.033) GRBs 500x more than

predicted, neutrinos are more energetic (N.Gupta&B.Zhang, 2006)• Cosmogenic neutrinos with IR background (T.Stanev on CRIS, 2006)• New Physics beyond SM• New simulation tool for neutrino detection

GX339-4SS433

Crab

VELA

South Pole North hemisphere

• The whole sky coverage needs two telescopes in different Hemispheres

• The Galactic Centre is observable only from the Northern Hemisphere

GX339-4SS433

Crab

VELA

Galactic Centre

HESS data

HESS Sources

Observable from the km3

in the Mediterranean

MAGIC ： Micro Quasar （ Sci.312,23,2006)

HESS: Micro Quasar （ Sci.309,746,2005)

γ-burst

Cosmogenic on IR background

T.Stanev on CRIS 2006

New Physics Beyond SM

• N cross section may be different at UHE

• Super symmetry

• Dark Matter: sterile neutrinos

• Cosmos distance Oscillation: – :e:=1:1:1 ?

Stau??

Outlook

• Cosmogenic Neutrinos: 10x(IceCube aperture)– IceCube: radio and acoustic detector array– ANITA– SALSA

Hybrid IceCube+Radio+Acoustic

• Simulations* have been made of a hybrid detector consisting of– IceCube plus 13 “outrigger”

strings (×)– 91 additional radio/acoustic

holes with 1 km spacing (o)• 5 radio receivers 200-600

m• 300 acoustic receivers, 5-

1500 m• 2 acceptance, hadronic shower

only (LPM stretches EM showers), Esh = 0.2E

*See D. Besson et al., ICRC 2005

Saltdome Shower Array (SalSA) concept

1

2

3

4

5

6

7

Depth (km)

Halite (rock salt)• L(<1GHz) > 500 m w.e.• Depth to >10km• Diameter: 3-8 km• Veff ~ 100-200 km3 w.e.• No known background• >2 steradians possible

Antenna array

Qeshm Island, Hormuz strait, Iran, 7km diameter

Isacksen salt dome, Elf Ringnes Island, Canada 8 by 5km

Salt domes: found throughout the world

• Rock salt can have extremely low RF loss: as radio-clear as Antarctic ice• ~2.4 times as dense as ice• typical: 50-100 km3 water equivalent in top ~3km ==>300-500 km3

sr possible

Summary

• AMANDAII, HiRes & Auger have not seen any UHE so far

• Many UHE -telescopes are constructing and aiming at AGNs & Galactic sources

• Exciting physics including SM and beyond

• Next generation -telescopes are targeting “guaranteed” UHE cosmogenic neutrinos