kilometer-scale neutrino observatories

AMANDA: Proof of Concept

• • •

since 1992 we have deployed with more than 750 24 strings photon detectors (basically 8-inch photomultipliers).

R&D detector for proof of concept: 375 times SuperK instrumented volume with 1.5% the total photocathode area.

IceCube: 45 times AMANDA II instrumented volume with 7 times the total photocathode area.

IceCube

IceTop

• • • •

80 Strings 4800 PMT Instrumented volume: 1 km3 (1 Gton) 1400 m IceCube is designed to detect neutrinos of all flavors at energies from 10 7 eV (SN) to 10 20 eV 2400 m AMANDA South Pole Runway

South Pole

AMANDA– 1 mile deep

South Pole

Dark sector AMANDA Skiway

Dome

IceCube Planned Location 1 km east

South Pole

Dark sector

AMANDA

Skiway Dome

IceCube

µ-event in IceCube

300 atmospheric neutrinos per day

AMANDA

II

IceCube : -> Larger telescope -> Superior detector

1 km

E µ = 6 PeV

Muon Events

E µ = 10 TeV Measure energy by counting the number of fired PMT.

(This is a very simple but robust method)

Cherenkov light from muons and cascades muon cascade: e or

t

Reconstruction

• Maximum likelihood method • Use expected time profiles of photon flight

times

AMANDA Event Signatures: Cascades



CC electron and tau neutrino interaction:



(e,

t

,) + N



(e,

t

) + X



NC neutrino interaction:



x + N

 

x + X Cascades

Cascade event

• the length of the

e cascade is small compared to the spacing of sensors.

• roughly spherical

density distribution of light.

• 1 PeV ≈ 500 m

diameter, additional 100 m per decade of energy

• linear energy

resolution



e + N --> e- + X Energy = 375 TeV

PeV

t

(300m)

 t t t

decays

Neutrino ID (solid) Energy and angle (shaded)

•

Filled area: particle id, direction, energy

•

Shaded area: energy only

enhanced role of tau neutrinos:

• cosmic beam: 

e =

 m

=

 t

because of oscillations

•  t

not absorbed by the Earth (regeneration)

• pile-up near 1 PeV

where ideal sensitivity

IceCube

• start 02 • first strings 04 • completed 09

Amanda (3-reel) and ICECUBE (1-reel) Drill Drilling

Drilling

ICECUBE

03-04 04-05 05-06 06-07 07-08 08-09 09-10

Schedule and Cost

drill equipment to Pole first strings (proof that 16/season are feasible, prepare 10 full strings) 16 strings 16 strings 16 strings 16 strings remaining strings Overall cost with personnel, contingency, overhead: ~ 250 M$ Detector: ~ 55 M$ Logistics, including drilling: ~ 40 M$

evolution of read-out strategy -

timing - dyn. range - no x-talk - easy calibration

-

cost - robustness - dynamic range 01/02 - 03/04: Equipping all Amanda channels with FADCs to get full waveform information (IceCube compatibility)



better reconstruction, particularly cascades and high energy tracks

Assembled DOM

IceCube has been designed as a discovery instrument with improved :

•

telescope area ( > 1km 2 after all cuts)

•

detection volume ( > 1km 3 after all cuts)

•

energy measurement: secondary muons ( < 0.3 in ln E) and electromagnetic showers ( < 20% in E)

•

identification of neutrino flavor

•

Sub-degree angular resolution (< unavoidable neutrino-muon misalignment)

AMANDA

•

AMANDA collected > 3,000



’s

•

4 more every day on-line

•

neutrino sensitivity has reached



=

g •

> 300,000 per year from IceCube

•

race for solving the CR puzzle is on!

conclusions

•

nu astronomy reached ~ 0.1 km 2 year

•

will reach km-scale in < 5 years

•

northern hemisphere detectors soon

•

EeV detectors over similar time scale

•

if history repeats, I did not tell you about the science !!!

• • • • • • • • • • • • • • • • • • • • • • • • •

The IceCube Collaboration

Bartol Research Institute, University of Delaware BUGH Wuppertal, Germany Universite Libre de Bruxelles, Brussels, Belgium CTSPS, Clark-Atlanta University, Atlanta USA DESY-Zeuthen, Zeuthen, Germany Institute for Advanced Study, Princeton, USA Dept. of Technology, Kalmar University, Kalmar, Sweden Lawrence Berkeley National Laboratory, Berkeley, USA Department of Physics, Southern University and A\&M College, Baton Rouge, LA, USA Dept. of Physics, UC Berkeley, USA Institute of Physics, University of Mainz, Mainz, Germany Dept. of Physics, University of Maryland, USA University of Mons-Hainaut, Mons, Belgium Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, USA Dept. of Astronomy, Dept. of Physics, SSEC, PSL, University of Wisconsin, Madison, USA Physics Department, University of Wisconsin, River Falls, USA Division of High Energy Physics, Uppsala University, Uppsala, Sweden Fysikum, Stockholm University, Stockholm, Sweden University of Alabama, Tusceloosa, USA Vrije Universiteit Brussel, Brussel, Belgium Chiba University, Japan Imperial College London, UK Utrecht University, Utrecht, The Netherlands Universidad Simon Bolivar, Caracas, Venezuela University of Canterbury, Christchurch, New Zealand

super-EeV detectors

GZK Cosmic Rays & Neutrinos

• cosmogenic neutrinos are guaranteed • fluxes may be larger for some models, such as topological defects

p +

g

CMB

 p

+ n

Radio Emission from neutrino induced electromagnetic cascades • Electromagnetic cascades: electron-positron pairs and (mostly) gammas  electrically neutral, no radio emission.

• Compton scattering of photons on atomic electrons creates negative charge excess of ~ 20% • Negative charge radiates coherently at MHz ~ GHz  Power = Energy 2 • Askarian effect demonstrated at SLAC: consistent with calculations

RICE Radio Detection in South Pole Ice

Neutrino enters ice Neutrino interacts •

Installed ~15 antennas few hundred m depth with AMANDA strings.

Cube is .6 km on side Antenna & Cable

• Tests and data since 1996.

• Most events due to local radio noise, few candidates.

• Continuing to take data, and first limits prepared.

• Proposal to Piggyback with ICECUBE

Two cones show 3 dB signal strength

TauWatch Using Mountains to Convert ν

τ 3/02 Workshop in Taiwan, see http://hep1.phys.

ntu .edu.tw/vhetnw also, HiRes, Auger….

ANITA : Radio from EeV



’s in Polar Ice

• Antarctic Ice at

•

f<1GHz, T<-20C largest homogenous, RF-transmissive solid mass in the world

Antarctic Impulsive Transient Antenna (ANITA) Solar Panels ANITA Gondola & Payload Antenna array Cover (partially cut away) • ANITA Goal: Pathfinding mission for GZK neutrinos • NASA SR&T start expected this October, launch in 2006

Ocean Acoustic Detection

New Stanford Effort using US Navy Array

US Navy acoustic tracking range in Tongue of the Ocean, Atlantic

Hydrophones 1550-1600 m deep pancake beam pattern

G.Gratta, atro-ph/0104033

Summary on Technology

    

Over 5 years, Amanda has evolved into a 30.000 m 2 neutrino telescope Construction and improvement hand in hand Developed and tested IceCube technology Detailed measurement of ice down to 2.4 km Clear record in performance, reliability, time schedule and cost



We know that we can build a km3 telescope

Summary Amanda Physics

      

Diffuse flux: Best limits. Entering interesting range.

EHE fluxes: 0.3 km 2 at EeV. A-II testing EeV blazar models.

Point sources: Best limits. Testing first models.

GRB: sensitivity after 4 years close to predictions Relativistic Magnetic Monopoles: Best limits (0.05 x Parker bound) WIMP search: high mass limits ~ Underground limits Monitoring Galaxy for SN bursts



Cosmic Ray Composition at knee

... and IceCube Physics

      

Diffuse flux: sensitivity nearly factor 10 below WB limit EHE fluxes: IceCube testing some GZK models Point sources: sensitivity ~ 10 -12 cm -2 s -1 for > 1 TeV Many models predict up to few tens of events/year GRB: 10-100 events per year. Test WB model Rel.Magnetic Monopoles: < 1/1000 Parker bound) WIMPs: complementary to future direct search expts.

SN monitoring up to LMC. Triangulation ?



Cosmic ray composition at knee