The ICE 3 Experiment Thanks to O. Botner (Neutrino-2004)

The ICE3 Experiment

Thanks to O. Botner (Neutrino-2004)

D. BertrandIAP meeting 2004/12/02 2

Acceleration up to 1021 eV ? ~102 Joules

~0.01 MGUT

Dense regions with exceptionalgravitational force creating relativisticflows of charged particles, e.g.

•coalescing black holes/neutron stars•dense cores of exploding stars•supermassive black holes

Ultra high energy ’s are associated with the sources of high energy cosmic rays

p + p() e ,


Supernova Remnant in X-rays

Shock fronts

Fermi acceleration


Fermi acceleration

Jets

Black HoleAccretion Disk

Shock frontsActive Galactic Nucleus

(Artist impression)


IceCube – a ”next generation” observatory kilometer-scale successor to AMANDA

DistanceDistance LumLumnn >>

examplesexamples

4000 Mpc 1047 erg/s AGN 4000 Mpc

1052 erg/100s GRB

100 Mpc

5 1043 erg/s Markarians

8 Kpc 4 1035 erg/s

Pulsars, micro-

quasars

A 1 kilometer squared area is needed to see the

potential energetic sourcesCandidates for 10 events/year/km² ( ~ )


ICE3

Dark sector

AMANDA

Dome

Skiway

South Pole

Planned Location 1 km “west”

“North”


The ICE3 detector

• 80 strings• 17 m OM spacing• 125 m between strings• Geometry optimized for a detection range [TeV-PeV(EeV)]

• 160 frozen water tanks (2/string)• Ice cylinder (2 m diameter; 0.9 m height)• 2 OM’s each


AMANDA integrationAMANDA now runs with TWR• Data similar in structure to ICE3

• Work on a combined trigger

Position of 1st ICE3 strings• As close to AMANDA as possible• But … logistics and safety requirements

AMANDA• Calib. device for 1st ICE3 strings• + 20 ICE3 strings = powerful combined detector• Fully integrated low threshold subdetector of ICE3


VETO against All downward events E > 300 TeV with trajectories inside IceTop Larger events falling outsideCALIBRATION of angular response with tagged µMeasure Energy spectrum Chemical composition

Expect ~100 tagged air showers/daywith multi-TeV µ’s in Ice3

Muon survey of Ice3

Energy range 1015 eV - 1018 eV

IceTop+ICE3: 1/3 km².sr (for coincident tracks)


IceCube - Icetop coincidences

Cosmic ray physicsLarge showers with E ~ 100-1000 PeVwill clarify transition from galactic toextra-galactic cosmic rays

Showers triggering 4 stations give

~300 TeV threshold

Small showers (2-10 TeV)associated with the dominant background detected as 2-tank coincidences at a station.


Local digitization :

• Time stamp• Wave form• Buffer• Digital

transmission to surface on request

Optical sensor :10 inch Hamamatsu R-7081

mu metal cage

PMT

penetrator HV board

flasher board

DOMmain board

pressure sphere

optical gel

delay board

Digital Optical Module (DOM)

Local Controls :•HV•Discriminators•Global synchronization

Sampling at 300 MHz over 0.5 µsat 40 MHz over 5 µs

Dynamic range 200 p.e./15 ns 2000 p.e./ 5µs


AMANDA system

ICE3

AMANDA ICE3

Power consum. 2 MW 5 MWTime to 2400 m 120-140 h35-40 hFuel (gal/hole) 10000-12000 7000-8000 Set-up time 5 – 6 weeks18-25 d

Goals 18 holes/season 2450 m deep straight within 1m quality logged

Enhanced hot water drillAMANDA (3-reel) and ICE3 (1-reel) drill


ICE3 DAQ architecture

80 DOM hubs for thein ice devices

5 DOM hubs for ICETOP

DOM hub : • Industrial PC• Dual 1 GHz PIII processor• 2 GB memory• 250 GB hard-drive• dual 400W power supply for DOM’s


ICE3 physics performanceICE3 will be able to identifyo tracks from for E > 1011 eVo cascades from e for E > 1013 eVo for E > 1015 eV

Background mainly downgoing cosmic ray ’s(+ time coinc. ’s from uncorrelated air showers)• exp. rate at trigger level ~1.7 kHz• atm. rate at trigger level ~300/day

Rejected using direction/energy/flavor id temporal/spatial coincidence w. source

for E < 1 PeV focus on the Northern skyfor E > 1 PeV sensitive aperture increases w. energy

full sky observations possible

Eµ=10 TeV


Galactic center

E-2 spectrum After quality cuts and bgr suppression (atm µ reduction by ~106)

Further improvement expected

using waveform info

Median angular reconstructionuncertainty ~ 0.8

ICE3 effective area & angular resolution (µ)


Objective (after removal of atm µ background): Reject the steep energy spectrum of atm Retain as much signal as possible from a (generic) E-2 spectrum

Use optimized energy cut Eµ number of hit OM’sEµ= 6 PeV, 1000 hitsEµ= 10 TeV, 90 hits

Diffuse hard Eµ cutEµ > 100 TeV

Point sources softer Eµ cut

+ spatial correlation

Diffuse µ flux & Point sources


Assume generic flux dN/dE = 10 –7 E-2 (cm-2s-1sr-1GeV)Expect ~ 103 events/year after atm µ rejection~ 75 events/year after energy cut cf background 8 atm

atm v

signal

Sensitivity (1 y): 8.110-9 E-2

(cm-2s-1sr-1GeV)

blue: after atm µ rejectionred: after Eµ cut

Diffuse µ flux


Search cone 1 opening half-angle+ ”soft” energy cut (< 1 TeV)

Essentially background-free search :

Energy, spatial and temporal correlation with independent

observation For ~1000 GRB’s observed/yearexpect (looking in Northern sky only) Signal: 12 Background (atm ): 0.1 Sensitivity GRB (1 y):

~0.2 fWB

Sensitivity point sources (1 y):

5.510-9 E-2 (cm-2s-1GeV)

Steady point sources

Transient point sources – ex GRB


~10% in log(E/TeV)

IceTop veto on cosmics

C.O.G. insidearray

sensitivity to all flavors4 coverage

Cascades

~300m

“double bang”E = 1PeV

E << 1 PeV 2 cascades coincideE 1 PeV ”double bang”E >> 1 PeV ”lollipop” (partial containment, reconstruct track + 1 cascade)

E = 375 TeVe e

Lcascade ~10 m small cf sensor spacing”spherical” energy deposition

at 1 PeV, Øcascade ~ 500 m

For diffuse flux expect s

imilar sensiti

vity

in the ca

scade ch

annel as in th

e muon channel

Considerable im

provement of overall s

ensitivity


astro-ph/0401113 (Lundberg/Edsjö)WIMP orbits in the solar system

perturbed

Direct and indirect searches might not be directly comparable Past/present history of solar syst. Low/high energy tail of vel. distr.

Sun

Neutralino dark matter

Rates from the Earth affected

Rates from the Sun less affected


Many reviews – international and within the U.S. - strongly emphasize

the exciting science which can be performed with ICE3

In Jan 2004, the U.S. Congress approvedthe NSF budget including the full ICE3 MRE

Significant funding approved also in Belgium, Germany and Sweden

In Feb 2004, NSF conducted a baseline review “go ahead”

However … revised baseline preserving original scientific goals preserving current detector design straightforward upgrade path

ICE3 strings IceTop tanks4 8 Jan 200516 32 Jan 200632 64 Jan 200750 100 Jan 200868 136 Jan 2009

70+n 140+2n Jan 2010

Status of ICE3


1st challenge – successful deployment

of strings 2004/2005

ICE3 is for real ! - and moving ahead at full speedAMANDA experience provides for huge benefits

- both logistics-wise and for simulations/reconstructionICE3 is expected to be Considerably more sensitive than AMANDA Provide new opportunities for discovery With IceTop – a unique tool for cosmic ray physics

Data taking during construction First data augment AMANDA data

Later AMANDA an integral part of ICE3

Decision on total number of strings

summer 2006

Summary


Transmission of µ through the earth

TeV: use upward going muonsPeV: use horizontal eventsEeV: use events from above

AMANDA-II


Drill development on schedule for operation at Pole in Jan 2005

Instrumentation Production for the 4 string first season starts this summer

50% PMTs delivered – on schedule 3 DOM production sites

Wisconsin 290 1st season DESY 60 1st season Sweden 50 1st season

Spheres ordered – 40K depleted Benthos (dark noise ~0.8 kHz) DOM mainboard – designed @ LBNL tests OK DAQ S/W developed Data transfer DOM DOM Hub Data Collection prog tested Implementation for first season’s DAQ Cables – Ericsson, Sweden / JDR, Netherlands Preparing for analysis of early data (calibration, testing) 4 DOM’s are collecting IceTop data using test s/w

Status of ICE3


View of DOMs

IceTop tank with hood at the South Pole – Nov 2003

Documents

The ICE 3 Experiment Thanks to O. Botner (Neutrino-2004)