The IceCube High Energy TelesoThe IceCube High Energy Telesopepe

The detector elementsExpected SensitivityProject Status

Shigeru Yoshida

Dept. of Physics

CHIBA Univ.

ICRC 2003

The IceCube CollaborationThe IceCube CollaborationInstitutions: 11 US, 9 European institutions and 1 Japanese institution; ≈150 people 1. Bartol Research Institute, University of Delaware, USA2. BUGH Wuppertal, Germany3. Dept. of Physics, Chiba University, JAPAN4. Universite Libre de Bruxelles, Brussels, Belgium5. CTSPS, Clark-Atlanta University, Atlanta USA6. DESY-Zeuthen, Zeuthen, Germany7. Institute for Advanced Study, Princeton, USA8. Dept. of Technology, Kalmar University, Kalmar, Sweden9. Lawrence Berkeley National Laboratory, Berkeley, USA10. Department of Physics, Southern University and A\&M College, Baton Rouge, LA, USA11. Dept. of Physics, UC Berkeley, USA 12. Institute of Physics, University of Mainz, Mainz, Germany13. Department of Physics, University of Maryland, USA14. University of Mons-Hainaut, Mons, Belgium15. Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, USA16. Dept. of Astronomy, Dept. of Physics, SSEC, University of Wisconsin, Madison, USA17. Physics Department, University of Wisconsin, River Falls, USA18. Division of High Energy Physics, Uppsala University, Uppsala, Sweden19. Fysikum, Stockholm University, Stockholm, Sweden20. University of Alabama, USA21. Vrije Universiteit Brussel, Brussel, Belgium

South PoleSouth Pole

Dark sector

AMANDA

IceCube

Dome

Skiway

IceCubeIceCube

1400 m

2400 m

AMANDA

South Pole

IceTop

Skiway

80 Strings 4800 PMT Instrumented volume:

1 km3 (1 Gt) IceCube is designed to

detect neutrinos of all flavors at energies from 107 eV (SN) to 1020 eV

Design goalsDesign goals

IceCube was designed to detect to neutrinos over a wider range of energies and all flavors.

If one would wish to build a detector to detect primarily PeV or EeV neutrinos, one would obviously end up with a different detector.

Neutrino flavor

e

Log(ENERGY/eV)

12 18156 219

e

１．４ｋｍ

１ｋｍ

Upward

Ice

Rock ν

±πγ

ν

+e －e１ｋｍ

Downward

ν

γ

γ

+e －e

lepton

lepton

Eµ=10 TeV ≈ 90 hits Eµ=6 PeV ≈ 1000 hits

How our events look like

The typical light cylinder generated by a muon of 100 GeV is 20 m, 1PeV 400 m, 1EeV it is about 600 to 700 m.

Assembled DOMAssembled DOM

DAQ design: Digital Optical ModuleDAQ design: Digital Optical Module- PMT pulses are digitized in the Ice- PMT pulses are digitized in the Ice

Photomultiplier

Design parameters: Time resolution:≤ 5 nsec (system lev

el) Dynamic range: 200 photoelectrons/1

5 nsec (Integrated dynamic range: > 2000 p

hotoelectrons) (1.p.e. /10ns ~ 10^7G ~8mV 504V saturation500p.e. Digitization depth: 4 µsec. Noise rate in situ: ≤500 Hz Tube trig.rate by muons 20Hz

33 cm

DOM

Capture Waveform information (MC)Capture Waveform information (MC)

ATWD 300MHz 14 bits.

3 different gains (x15 x3 x0.5)

Capture inter. 426nsec

10 bits FADC for long duration pulse.

E=10 PeV

0 - 4 µsec

Events / 10 nsec

String 1 String 2 String 3 String 4 String 5

Photomultiplier:Photomultiplier: HamamatsuHamamatsu R7081-02 R7081-02

(10”, 10-stage, 1E+08 gain)(10”, 10-stage, 1E+08 gain)

• Selection criteria (@ -40 °C)• Noise < 300 Hz (SN,

bandwidth)• Gain > 5E7 at 2kV (nom. 1E7

+ margin)• P/V > 2.0 (Charge res.; in-situ

gain calibration)

• Notes:• Only Hamamatsu PMT meets

excellent low noise rates! • Tested three flavors of R7081.

DAQ DAQ Network Network

architecturearchitecture

McParland et. al. -- A Preliminary Proposal for the IceCube DAQ System Architecture -- DRAFT7

DOMPair

20 kB/sec

StringProcessor

N x 20 kB/sec

.

All Hits -0.6 MB/sec

80 Strings

String Subsystem:60 DOMs

N pairs

Event LAN100 BaseT

Total traffic: 1.6 MB/secString

CoincidenceMessages

GlobalTrigger Event Triggers /

Lookback Requests forall Strings - 0.8 MB/sec

EventBuilder

Built events ~ 1 MB/sec(all event builders)

SAN(Network

Disk Storage)

"DOMHUB"

Lookback Requests

String CoincidenceMessages - 170 kB/sec

Fulfill Lookback Messages 0.6 MB/sec

FulfillLookbackMessages

Online LAN100 BaseT

Total traffic: 1MB/sec

Proposed IceCube DAQ Network Architecture

String LAN100 BaseT

Total traffic: 0.6 MB/sec

OfflineData

Handling

Tape

Satellite

Custom design: 5000 DOMs,

2500 copper pairs, 800 PCI cards

(10 racks)

Off the shelf IT infrastructure, Computers, switches, disks

DAQ SoftwareDatahandling software

Digital Optical Module (DOM) Main Board Test Card

SPE Discriminator Scan – PMT SPE Discriminator Scan – PMT Pulses Input (71DB)Pulses Input (71DB)

450 500 550 600 650 700 750 800 850 900 95010

0

101

102

103

104

105

DAC 9

1400 V1500 V1600 V

SPE WaveformsSPE Waveforms

0 20 40 60 80 100 120 1400

10

20

30

40

50

60

70

80

90

100

ATWD Sample

AT

WD

Counts

ATWD-Ch1 at 1500V spe trigger

0 20 40 60 80 100 120 140-80

-60

-40

-20

0

20

40

ATWD Sample

AT

WD

Counts

ATWD-Ch0 at 1500V spe trigger

20 40 60 80 100 120

0

100

200

20 40 60 80 100 120

-20

0

20

20 40 60 80 100 120

0

100

200

20 40 60 80 100 120

-20

0

20

CH0

CH1

CH2

The big reel for the hotwater drillThe big reel for the hotwater drill

Angular resolution as a function of zenith angle

above 1 TeV, resolution ~ 0.6 - 0.8 degrees for most zenith angles

0.8°0.6°

Waveforminformationnot used.Will improveresolution forhigh energies !

Event rates for

-atmospheric

- AGN (E-2 flux 10 times below MPR bound and present exp. limits)

- atm. from 1 EAS

- atm. from 2 EAS

after trigger

after cuts toreject atm.background(Level 2)

Energy Spectrum Diffuse SearchEnergy Spectrum Diffuse Search

Blue: after downgoing muon rejectionRed: after cut on Nhit to get ultimate sensitivity

Energy Spectrum Point Source Energy Spectrum Point Source SearchSearch

Blue: after downgoing muon rejectionRed: after cut on Nhit to get ultimate sensitivity

cos

Aef

f /

km2

Effective area vs. zenith angle after rejection of background from downgoing atmospheric muons

Effective area vs. muon energy - after trigger- after rejection of atm - after cuts to get the ultimate sensitivity for point sources (optimized for 2 benchmark spectra)

Effective area of IceCube

E2dN/dE ~10-8 GeV/cm2 s sr (diffuse)E2dN/dE ~7x10-9 GeV/cm2 s (Point source)200 bursts in coincidence (GRBs – WB flu

x)

In three years operation…In three years operation…

ICRC 2003

For 5

dete

ction

Construction: 11/2004-01/2009Construction: 11/2004-01/2009

FY04:6

FY05:12FY06:16

FY07:16

FY08:16 FY09:14

AMANDA

SPASE-2 South Pole

Dome

Skiway

100 m

Grid North

Next season: Buildup of the Drill and IceTop prototypes

Project statusProject status

Approved by U.S. the National Science Board Startup funding is allocated. 100 DOMs are produ

ced and being tested this year. Assembling of the drill/IceTop prototypes is carrie

d out at the pole this season. Full Construction start in 04/05; takes 6 years to c

omplete. Then 16 strings per season, increased rate may be

possible.

ICRC 2003

ICRC 2003

Down-going events dominates…

1400 m

2800 m

11000mUp Down

ICRC 2003

Downward going!!

1 km2 year

ICRC 2003

Intensity of EHE Intensity of EHE and and

GZK model I(E>10PeV) I(E>10PeV) RATE [/yr/km2]

m=4 Zmax=4

Down 5.90 10-19 5.97 10-19 0.37

Up 3.91 10-20 6.63 10-20 0.03m=7 Zmax=5

Down 8.88 10-17 9.10 10-17 53.4

Up 5.72 10-19 9.73 10-18 4.64

[cm-2 sec-1]