The IceCube High Energy Telesope
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Transcript of The IceCube High Energy Telesope
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]