Transcript AMANDA and IceCube neutrino telescopes at the South Pole

AMANDA and
IceCube
neutrino telescopes
at the South Pole
Per Olof Hulth
Stockholm University
Members of the AMANDA SU
group
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Senior members
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Forskarassistent
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Stephan Hundertmark
Resarch students
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Christian Bohm
Per Olof Hulth
Klas Hultqvist
Christian Walck
Thomas Burgess
Patrik Ekström (Wuppertal)
Yulia Minaeva
Julio Rodriguez Martino
Christin Wiedemann
Electronic engenieer
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Lars Thollander
Scientific goal
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Detect High Energy cosmic neutrinos by
using the ice sheet at The South Pole as a
target.
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Method:
Detect the emitted Cherenkov light from
neutrino induced interactions in the ice.
Activities
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Mainly analysis and software development
Preamplifiers designed and built in
Stockholm (SWAMPS)
Neutrino interaction
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< 1 degree
The muon can travel
several km in e.g. ice
South Pole
Dark sector
Skiway
AMANDA
Dome
IceCube
Hot water heaters
-50 m
-55 C
1400 m
-42C
-2400 m
-20 C
Photomultipliers:
Hamamatsu 20 cm 14 dynodes
Gain 109
AMANDA electronics
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Three different cable types (2400 -2600 m)
Strings 1-4 coax cable, rise time 250 ns
 Strings 5-10 twisted pair rise time, 50-70 ns
 Strings 11-19 twisted pair rise time 100-150
ns
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Analog signal at surface about 1-10 mV
Amplified 100 times by Stockholm
“SWAMP” (Lars Thollander)
Technical requirements
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Absolute timing <7 ns from any OM
Geometrical position uncertainty < 1m
Electronic in ice should stand -50 C
Low noise
Building AMANDA: The Optical
Module and the String
Evolution of read-out strategy
- timing
- dyn. range
- no x-talk
- easy
calibration
Strings 1-10
Strings 11-17,19
- cost
- robustness
- dynamic
range
String 18
New Project IceCube
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Increase volume to 1 km3
80 strings with 60 modules each
Photomultiplier 25 cm (10 inch) 10 dynodes
(preliminary Hamamatsu)
Air shower detector on top (IceTop)
Transport drill to Pole 03/04
First 1-7 strings in 04/05
IceTop
AMANDA
South Pole
IceCube
80 Strings
4800 PMT
1400 m
2400 m
Skiway
IceCube:Top View
Grid
North
100 m
AMANDA
80 strings
60 modules/string
Volume 1 km3
Depth 1400-2400 m
Counting
House
South Pole
SPASE-2
Dome
Skiway
µ-events in IceCube
Eµ=10 TeV
Eµ=6 PeV
AMANDA-II
1 km
Measure energy by counting the number of fired PMT.
(This is a very simple but robust method)
1. Digital Optical Module
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Self-triggers on each pulse
Captures waveforms
Time-stamps each pulse
Digitizes waveforms
Performs feature extraction
Buffers data
Responds to Surface DAQ
Set PMT HV, threshold, etc
Noise rate in situ: ≤500 Hz
DOM
Photomultiplier
33 cm
1400 m
IceCube
String
2400 m
OM Spacing: 17 m
Experimental Requirements
IceCube
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Time resolution:
<5 ns rms
Waveform capture:
>250 MHz - for first 500 ns
~40 MHz
- for 5000 ns
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Dynamic Range:
>200 PE / 15 ns
>2000 PE / 5000 ns
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Dead-time:
< 1%
OM noise rate: < 500 Hz (40K in glass sphere)
2. DAQ
Network
architectu
re
In-Door deployment
Hose Winch for the Ice Cube Project
ENGINEERING AND INSTRUMENTATION
UNIVERSITY OF WISCONSIN - MADISON
Receiving drum weldment
POSITION OF DRILL
(30HOUR ANALYSIS)
0
0
5
10
15
20
-500
-1000
DEPTH
-1500
-2000
-2500
-3000
TIME(hrs)
25
30
35
40