1. Christian Spiering, ESC DESY, Sept.2003
Neutrino-Astrophysics
Baikal, Amanda, IceCube
Lake Baikal
South Pole
Christian Spiering, ESC DESY, Sept.2003

2. Baikal and Amanda 1. The present detectors 9/18/2018
Christian Spiering

3. The Baikal Collaboration
Institute of Nuclear Research, Moscow
Irkutsk State University, Irkutsk
DESY Zeuthen, Zeuthen
Moscow State University, Moscow
Nishni Novgorod State Technical University
State Marine Technical University, St.Petersburg
Kurchatov Institute, Moscow
JINR, Dubna
since 1988
9/18/2018
Christian Spiering

4. Baikal History
>
#OM
228
first 2 neutrino
candidates
NT-200
NT-200+
upgrade
Baikal will likely stay largest H.E.
neutrino telescope on northern
hemisphere for another 2-3 years
and nicely complement Amanda.
One of the first neutrino
events recorded with the
1996 four-string version
of the Baikal Telescope

5. Baikal Upgrade NT200+ NT-200 cascades NT-200
140 m
36 additional PMTs  4 times better sensitivity !
9/18/2018
Christian Spiering

6. The AMANDA Collaboration
Bartol Research Institute
UC Berkeley
UC Iivine
Pennsylvania State
UW Madison
UW River Falls
LBL Berkeley
U. Simón Bolivar, Caracas
VUB, Brussel
ULB-IHEE, Bruxelles
U. de Mons-Hainaut
Imperial College, London
DESY, Zeuthen
Mainz Universität
Wuppertal Universität
Stockholm Universitet
Uppsala Universitet
Kalmar Universitet
South Pole Station
Antarctica
New Zealand
Venezuela (1)
Japan
USA (7+3)
Europe (10+1)
+ associated IceCube institutes in
USA, Europe, Japan, New Zealand
9/18/2018
Christian Spiering

7. AMANDA-II and SPASE 1996-2000 construction 19 strings 677 PMTs optical
South Pole Air Shower Experiment
inner 10 strings:
Amanda-B10
19 strings
677 PMTs
optical
module
construction
AMANDA II
9/18/2018
Christian Spiering

8. 2. Selected Physics Results
Search for point sources (AMANDA)
Search for a diffuse extraterrestrial flux (Amanda & Baikal)
Indirect Search for Dark Matter (Amanda & Baikal)
Search for neutrinos coincident with Gamma Ray Bursts
(Amanda & Baikal)
5. Measurement of the spectrum of atmospheric neutrinos
(Amanda)
6. Measurement of the spectral composition of primary cosmic
rays (Spase/Amanda)
9/18/2018
Christian Spiering

9. Search for extraterrestrial point sources
697 events below horizon
below horizon: mostly atmospheric ‘s
above horizon:mostly fake events
AMANDA-II 2000 data
Submitted to PRL
9/18/2018
Christian Spiering

10. AMANDA-II 20% of 2001 data Now analyzed: 1997, 1999, 2000 Started:
2001, 2002
AMANDA-II
20% of 2001 data
Planned until
Summer 2004:
combined
analysis 97-99
analysis 00-03
9/18/2018
Christian Spiering

11. SS-433
9/18/2018
Christian Spiering

12. Amanda-II, 2000 data:
Neutrino flux upper limit (90% C.L.) in units of 10-7 cm-2 s-1
for an assumed E -2 spectrum, integrated above E = 10 GeV.
9/18/2018
Christian Spiering

13. Selected point source flux limits
sensitivity  flat above horizon - 4 times better than B10 ¶ !
Sources
declination
1997 ¶
2000
SS433
5.0o -
0.7
M87
12.4o
17.0
1.0
Crab
22.0o
4.2
2.4
Mkn 421
38.2o
11.2
3.5
Mkn 501
39.8o
9.5
1.8
Cyg. X-3
41.0o
4.9
Cas. A
58.8o
9.8
1.2
declination averaged sensitivity:
lim  0.23•10-7
upper 90% CL in units of 10-8cm-2s-1
¶ published Ap. J, 582 (2003)
9/18/2018
Christian Spiering

14. the sensitivity needed to search from neutrino fluxes
Intrinsic source
 spectrum
(corrected for
IR absorption)
Measured 
spectrum
AMANDA average flux limit for two assumed
spectral indices , compared to the average
gamma flux of Markarian 501 as observed in
1997 by HEGRA.
AMANDA-II has reached
the sensitivity needed to
search from neutrino fluxes
from TeV gamma sources
of similar strength to the
instrinsic gamma flux.
9/18/2018
Christian Spiering

15. Search for an diffuse excess of extra- terrestrial high energy neutrinos
 bound
WB bound
DUMAND
FREJUS
MACRO
Muons in Amanda-B10 (1997)
Expectation Amanda-II, 3 years
Expectation IceCube, 3 years
log E /GeV

16. ... look also to cascades from electron and tau neutrino interactions
Assuming
e:: =1:2:0 at source
e:: =1:1:1 at Earth
factor 3 applied to
 channel
AMANDA-II
cascades
2000  analysis will yield
an all-flavour limit close to
the cascade limit
9/18/2018
Christian Spiering

17. Indirect Search for WIMPs 
(a)
Neutrinos from
the Center of Earth
 + 
 b + b
„soft spectrum“ 
 W + + W -
„hard spectrum“
9/18/2018
Christian Spiering

18. Upper limits on muon flux from neutralino
annihilations in center of Earth
Green dots:
Excluded by present
direct searches
Blue crosses:
can be excluded
by 10 times more
sensitive
Baikal 98/99 data
9/18/2018
Christian Spiering

19. Indirect Search for WIMPs
(b)
Neutrinos from
the Sun   
Amanda
At South Pole the Sun sinks maximally 23° below horizon. Therefore
only Amanda-II with its dramatically improved reconstruction capabilities
for horizontial tracks (compared to Amanda-B10) can be used for
solar WIMP search.
9/18/2018
Christian Spiering

20. preliminary Upper limits on muon flux from
neutralino annihilations in center of Sun
AMANDA-II results:
• based on 193 days
of live time
• Exclusion sensitivity
from analyzing the
off-source bins
Will un-blind data soon
and look to the Sun.
preliminary
ANTARES and ICECUBE:
MC-calculated
sensitivities

21. 3. IceCube
9/18/2018
Christian Spiering

22. IceCube Collaboration
Institutions: 11 US, 10 European, 1 Japanese and 1 Venezuelan
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
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
University of Mons-Hainaut, Mons, Belgium
Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, USA
Dept. of Astronomy, Dept. of Physics, SSEC, University of Wisconsin, Madison, USA
Physics Department, University of Wisconsin, River Falls, USA
Division of High Energy Physics, Uppsala University, Uppsala, Sweden
Dept. of Physics, Stockholm University, Stockholm, Sweden
Dept. of Physics, University of Alabama, USA
Vrije Universiteit Brussel, Brussel, Belgium
Chiba University, Japan
Dept. of Astrophysics, Imperial College, UK
Dept. of Physics, University of Maryland, USA
Universidad Simon Bolivar, Caracas, Venezuela
University Utrecht, Netherlands
9/18/2018
Christian Spiering

23. IceCube - 80 Strings - 4800 PMT Instrumented volume: 1 km3
AMANDA
South Pole
IceTop
IceCube
- 80 Strings
PMT
Instrumented volume: 1 km3
Installation:
~ atm. per year
9/18/2018
Christian Spiering

24. Schedule 03-04 drill equipment to Pole 04-05 first 5 strings
(proof that 16/season are feasible)
strings
strings
strings
strings
09-10 remaining strings
9/18/2018
Christian Spiering

25. 4. DESY Tasks in IceCube
Simulation & optimization IceCube  accepted by Astropart.Phys.
Design of Front-End-Electronics (Communication to Optical Module)
German production site for 1300 optical modules
(1/4 of all 5200 modules)
IceCube lead for Amanda-IceCube integration
IceCube lead for reconstruction
German/European data processing center
R&D wavelength shifter for optical modules
R&D acoustic detection
analysis:
search for extraterrestrial diffuse and point-like sources,
relativistic magnetic monopoles, slowly moving exotic particles

26. DOR: DOM Readout card 9/18/2018 Christian Spiering 96V DOM Power
Quad Cable Con.
Power Switch
Comm. DAC
Clock &
Time String port
Comm. ADC
PLD
Comm. Rec.
FPGA
FLASH
SRAM
JTAG
I would like to present you two examples of fast link interfaces, designed in our lab.
For both cards block schemes, test results and conclusions will be presented.
DOR: DOM Readout card
9/18/2018
Christian Spiering
9/18/2018
Christian Spiering

27. DOR DOM Traffic over 2 km twisted pair cable: supply voltage
slow control
FADC output (up to 1 Mbit/sec)
synchro-signals
( require 5 nsec accuracy)
DOM
9/18/2018
Christian Spiering

28. Production of 1300 Optical Modules
1-3/2004
4-9/2004
total
Germany 5 60
1300
Sweden
900
USA
300
3000
Includes 10 weeks test in Dark Freezer at -45 ºC
9/18/2018
Christian Spiering

29. Dark Freezer Lab - 45 °C Up to 120 Optical Modules 9/18/2018
Christian Spiering

30. Enhancing the Sensitivity of IceCube Optical Modules by Application of
Wave Length Shifters
Elisa Resconi
EU post-doc in DESY
guest at MPIK-Heidelberg

31. Deep Sea Water
9/18/2018
Christian Spiering

32. Light lost Light detected Ice, in contrast to water, is UV trans-
INTENSITY (a.u)
OM glass, 11.5 mm
Gel 10 mm
PMT glass, 2.6mm
Cherenkov spectrum
(a.u.)
Ice, in contrast to
water, is UV trans-
parent down to
230 nm.
The glass of the
pressure sphere
absorbs most light
below 350 nm.
Light lost
Light detected
Cherenkov
Spectrum
9/18/2018
Christian Spiering

33. Application of Wavelength Shifters (WLS)
Earlier attempts indicated that an overall gain of 40% can be achieved.
However, WLS layers deteriorated in water and where mechanically unstable.
Now, a water-proof and mechanically stable WLS foil exists.
BPO
PPO
Butyl-PBD
Benthos glass
(11.5mm)
Transmittance (%)
100 80 60 40 20
Nauthilus glass
(15 mm)
Transmittance (%) 50 25
100 75
9/18/2018
Christian Spiering

34.  lower threshold, better reconstruction
10 cm
THV granulate
doped with PPO
Extrusion of
transparent foil
Thermo-forming of cap
Will be optically coupled with a very
thin layer of gel (less then 1mm)
and fixed at optical module support.
Effect: ~ 40% more light
 lower threshold, better reconstruction
 next: Tests in Dark Freezer Room
 if success: Test at 04/05 at Pole
9/18/2018
Christian Spiering

35. R&D on acoustic detection: 10-100 cubic kilometer
volume for extremely high energies ? P t
50s
Particle cascade  ionization
 heat
 pressure wave
Maximum of emission at ~ 20 kHz
Attenuation length of cold ice
at kHz: ~ 2 km
(light: ~ 100 meters)
→ given a large initial signal,
huge detection volumes
can be achieved.
9/18/2018
Christian Spiering

36. Development and test of a variety of acoustic sensors in Zeuthen
Rolf Nahnhauer et al.
9/18/2018
Christian Spiering

37. Threshold with present sensors: ~ EeV
tests with laser light dumped to ice and water
tests with protons dumped into ice and water
tests in open water
development of hardware and software filters
Hearing 180 MeV protons
dumped into ice
Threshold with present sensors: ~ EeV
Expected improved threshold: ~ 100 PeV
9/18/2018
Christian Spiering

38. Request for a test at South Pole in 2004/05
 Study ambient noise
 Measure absorption length
See also talk in closed session
9/18/2018
Christian Spiering

39. 5. Summary
Amanda-II produces new limits on point sources, diffuse fluxes, GRB, WIMPs, and measures atmospheric neutrino spectrum up to 100 TeV.
AMANDA-II has reached the sensitivity needed to search from neutrino fluxes from TeV gamma sources of similar strength to the instrinsic gamma flux.
Next: data coherently processed
Baikal produces new limits on diffuse flux, WIMPs, and GRB and will stay largest neutrino telescope on northern hemisphere for 2-3 years.
IceCube is established as MRE, 6 strings to be produced in 2004.
DESY-Zeuthen ready for OM production
New methods - WLS and acoustic – may enhance IceCube performance considerably. R&D in Zeuthen.
9/18/2018
Christian Spiering