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The Baikal neutrino telescope: Physics results and future plans V. Aynutdinov, INR RAS for Baikal collaboration Moscow, 18.10.2005 Baikal - Optical Properties Baikal ... – PowerPoint PPT presentation

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Title: The Baikal Neutrino Telescope: Physics Results and Future Plans


1
The Baikal neutrino telescope Physics
results and future plans
V. Aynutdinov, INR RAS for Baikal collaboration
Moscow, 18.10.2005
2
Collaboration
  • Institute for Nuclear Research, Moscow, Russia.
  • Irkutsk State University, Russia.
  • Skobeltsyn Institute of Nuclear Physics MSU,
    Moscow, Russia.
  • DESY-Zeuthen, Zeuthen, Germany.
  • Joint Institute for Nuclear Research, Dubna,
    Russia.
  • Nizhny Novgorod State Technical University,
    Russia.
  • St.Petersburg State Marine University, Russia.
  • Kurchatov Institute, Moscow, Russia.

BAIKAL in CernCourier 7/8-2005
3
Outline
Baikal
A
N
N
Neutrino telescope NT200 (1998)
Design Physics Results (selected)
NT200 upgrade -gt NT200 (2005) New
Design Calibration (new
laser) Perspectives Gton scale detector (GVD) at
Baikal NT200 as a basic cell of
future Gton detector Summary
Motivation Present
telescope configuration is perfect test facility
for future Gton detector
Amanda/IceCube
4
The Site
1070 m depth Absorption length 20-30
m Scattering length 30-70 m Ice as a natural
deployment platform
51 d 45 59 N 104 d 25 09 E
Shore station
4000 m
1366 m
5
Ice as a natural deployment platform
  • Ice stable for 6-8 weeks/year
  • Maintenance upgrades
  • Test installation of new equipment

6
(No Transcript)
7
Baikal - Optical Properties
Scatt. Length (geom) 30-50 m ?cos
?? 0.85-0.9
Abs. Length 22 2 m
Open configuration of the Telescope and good
water parameters of Baikal water allow to
observe big water volume much more than
geometrical boundaries
8
Baikal-NEMO Campaign March, 2001
  • Example of interaction between ANTARES,NEMO ? ?
    Baikal
  • ? Verification of Lake Baikal Attenuation /
    Absorb. / Scatt. results
  • Cross-Calibration AC9 (Antares/Nemo) vs. Burhan
    ASP15

see NIM A498 (2003)
9
Project Milestones 1991 Project NT200 approved
1993 NT36 36 OM at 3 strings The first
underwater array operates First ?s and ?s in
Neutrino Telescope
1998 NT200 192 OM at 8 strings 1 Mton
at 1 PeV
1996 NT96 96 OM at 4strings
2005 NT200 228 OM at 8 3 strings
10 Mton at 10 PeV
10
-8 strings 72m height - 192 optical modules
? 96 measuring channels ? T, Q measure
Timing 1 nsec Dyn. Range 1000 pe
Effective area 1 TeV 2000 m² Eff. shower
volume 10TeV 0.2Mt
  • Quasar PMT d 37cm

Height x ? 70m x 40m, Vgeo105m3 0.1Mton
11
Selected ResultsNT200
Low energy phenomena (muons) - Atmospheric
neutrinos - WIMP neutrinos High energy
phenomena (cascades) - Diffuse neutrino flux
- Neutrinos from GRB - Prompt muons and
neutrinos - Exotic HE muons Search for
exotic particles - Magnetic monopoles
12
Atmospheric Neutrinos
372 Neutrinos in 1038 Days (1998-2003)
Important calibration tool
ETHR 15-20 GeV
Skyplot (equatorial coordinates) of neutrino
events
13
Search of nearly vertically upward going muons ,
exceeding the flux of atmospheric neutrinos
Angular distribution of selected
neutrino candidates as well as background
expectation
C ? ??
Limits on the excess muon flux from the centre
of the Earth as a function of WIMP mass
14
Look for upward moving light fronts. Signal
isolated cascades from neutrino
interactions Background Bremsshowers from h.e.
downward muons Final rejection of background by
energy cut (Nhit)
  • Physics topics
  • HE cascades from
  • ?e ?? ?? - NC/CC
  • Diffuse astroph.flux
  • GRB correlated flux
  • HE atmospheric muons
  • Prompt ?
  • Exotic ?

? (BG)
NT-200 is used to watch the volume below for
cascades.
15
tmin gt -10ns Nhit gt 15 ch.
Hit channel multiplicity (experiment and
background expectation)
Shape of signal in Nhit distribution for Fn A
E-g (g1.5, 2.0, 2.5).
16
Experimental limits bounds/ predictions
Models already ruled out by the experiments SS
- Stecker, Salamon96 (Quasar) SeSi -
Semikoz, Sigl (Models/Expts. are rescaled for 3
flavours)
17
New configuration NT200
36 additional PMTs on 3 far strings ? 4
times better sensitivity ? Improve cascade
reconstruction
Vgeom 4 106 m3 Eff. shower volume 104TeV 10
Mton Expected ?-sensitivity (3 yrs NT200)
E2 ?V lt 0.9 10-7 GeV cm-2 s-1 sr-1
NT200 as test facility for Gton scale
detector 1. Optical module
2. Calibration system 3. New electronics
4. Data acquisition system 5. Time
synchronization 6. Cable
communications
18
NT200 commisioned April 2005
1. 3 outer strings were instaled 2. New DAQ
final modernization - 2 Underwater PC with
Flex DSL modem (1 Mbod), Underwater
Ethernet - Synchronization system
time synchronization NT200 lt-gt outer
strings event clusterisation 3. New
Software DOS -gt Linux, Remote control 4.
New 2 cables to shore (2x4 km) 5. Calibration -
New bright Laser
19
DAQ and control system of NT200
Two subsystems NT200 and NT Two-level time
measurement and data acquisition systems Low
level - Strings PMT time and amplitude
measurements - DEM trigger and event
clusterisation systems - SEM slow control
DAQ Center - 2 underwater PC connected to
shore - CEM trigger time measurement
20
Underwater PCs
PC104 Advantech-PCM9340 DSL-M DSL-modem
FlexDSL-PAM-SAN with hub and
router, 2 Mbit/s. SwRSTP a managed
Ethernet switch RS2-4R CSrv
WUT-58211, for PC-terminal
emulation Mc two media-converters for
coaxial connection D-Mod, C-Mod
experiment data and control
modems
21
New Laser
Laser intensity cascade energy (1012 5
1013 ) g (10 500) PeV
RMS of arrival time distribution 2 ns
? Laser is visible gt200m with high Ampl. (NT and
ext.strings)
22
NT200 time resolution
Dt t1 t12 t2 st1, st2 - PMT jitter and
light scattering s( t12) ? 2 ns - electronics
jitter
Light scattering - scattering length 30 m -
distance to Laser 200 m
5 series of Laser pulses
Jitter of electonics 2 ns - synchro cable
length 1.2 km - TDC bin 2 ns
t12
t2
The amplitude dependence of relative time jitter
measured for several pairs of channels of NT200
and external string. Red line is result of
calculations
t1
23
NT200 efficiency of cascade reconstruction
Laser coordinates reconstruction
NT200
Reconstructed vs. simulated coordinates of
cascades in NT200 (blue) and NT200 (red)
3 extern. str.
NT200
Dr lt 1 m
24
NT200 as a subunit of a Gton scale detector
For High Energy Cascades A single string
replacing the NT200 central core reduces Veff
less than x3 for Egt100TeV. ? 12 OMs strings as
a subunit for a Gton scale detector ok.
Effective volume with
25
A future Gigaton (km3) Detector in Lake Baikal.
Sparse instrumentation 91 strings with 12/16
OM 1308 OMs (NT200 192 OMs) ?
effective volume for 100 TeV cascades
0.5 -1.0 km³ ? muon threshold between
10 and 100 TeV
26
Gton detector at Baikal lake
RD on the basis of NT-200 configuration
1. Optical module PMT selection 2.
Detector configuration PMT location, string
configuration, distances, 3. Electronics
flash ADC, trigger conditions, 4.
Communications optical cables, connectors, 5.
Data acquisition system, time synchronization
27
CONCLUSION
1. BAIKAL lake experiment running since 12
years - Diffuse Neutrino flux
limit - Limit on an excess flux due to WIMP
annihilation in the Earth - Limit on the flux
of fast magnetic monopoles 2. NEW configuration
NT200 start of operation April 2005 -
NT200 is tailored for diffuse cosmic neutrinos
Veff 10 Mton at 10PeV
Expected ?-sensitivity (3 yrs NT200) E2 ?v
lt 10-7 GeV cm-2 s-1 sr-1 - NT200 gives
good possibilities to optimise the structure and
to investigate the basic
elements of future Gton scale detector 3. RD
Gigaton Volume Detector (km3) at Baikal lake was
started
28
Flux upper limit (cm-2 s-1 sr-1)
29
NT200 Start of operation April 2005
  • 13 Apr - 23 May 2005
  • Exposition time 640 hours
  • Events number 7.6 ? 104
  • - More than 1 outer string 20 events

Examples of events
30
NT200 Start of operation April 2005
  • 13 Apr - 23 May 2005
  • Exposition time 640 hours
  • Events number 7.6 ? 104
  • - More than 1 outer string 20 events

Examples of events
31
New Laser Design
  • Isotropizer
  • - Glass bulb filled with MicroGlassSpheres
  • (S32 from 3M 20-70um dia.) mixed with
    OpticalGel
  • ? A LaserBall similar to the SNO
    calibration device.
  • - Total loss is low 12 - 25 only !
  • calibrated with Ulbricht Sphere (1.5m
    diam.)
  • Absolute LaserCalibration
  • (with commercial Laser-PowerMeter) to
    optimize yield
  • also at the lake (monitor laser vs. years)
  • Expect gt1012 photons/pulse
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