KM3NET
24 September 2004Gerard van der Steenhoven (NIKHEF)
What is KM3NET?
• Design study for a Deep Sea Facility in the Mediterranean for Neutrino Astronomy and Associated Sciences
• Objective: develop cost-effective design of a 1 km3 neutrino telescope (~ 200 M EUR)
• Participants from existing collaborations:
+ …
KM3NET: participating countries
Outline
• Purpose of km3 -detector– Neutrino Astronomy: identify point sources
– Particle Physics: dark matter searches
• The KM3NET project– Basic concept
– Count rates
– Work packages
– Challenges
• Outlook
Gamma-Ray Bursts Active Galactic Nuclei
Purpose of km3 -detector
• Astrophysics (-astronomy):– Identify point sources– Composition of jets– Origin of cosmic acceleration– Diffuse fluxes
• Particle physics:– Dark Matter searches:
• Neutralinos, Monopoles
– Origin of UHE-cosmic rays– Neutrino oscillations
(extra) galactic -sources
Neutralino search: → +…
Neutrino Astronomy• Consider distant sources of radiation:
– Supernovae, Quasars, GRBs, AGNs, ….
• Effect of interstellar medium:– High-energy EM radiation is (partly) absorbed– Protons are bent can be traced back to the source
p
Active Galaxy(e.g. M87)
Black hole with108 x mass of sun
104 ly
extra-galactic
Microquasar(SS433 etc.)
Black hole with mass of sun
1 ly
galactic
Possible neutrino point sources
Supernova remnant(Crab nebula)
Composition and origin of jets• GRBs, Microquasars, Pulsars, AGNs,….
• Ideas and proposed schemes:
GRB 971214 Crab
SS433 - Quasar
Origin of cosmic acceleration
Black Hole ?
Active Galactic Nucleus (AGN) Black Hole is possibleengine of AGN, but nopresently available EMwavelength gives directaccess to center of AGN
Optical and radio emission of AGN
[AGN luminosity ~ 1010 x luminosity of the sun]
Evidence for Dark Matter
Rotation of galaxies Gravitational lenses Microwave background
Dark Matter: where to find it?
• Gravitational capture of ’s:
• Annihilation of neutralinos:
in Earth, Sun, or Galactic Centre:
W
W
cb
cb
Hard neutrino spectrum Soft neutrino spectrum
→ directionally sensitive trigger
+ b~
Annihilation of dark matter in the sun
neutralino
sun
earth
Dark Matter Searches
Origin of high energy cosmic rays
~ E-2.7
• Scientific issues:
• How to get info:– Protons are bent…– High energy ’s ?
→ What is the origin of
(U)HE cosmic rays?
GZK limit: 5 x 1019 eV
→ Data beyond GZK limit: new physics?
The absorption of HE gamma’s• High-energy ’s interact with IR, CMB, Radio:
+Radio
+IR
+CMB
Local Group
3C279
Galactic Center
Mrk421
pee p → → For 1012 < E < 1022 eV photons cannot travel further than 100 Mpc
→ Search for neutrinos with E > 1012 eV: 1012 – 1016 eV: upward
1016 – 1021 eV: downward
Unique feature KM3NET:access to UHE neutrinos
• Atmospheric neutrinos
• Observation of -s: regeneration effect
– observe secondary
with energy > 107 GeV
(Most -s with E > 107 GeV are screened by the Earth!)
Neutrino Oscillations
........
[Bugaev, Sokalski & Shlepin, Astropart. Phys., 2004][Bugaev, Sokalski & Shlepin, Astropart. Phys., 2004]
p
p
KM3NET: basic concept• Underwater Cerenkov detector of ~ 1 km3
Expected rates: diffuse fluxes
Waxman-Bahcall Limit for extra-galactic sources: ~ 250 ev/yr/km2
NT-200
DUMAND
W&B
MPRMPR
+ NT-200
AMANDA-II/ANTARES
IceCube/KM3NeT
AMANDA-B10
GRB
atmospheric neutrinos
Mannheim et al: refinement of WB-limit +individual src-s.
Total expected diffuse rate: 20 x ANTARES ~ 100.000 per year
• Compare to– MACRO limits– -quasar est.
(Distefano et al., 2000)
– GRB estimate (Razzaque et al., 2003)
KM3NET has best sensitivity
Expected rates: point-like sources
KM3NET 1 yr
Expected rates: dark matter annihilation in the sun to WW (100% BR)
Scattered points: mSUGRA parameter space for various h2 combinations
: neutralino density (wrt to critical density); h: dimensionless expansion rate
KM3NET versus ICECUBE
• Complementary sky views*:
• Angular resolution:• Energy threshold:
(*) ANTARES location provides a sky coverage of 3.5 sr and an instantaneous common view with AMANDA
of 0.5 sr, and about 1.5 sr common view per day. The Galactic centre is visible 2/3 of the time.
KM3NET ICECUBE
galactic
centre
KM3NET ICECUBE
0.1 deg 0.5 deg
1 TeV 10 TeV
The KM3NET project• Design requirements:
– Effective volume: 1 km3 (> 20 x ANTARES)– Angular resolution: 0.1 deg (1/2 x ANTARES)– Energy threshold: 1 TeV (and pointing 100 GeV)– Field of view: 4– Source tracking (M Bouwhuis) → from satellites:
• Milestones:– Conceptual design report– Technical design report
• Financial request:– 9976 kEUR
KM3NET work packages1. Management (Erlangen, D)
2. Astroparticle Physics (IN2P3, Fr)
3. Physics Analysis (Patras, Gr)
4. System Engineering (Saclay, Fr)
5. Information Technology (FOM, NL)
6. Deep-Sea Infrastructure (INFN, It)
7. Sea-surface Infractructure (NESTOR, Gr)
8. Risk assessment (INFN, It)
9. Resource exploration (NCSR, Gr)
10. Associated science (Aberdeen, UK)
Dutch involvement
• Personel:– UvA: P. Kooijman, E. de Wolf– NIKHEF: M. de Jong, G. van der Steenhoven – KVI/RuG: <being considered>
• Projects:– Coordination WP5 ‘Information Technology’– Calibration procedures, off-line event selection– PMT readout, design optical module
• Financial support:– 696 kEUR (~7% of total budget request)
KM3NET Challenges• Design:
– Simplify off-shore electronics (‘all-data-to-shore’)– Separate detection and calibration functionalities
• Production model:– Start construction at end of design study– Multiple production and assembly lines – Pressure and shallow water tests at prod. sites– Transport and deployment ‘as is’
• Site selection:– France, Italy or Greece
KM3NET Design• Design:
– ANTARES too expensive!
– Simplify electronics:• All-data-to-shore
• Increase reliability
• low power
– Optimize optical module:• Many small PMTs??
• Few connectors
– Separate detection and calibration functionalities
– Towers lines
Antares Design
Profiler for Sea currant
(ADCP)
Probe for salinity and temperature (CTD)
Probe for Sound velocity
J unction Box
LED Beacon
Laser Beacon
Seismograph
hydrophones hydrophone
5 Storeys of Optical Modules
Anchor with electronics containers Link Cables
KM3NET Production Model
• Estimated size of the production:– 100.000 PMTs
– 10.000 optical modules
– 400 detector units (“lines”)
– 40 calibration units
• Start of data taking: 2012– Start design study: 2006
– Start of production: 2009
Production time of 3 years
5 – 6 production sites are needed
150 / day
15 / day
12 / month
1.5 / month
4100m
2400m
3400mANTARESNEMO NESTOR
KM3NET: site selection
KM3NET: outlook
• Status proposal:
– approved by EU; negotiations in 2005
– expected starting date: january 2006
• Activities in the Netherlands:
– initial discussions on planning design work
– initiate discussions with funding agencies