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