ANTARES

Physics motivation Recent results Outlook

4 senior physicists, ~5 PhD students, ~5 technicians

M. de JongRECFA

23 September 2005

Neutrino telescope

Neutral point back Weak interaction no absorption

Need huge detector

X

N

1.5deg.

θE TeV

1960 Markov’s idea:

Range of muon:

Detect Cherenkov light:

Transparency of water:

R 1 km at 200 GeV

Use sea water as target/detector

c90 A

N sin θcm 2 d

λ 50 100 m

Antares detector

Equipped volume 0.1 km2 x 0.4 km (=800 x SuperK)

42° 50’ N 6° 10’ E

Atlas

All particle cosmic ray spectrum

= E-2.7 (

m2 s

r s

GeV

)-1

E (GeV)

1 / km2 /year

Where do they come from?

Pierre Auger Observatory

Emax = 1021 eV > 5 x 1019 eV (GZK)

1 GeV 1010 GeV

Dark Matter

4%23%

73%

atoms

dark matter

dark energy

Rotational light curves Gravitational lensing Temperature fluctuations

Dark matter

Annihilation of neutralinos in the sun

Μ2E

Neutralino detection with Antares

HESS: Supernova remnants

No synchrotron radiation seen 0 +

E-2.2

Astrophysics– Neutrino astronomy

– Composition of jets

– Engine of cosmic accelerators

Particle physics– Origin of UHE cosmic rays

– Massive particles (GUT)

– Dark matter

– Neutrino properties (, )

Physics motivation

Detection principle

c (tj - t0) = lj + dj tan(c)

+ N + X

= 0.2 deg.x = 20 cmt = 1 ns

mediumproperties

“All-data-to-shore” conceptpo

sitio

n

time

10 ms

Software Trigger

2 s

offline reconstruction

<1 MB/s

determination of trajectory

1 GB/s

events

All-data-to-shore (2)

Fast front-end electronics

– Analogue Ring Sampler chip

High bandwidth

– DWDM technology

Software Trigger

– Fast algorithms

Software Trigger

100 PCs @ 600 MHz 1999

– CPU 600 MHz 3 GHz × 5

– New algorithm × 3

– C++ compiler 2.96 3.3 × 1.5

5 PCs @ 3 GHz

2005

GRB alert systems

Data taking in case of a GRB alert

GRB trigger

GRB events

write all data to disk, including all data in memory

all data1 GB/s

100 CPUs with each 1 GB RAM

location of the GRB

detector

data filtered offline100 s of raw data prior to the alert

+few minutes of raw data

after the alert

disk

disk

10log E (GeV)

effe

ctiv

e v

olu

me

[km

3]

Detection efficiencies

With satellite information

Improved detection efficiency

Standard

4 optical modules 1 laser beacon 2 LED beacons Seismometer, ADCP, etc.

April 13 2005:

Connection with VICTOR

Instrumentation line:

Time calibration

PMT time

- LED beacon time

14.5 m

PMT

LED beacon

Short (1 ns) light flash

Time calibration

= ~1 ns

3 optical modules

6 ARS

t [ns]

even

ts

t [ns]

even

ts40K background

~MeV e-

40K 40Ca + e- 1

KM3NeTJuly 2005: Start of negotiations EU (FP6) 9 M€

Summary

Proof of concept of time calibration system

Mass production started

Deployment of first complete line before end this year

Outlook

Approaching physics exploitation– First Atmospheric muons before spring 2006

KM3NeT– EU funding (FP6)– ESFRI list of opportunities– NIKHEF well positioned with “all-data-to-shore”