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The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006
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The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Dec 22, 2015

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Page 1: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

The ANTARES Neutrino Telescope

Mieke Bouwhuis27/03/2006

Page 2: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Broadband light source

1’ 1’1’ 1’

radio 10-8 eV optical 10 eV x rays 104 eV gamma rays 1012 eV

The pulsar in the Crab nebula

Page 3: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

The observed radiation

e-

e-

Synchrotron radiation Inverse Compton scattering

But: for some sources no synchrotron radiation is seen…

Page 4: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

All particle cosmic ray spectrum

energy (eV)

rela

tive

part

icle

flu

x (lo

garit

hmic

uni

ts)

No point sources found yet

Page 5: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

e, , p and from cosmic accelerators

e

e e

e

0,p X accp

Page 6: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Neutrinos from high-energy sources

Neutral point back Weak interaction no absorption

Active GalacticNucleus (AGN)

SupernovaRemnant (SNR)

Gamma-rayBurst (GRB)

Pulsar Microquasar

Page 7: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Indirect neutrino detection

Neutrino interaction (e, , ):

med

ian

scat

terin

g an

gle

(deg

rees

)

neutrino energy (GeV)

Scattering angle

s

1.5θ

TeVE

Page 8: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Neutrino cross section

neutrino energy (GeV)

cros

s se

ctio

n (c

m2 ) 1

AN

Mean free path:

~108 m at 1 TeV

Very large volume needed

Page 9: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

The ANTARES neutrino telescope

Mediterranean Sea, near Toulon

Page 10: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Detection volume and medium

sea + earth = large volumeInstrumented volume = 0.02 km3

Effective volume = 0.2 km3 (at 10 TeV)

= 1 km3 (at 10 PeV)

water for production of Cherenkov light

water is transparent

depth of 2.5 km for shielding against atmospheric background

Page 11: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

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

= 0.2°x = 20 cmt = 1 ns

Detection principle

water properties

Page 12: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Signals in the detector

Page 13: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Signals in the detector

crosses the detector in 2 s

100 kHz

Page 14: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Different types of background

atmosphere

sea

Earth

proton

proton

cosmic

atmospheric

atmospheric

random background 100,000 hits/s per phototube

atmospheric ~300/s

atmospheric ~10-3/s

Page 15: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

ANTARES data processing system

filter

PC physics data

all raw data10 Gb/s

1 Mb/sanalysis

shore station

• finds all correlated data• real time• data reduction by factor 104

• high efficiency (50%)• high purity (90%)• low threshold: E > 200 GeV

finds cosmic neutrinos

Page 16: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Angular resolution

Page 17: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

February 14, 2006

Page 18: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
Page 19: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
Page 20: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
Page 21: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
Page 22: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

March 2, 2006

Page 23: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
Page 24: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
Page 25: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
Page 26: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Line 1: data taking

LED beaconcalibration

Physicsdata taking

Page 27: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

LED beacon for time calibration

MILOM

Line 1

~70 m

Page 28: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Event Display – LED beacon

Page 29: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Muon trigger ratera

te (

Hz)

number of correlated hits

real data

Monte Carlo

Physics event found by filter:

space-time correlated hits

“snapshot” hit

4 s

Page 30: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Event Display

Physics event found by filter:

space-time correlated hits

“snapshot” hit

4 s

: hits used by the fit

Physics event 17267 in run 21241

Page 31: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Event Display

zenith angle = 179°

Physics event 17267 in run 21241

Page 32: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Event Display

zenith angle = 146°

Page 33: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Event Display

zenith angle = 80°

Upgoing!

Page 34: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Zenith angle distribution

1394 events after 14 hours of data taking

Page 35: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Gamma-ray bursts (GRB)

short and intense flashes of MeV gamma rays

happen unexpectedly, and take place at random locations in the sky

detected by satellites

most information from the observation of the ‘afterglow’

mechanism:

Page 36: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

GRB warning systems

Page 37: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Detection of neutrinos from GRBs

filter

PC

• All-data-to-shore concept

• Data processing farm

• Software filters

Specific ANTARES featuresGRB warning systems GRB features

GRB duration (s)

Combine into the “GRB method”

Page 38: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Data taking after a GRB alert

Page 39: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Delays and buffering

Page 40: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Gain in sensitivity for GRBs

neutrino energy (GeV)

ratio

of

effe

ctiv

e vo

lum

es

standard

GRB method

Page 41: The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

Conclusions

Composition of jets → e versus p

Origin of UHE cosmic rays

Line 1 operational, 12 lines end of 2007

Measured time resolution of ~1 ns

Expected angular resolution 0.2°

GRB method increases the sensitivity