Antares/KM3NeT

M. de Jong

neutrinos g

np

Scientific motivation:– origin cosmic rays– birth & composition relativistic jets– mechanism of cosmic particle acceleration– dark matter

neutrino telescope

Why neutrinos:– no absorption– no bending–‘remote microscope’

Neutrino astronomy

10,000 sparser than Super-K

Antares

Operation and physics analyses

Detector operation

date

onlin

e ne

utrin

o co

unt complete direction information

zenith angle only

main cable repairtwelve linesoperational!

%90detector construction

completed

Neutrino detection

L cos q

num

ber o

f eve

nts

Antares: angular resolution 0.5±0.1 degrees

upward going muons good quality events

neutrinosneutrinos

dataMonte Carlo totalMonte Carlo neutrinoMonte Carlo muon

Neutrino sky map (2007‒2008)

2°

Limits on neutrino fluxes, world’s best for some specific sources.

part of sky invisible to Antares

PSF

Nikhef analyses in Antares Point source search, A. Heijboer et al.– 1st point source search to be published soon

Antares‒Auger correlation, J. Petrovic et al.– approved unblinding of data (December 2010)

GRB: muon neutrino, M. Bouwhuis et al.– approved unblinding of data (January 2011)

GRB: electron neutrino, C. Reed & E. Presani– approved unblinding of part of data (January 2011)

Nikhef is leading analysis efforts

KM3NeT

convergence on the design¶

¶ unanimous decision of the institute board, d.d. 25 January 2011

31 x 3” PMTETeL, Hamamatsu, ...

concentrator ring

increase of photocathode area by 20‒40%

Optical module

6 m

Mechanical cable connection

Data cable storage

Mechanical cable storage

Frame

Optical module

Mechanical holder

Needs new deployment technique

Storey

1 Digital Optical Module = Dom2 Dom’s on 1 bar = Dom-bar

20 Dom-bar’s on 1 tower = Dom tower

NIOZ operations

1st deployment test SeaWiet line December 2010

new set of deployment tests last & this week

deployment & unfurling successful, but some problems with detachment of launcher

data from 2 autonomous lines with 3” PMTs will become available next week after 1 year of operation

Atmospheric muon rates

5 10 15 20 25 30 35 4010-2

10-1

1

number of Lx

Rate

[kHz

]

L0L1L2

70% of L0s contribute to L1s

Effective area

En [GeV]

A [m

2 ]ra

tio

TeV PeV

Antares labs

bar 0 m

standard

SeaWiet

Angular resolution

angle [degrees]

prob

abili

typr

obab

ility

E-2 muon

E-2 neutrino

Antares labs

bar 0 m

standard

SeaWiet

SensitivityE2 F

[GeV

cm-2

s-1]

ratio

sin(d)

Dt [ns]

R = 10 mR = 20 mR = 30 mR = 40 mR = 50 m

Sky map of event PDFs

Event reconstruction4D-PDF

cos q

f

-1 +100

2p

p

2D-PSF

comparison with IceCube

3s limit

sind

Galactic centre

5s discovery

E2 F [G

eV-1

cm-2

s-1]

IceCubeKM3NeT

Nikhef contributions to KM3NeT Technical design

‒ multi-PMT optical module‒ data acquisition system design

• “All-data-to-shore” has become a standard• fibre-optics network & transceivers• online data filter

– HV PMT-base, vertical electro/fibre-optics cable, power system, ...– deployment procedures (NIOZ)

Science‒ Monte Carlo simulation tools‒ Event reconstruction & physics analyses

Nikhef is a main contributor

Summary & outlook

Antares‒ taking data routinely (24h/day)‒ superior angular resolution compared to ice‒ new MoU in preparation (5 years)

KM3NeT‒ established technical convergence‒ cost estimates remain stable (200‒250 M€)‒ new ways in event reconstruction explored‒ deployment prototype model before end 2011

personal remarks site issue

– top-down• requires one of the host countries to cover 50% (?) of cost

– natural way• takes time for some of us to come to terms with the outcome

– multi-site• may be steered by funding prospects

technical design– established convergence provides necessary focus

• simulations & prototyping efforts are now made in a coherent way• [re-]evaluation by early 2012

science– strong case for neutrino astronomy beyond IceCube (and Antares)

• world-wide collaboration between IceCube, Antares and KM3NeT• “Beyond deep core” IceCube workshop, Amsterdam 26‒27 March