1

KM3NeT

IDM/TeVPA conference2328 June 2014, Amsterdam, the Netherlands

Maarten de Jong on behalf of the KM3NeT collaboration

The next generation neutrino telescope in the Mediterranean

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Introduction

• Discovery and subsequent observation of high-energy neutrino sources in Universe– field of view includes central region of our Galaxy– synergy with Earth & Sea sciences

• KM3NeT is a new Research Infrastructure– network of cabled observatories– located in deep waters of Mediterranean Sea– hosting multi-km3 neutrino telescope

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Astro-Particle Physics

p

n

g

p + p p+, p‒, p0

p± m±,nm ,ne

p0 g g

e + g e + g Electro-Magnetic

Hadronic

?

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Detection principle

muon

wave front1 2 3 4 5

~ km

~ 100 mneutrino

interaction

time resolution 1 nsposition resolution 10 cm angular resolution 0.1 deg

PDF of light

Dt [ns] Dt [ns]

R = 50 m R = 100 m

1 TeVmuon

optical backgroundR

S/N ~102

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KM3NeT

Architecture

neutrino telescope

shore station

remote accessto data

remoteoperationon off

computercenter

0.1

1 Tb/

s

10100 Mb/s

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Design~

600 m

Optical module

Launcher vehicle

‒ 31 x 3” PMTs‒ low-power HV‒ LED & piezo inside‒ FPGA readout‒ White Rabbit‒ DWDM

‒ rapid deployment‒ autonomous unfurling‒ recoverable

17”

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1st prototype

April 2013 KM3NeT@Antares

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Multiplicity

Rate

[Hz]

PMT orientation [deg.]

atmospheric muons K40 random coincidences+ data

photon counting directionality

1st prototype¶

atmospheric muons+ data (M ≥ 7)

shadowing

Rate

[a.u

.]0

10

20

30

40

50

¶ http://arxiv.org/abs/1405.0839

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2nd prototype

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2nd prototypeRa

te [H

z]

Multiplicity

May 2014, KM3NeT-Itonline monitoring

Atmosphericmuons

num

ber o

f eve

nts

Dt [ms]

Time difference betweenoptical modules

Atmosphericmuons

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Phase Total costs¶

[M€]Primary deliverable Status

1 31 Proof of feasibility of network of distributed neutrino telescope

Funded

1.5 80–90 Measurement of neutrino signal reported by IceCube

Letter of Intent

2 220–250 Neutrino astronomy ESFRI road map

Phased implementation

¶ Total costs ≡ Total cumulative costs.

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KM3NeT phase-1.5

Measurement of neutrino signal reported by IceCube

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IceCube

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Cascade analysis 1.0 cut & count

1. Online data filter– 5 (or more) coincidences between PMTs in same optical module

(DT = 10 ns)

2. Event filter– number of hits ≥ 2000

3. Vertex cut– veto atmospheric muons

4. Energy cut– total time-over-threshold ≥ 15 ms

5. MRF/MDP cut– 2D cut based on Boosted Decision Tree & energy estimate

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3.) Atmospheric muon veto

cosmic neutrinos atmospheric muons

R2 [103 m2] R2 [103 m2]

z [m

]

vertex cutdetector volume

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5.) Signal / Noise

BDT (topology of event)

S e

vent

s / 6

mon

ths

atmospheric muonsatmospheric neutrinos (tracks)atmospheric neutrinos (showers)cosmic neutrinos (tracks)cosmic neutrinos (showers)

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Sensitivity¶

¶ Standard footprint; 30% better FOM with 30% larger inter-string distance.

years

sign

ifica

nce

[s]

0 1 2 3 4 5 6 7

1

2

3

4

0

5

6

7

muon tracks

cascades

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KM3NeT phase-2

Neutrino astronomy

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Galactic sourcesRXJ1713¶

Vela X§

years

sign

ifica

nce

[s]

RXJ1713-3946

Vela X

¶ S.R. Kelner, et al., Phys. Rev. D 74 (2006) 034018. § F.L. Villante and F. Vissani, Phys. Rev. D 78 (2008) 103007.

(binned analysis)

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suddenEddy currents

Temperature

France

observatoryfood supply

Bioluminescence

short lived (rare) eventsdominate deep-sea life

permanent observatory

time profile

Earth & Sea sciences

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Addendum

ORCA is a feasibility study for a measurement of the mass hierarchy of neutrinos

with the KM3NeT research infrastructure

– ORCA (and other detectors) can use same technology but with different topologies of the photo-sensor grid

– ORCA (and other detectors) can be embedded in the KM3NeT research infrastructure at (relatively) low cost

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KM3NeT outlookNeutrino physics Neutrino astronomy

mn

0 1 2 30

1

2

3

4

5

ORCA+40 M€

Phase-2+130170 M€

Phase-1.5+5060 M€

years

sign

ifica

nce

[s]

1

2

3

4

5

0 1 2 3 4 5 6years

Vela XRXJ1713

years0 1 2 3 4 5 6 7

1234

0

567

muon trackscascades

combinedcascadestracks