RICH 2007 6 th International Workshop for Ring Imaging Cherenkov Counters September 15 th – 20 th 2007, Trieste – Italy September 15 th – 20 th 2007, Trieste

RICH 2007RICH 200766thth International Workshop for Ring Imaging Cherenkov Counters International Workshop for Ring Imaging Cherenkov Counters

September 15September 15thth – 20 – 20thth 2007, Trieste – Italy 2007, Trieste – Italy

KM3NeTKM3NeT

Towards a kmTowards a km3 3 volume volume neutrino telescope in the neutrino telescope in the

Mediterranean SeaMediterranean Sea

Christos MarkouChristos MarkouNational Center for Scientific Research ‘Demokritos’National Center for Scientific Research ‘Demokritos’

For the KM3NeT CollaborationFor the KM3NeT Collaboration

Christos Markou, NCSR ‘Demokritos’ RICH2007, September 16Christos Markou, NCSR ‘Demokritos’ RICH2007, September 16thth 2007, Trieste, Italy2007, Trieste, Italy

What is KM3NeT?What is KM3NeT?

Future deep sea research facilityFuture deep sea research facilityNext generation water Cherenkov Next generation water Cherenkov

neutrino telescope in the neutrino telescope in the MediterraneanMediterranean

Deep sea infrastructure for Deep sea infrastructure for associated sciences:associated sciences:

Oceanography, Marine Oceanography, Marine Biology, Biology, Environmental Science, Environmental Science, Geology and Geology and GeophysicsGeophysics


KM3NeT consortiumKM3NeT consortium

38 Institutes from 11 European 38 Institutes from 11 European Countries:Countries:

Cyprus, France, Germany, Greece. Cyprus, France, Germany, Greece. Ireland, Italy, Malta, The Ireland, Italy, Malta, The

Netherlands, Romania, Spain, UKNetherlands, Romania, Spain, UK


KM3NeT Scientific KM3NeT Scientific goalsgoals

High Energy neutrino observation High Energy neutrino observation Investigation of the nature of astrophysical Investigation of the nature of astrophysical

objectsobjects

Production mechanisms of High energy Production mechanisms of High energy neutrinosneutrinos

(acceleration mechanisms, top-down (acceleration mechanisms, top-down scenarios, etc) scenarios, etc)

Origin of cosmic raysOrigin of cosmic rays

Indirect search for dark matterIndirect search for dark matterAssociated sciencesAssociated sciences


Astroparticle physics with Astroparticle physics with ν ν Telescopes Telescopes

Low-energy limit:• short muon range• small number of

photons detected• background light

from K40 decays

High-energy limit:• neutrino flux

decreases like E–n (n ≈ 2)

• large detectionvolume needed.


Point SourcesPoint Sources

Association of specific astrophysical objects to Association of specific astrophysical objects to observed neutrino fluxobserved neutrino flux

Combination with other observations, energy Combination with other observations, energy spectrum and specific time stamp and spectrum and specific time stamp and structure, will provide clues and insight on structure, will provide clues and insight on specific physical processes in the sources. specific physical processes in the sources.

Simultaneous observations of GRB’s will allow Simultaneous observations of GRB’s will allow for lower thresholds, larger efficiency, lower for lower thresholds, larger efficiency, lower backgroundsbackgrounds

Very good angular resolution of water Very good angular resolution of water Cherenkov telescopes (0.3Cherenkov telescopes (0.3oo for for ν ν energy ~10 energy ~10 TeV, better than 0.1TeV, better than 0.1oo above 100 TeV) above 100 TeV)


Possibilities…Possibilities…

Galactic :

Extra-galactic :

Nebulae Supernova remnants Microquasars

AGN’s GRB’s


Neutrino flux Neutrino flux predictionspredictions

mean atm. flux (Volkova, 1980, Sov.J. Nucl.Phys., 31(6), 784

Kappes et al.,

ApJ 656:870, 2007

(astroph/0607286)

Estimated Estimated neutrino neutrino flux – in flux – in

reach for reach for KM3NeTKM3NeT

All calculations show that we need kmAll calculations show that we need km33 –scale detectors –scale detectors


Neutrino HuntersNeutrino Hunters


Northern Hemisphere?Northern Hemisphere?

Mkn 501Mkn 421

CRAB

SS433

Mkn 501RX J1713.7-39

GX339-4

SS433

CRAB

GalacticCentre

VELA

South Pole Mediterranean


……Definitely!Definitely!

We certainly need Northern telescope to cover the galactic plane!


Why in the Why in the Mediterranean sea?Mediterranean sea?

Complementary observations to ICECUBEComplementary observations to ICECUBE Observation of the Galactic centerObservation of the Galactic center Good water qualityGood water quality Deep waters close to shoreDeep waters close to shore Existing infrastructuresExisting infrastructures Favorable weather and sea conditions for Favorable weather and sea conditions for

sea operationssea operations Significant expertise for sea water v

telescopes already exists in European Countries


How to design a kmHow to design a km33 ν ν telescope?telescope?

dilute

scale up

Existing telescopes “times 30” ?

•Too expensive•Too complicated

(production, maintenance)•Not scalable

(readout bandwidth, power, ...)

Large volume with same number of PMs?

•PM distance: given by absorption length inwater (~60 m) and PM properties

•Efficiency loss for larger spacing

R&D needed:•Cost-effective solutions

to reduce price/volume by factor ~2

•Stabilitygoal: maintenance-free detector

•Fast installationtime for construction & deploymentless than detector life time

• Improved components

new design


KM3NeT timelineKM3NeT timeline

Feb 2006 Jan 2008 Mid 2010

CDR TDR

Design Study Design Study

Preparatory PhasePreparatory Phase

Production model for detection unit

Financial plan

Assembly model

ConstructionConstruction

Tenders

Now

Targeted Budget: 220 – 250 M€ (ESFRI Roadmap)


KM3NeT Design ReportKM3NeT Design Report

DS is funded by EU FP6DS is funded by EU FP6 Design of a detector with the followingDesign of a detector with the following

specs:specs: Effective volume ≥ 1 kmEffective volume ≥ 1 km33

Muon angular resolution ~ 0.1Muon angular resolution ~ 0.1oo for for νν’s above 10 TeV’s above 10 TeV Energy threshold ~ few 100s GeV (~100 GeV Energy threshold ~ few 100s GeV (~100 GeV

pointing)pointing)Sensitivity to all neutrino flavors, CC/NC reactionsSensitivity to all neutrino flavors, CC/NC reactionsField of view: close to 4Field of view: close to 4π π for high energiesfor high energies

Deliverables : Deliverables : Conceptual Design Report (workshop in Amsterdam Conceptual Design Report (workshop in Amsterdam

next month)next month)Technical Design Report (Spring 2009)Technical Design Report (Spring 2009)


Questions needing Questions needing answers:answers:

Architecture ? (strings vs. towers vs. new Architecture ? (strings vs. towers vs. new design)design)

Detector configuration? (cubic vs. ring vs. Detector configuration? (cubic vs. ring vs. clustered vs...)clustered vs...)

How to get the data to shore? (optical vs. How to get the data to shore? (optical vs. electrical, electronics off-shore vs. on-shore)electrical, electronics off-shore vs. on-shore)

Calibration? Calibration? Design of photo-detection units? (large vs. Design of photo-detection units? (large vs.

several small PMs, directionality, …)several small PMs, directionality, …) Deployment? (dry vs. wet by ROV/AUV vs. wet Deployment? (dry vs. wet by ROV/AUV vs. wet

from surface)from surface) Site selection? Site selection?


Detector optimisation: Detector optimisation: Sensitivity and efficiencies Sensitivity and efficiencies calculated using different calculated using different

configurationsconfigurations

Cuboidal, ring, clustered, etc, with various string Cuboidal, ring, clustered, etc, with various string configurations configurations


Effective areaEffective area

Effective area is calculated:Effective area is calculated:

AAeffeff(E,(E,θ,φ) = θ,φ) = S NS Nrecrec(E,(E,θ,φ)θ,φ) / / NNtottot

∫ ∫ AAeffeff(E,(E,θ,φ) θ,φ) F(E,F(E,θ,φ) θ,φ) ddΩΩ

∫ ∫ F(E,F(E,θ,φ) θ,φ) ddΩΩSSeffeff(E)(E) = =


Neutrino effective area Neutrino effective area estimationestimation

Configuration 1 (1 km3):127 lines in hexagonal array100m line spacing25 stories, 15 m apart3 Antares (10”) PMTs per storey

Configuration 2 (1 km3):225 lines in a cubic grid95m line spacing36 stories, 16.5 m apart21x3”PMTs per storey

Antares site parameters Ref. ICRC0865, J. Carr et al Thesis S. Kuch, Erlangen


Sensitivity to HESS Sensitivity to HESS sourcessources

Ref. ICRC0865, J. Carr et al

Neutrino energies 1TeV – 1 PeVMuon event rates for 5 years of data

takingSources (~0.2o in extent) on the galactic

disk

ττ11, τ, τ11΄ - ΄ - full recostruction of eventsfull recostruction of events

ττ22, τ, τ22΄ - ΄ - simple selection (at least 6 OM hits)simple selection (at least 6 OM hits)


Optical modules: Optical modules: Exploring new ideasExploring new ideas

Segmentation of photo cathode of 10” PMT

Smart tubeX-HPD(R&D)

multi PMTs in one glass sphere Ref. ICRC0489, P. Kooijman

“Flykt” sphere


Readout/data Readout/data transmissiontransmission

Three options studied: a la Antares

Improved front-end chip new FPGA/CPU

1-1 wire/fiber network new front end chip multi-functional FPGA system

1-1 photonics based network front-end chip or pic on-shore timestamp on-shore multi-l laser reflective optical modulator off shore on-shore smart TDC

multi cw laser

50 .. 100 ’s GPSclock

dispersion comp.

12

3

45

123

45

To

optic

al

m

od

ule

s

3ns strobe

12345

To

rea

dout

m

od

ule

s

1234512345

1 0 1 0 0 0 0 0 01 0 1 0 0 0 0 0 0

101000000101000000111000101111000101

time-stampbitpattern

Bitpattern every 3ns

Po

ssib

le z

ero

sup

pre

ssio

n Time callibration signal

Bidirectional optical

amplifier.

modulator.

deserializer

serializer

Reflective modulator

To analysis farm

Ref. ICRC. 0490, P. Kooijman et al


Detector UnitDetector Unit

Rigid or flexible structure?Rigid or flexible structure?Both options are feasible, but have to Both options are feasible, but have to

assess:assess:ReliabilityReliability

#(wet mateable) connectors#(wet mateable) connectorsProduction modelProduction model

Distributed versus single assembly siteDistributed versus single assembly siteTransport to deployment siteTransport to deployment site

Deployment modelDeployment modelDependence on weather conditionsDependence on weather conditions#(sub)sea operations: #OM per hour deployment#(sub)sea operations: #OM per hour deployment


SeaTop calibrationSeaTop calibration

Three stations at 20 m distances with 16 m2

scintillators each

Calibration: angular offset efficiency angular

resolution absolute position


Site SelectionSite Selection KM3NeT report input for discussion:KM3NeT report input for discussion:

Evaluation of existing water, oceanographic, Evaluation of existing water, oceanographic, biological and geological data from candidate sitesbiological and geological data from candidate sites

Final choice will depend on issues like:Final choice will depend on issues like: DepthDepth Distance from shoreDistance from shore Bioluminescence rateBioluminescence rate SedimentationSedimentation BiofoulingBiofouling Sea currentsSea currents Earth quake profileEarth quake profile Access to on-shore high speed networksAccess to on-shore high speed networks …………

Socio-political/regional considerationsSocio-political/regional considerations


Conclusions and Conclusions and Outlook Outlook

The ANTARES, NEMO and NESTOR projects The ANTARES, NEMO and NESTOR projects have proven the feasibility of building and have proven the feasibility of building and operating deep sea neutrino telescopes in the operating deep sea neutrino telescopes in the Mediterranean.Mediterranean.

There are compelling scientific reasons for the There are compelling scientific reasons for the construction of neutrino telescopes of kmconstruction of neutrino telescopes of km33-scale. -scale.

It is essential to complement IceCube with a It is essential to complement IceCube with a detector in the Northern Hemisphere. detector in the Northern Hemisphere.

The KM3NeT Design Study is well under way, The KM3NeT Design Study is well under way, with EU FP6 funding a 3-year R&D phase, with EU FP6 funding a 3-year R&D phase, resulting in the resulting in the Conceptual Design ReportConceptual Design Report in in November 2007 and the November 2007 and the Technical Design ReportTechnical Design Report by early 2009.by early 2009.


Conclusions and Outlook Conclusions and Outlook (cont.)(cont.)

We hope for the next step: the We hope for the next step: the ‘Preparatory Phase’ in FP7 (2008 – 2011)‘Preparatory Phase’ in FP7 (2008 – 2011) Site selectionSite selectionCommitment for constructionCommitment for constructionGovernance and legal structureGovernance and legal structureSystem prototypeSystem prototype TendersTenders

To be followed by the Construction Phase To be followed by the Construction Phase 2010 – 2013 for the KM3NeT detector.2010 – 2013 for the KM3NeT detector.

Documents

RICH 2007 6 th International Workshop for Ring Imaging Cherenkov Counters September 15 th – 20 th 2007, Trieste – Italy September 15 th – 20 th 2007, Trieste