Deep-sea research infrastructure for high-energy neutrino ... · NESTOR 1992 2008 Attenuat NESTOR 1992: S A Khanaev et al (1992) G.Riccobene et al. S.A.Khanaev et al.(1992) SB: Smith,

Deep-sea research infrastructure for high-energy neutrino astronomyneutrino astronomyresearch goalsdetection principledetection principleKM3NeT concept / layoutEarth and Marine sciencesEarth and Marine sciencesoptical sensors deploymentdeploymentdata transfersummary

Herbert Löhner, KVI, University Groningen, The Netherlandson behalf of the KM3NeT Consortium

summary

11th Pisa Mtg. 24-30 May 2009 H. Löhner, Deep-sea research infrastructure 1

neutrino astronomyorigin of extreme energies observed in cosmic rays?• ? origin of cosmic rays 1020 eV• ? astrophysical acceleration mechanism HESSp y• ? origin of relativistic jets• ? dark matter

cosmic sources of neutrinos• Active Galactic Nuclei: super-massive

bl k h l i t f l iblack hole in center of galaxies• micro quasars: X-ray binaries (in our galaxy)• supernova remnants and shock acceleration

TeV γ rays (p+X → π0 → γγ) in centre of our galaxy from supernova remnant RX J1713.7-39.supernova remnant RX J1713.7 39.

Expect:p+X → π±

→ ( )νννn

γ

( )

p


neutrinos reach Earth undisturbed: need sensitivity and angular resolution

complementary sky views (galactic coordinates)(g )

AMANDA / IceCube ANTARES (43o N)(South Pole) (Mediterranean Sea)(South Pole) (Mediterranean Sea)

includes Galactic Center

acceptance range1.5 π sr common view per day


detection principleνμ μ

W

Neutrinos can interact through charged current interactionin the vicinity of a neutrino telescope -ν

νN XW in the vicinity of a neutrino telescope

up-going neutrinos passing through the Earth are free from atmospheric muon background

µγc

atmosphere

107 atmospheric μ per yearknown atmospheric

ν background

º70θc = 42º

Earth

Sea [ ] 6.0)TeV(º7.0

ν

μνE

≤Θ −

νμ

Earth

cosmic ν

νμ track reconstructed from μ Cherenkov cone passing 3D grid of PMTs


μ Cherenkov cone passing 3D grid of PMTs

KM3NeT conceptarray of optical modules (OM)sensing Cherenkov light

instrumented volumemin. 1 km3

sensitive to all ν flavourssensitive to all ν flavours

Eν > 0.1 TeV

angular resolution min 0.1o for Eν > 10 TeV

acceptance: up-going tracks,μ


up to 10o above horizonνμ

KM3NeT Consortium42 institutes from:42 institutes from:Cyprus, France, Germany, Greece, Ireland, Italy, Cyprus, France, Germany, Greece, Ireland, Italy,

Netherlands, Romania, Spain, UKNetherlands, Romania, Spain, UKpilot projects:pilot projects:

+ + ++ + +..

funded by FP6 for Design Study, by FP7 for Preparatory Phase,on the ASPERA roadmap

Conceptual Design Report public since April 2008, aim for: Technical Design Report until end 2009,

t t C t ti Ph i 201111th Pisa Mtg. 24-30 May 2009 H. Löhner, Deep-sea research infrastructure 6

start Construction Phase in 2011

candidate deployment sites

criteria:bioluminescence,40K background40K background,salinity, currents,water transparency:water transparency:transmission length(recent LAMS data) ≤ (46+3) m at

ANTARES, NEMO, NESTORdeployment sites

≤ (46 3) m at depth 2500 - 3000 m at λ = 450 - 470 nm


data from LAMS (Light Amplitude Measurement Station) 2008light attenuation

h (m

)data from LAMS (Light Amplitude Measurement Station) 2008

Zhukov et al.,combined with

i d t

ion

leng

th

(pure water)

previous data

NEMO data:G Riccobene et al (2006)

NESTOR1992

2008Atte

nuat

i ( )

NESTOR 1992:S A Khanaev et al (1992)

G.Riccobene et al. (2006)

2008 S.A.Khanaev et al.(1992)

SB: Smith, Baker (1981)

Max. attenuation:(46+3) m in the depth of 2500 m and 3000 m at

t≅ pure water

450 nm and 470 nm

determines distance b t d t ti it

t


Wavelength (nm) between detection units

bioluminescence• abundance of

bioluminescent sourcesbioluminescent sources as function of depth estimated fromestimated from measurements

Abundance of bioluminescent animals

Black: east Med. Sea.Grey: west Med. Sea.

bioluminescent animals per m3 of sea water as function of depth off Pylos

deeper less bioluminescence

o y os


deeper less bioluminescence

Earth and Marine sciencesstudies of

l l i l ti• large-scale ocean circulation• specific processes, e.g. internal waves e.g. internal waves • effects on sediment and nutrients redistribution• bio-acoustics high resol tion temperat re profilinghigh resol tion temperat re profilingbio acoustics• …

ve

ve

))high resolution temperature profilinghigh resolution temperature profiling

ght a

bov

ght a

bov

tom

(m)

tom

(m)

dd

heig

heig

bott

bott

H. H. vanHarenvanHaren, NIOZ, NIOZ


yeardayyearday

mechanical structures

NEMO flexible tower

NESTOR rigid towerNESTOR rigid tower


ANTARES flexible strings

buoy

storey

3 10” PMT/storey25 storeys/line12 detection lines:~900 PMT +

ti d t ti

350 m

acoustic detection

14 5 m

350 m

14.5 m

100 m

Junctionbox

45 km

~60-75 mreadout cables

45 km electro-optical cable


status of ANTARES experimentinstallation completed May 2008

footprint of the 12-line detector in atmospheric muons

x, y coordinates of track fits at the

f ftime of the first triggered hit

~ 0.05 km2

sensitive surface

Poster byJ A M ti M


J.A. Martinez-Mora

up-going muon: neutrino candidateANTARES 12-line data: reconstruction of muon trajectory from time, charge and position of PMT hitsassuming relativistic muons emitting Cherenkov light

heig

ht (m

)


time (ns)h

neutrino candidatesfrom track zenith distributionfrom track zenith distribution

5-line data (May-Dec. 2007) 121 days121 days,multi-line fit,1.3 ν candidates/day (hi h it l )i d i (high purity sample)up-going down-going

( ith l ) up-going down-going

10-line data (Dec. 2007 – May 2008) 109 days

- cos(zenith angle) up going down going

109 days,multi-line fit,2 ν candidates/day (high purity sample) sin(zenith 90)


(high purity sample) sin(zenith-90)- cos(zenith angle)

design options for KM3NeT detection units

h i t l t t N h i t l t t

for KM3NeT detection units

horizontal structures> 2 OMs per storey

No horizontal structures1 OM per storey

1 large(10”) PMT per OMcopper/fiber readout

31 small (3”) PMTs per OMfiber readoutpp /

sensitivity sensitivity, cost and reliability, production technique and deployment being studied to constrain final TDR decisions

acoustic detection:Poster by


J.A. Martinez-Mora

optical module design options

1 10” PMT1 10” PMT 31 3” PMTs 31 3” PMTs 17”glass container:17”glass container:improved Antares OM improved Antares OM with electronics insidewith electronics inside

possibly with 13” glass possibly with 13” glass containercontainer

17” glass container17” glass containerhigh 2high 2‐‐photon purity (sea background) photon purity (sea background) looking down + ~upwards (atm. muons)looking down + ~upwards (atm. muons)g p ( )g p ( )large photocathode arealarge photocathode area

aim for

17” glass container17” glass container4 anodes + mirrors:4 anodes + mirrors:di ti itidi ti iti

higher Quantum Efficiency:Super bialkali with ca. 35%Ultra bialkali with > 40%


direction sensitivedirection sensitive

… or hybrid solutionsy• use high voltage (~20kV) to

accelerate photo electronsaccelerate photo electrons onto scintillator

• detect scintillator light withdetect scintillator light with small standard PMT

Quasar 370(Baikal)

advantages:advantages:very good photo-electron counting, high quantum efficiency (40%),large angular sensitivity (3 π)g g y ( )

prototype development byCERN/Photonis/CPPM collaboration,


Photonis PMT development terminated

simulations of storey configurationsin hexagon base arrangementin hexagon base arrangement

by J. Carr, D. Dornic

8m

NuOne6 PMT 8” QE35%

1m

6 PMT 8 QE35%

12m

ANTARES3 PMT 10” QE23%

0.4m

NEMOMultiPMT/SEAWiet31 PMT 3” QE42%


4 PMT 10” QE23%

overall efficiency:trigger reconstruction selectiontrigger, reconstruction, selection

e.g. 130m spacingbetween Detection Units (DU)

up to x2 improvement b ANTARES iblabove ANTARES possible


point-source sensitivity

Antares sensitivity:comparable withcomparable with Amanda,extended to

i d li inegative declinations

KM3NeT referencedetector sensitivityx3 better than IceCube


cable structure

pressure tests of cableand fibre connections


Option: optical network shore deep-sead i d t t d bCW DWDM (Dense Wavelength Division Multiplexing) designed, tested byJ. Hogenbirk et.al. , Nikhef

CW DWDM (Dense Wavelength Division Multiplexing) lasers (up to 100 wavelengths)

DWDM Mux

100 km fibre path

reflectiveSingle fibre feed sharedfor feed wavelength comb

l1

DU OM/node

Comms & Timing

Data out

reflectivemodulator

Power splitters to feed up to 100 units1 of 100fibres

for feed wavelength comb

PMTsWDM Demux

Data Receiver

Data out

Optical Amplifiers

2km

DWDMDemux

Optical

Receiver

shore stationl1

OMs

Optical receiverElectrical drive

to modulator.(single modulator gates all DWDM Wavelengths)

10 Gb/s bandwidth, 50 GHz channel spacing


DWDM Wavelengths)deep-sea stationσ propagation time) < 1 ns

SummaryKM3NeT: door to neutrino astronomy

viewing the Galactic Center

integral platform for Marine and Earth sciences

milestones:Conceptual Design Report early 2008

Technical Design Report end 2009g p

pilot studies with ANTARES, NEMO, NESTOR exploited for optimization:

point source sensitivity ~50 times that of ANTARES~ 3 times that of IceCube

optical network for data transmission to shore

i i f t t f t ti i 2011


aiming for start of construction in 2011

Documents

Deep-sea research infrastructure for high-energy neutrino ... · NESTOR 1992 2008 Attenuat NESTOR 1992: S A Khanaev et al (1992) G.Riccobene et al. S.A.Khanaev et al.(1992) SB: Smith,