The ANTARES Deep Sea Neutrino

Telescope CRIS2010, 14th Sept 2010

Paschal Coyle Centre de Physique des Particules de Marseille

SN oscillations dark matter SNR AGN/GRB

Science with High Energy Neutrino Telescopes

• High energy neutrino astrophysics: galactic: SN, SNRs, m-quasars, molecular clouds, etc...

extra-gal: AGNs, GRBs, dark-GRBs, GZK, etc....

• Search for New Physics: Dark matter (Sun, GC), Monopoles, ??

• Earth-Sea Science: oceanography, sea biology, seismology, environmental monitoring...

~MeV GeV-100 GeV GeV-TeV TeV-PeV PeV-EeV > EeV

?

m

42°

interaction

Sea floor

Cherenkov light from m

3D PMTarray

nm

- Main detection channel: interaction giving an ultra-relativistic (e and tau also)

- Energy threshold ~ 10 GeV - 24hr operation, more than half sky coverage

The reconstruction is based on local coincidences compatible with the Cherenkov light front

Detection Principle

nm

p

nm

nmmp, a

4

CPPM, Marseille DSM/IRFU/CEA, Saclay APC, Paris LPC, Clermont-Ferrand IPHC (IReS), Strasbourg Univ. de H.-A., Mulhouse IFREMER, Toulon/Brest C.O.M. Marseille LAM, Marseille GeoAzur Villefranche

University/INFN of Bari University/INFN of

Bologna University/INFN of

Catania LNS – Catania University/INFN of Pisa University/INFN of Rome University/INFN of

Genova

IFIC, Valencia UPV, Valencia UPC,

Barcelona

NIKHEF, Amsterdam Utrecht KVI Groningen NIOZ Texel

ITEP,Moscow Moscow State

Univ

University of Erlangen

Bamberg Observatory

ISS, Bucarest

The ANTARES Collaboration

7 countries29 institutes~150 scientists+engineers

Region of Sky Observable by Neutrino Telescopes

Mkn 501

Mkn 421

CRAB

SS433

Mkn 501

RX J1713.7-39

GX339-4SS433

CRAB

VELA

GalacticCentre

AMANDA/IceCube (South Pole)(Ice: ~2°/0.6°)

ANTARES/KM3 (43° North)(water: ~0.2°/0.1°)

V. B

erti

n -

CP

PM

- A

RE

NA

'08

@ R

oma

Submarine cable

The ANTARES Site & Infrastructure

40 km

Site20 km from nearest land

Shore Station

IFREMER Toulon Centre FOSELEV Marine Shipyard

V. B

erti

n -

CP

PM

- A

RE

NA

'08

@ R

oma

70 m

450 m

JunctionBox

Interlink cables

40 km toshore

2500m• 900 PMTs • 12 lines• 25 storeys / line• 3 PMTs / storey

The ANTARES Detector

2006 – 2008: Building phase of the Detector

• Line 1, 2: 2006

• Line 3, 4, 5: 01 / 2007

• Line 6, 7, 8, 9, 10: 12 / 2007

• Line 11, 12: 05 / 2008

70 m

Detector Status after Completion

• 88% of modules operational at detector completion

(May 2008)

• Line 6 and Line 9

recovered for maintenance

ROV reconnection planned oct 2010

2 min

Continuous baseline: Radioactivity in the sea (40K)+ bioluminescent bacteria

Bursts: bioluminescence fromMacroscopic organisms

Counting Rates (short timescale)

40K

e4020

4019 +e+CaK →

In situ calibration with Potassium-40

40K

40Ca

g

e- (b decay)

Cherenkov

Gaussian peak on coincidence plot

Peak offsetPrecision (~5%) monitoring of OM efficiencies

Cross check of time calibration

Integral underpeak

Time evolution of K40 coincidence rate

• All OM pairs of Line1 during more than 2 years• OM gain drop reduces efficiency• Recovery after threshold retuning• Recovery due to HV off during period of cable repair

Optical Beacons: time calibration, absorption length

~70 m

~150 m

Acoustic Position Alignment

r = (a z - b ln[1-cz] ) v2

Z(m)

r(m)

Example forSea currentv= 25 cm/srmax = 22m

Measure every 2 min:Distance line bases to 5 storeys/line

and also storeyheadings and tilts

Line position measurements

Acoustic positioning:Hydrophone positionsfrom JulyDec 2007

Storey 1Storey 8

Storey 14Storey 20Storey 25

Radial displacement

Within a line Between lines

Acoustic positioning:Precision ~ few cms

Track Reconstruction

Online Algorithm Offline Algorithm• Storey rotation ignored -single points• Line assumed vertical (no acoustic info)

• Immediately available• non-optimal angular resolution

• Uses final alignment • Loose selection• Full likelihood fit• Multiple starting points

• not immediately available• excellent angular resolution

12 line detector

Expected Performance (full detector)

Neutrino effective area

Ndet=Aeff × Time × Flux

• For E<10 PeV, Aeff grows with energy due to the increase of the interaction cross section and the muon range.

• For E>10 PeV the Earth becomes opaque to neutrinos.

Angular resolution

• For E<10 TeV, the angular resolution is dominated by the - angle.

• For E>10 TeV, the resolution is limited by track reconstruction uncertainties.

n

m

reconstructed up-going neutrino: detected in 6/12 detector lines:

Event Displays

reconstructed down-going muon: detected in all 12 detector lines:

Coincidences between adjacent storeys (low E muons)

Energy threshold ~ 4 GeV(track length)

Delay between storeys

Δt

Pedestal = random background (K40, bio)

Integral under peak ~ event rate ~ muon flux

Peak offset, width and shape = f (muon angular distribution, OM angular acceptance, …)

µ

Event rate as function of floor depth

By repeating the analysis for every detector storey the muon flux reduction with depth is directly measured

Systematic errors mainly in normalization (+50/-35%), otherwise ~3%

Published in Astrop. Phys 33 (2010) 86-90

Depth Intensity Relation from Zenith Distribution

Zenith angle distribution of muon flux at 2000 m

accepted for publication in Astroparticle Physics11 july 2010, arXiv:1007.1777

2,5km

6km

Livetime:168 days276 upward events

(multi-line fit)

5-Line Data: Zenith Distribution

downup

horizontal

p

nm

nm

p, a

g

Candidate List Search

Search applied to 24 pre-selected sources

276 neutrino candidates

Candidate List Search

Largest excess (4.1 events) at HESS J1023-575: post-trial prob=3.4% (1.8sigma, 1-sided)

Nevents p-value

(Pre-trial)

1.0 0.08235

1.6 0.00773

4.1 0.00142

0.00.5

0.1720.00.00.00.01.6

0.048940.00.00.00.00.00.00.00.00.00.00.01.1

0.1020.00.0

All Sky Search

• Most significant cluster 4.2 events decl =-9.5 degree, RA=222.15 degree

This value or higher expected in 31% of toy Monte Carlo experiments

276 neutrino candidates

Coming Very Soon….2007+2008 data

Live time: 295 days2040 upgoing events

+ significantly better angular resolution

Zenith distribution Scrambled skymap

Point Search Limits and Sensitivity

6 months of half detector already similar sensitivity to many years of MACRO, SK

2007-2008 data will give best sensitivity in Southern Sky

2009-2010 data in the pipeline

Assumes E-2 flux spectrum

Diffuse Flux Search

# of PMTs with prompt and late photons R= ---------------------------------------------------- # of all PMTs contributing to the event

(See presentation of Simone Biagi- later today)

<

Diffuse Flux Search

Transients with ANTARES

Requires Satellite trigger (Swift, Fermi)

Low backgrounds due to direction and time coincidences

Full sky search (see all GRBs)

24hr/24hr

Sliding time window around events

Sensitive to dark bursts

optical follow up to identify source Fast online reconstruction

Rolling searchTriggered search

GRB Neutrino Spectrum

II. Or use of the Swift, Fermi LAT γ-ray spectrum: p-γ interaction model neutrino spectrum

I. The so-called Waxman–Bahcall GRB flux, issued from average GRB parameters measured by BATSE to determine an all-sky neutrino flux from the GRB population.

Guetta et al, Astropart. Phys. 20 (2004) 429

Waxman and Bahcall, PRL 78 (1997) 2292

20 GRB with measured redshift

37 GRB with no redshiftz = 2

For all GRB in 2008:

A special case, the GRB080916C

Opacity constraints lower limit on the boost Lorentz factor (600-900)

sensitivity ~50 above the W&B fireball model (Г=600)

analysis of the ANTARES data on-going (unblinding requested)

Sensitivity of ANTARES to GRB080916C (LAT)

Discovered by the Fermi-LAT (redshift z=4.35)

One of the most powerful GRB (Eiso~8.8x1054ergs)

Abdo et al, Science 323 (2009) 1688

Optical Follow-Up with TAROT

FoV 1.86°x1.86°10s pointing V<17 (10s) V<19 (100s)

TAROT La Silla

Doublets (15min, 3°*3°) or Singlet (high-energy) triggers

Dark Matter: Spin DependentEarth

Sun WIMPs gravitational trappedvia elastic collisions in the sun

Antares

“soft” annihilation : χχ -> bb

Mc = 1 TeV

“hard” annihilation : χχ -> W+W-

: neutrino : anti-neutrino

Mc = 1 TeV

Limits from 5-line data

• Extremely high energy deposition

• Direct Cherenkov light for > 0.74

• light from δ-rays for > 0.51

• Dedicated reconstruction ( free)

• likelihood ratio free to =1

• Expected Sensitivity using 2008 data

AMANDA II 137 days

M.M. with =b 0.65

MAGNETIC MONOPOLES

Summary

ANTARES infrastructure completed since May 29th 2008 • Detector operation and calibration understood• Maintenance capability demonstrated

Exciting physics program ahead many thousands of neutrinos already reconstructed Unexplored regions of sensitivity in southern hemisphere astronomical sources, dark matter, oscilllations, …… Multi-messenger approach strongly pursued

Real-time readout and in-situ power capabilities facilitates a large program of synergetic multi-disciplinary activities:

acoustics, biology, oceanography, seismology……

Major step towards the KM3NeT multi-disciplinary deep-sea research infrastructure (Piera Sapienza talk)

The KM3NeT Challenge

12 lines, 900 PMTs

~250 lines, ~30000 PMTs

– Maximise physics potential• Substantial improvement over ICECUBE• Instrumented volume ~5 km3• Angular resolution ~0.1 degrees (E>10 TeV)

– Build in a reasonable time 4 years• New deployment techniques• Speed-up integration time• Sub contract part of the production• …

– At a reduced cost• Factor 2 reduction cf ANTARES• Simplified architecture• Reduced maintenance• Multi-line deployments• …

(See presentation Piera Sapienza later today)

Sensitive to Cosmic Ray Composition

Preliminary

Preliminary

Transient Sources

GRB neutrinos: Relatvistic Jets (Fireball Modèl) Meszaros & Rees, Waxman

SN neutrinos: mildy relativistic choked jet,no prompt optical counter-partRazzaque & al,, Ando & Beacom