Results from the ANTARES Deep Sea Neutrino Telescope

Maurizio SpurioOn behalf of the ANTARES Collaboration

Università di Bologna and INFN

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SNR oscillations dark matter m-quasars GRBs magnetic Fermi-bubbles monopole

Science with Deep Sea Neutrino Telescopes• High energy neutrino astrophysics:

• galactic: SN, SNRs, m-quasars, molecular clouds, etc…• extra-galactic: AGNs, GRBs, choked-GRBs, GZK, etc....

• Search for New Physics: Dark matter (Sun, Galatic Centre), Monopoles, nuclearites, ??

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

GeV-100 GeV GeV-TeV TeV-PeV PeV-EeV > EeVM.S

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Neutrinos and Multi-Messenger Astronomy

Protons/ Cosmic Rays:• Detected on Earth up to extremely high energies: 108 TeV• Hard to study sources due to deflection by magnetic fieldsPhotons:• Produced in leptonic (synchrotron, IC) and hadronic (0) processes• Absorbed at higher energies and large distancesNeutrinos (and GW):• Unambiguous signature of hadronic acceleration• Not deflected by magnetic fields or absorbed by dust• Horizon not limited by interaction with CMB/IR• Can escape from region of high matter density• Can be time correlated with optical signals

® leptonic vs hadronic models

® identify Galactic and extraGalactic cosmic ray sources

® hadronic accelerators exist, but where?

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Cosmic Rays, photons and neutrinos

• Hadronic cascades (as for atmospheric showers) p/A + p/ ®

m m

m m

e e m e e m

• Primary acceleration («Bottom-Up»)Stochastics shocks (Fermi mechanism)Explosion /Accretion / Core collapse • Benchmark Extra Gal. flux Waxman-Bahcall

• But HE also from electromagnetic processes Synchrotron Inverse Compton

e:m: =1:2:0 source e:m: =1:1:1 Earth ® nsoscillatio

~ 500 events /yr/ km2

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m

42°

interaction

Sea floor

Cherenkov light from m

3D PMTarray

m

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

- Energy threshold ~ 20 GeV- 24hr operation, more than half sky coverage

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

Detection Principle

m

p

m

mmp, a

Physical Background sources

Atmospheric m 109 per yearAtmospheric 104 per yearCosmic 0-10 per year ?

Atmospheric muons: only downgoingShield detector & reject downward goingmuons

downgoingupgoing

T. Chiarusi, M.S. Eur. Phys. Journal C (2010) 649-701 . arXiv:0906.2634M.S

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CPPM, Marseille DSM/IRFU/CEA, Saclay APC, Paris LPC, Clermont-Ferrand IPHC, Strasbourg Univ. de H.-A., Mulhouse LAM, MarseilleCOM, MarseilleGeoAzur Villefranche INSU-Division Technique

Univ./INFN of Bari Univ./INFN of Bologna Univ./INFN of Catania LNS–Catania Univ./INFN of Pisa Univ./INFN of Rome Univ./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• Univ. of Wurzeburg

ISS, Bucarest

The ANTARES Collaboration

8 countries31 institutes~150 scientists+engineers LPRM, Oujda

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The ANTARES Site & Infrastructure

Shore Station

IFREMER Toulon Centre

FOSELEV Marine

-2475m

40 km submarine cable

70 m

450 m

JunctionBox

Interlink cables

40 km toshore

2500m•~20 Mton instr vol•885 10inch PMTs • 12 lines• 25 storeys/line• 3 PMTs / storey

The ANTARES Detector M

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rio-M

G13

@ S

toko

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2006 – 2008: Building phase of the Detector

Junction box 2001Main cable 2002Line 1, 2 2006Line 3, 4, 5 01 /

2007Line 6, 7, 8, 9, 10 12 / 2007Line 11, 12 05 /

2008

~70 m

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Earth and Sea Sciences

Instrumentation module

Seismograph

Connected30 Oct 2010 Secondary Junction Box

O2, CTD, P

BioCam

Currentmeter

Turbidity

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

Up- and down-going Events

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

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Region of Sky Observable by Neutrino Telescopes

Mkn 501

Mkn 421

CRAB

SS433

Mkn 501

RX J1713.7-39

GX339-4SS433

CRAB

VELA

GalacticCentre

IceCube (South Pole) ANTARES(43° North)

® Emphasis on study of Galactic sources

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Selected ANTARES physics results

1. Cosmic sources searches2. Diffuse flux from ExtraGalactic sources3. Multimessenger approach and

Gravitational Waves coincidences4. Neutrino oscillations

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1. Point Source Search

•Neutrino candidates: Upgoing particles•Background for neutrinos: mis-reconstructed atmospheric muons•Track fit quality used to reject mis-reconstructed downgoing muons•Number of hits used as estimator of muon (~neutrino) energy

upgoing

Number of up-going events as a function of the track quality parameter L

Angular distribution of well-reconstructed tracks

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1. Angular Resolution for Neutrinos

m

Full 12 line detector

cumulative distribution of the angle between the true neutrino track and the reconstructed muon event (assuming E-2 spectrum).

The median is 0.46°83% of the events within 1°

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1. Full-Sky Search (2007-2010)

Most significant cluster at: RA= ‒46.5°, δ= ‒65.0°

Nsig = 5p-value=0.026 (post-trial)Significance = 2.2 σ

Sky map in equatorial coordinates (3058 candidates)

Results compatible with the background hypothesis

3⁰

1⁰

Pre-trial prob

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1. Source Candidate List

Look in the direction of a list of 51 predefined candidate sources(selection of sources mostly based on γ-ray flux and visibility)

HESS J1023‒575 most signal-like, p–value 41% (post trial)

Compatible with the background hypothesis

First eleven sources sorted by p-value. Last column shows the 90% CL upper limit on

the flux (E / GeV)-2 GeV-1 cm-2 s-1

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1. Candidate List Search – 90%CL Limits

• Assumes E-2 flux for a possible signal•ANTARES has the most stringent limits for the Southern Sky•Galactic sources expected to have energy cutoff- not visible to IceCube • 2016: expect limits to improve by another factor ~2.5

ANTARES 2016

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2. Diffuse m flux

E2F(E)90%= 5.3×10-8 GeV cm-2 s-1 sr-1

20 TeV<E<2.5 PeV

Phys. Lett. B696 (2011) 16-22

IC40

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2. Search for diffuse from Fermi Bubbles

For 100% hadronic models:E2dF/dE=1.2*10-7 GeV cm-2s-1sr -1

Ecutoff protons: 1PeV-10 PeV

Background estimated from average of three ‘OFF’ regions (time shifted in local coordinates)

Galactic coords

• Fermi-LAT data provided evidence of the emission of HE rays with a high intensity E-2 spectrum from two large areas above and below the Galactic Center (the "Fermi bubbles").• A hadronic mechanism has been proposed for thisrays emission making the Fermi bubbles promising sources of high-energy neutrinos

Detector coords

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2. Search for Neutrinos from Fermi Bubbles

Live time = 588 days

Cuts optimised for best MRF and a cutoff at 100 TeV

Nback (OFF) = 90±5(stat)±3(sys)Nsignal (ON) = 75

No signal ® exclude fully hadronic FB model without cutoff (90%CL F&C)

Future: full dataset and improved energy estimator

ANTARES preliminary

ON ZONE<OFF ZONE>

dotted: model predictionsolid: 90% CL limits

50 TeV cutoff100 TeV cutoff500 TeV cutoffno cutoff

ANTARES preliminary

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3. Multimessenger approach

Strategy: higher discovery potential by observing different probeshigher significance by coincidence detectionhigher efficiency by relaxed cuts

GCNGRB Coord. Network:γ satellites

Alerts

Ligo/VirgoGravitational waves:trigger + dedicatedanalysis chain

TAROTROTSEoptical follow up:

MoUs for joint research

arXiv:1111.3473.arXiv:1205.3018  Astropart.Phys.35(2012) 530-536        arXiv:1103.4477

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3. Search for GW coincident signal

Common data takingSearch strategy

Instantaneous Antares+Ligo+Virgo common view

V. V. Elewyck et al. Int.J.Mod.Phys. D18 (2009) 1655-1659B. Baret et al. Astropart.Phys. 35 (2011) 1-7B. Baret et al. arXiv:1112.1140.

Done On going

0 1

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3. 2007 Dataset Analysis

Distance within which

there is a 90% detection

probability with a 1% false

alarm rate per neutrino

I. Di Palma et al. TAUP 2011B. Bouhou et al. arXiv:1201.2840

•Sub-optimal detectors•No dedicated optimisation

NO DETECTION

set limits on distance of occurrence of NS-BH and NS-NS mergers

3. Correlation with Gravitational Waves

- plausible common sources (microquasars, SGR, GRBs)- discovery potential for ‘hidden’ sources (e.g. failed GRBs)

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2007 ANTARES 5-line detector2009-2010 12-line detector2015-2016 adv LIGO/VRIGO

2007: No statistical significant correlation

⇒ set limits on distance of occurrence of NS-BH and NS-NS mergers

First joint ANTARES/LIGO/VIRGO publication: arXiv:1205.3018v2

2009-2010: expect to constrain fraction of star collapses accompanied by coincident emission of jets beamed towards Earth

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4. Oscillations with Atmospheric Neutrinos

L=2 REarth cos, from track fit E from muon range

• Oscillations maximal at E=24 GeV for vertical neutrinos• Dashed line: oscillation effect • Larger effect on single-line (low energy) than multi-line (higher energy) events

E<100 GeV

MC truth

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3. Neutrino Oscillations: Track Selection

Multi-line Single-line

• Select pure sample of atmospheric neutrinos (<5% muon contamination) using a cut on the track fit quality• Blue: misreconstructed atmospheric muons• Green: atmospheric neutrinos• Red: neutrino with oscillations

zenith angle resolution: 0.8 degrees for multi-line events 3 degrees for single-line events

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3. Neutrino Oscillations: Result

ANTARESK2KSuper-KMINOS

2008-2010 data (863 days):No oscillation: 2/NDF = 40/24 (2.1%)Best fit: 2/NDF = 17.1/21 Δm2 = 3.1 10-3 eV2 sin22 =1.00

Assuming maximal mixing: Δm2=(3.1±0.9) 10-3 eV2

Systematics:(Absolute normalisation free)Absorption length: ±10%Detector efficiency: ±10%Spectral index of flux: ±0.03OM angular acceptance

Accepted by PLB: arXiv:1206.0645

68%CL contoursno osc

best osc

ANTARES preliminary ANTARES preliminary

5% erroron slope vs ER/cosR

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Summary ANTARES infrastructure completed:

Only operating deep sea neutrino telescope Largest neutrino telescope in the Northern hem. Operating smoothly, maintenance capability proven Good understanding of detector Important testbed for KM3NeT R&D and software

Exciting and broad physics program …. Unexplored regions of sensitivity for gal. sources Steady/transient sources, monopoles, DM,

oscillations … multi-messenger approach (optical, satellite, GW)

Real-time readout and in-situ power capabilities a large program of multi-disciplinary activities: acoustics, biology, oceanography, seismology……

Major step towards the multi-kilometre cube deep-sea Neutrino telescope: KM3NeT

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Spares

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

Bursts: bioluminescence fromMacroscopic organisms

Counting Rates (short timescale)

40Ke

4020

4019 eCa→K

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Acoustic Positioning

Storey 1Storey 8Storey 14Storey 20Storey 25

Radial displacementPrecision ~ few cms

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

and also storeyheadings and tilts

884 days live time (2007-2010)

2.7 sigma significance Agrees with Monte Carlo expectations

Absolute Pointing: Moon Shadow

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