Post on 20-Jan-2016
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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 fields
Photons:• Produced in leptonic (synchrotron, IC) and hadronic (0) processes• Absorbed at higher energies and large distances
Neutrinos (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/
ee ee
• Primary acceleration («Bottom-Up»)Stochastics shocks (Fermi mechanism)Explosion /Accretion / Core collapse • Benchmark Extra Gal. n flux Waxman-Bahcall
• But HE also from electromagnetic processes Synchrotron Inverse Compton
e:: =1:2:0 source e:: =1:1:1 Earth nsoscillatio
~ 500 events /yr/ km2
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5
m
42°
interaction
Sea floor
Cherenkov light from m
3D PMTarray
nm
- Main channel: interaction giving an ultra-relativistic (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
nm
p
nm
nmmp, a
Physical Background sources
Atmospheric 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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2006 – 2008: Building phase of the Detector
Junction box 2001
Main cable 2002
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
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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
n
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 n 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 n 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 -g 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 this-g rays 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 taking
Search 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
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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 En=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: ±0.03
OM 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 min
Continuous baseline: Radioactivity in the sea (40K)+ bioluminescent bacteria
Bursts: bioluminescence fromMacroscopic organisms
Counting Rates (short timescale)
40K
e4020
4019 eCa→K
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Acoustic Positioning
Storey 1Storey 8
Storey 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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