High Energy Neutrino Astronomy with the ANTARES Deep-Sea Telescope
Status of the ANTARES Neutrino Telescope
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Transcript of Status of the ANTARES Neutrino Telescope
Stéphanie ESCOFFIERCPPM Marseille, France
on behalf of the ANTARES Collaboration
• research goals
• detector setup
• selected results
• summary
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 2
Neutrino astronomy
Cosmic sources of neutrinos• micro quasars: X-ray binaries • supernova remnants and shock acceleration• Active Galactic Nuclei• Gamma Ray Bursts
Intriguing science questions:• astrophysical acceleration mechanism ?• origin of cosmic rays ?• dark matter ?• other exotic physics (magnetic monopoles) ?
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 3
The ANTARES Collaboration
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
IFIC, ValenciaUPV, ValenciaUPC, Barcelona
NIKHEF (Amsterdam) KVI (Groningen) NIOZ Texel
University of Erlangen Bamberg Observatory
ISS, Bucarest
ITEP, Moscow Moscow State
Univ
7 COUNTRIES7 COUNTRIES28 INSTITUTES28 INSTITUTES
~ 150 SCIENTISTS AND ~ 150 SCIENTISTS AND ENGINEERSENGINEERS
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
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 4
The ANTARES detector
~60 m
350 m14.5 m
Submarine links
JunctionBox
40 km toshore
BuoyStorey
Completed in May 2008
• 12 lines of 75 PMTs• 25 storeys / line• 3 PMTs / storey• ~900 PMTs
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 5
Optical background• constant 40K (~40 kHz)
The background
2 min
PMT counting rates
40K
40Ca
e-
Cherenkov light
beta decay
40K is used to check the time calibration of the detector
• bioluminescence of micro-organisms• bursts from macro-organisms
(Particle) Physics background
• cosmic rays (atmospheric μ and ν)
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 6
Optical background• constant 40K (~40 kHz)
• bioluminescence of micro-organisms• bursts from macro-organisms
The background
2 min
PMT counting rates
strongly correlated to sea currents
(Particle) Physics background
• cosmic rays (atmospheric μ and ν)
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 7
Optical background• constant 40K (~40 kHz)
The background
2 min
PMT counting rates
• bioluminescence of micro-organisms• bursts from macro-organisms
special event in 2006:ANTARES Coll.,Deep-Sea Res. I 58 (2011) 875.
(Particle) Physics background
• cosmic rays (atmospheric μ and ν)
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 8
The online/precise trackingOnline tracking • fast, to discriminate atmospheric muons from neutrinos• No detailed calibration/ no real time detector positioning needed• Angular resolution: Δθ 3o
The precise tracking• detailed real-time positioning of the detector• detailed PMTs charge/time calibration• detailed systematic knowledge of the apparatus (OMs angular acceptance, etc.)• Angular resolution: up to Δθ0.2o
arXiv 0908.0816
Astropart.Phys. 34 (2011) 652
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 9
Event display: a neutrino candidate
Example of a reconstructed up-going muon (i.e. a neutrino candidate) detected in 6/12 detector lines:
time
height
online tracking
•atmospheric muon flux•atmospheric neutrinos•point sources see talk by Juan Pablo
Gomez •diffuse νμ flux•magnetic monopoles
•dark matter see talk by Juande Zornoza
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 11
Atmospheric muons
online tracking
Zenith angle distribution of reconstructed tracks from atmospheric muons with a 5 line detector.
Astropart.Phys. 34 (2010) 179.
Within systematic uncertainties the measurements cannot distinguish between the models considered
• systematic error due to +/- 10% on absorption length = +25%/-20%;• syst. err. due to -15% on PMT efficiency (QE, eff. area etc) = -15%;• syst. err. due to cutoff in angular accept. = +20%/-15%;• total systematic uncertainty +/- 30%.Systematic uncertainties: +30% primary flux; +25% hadronic interaction model
DataMC (corsika + qgsjet)Systematics on MC
corsika + qgsjet (poly)corsika + sibyllmupage
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 12
Muon depth-intensity relation
Astropart.Phys. 34 (2010) 179.
Results are in agreement, within the systematic uncertainties, with the theoretical predictions and previous measurements
2,5km6km
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 13
Atmospheric neutrinos
341 days detector live time,single- and multi-line fit
elevation angle
up-going
good agreement with Monte Carlo • atmospheric neutrinos: 916 (30% syst. error)
• atmospheric muons: 40 (50% syst. error)
1062 cand.
down-going
1062 neutrino candidates: 3.1 candidates/day
online tracking
data set:2007-2008 data taken with 5 lines (2007)and 9, 10, and 12 lines (2008)
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 14
Search for point-like sources
Well reconstructed
Badly reconstructed
uncertainties inangle reconstruction: median: 0.5 0.1O
12-line data: 0.4 0.1O
absolute orientation: 0.1O
data set:2007-2008 data taken with 5 lines (2007)and 9, 10, and 12 lines (2008)
precise tracking
arXiv:1108.0292v1 [astro-ph.HE]
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 15H. Löhner, High Energy Neutrino Flux 15
Search for point-like sourcesEquatorial coordinates
Two distinct approaches:• all sky search• list of candidates
24 source candidates
point-like sources search see J. Gomez’s talk
arXiv:1108.0292v1 [astro-ph.HE]
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 16
Search for diffuse νμ flux
no excess of high-energy events above expected flux from atmospheric
background from atmospheric : ~ E-3.5
+ prompt neutrinos
cosmicneutrino models: ~ E-2
search for high-energy diffuse-flux tail
Phys. Lett. B 696 (2011) 16.
Energy estimate R based on extra light fromdelayed OM hits due tohigh-energy EM showers
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 17
Diffuse flux: upper limits
Upper limit is E2(E)90%= 4.8×10-8 GeV cm-2 s-1 sr-1 for 20 TeV<E<2.5 PeV
Phys. Lett. B 696 (2011) 16.
(334 days of equivalent live time)
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 18
Search for magnetic monopoles
Magnetic monopoles emit 8500 more Cherenkov light than a muon can be detected by ANTARES
Two estimators to discriminate MM from atmospheric background• The number of hits estimates the quantity of light• The ratio of two tracking reconstruction,
where χ2β=1 standard muon
algorithm (β =1)
χ2β modified algorithm (β
free)
λ=log(χ2β=1 /χ2
β)
Selection optimized for the discovery potential (in a blind way)
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 19
Monopoles: upper limits
no excess of events above the expected atmospheric background flux
Upper limit is (E)90%= 1.3×10-17 cm-2 s-1 sr-1 at β≈1
(116 days of equivalent live time with 2008 data)
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 20
Multimessenger astronomy
GCNGRB Coord. Network:γ satellites
SNEWSSuperNova Early Warning System
Ligo/VirgoGravitational waves:trigger + dedicatedanalysis chain
TaToOoptical follow up
Strategy• higher discovery potential by observing different probes• higher significance by coincidence detection• higher efficiency by relaxed cuts
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 21
TAToO projectTAToO
Optical follow-up of neutrino alerts from ANTARES in order to search for and identify transient sources (GRB, AGN flares…)
ν
ANTARES
Reconstruction “on-line” (<10ms)Trigger: multiplet / HE singlet Alert neutrino (GCN)
Real time
send <10s
1.9° x 1.9°
Large sky coverage (>2π sr) + high duty cycleImproved sensitivity (1 neutrino may lead to a discovery !!!)No hypothesis on the nature of the sourceNon dependent on the availability of external triggers
Advantages:
Tarot and ROTSE
S. Escoffier – Status of the ANTARES telescope - TeVPA 2011 - Stockholm 22
Future plans: KM3NeT concept
array of multi-PMToptical modules (OM)sensing Cherenkov light
instrumented volumeseveral km3
sensitive to all flavours
E > 0.1 GeV
angular resolution min 0.1o for E > 10 TeV
acceptance: up-going tracks,up to 10o above horizon
•ANTARES completed since May 2008•complements the sky coverage of IceCube•has a broad physics program•new diffuse-flux limit•competitive new magnetic monopoles flux
limit•multi-messenger observations on alert•paves the way for KM3NeT