high energy neutrino astronomy with cherenkov telescopes l. moscoso cea/irfu/spp & apc – paris...
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High energy neutrino High energy neutrino astronomy with Cherenkov astronomy with Cherenkov
telescopestelescopes L. MoscosoL. Moscoso
CEA/Irfu/SPP & APC – Paris Rive GaucheCEA/Irfu/SPP & APC – Paris Rive GaucheXI ICATPP ConferenceXI ICATPP Conference
Villa Olmo, Como, Italy, 5-9/10/2009Villa Olmo, Como, Italy, 5-9/10/2009
i r f u
yalcas
i r f u
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yalcas
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The history of the sky The history of the sky surveysurvey
The light since the origins
Extension to the non visible since tens of years (Radio, IR, UV, X and gamma)
Satellites tens of GeV
Large arrays tens of TeV
Multi-wavelenth astronomy
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Cosmic ray spectrumCosmic ray spectrum
50 J
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The GZK effectThe GZK effectInteraction withInteraction withIR, CMBR, Radio IR, CMBR, Radio absorption of HEabsorption of HEphotons andphotons anddegradation of thedegradation of theproton energyproton energy
Region aboveRegion above100Mpc cannot be100Mpc cannot beexplored withexplored withphotons abovephotons above10TeV10TeV
Protons:Protons:UsefulUsefulaboveabove10102020eV only.eV only.
Galaxy
Local cluster
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High energy neutrinosHigh energy neutrinos
The neutrino as an alternative solutionThe neutrino as an alternative solution
• Multi-wavelength and multi-messenger studies Multi-wavelength and multi-messenger studies
• Exploration of the most remote regions of the Exploration of the most remote regions of the UniverseUniverse– Not absorbed (weak cross section)Not absorbed (weak cross section)– Electrically neutral: not deflected by magnetic Electrically neutral: not deflected by magnetic
fieldsfields
But at least a kmBut at least a km33 is necessary! is necessary!
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Synchrotron radiation followed by inverse Compton
The mechanismThe mechanism
HE electron LE
HE electron
HE
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Synchrotron radiation followed by photo-production
The mechanismThe mechanism
HE electron LE
HE proton
HE °
HE
nucleonHE
HE
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Synchrotron radiation followed by ± photo-production
The mechanismThe mechanism
LCR L L
HE electron LE
HE proton
HE
±
HE
nucleon H
E m
uon
HE
HE electron
HE
HE
e
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Scientific issuesScientific issues
Particle physics and CosmologyParticle physics and Cosmology–DM indirect searchDM indirect search
–Neutrino oscillationsNeutrino oscillations
AstrophysicsAstrophysics–QuasarsQuasars–Gamma ray bursts (GRB)Gamma ray bursts (GRB)–MicroquasarsMicroquasars–PulsarsPulsars–SNRSNR–Topological defects + other exoticsTopological defects + other exotics
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Difficult detectionDifficult detection
•Very weak cross section Very weak cross section Huge detectorHuge detector
kmkm33
•Very high cosmic ray flux Very high cosmic ray flux shielded detectorshielded detector
Underground or submarineUnderground or submarine
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Detection techniquesDetection techniques
• HE induced muon produced in the HE induced muon produced in the surrounding medium by HE neutrinosurrounding medium by HE neutrino– Upward-going neutrinos only (2Upward-going neutrinos only (2))– Mass = RMass = RS (RS (R2.5 km we @ 1 TeV; 10 km 2.5 km we @ 1 TeV; 10 km
@10 TeV)@10 TeV)• HE muons produced inside the detector by HE muons produced inside the detector by
HE neutrino interactions (4HE neutrino interactions (4))– Requires a very large detector (IceCube or Requires a very large detector (IceCube or
KM3NeT)KM3NeT)• VHE VHE e e interaction inside the detector (4interaction inside the detector (4))
– Detection of cascadesDetection of cascades
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Induced muonsInduced muons
detectordetectorThe cherenkov light is detected by the PMTs
The neutrinos interactWith the surrounding
matter
The muon generates the Cherenkov light
p
c=43°
Correlation time-position direction of the muon
Precision on the position: 10cm
Precision on time: 1ns
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The advantagesThe advantages
• Target mass Target mass R R increasesincreases with the with the neutrino energyneutrino energy
• Interaction cross sectionInteraction cross section increasesincreases with with the neutrino energythe neutrino energy
• Detection efficiencyDetection efficiency increasesincreases with the with the muon energy and therefore with the muon energy and therefore with the neutrino energyneutrino energy
Enrichment of the high energy neutrinosEnrichment of the high energy neutrinos
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PhysicPhysicss background background
Atm. muons
Atm.
106
d
/d
cm
-2 s
-1 s
r-1
cos
2400 m depth, E > 1 TeV
Atmospheric showersatmospheric muons 109 events/yearAtmospheric neutrinos 3000/year
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The neutrino telescopesThe neutrino telescopes
NESTOR : Pylos, Greece
ANTARES La-Seyne-sur-Mer, FranceBAIKAL: Baikal lake, Siberia
DUMAND, Hawaii (cancelled 1995)
AMANDA, IceCubeSouth Pole
NEMO Catania, Italy
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The Mini Tower for NEMO The Mini Tower for NEMO Phase-1Phase-1
Optical modules
Floor control module
Mechanical stresses are applied only to the tensioning ropesTower Base
Module
Floor 1
Floor 2
Floor 3
Floor 4
Backbone e.o. cable
Tensioning ropes
Tensioning ropes
e.o. Jumper cableTower base - JB
Break-out
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Nemo Phase 1Nemo Phase 1Shore station
2.5 km e.o. Cable with double steel shield
21 km e.o. Cable with single steel shield
J BUJ
J
5 km e.o. cable
Geoseismic station SN-1 (INGV)
5 km e.o. cable
10 optical fibres standard ITU- T G-652 6 electrical conductors 4 mm2
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The Antares stationThe Antares station
Submarine cable
-2475m
La Seyne sur Mer
Michel Pacha institute
On shore On shore stationstation
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The ANTARES detectorThe ANTARES detector
vincenzo flaminio
~60 m
100 m
350 m
14.5 m
Link cable
JunctionBox
Cable toshore
2500m depth
Storey
45°
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Number of TriggersNumber of Triggers
CABLEREPAIR
5 lines (2007)5 lines (2007)
19.1019.1066 μ μ10 or more lines (2008)10 or more lines (2008)
65.1065.1066 μ μ
Total : 240 days = 80% of calendarTotal : 240 days = 80% of calendarSelected :167d = 70% of totalSelected :167d = 70% of total
Total : 243 days = 83% of calendarTotal : 243 days = 83% of calendarSelected :173d = 71% of totalSelected :173d = 71% of total
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Zenith angular distributionZenith angular distribution
neutrinos
June 2007 – Dec 2008
5+10+12 lines
341 active days
1062 upward neutrino candidates
upgoing downgoing
Good agreement with “standard” neutrino oscillationsGood agreement with “standard” neutrino oscillations:: sinsin22 2 2θθ = 1; = 1; ΔΔmm22 = 2.4 = 2.4 ·· 10 10-3-3 eV eV22
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Search for point-like Search for point-like sourcessources
Upper limits obtained with Upper limits obtained with 2007 data (5 lines, 140 day 2007 data (5 lines, 140 day lifetime), compared with 1 lifetime), compared with 1 year of complete detector year of complete detector (12 lines) and other (12 lines) and other experimentsexperiments
Analysis of 12-line data is Analysis of 12-line data is ongoingongoing
For further information see talks given by M. Vecchi (INFN-Roma1) & U. Fritsh (ECAP Univ. Erlangen)
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5 lines (2007): Depth vs. 5 lines (2007): Depth vs. IntensityIntensity
Preliminary
Preliminary
Work on reducing systematics is ongoing
2,5km6km
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Transients with ANTARESTransients with ANTARES
•Triggered searches (alerts from satellites: Integral, Triggered searches (alerts from satellites: Integral, Swift, Fermi) Swift, Fermi)
•Low backgrounds due to direction and time coincidencesLow backgrounds due to direction and time coincidences•Dump all L0 data in 2min window around trigger (i.e. no trigger Dump all L0 data in 2min window around trigger (i.e. no trigger losses)losses)•Special track reconstruction using known directionSpecial track reconstruction using known direction
•Neutrino multiplets in time optical follow-up (Tarot in Neutrino multiplets in time optical follow-up (Tarot in France and at La Silla)France and at La Silla)
•Full sky 24h/24 searchFull sky 24h/24 search•Sliding time window around eventsSliding time window around events•Fast online reconstruction Fast online reconstruction optical follow up to identify source optical follow up to identify source
•Gravitational waves and neutrinos (Virgo + Ligo + Gravitational waves and neutrinos (Virgo + Ligo + Antares)Antares)
•Drafting a MoU in progressDrafting a MoU in progress
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IceCubeIceCube
• Full project: 80 60-floors detectorFull project: 80 60-floors detector
• First analysis results on 22 stringsFirst analysis results on 22 strings
• 40 strings now installed: will allow a 40 strings now installed: will allow a 44surveysurvey
• Installation of a deep dense core (7 Installation of a deep dense core (7 strings) foreseenstrings) foreseen
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Flux upper limits vs Flux upper limits vs declinationdeclination
2009.09.26 Chad Finley 27
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See T. Montaruli, ICRC09
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Solar wimp Solar wimp limitslimits
Phys.Rev.Lett.102:201302,2009,C. Rott, ICRC 09
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KM3NeTKM3NeT
+ + +…
A research facility in the Mediterranean A research facility in the Mediterranean SeaSea
A next generation neutrino telescope (at the km-scale)A next generation neutrino telescope (at the km-scale)
Cabled observatory for Earth and Marine sciencesCabled observatory for Earth and Marine sciences
38 institutes from 10 38 institutes from 10 European countriesEuropean countries
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Design goalsDesign goals
Substantially competitive with IceCubeSubstantially competitive with IceCube Volume > 1 kmVolume > 1 km33
Optimized for energy range 1 TeV – 1 PeVOptimized for energy range 1 TeV – 1 PeV Angular resolution < 0.1Angular resolution < 0.1oo
Zenith angle:Zenith angle: Full acceptance for neutrinos originating from Full acceptance for neutrinos originating from
directions up to at least 10° above the horizondirections up to at least 10° above the horizon For energies > 100 TeV angular acceptance For energies > 100 TeV angular acceptance
limited only by the absorption of the Earth limited only by the absorption of the Earth
See the talk given by G. De Bonis (INFN-Pisa)
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KM3NeT Design StudyKM3NeT Design StudyDesign study Design study funded by EU FP6 in February 2006funded by EU FP6 in February 2006
Development of a cost-effective design for a cubic km sizedDevelopment of a cost-effective design for a cubic km sizeddeep-sea infrastructure housing a neutrino telescope….deep-sea infrastructure housing a neutrino telescope….
Conceptual Design ReportConceptual Design Report released in April 2008released in April 2008
(www.km3net.org)(www.km3net.org)
Includes:Includes:
Science caseScience case
Site studiesSite studies
Design goalsDesign goals
Technical implementationTechnical implementation
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Km3Net Design StudyKm3Net Design Study
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Funded by the EU FP7 framework in March 2008
Primary objective pave the path to political and scientific convergence on the legal, governance, financial engineering and siting aspects of the infrastructure…..
Km3Net Preparatory PhaseKm3Net Preparatory Phase
Km3net timeline
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ConclusionsConclusions• Since many years the neutrino has been considered Since many years the neutrino has been considered
as an alternative way to observe the Universeas an alternative way to observe the Universe• It was a long way to achieves some very large It was a long way to achieves some very large
volume neutrino telescopesvolume neutrino telescopes• Now two devices are operatingNow two devices are operating• 50% of the km50% of the km33 detector at the South Pole is detector at the South Pole is
achieved and the full detector will be completed in achieved and the full detector will be completed in 20112011
• The first neutrino telescope in the Mediterranean The first neutrino telescope in the Mediterranean has been achieved too and is operatinghas been achieved too and is operating
• The study for a kmThe study for a km33 detector in the Mediterranean detector in the Mediterranean is reaching the final phase (TDR editing). The is reaching the final phase (TDR editing). The construction will probably start at the end of the construction will probably start at the end of the preparatory phase (2011)preparatory phase (2011)