high energy neutrino astronomy
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High Energy Neutrino Astronomy. Status and perspectives of the high energy neutrino observatories. Paolo Piattelli, INFN Laboratori Nazionali del Sud Catania. Layout of the talk. High Energy Neutrino Astronomy Scientific motivations Experimental techniques - PowerPoint PPT PresentationTRANSCRIPT
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
High Energy Neutrino AstronomyStatus and perspectives of the high
energy neutrino observatories
Paolo Piattelli, INFN Laboratori Nazionali del Sud Catania
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Layout of the talk• High Energy Neutrino Astronomy
– Scientific motivations– Experimental techniques
• Status of the presently active neutrino detector projects
– The currently active neutrino detectors: Baikal and Amanda– The ongoing projects: Antares, Nestor, Nemo
• What comes next– The km3 at the South Pole: IceCube– The km3 in the Mediterranean sea: KM3NeT
• Conclusions and outlook
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Why neutrino astronomy?• Neutrinos traverse space without being deflected or
attenuated– They point back to their sources– They allow to view into dense environments– They allow to investigate the Universe over cosmological
distances• Neutrinos are produced in high energy hadronic
processes– They can allow distinction between hadronic and leptonic
acceleration mechanisms• Neutrinos could be produced in Dark Matter
annihilation
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Particle propagation in the Universe
Photons are absorbed on dust and radiationProtons are deviated by magnetic fieldsExtremely high energy protons interact with background radiationOnly neutrinos are direct
1 parsec (pc) = 3.26 light years (ly)
High energy particles > 1017
eV
gamma rays (0.01 - 1 Mpc)
protons E>1019 eV (10 Mpc)
protons E<1019 eV
neutrinos
Cosmic accelerator
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Particle astrophysics with telescopes
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Neutrino production in cosmic accelerators
Proton acceleration
• Fermi mechanism
proton spectrum dNp/dE ~E-2
Neutrino production• Proton interactions
p p (SNR,X-Ray Binaries)
p (AGN, GRB, microQSO)
• decay of pions and muons
Astrophysical jet
Particle accelerator
electrons are responsible for gamma fluxes (synchrotron, IC)F. Halzen
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Principles of neutrino astronomyNeutrino telescopes search for muon tracks induced by neutrino interactions
The downgoing atmospheric flux overcomes by several orders of magnitude the expected fluxes induced by interactions.
On the other hand, muons cannot travel in rock or water more than 50 km at any energy
Upgoing and horizontal muon tracks are neutrino signatures
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Principles of neutrino astronomy
neutrino
muon
Cherenkov light
~5000 PMT
neutrino
Flux estimate need km3 scale detectors
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
The HE neutrino telescope world map80’s: DUMAND R&D90’s: BAIKAL, AMANDA, NESTOR2k’s: ANTARES, NEMO R&D2010: ICECUBE
Mediterranean KM3 ?
AMANDAICECUBE
Mediterraneankm3
BAIKAL
DUMAND
Pylos
La Seyne
Capo Passero
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
A closer look at the Mediterranean Sea
ANTARES
3800:4000 m
2400 m
3400 m
NEMONESTOR
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Baikal192 OM arranged in 8 strings, 72 m heighteffective area >2000 m2 (E>1 TeV)
3600 m
1366
m
• Successfully running since 10 years• Atmospheric neutrino flux measured• Further upgrades planned, but km3 hardly reachable
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Amanda
Optical Module
AMANDA-II19 strings677 OMsDepth 1500-2000m
Effective Area 104 m2 (E TeV)Angular resolution 2°
above horizon: mostly fake events
below horizon: mostly atmospheric
959 events
The AMANDA sky map
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
The ANTARES neutrino telescope• string based detector • 12 lines• 900 PMTs• 2400 m deep
~70 m
350 m
100 m
14.5 m
Submarine links
JunctionBox
40 km toshore
Anchor/line socket
a storey
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
ANTARES status and realization plan
• 2003: Deployment and operation of two prototype lines
• Several months of data taking
• Technical problems(broken fiber, water leak)
no precise timing,no reconstruction.
• Early 2005: 2 upgradedprototype lines
• Mid-2005: Line 1• 2007: Detector completed
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
NESTOR• Tower based detector• Up- and downward looking PMTs• 3800 m deep• Dry connections• First floor (reduced size) with
12 PMTs deployed and operated in 2003
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
NEMO
The NEMO Collaboration has dedicated special efforts in:• development of technologies for
the km3 (technical solutions chosen by small scale demostrators are not directly scalable to a km3)
• search, characterization and monitoring of a deep sea site adequate for the installation of the Mediterranean km3 (Capo Passero near Catania, depth 3400 m)
Modular detector concept based on semi-rigid structures16 storey towers with 4 OM per storey20 m storey length40 m spacing between storeys
Underwater connections
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
NEMO Phase 1 project
2.330 mDouble Armed Cable
20.595 m Single Armed Cable
Drop cable 2Drop cable 25.220 m5.220 m
Drop cable 1Drop cable 15.000 m5.000 m
joint BUjoint
joint
NEMO Phase 1 LabLong term tests for:underwater connections, electronics, mechanical structures, optical and acoustic detectors.
Multidisciplinary laboratory (will host an on-line underwater seismic station of the Istituto Nazionale di Geofisica e Vulcanologia) SN-1
• Realization of a detector subsystem including all critical components
• Site infrastructures at 2000 m already realized 30 km offshore Catania
• Project completely funded by INFN and MIUR• Completion foreseen in 2006
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
The Catania Test Site and ESONETThe NEMO test site in Catania will also host SN-1 a deep sea station for on-line seismic and environmental monitoring by INGV.The NEMO test site will be the Italian site for ESONET (European Seafloor Observatory NETwork).
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
NEMO Phase 2A deep water station at the Capo Passero site
PROPOSED INFRASTRUCTURE- Shore station at Portopalo di Capo
Passero to host the power system the data acquisition and detector integration facilities
- 100 km electro optical cable- Underwater infrastructures (main
junction box)- Two intermediate connection
stations in shallow and medium deep waters for interdisciplinary activities (agreement with INGV and SACLANTCen)
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
ICECUBEThe technology for underice detectors is well established.The next step is the construction of the km3 detector ICECUBE.
• 80 strings (60 PMT each) • 4800 10” PMT (only downward
looking)• 125 m inter string distance• 16 m spacing along a string• Instrumented volume: 1 km3 (1 Gton)• First string to be deployed in january
2005
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Status of the IceCube project many reviews – international and within the U.S. - strongly emphasize
the exciting science which can be performed with IceCube
in Jan 2004, the U.S. Congress approvedthe NSF budget including the full IceCube MRE
significant funding approved also in Belgium, Germany and Sweden
in Feb 2004, NSF conducted a baseline review “go ahead”
deployment over 6 years IceCube strings IceTop tanks4 8 Jan 200516 32 Jan 200632 64 Jan 200750 100 Jan 200868 136 Jan 200980 160 Jan 2010
From O. Botner, Neutrino 2004
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Do we need two km3 detectors?There are strong scientific motivations that suggest to install two neutrino telescopes in opposite hemispheres :
• Full sky coverage
The Universe is not isotropic at z<<1, observation of transient phenomena
• Galactic Center only observable from Northern Hemisphere
The most convenient location for the Northern km3 detector is the Mediterranean Sea:
vicinity to infrastructures
good water quality
good weather conditions for sea operations
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Sky coverage
TeV sourcesQSO
Galactic centre
Galactic coordinatesMediterranean km3
ICECUBE
1.5 sr common view per day
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
KM3NeT: a Design Study for the km3
Astroparticle Physics Physics Analysis System and ProductEngineering
Information Technology Shore and deep-seastructure
Sea surfaceinfrastructure
Risk AssessmentQuality Assurance Resource Exploration Associated Science
A Technical Design Report (including site selection) for a Cubic kilometre Detector in the Mediterranean
WO
RK
PA
CK
AG
ES
• Collaboration of 8 Countries, 34 Institutions• Aim to design a deep-sea km3-scale observatory for high energy neutrino
astronomy and an associated platform for deep-sea science• Request for funding for 3 years
The experience and know how of the ANTARES, NESTOR and NEMO collaborations is merging in the KM3-NET activity
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Objectives and scopes of the KM3NeT DS
• Critical review of current technical solutions• Thorough tests of new developments• Comparative studies of sites and recommendation
on site choice• Assessment of quality control and assurance• Exploration of possible cooperation with industry• Investigation of funding and governance models
Establish path from current projects to the KM3
Expected outcomeIn three years a complete Technical Design Report for the KM3 will be produced
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Exploitation model of the future KM3 facility
• Reconstructed data will be made available to the whole community
• Observation of specific objects with increased sensitivity will be offered
• Close relation to space and ground based observatories will be established (alerts for GRBs, Supernovae, etc…)
• “Plug-and-play solutions for detectors of associated science
Goal: facility exploited in multi-user and interdisciplinary environment
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Associated science
• Great interest in long term deep-sea measurements in many different scientific communities:
– Marine biology– Ocenography– Environmental science– Geology and geophysics– …
• Substantial cross-links to ESONET (the European Sea Floor Observatory Network)
• Plan: include the associated science communities in the design phase to understand and react to their needs and make use of their expertise (e.g. site exploration)
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Actions in the new I3 proposal• Networking
– A collaboration between the european projects (Antares, Nestor, Nemo) has been already established with KM3NeT)
– Increase collaboration with other neutrino projects (Baikal, Amanda, IceCube)
– Develop collaborations with gamma ray and space based observatories
– Other common fields of interest may be: massive computer simulations, development of common databases and source catalogues, development of computing and analysis tools
• JRAs– Overlap with KM3NeT should be avoided– Development of new detection methods for future neutrino
detectior projects (radio detection, acoustic detection, …)• Transnational access
– All the european existing projects can provide access for interdisciplinary studies as the future KM3NeT will do
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Conclusions• Baikal and Amanda have demonstrated the
feasibility of the high energy neutrino detection• Three projects in the Mediterranean are under way:
– Antares and Nestor are currently under construction (first data taken)
– NEMO is pursuing R&D for technical solutions for the km3– All three collaborations together in a common effort
towards the km3• To fully exploit neutrino astronomy we need 2 km3
scale detectors, one for each emisphere:– IceCube is starting construction soon and will be
completed by 2010– KM3NeT aims at producing a complete Technical Design
Report in 2008
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Remarks on EU applications
• The EU applies rather stringent and formal rules. These rules are not laws of nature - so physicists tend to ignore them!
• Writing proposals:– Take the evaluation criteria seriously:
• European added value• Scientific and technological excellence• Relevance of the objectives of the scheme• Quality of the management
– Read all available EU documentation and learn “EUish”• Evaluation process
– Well structured and transparent from inside …– … but completely opaque from the outside!– It helps a lot to take part in the EU evaluations
Lessons learned with the successful KM3NeT experience (from Uli Katzt, KM3NeT coordinator)
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
End of presentation
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Next slides are spares
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
ANTARES: first deep sea data
• Rate measurements: Strong fluctuation of bioluminescence background observed
10min 10min
Rate (kHz)
time (s)
Constant baseline ratefrom 40K decays
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
ANTARES: long term measurements
baseline rate (kHz)
burst fraction
time
• Also measured: current velocity and direction, line heading and shape, temperatures, humidities, ...
• Important input for preparation & optimization of ANTARES operation.
baseline rate =15-minute average
burst fraction =time fraction above1.2 x baseline rate
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
NESTOR: reconstruction of muon tracks• Track reconstruction using arrival
times of light at PMs.• Ambiguities resolved using signal
amplitudes in up/down PM pairs.
PMcalibration
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
The HE neutrino telescope world map80’s: DUMAND R&D90’s: BAIKAL, AMANDA, NESTOR2k’s: ANTARES, NEMO R&D2010: ICECUBE
Mediterranean KM3 ?
AMANDAICECUBE
Mediterraneankm3
BAIKAL
DUMAND
Pylos
La Seyne
Capo Passero
ANTARES
3800:4000 m
2400 m
3400 m
NEMONESTOR
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
Scientific goals• Astronomy via high energy neutrino observation
– Production of high energy neutrinos in the universe (acceleration mechanisms, top-down scenarios, …)
– Investigation of the nature of astrophysical objects– Origin of high energy cosmic rays
• Indirect search for Dark Matter• New discoveries• Associated science
P. Piattelli, CRNT meeting, Paris 16-17 december 2004
NEMO Phase 1 projectA step towards the km3 detector
EO CABLEEO CABLE
Length – 25 km10 Optical Fibres ITU- T G-652
6 Electrical Conductors 4 mm2
• Realization of a detector subsystem including all critical components
• Site infrastructures at 2000 m already realized 30 km offshore Catania
SHORE LABORATORYSHORE LABORATORY
Project completely funded (jointly by INFN and MIUR)Completion foreseen in 2006
UNDERWATER LABUNDERWATER LAB