Transcript KM3NeT

KM3NeT
L. Moscoso
DAPNIA/SPP
CEA/Saclay
23/06/2005
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Detection principle
Huge detection volume: km3
Shielded against cosmic rays
p
m
n
qc=43°
m
n
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Scientific topics
Astronomy
–Quasars
–Gamma-ray bursts
–Microquasars
–Pulsars
–SNR
Cosmology/ particle physics
–Dark matter
The Mediterranean is well suited to
observe the Galactic Centre.
Results from H.E.S.S. are encouraging.
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Neutrinos from the GC
HESS observations - Energy spectrum
Aharonian et al., A&A 425, L13-L17 (2004)
dF/dEg = F0 E- with = 2.2
F0 = 1.1×10-4 m-2 s-1 GeV-1
Km3 detector sensitive to a neutrino flux = gamma-ray flux
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HESS scan of the Galactic centre
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Possible combined observations
• Neutrinos from galactic centre detectable in KM3NeT in a few
weeks to years (Crocker, Melia, Volkas, Astrophys. J. 622 (2005)
L37-40);
• Other HESS observations like RX J1713.7-3946 and PSR B150958 in the GC proximity are promising;
• Integral and Swift are flying. Swift has reported 42 GRB in 6
months. Hopefully new space detectors in 2010-2020
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Nemo Phase 1
Geoseismic station
SN-1 (INGV)
Shore station
5 km e.o. cable
21 km e.o. Cable with
single steel shield
J
J
2.5 km e.o. Cable with
double steel shield
BU
J
5 km e.o. cable
 10 optical fibres standard ITU- T G-652
 6 electrical conductors  4 mm2
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Nestor prototype results
Recently published:
G. Aggouras et al.
Astropart. Phys.
23 (2005) 377
Zenith angle distribution
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Antares: MILOM & Line 0
MILOM
Line 0 – Cable test
Almost a complete line (23 storeys)
No electronics
Study optical fibre transmission
Autonomous recording devices (Tinytags)
and measurements from the shore (master
electro-optical and interlink cables)
Final version
of the
electronics
No water leaks in electronics containers
Successful deployment-recovery-checkdeployment-connection-recovery
Good and constant conductivity and
insulation
Optical transmission losses at a number of
locations (in the containers)
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Antares: The Junction Box
JB stable since 30 months.
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Antares MILOM: Timing resolution
s  0.75ns  for one PMT s  0.75/2
s 0.5ns
Will allow a 0.2° pointing resolution
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Antares-MILOM: ARS responses
Single pe
signal
wave-form
640MHz
sampling
Charge
distribution
(baseline
subtracted)
Single photoelectron peak
Main clock
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KM3NeT Design Study Participants
• Cyprus:
• France:
Univ. Cyprus
CEA/Saclay, CNRS/IN2P3 (CPP Marseille, IreS
Strasbourg), IFREMER
• Germany:
Univ. Erlangen, Univ. Kiel
• Greece:
HCMR, Hellenic Open Univ., NCSR Democritos,
NOA/Nestor, Univ. Athens
• Italy:
CNR/ISMAR, INFN (Univs. Bari, Bologna, Catania,
Genova, Messina, Pisa, Roma-1, LNS Catania,
LNF Frascati), INGV, Tecnomare SpA
• Netherlands: NIKHEF/FOM
• Spain:
IFIC/CSIC Valencia, Univ. Valencia, UP Valencia
• UK:
Univ. Aberdeen, Univ. Leeds, Univ. Liverpool,
John Moores Univ. Liverpool, Univ. Sheffield
Particle/Astroparticle institutes (17)
Sea science/technology institutes (7)
Coordinator
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KM3NeT Design Study: Resources
• Suggested overall budget of the Design Study: 24 M€
(mainly personnel, but also equipment, consumables, travel etc.).
• Amount requested from EU: 10 M€;
• Estimated overall labor power: ~3500 FTEMs
(FTEM = full-time equivalent person month)
→ 100 persons working full-time over 3 years!
Substantial resources (labor power)
additional to those available in the current
pilot projects will be required !
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The KM3NeT Design Study: Milestones
• Proposal submission 04.03.2004.
• Evaluation report received June 2004 (overall mark: 88%).
• Unofficial but reliable message (Sept. 2004):
The KM3NeT Design Study will be funded !
• Currently waiting for EU call to negotiation.
Negotiations expected between summer and end 2005
• KM3NeT in the ESFRI “List of opportunities”
• Strong support is asked to the funding agencies
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KM3NeT Consortium
Organizational structure (phase 1):
–
–
–
–
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Negotiation Preparation Group (NPG).
Task: preparation of the consortium agreement
Major legislative body: General Assembly;
One representative per institute;
Simple set of rules for phase 1 worked out by NPG.
Task: Approval of all documents, commitments, ...
Coordinator: U. Katz confirmed. In permanent contact with
Brussels.
WP responsibles: named by “Leading Institutes”
Task: establish communication between WP partners,
collect info., contact persons for NPG, WP summaries
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Working packages
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Task
Descriptive title
Leading participant
WP1
Management of the Design Study
Univ-Erlangen (D)
WP2
Astro-particle physics
IN2P3 (F)
WP3
Physics analysis
Hellenic Open Univ. (Gr)
WP4
System and product engineering
Saclay (F)
WP5
Information technology
FOM (NL)
WP6
Shore and deep-sea infrastructure
INFN (I)
WP7
Sea surface infrastructure
National Observatory of
Athens/Nestor (Gr)
WP8
Risk assessment and QA
INFN (I)
WP9
Resource exploration
NCSR Democritos (Gr)
WP10
Associated science
Univ-Aberdeen (UK)
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Time line
24/25 Feb. 2005:
1 March 2005:
First meeting of NPG;
Nomination of all WP coordinators approval by
GA;
14-15 June 2005: Second meeting of NPG;
End June 2005:
Guideline for WP coordinators;
5 Sept. 2005:
First common meeting of NPG and WP
coordinators;
(few pages, detailing plans, resources, ...);
8-11 Nov. 2005:
Second VLVnT workshop, Catania.
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Conclusions (1)
• HE neutrino observation is essential to achieve multimessenger and multi-wavelength astronomy;
• An equipped volume of at least one km3 is necessary;
• The Mediterranean Sea allows us to observe the
Galactic Centre;
• FP6 Design Study will combine the efforts of the three
pilot projects Antares, Nemo, Nestor;
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Conclusions (2)
The balance of these last few months is very positive:
– Scientific point of view
• The recent HESS observations in the TeV
range are very encouraging;
– Political point of view
• ESFRI adds KM3NeT to “List of opportunities”;
• The funding agencies show their intention to
reinforce their support to the pilot projects;
• New institutes (not present in the 3 pilot
projects) have joined KM3NeT;
– Technical point of view
• The recent results with the new Antares
prototypes are an important progress.
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