KM3NeT: A Next Generation Neutrino Telescope in the Mediterranean Sea
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Transcript of KM3NeT: A Next Generation Neutrino Telescope in the Mediterranean Sea
KM3NeT: A Next Generation
Neutrino Telescope in the
Mediterranean SeaAlexander KappesUniversity Erlangen-Nuremberg
For the KM3NeT Consortium
6th International Workshop on
New Worlds in Astroparticle Physics
6. – 8. September 2007, Faro Portugal
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 2
Outline of TalkOutline of Talk
Physics case
Towards a km3 detector
The KM3NeT Design Study
How does it go on?
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 3
Potential Cosmic Neutrino SourcesPotential Cosmic Neutrino Sources
Extra-Galactic: Active Galactic Nuclei Gamma Ray Bursts
Galactic: Pulsar Wind Nebula Supernova Remnants Microquasars
RX J1713.7-3946HESS
(GRB970228, BeppoSax)
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 4
Directional Sensitivity of Neutrino TelescopesDirectional Sensitivity of Neutrino Telescopes
Muons from for identification of individual sources (angular resolution)
Muons can penetrate several km of water if E > 1 TeV
⇒ huge background from atmospheric
Sensitivity for upward sources largely reduced
needs either very high energies
or short transients (e.g., GRBs)
horizon upwarddownward
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 5
Why a Neutrino Telescope in the Mediterranean ?Why a Neutrino Telescope in the Mediterranean ?
Mediterranean site:
>75% visibility
>25% visibility
Observed sky
region in
galactic
coordinates
assuming
efficiency only
for downward
hemisphere.
→ We need Northern telescopes to cover the Galactic Plane
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 7
Flux Predictions from Flux Predictions from -Ray Measurements-Ray Measurements
mean atm. flux(Volkova, 1980,
Sov.J.Nucl.Phys., 31(6), 784)
Example: Vela X (PWN)
expected neutrino flux –in reach for KM3NeT
measured-ray flux (H.E.S.S.)
1 error bands include sys. errors (20% normalization, 10% index & cut-off)
A. Kappes et al., ApJ 656:870, 2007 (astro-ph/0607286)
All calculations show that we need km3-scale detectors
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 8
The KM3NeT ProjectThe KM3NeT Project
Currently consisting of 37 institutes from 10 European countries
(Cyprus, France, Germany, Greece, Ireland, Italy, Netherlands,
Romania, Spain, UK)
Includes expertise from all pilot projects (ANTARES, NEMO, NESTOR)
Objectives:
build and operate a km3-scale next generation
water Cherenkov neutrino telescope
build and maintain a deep sea research infrastructure
for oceanographic sciences:
(Oceanology, Marine Biology, Environmental Sciences,
Geology and Geophysics)
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 9
The KM3NeT VisionThe KM3NeT Vision
KM3NeT will be a multidisciplinary research infrastructure:
Deep-sea access for marine sciences.
Data will be publicly available;
KM3NeT will be a pan-European project but non European institutes are highly welcome!
10 European countries already involved;
Substantial funding already now from national agencies;
KM3NeT on ESFRI roadmap.
KM3NeT will be constructed in time to take dataconcurrently with IceCube.
KM3NeT will be extendable.
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 11
The KM3NeT Design StudyThe KM3NeT Design Study
Supported by the European Union in FP6 with 9 M€, tot. volume ~20 M€.
Major Objectives:
Started on Feb. 1, 2006; will run for 3 years.
Conceptual Design Report by end 2007 (workshop Nov. 2007);
Technical Design Report by Spring 2009;
Detector target specifications:
Effective volume ≥ 1 km3
0.1˚ angular resolution for muons (E ≥10 TeV)
Energy threshold few 100 GeV (~100 GeV when pointing)
Sensitivity to all neutrino flavors
Field of view close to 4 for high energies
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 12
Some Key QuestionsSome Key Questions
Maximize physics output for given budget:
Which architecture to use? (strings vs. towers vs. new design)
How to get the data to shore?(optical vs. electric, electronics off-shore or on-shore)
How to calibrate the detector?(separate calibration and detection units?)
Design of photo-detection units?(large vs. several small PMs, directionality, ...)
Deployment technology?(dry vs. wet by ROV/AUV vs. wet from surface)
And finally: path to site decision.
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 20
Production model (example)Production model (example)
Configuration:
10000 optical modules
250 detector units
25 calibration units
3 years for construction (2010-2013)
15 / day
10 / month
1 / month
~ 5 assembly sites are needed
10 detector units / 400 OMs per month to be deployed !
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 25
KM3NeT PhasesKM3NeT Phases
Design study: 2006-2009
Technical Design Report
Preparatory phase: 2008-2010(invited for negotiations)
Political convergence
Commitment for construction of funding agencies/ministries
Governance and legal structure
System prototype
Tendering procedures
Construction phase: 2010-2013
Build a 1 km3 detector
Alexander Kappes, U-Erlangen Astro 2007, Faro Portugal, 6. - 8. Sept. 2007 26
Summary and OutlookSummary and Outlook
Compelling scientific arguments for neutrino astronomy and
the construction of large neutrino telescopes
It is essential to complement IceCube with a
km3-scale neutrino telescope in Northern Hemisphere
Joint effort of ANTARES, NEMO and NESTOR to realize
such a detector in the Mediterranean Sea
EU funded KM3NeT Design Study (2006–2009) is well on its way
CDR workshop in November
Technical Design Report early 2009
Start of “Prepatory Phase” expected early 2008 (until 2010)