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![Page 1: Alexander Kappes Forschungsseminar Institut für Physik, Humboldt-Universität Berlin, 11. February 2011 Fishing for Neutrinos in the Mediterranean Sea –](https://reader035.fdocuments.in/reader035/viewer/2022062801/56649e305503460f94b20f95/html5/thumbnails/1.jpg)
Alexander KappesForschungsseminarInstitut für Physik, Humboldt-UniversitätBerlin, 11. February 2011
Fishing for Neutrinosin the Mediterranean Sea –ANTARES and KM3NeT
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 2cc
Outline
Introduction to neutrino astronomy
The ANTARES neutrino telescope
Selected results from ANTARES
The future Mediterranean neutrino telescope KM3NeT
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 3cc
1912: Discovery of Cosmic Rays (Victor Hess)• Observations before 1912:
- Elektroscopes dischargedue to natural radioactivity
• Balloon experiments since 1912: (Hess, Kolhörster)
- Discharge increases above ~1.5 km altitude
- Conclusion: Ionising radiation from outer space
Measurements Victor Hess (1912)
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 4cc
Cosmic rays:
• spectrum measured over12 orders of magnitudein energy
• power law spectrum(non thermal)
• consists of particles
Sources still unknown !
. . . 99 Years LaterCosmic ray spectrum
109 1012 1015 1018 1021
energy (eV)
10-27
10-21
10-15
10-9
10-3
103
Flu
x (G
eV-1 m
-2 s
-1 s
r-1)
LHC
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 5cc
The High-Energy Universe
gamma-ray bursts(GRB 080319B, X-ray, SWIFT)
active galactic nuclei(artist’s view)
supernova remnants(SN1006, optical, radio, X-ray)
micro-quasars(artist’s view)
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 6cc
Accelerator (source)
• Shock fronts (Fermi acceleration)
• Objects with strong magnetic fields (pulsars, magnetars)
Beam dump (secondary particle production)
• Interaction with photon and matter near the source
• Protons: pion decay
• Electrons: inverse Compton-scattering of photons
e + γ → e + γ (TeV)
High-Energy Particle Production in the Universe
p + p(γ) → π± + X μ + νμ
e + νμ + νe
p + p(γ) → π0 + X γ + γ (TeV)
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 7cc
Why Neutrino Astronomy?
• Neutrinos are produced in cosmological objects
• Neutrinos point back to the source
• Neutrinos travel cosmological distances
• Neutrinos escape from optically thick sources
• Neutrinos are a clear sign for hadron acceleration
Neutrinos provide complementary information to gamma-rays and protons
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 8cc
Principle of Neutrino Detection
muon
νμnuclearreaction
cascade43°
νμ
μTime & position of hits
μ (~ ν) trajectory Energy
PMT amplitudes
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 9cc
• Flux from above dominated by atmospheric muons
• Neutrino telescopes mainly sensitive to neutrinos from below
Background: Atmospheric Muons and Neutrinos
atmosphere
cosmicrays
μνμ
νμ
signal
background
p
p
μνμ
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 10
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Neutrino Telescope Projects
IceCubeIceCube
BaikalBaikalBaikalBaikalANTARESANTARESANTARESANTARES
NESTORNESTORNESTORNESTORNEMONEMONEMONEMO
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 11
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Sky Coverage
Visibility ANTARES (Mediterranean) > 75% 25% – 75% < 25%
TeV γ-ray sources Galactic extra-Galactic
Visibility IceCube (South Pole) 100% 0%
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 12
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The ANTARES
Neutrino Telescope
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ANTARES in the Mediterranean
Submarine cable (45km)
Shore Station
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 14
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The ANTARES Neutrino Telescope
-1995 m
-2475 m
• 12 lines (885 PMTs)+1 instrumentation line
• Instrumented volume: ~0.01 km3
2 m
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 15
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ANTARES Storey
Hydrophone:acoustic positioning
Optical Module:10” Hamamatsu PMTin 17” glass sphere photon detection
Local Control Module(in Ti cylinder):Front-endClock, tilt/compass, power distribution…
Titanium frame: support structure
Optical Beaconwith blue LEDs:timing calibration
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 16
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Construction
Milestones
• 2001 Installation of 40 km electro-optical cable
• 2002 Deployment and connection
of junction box
• 2003–2005 Installation ofprototype lines
• 2006–2008 Installation of 12 lines
• Detector completed since May 2008
Line deployment
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Line Connection
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011cc
• Light scattering + chromatic dispersion: ~ 2 ns
• TTS in PMTs: ~ 1.2 ns
→ Intrinsic angular resolution 0.2˚– 0.3˚
Requires electronics + calibration: < 0.5 ns
Timing Calibration
Signal time in OMs relative to reference PMT
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011cc
• Acoustic positioning system
• Tiltmeter and compass on each storey
Accuracy = 10 cm (0.5 ns)
Position Calibration
20 day periodMarch 2007
0 4-4-8-12 X [m]
-4
0
4
-8
Y [
m] Horizontal storey movement
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 20
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Optical Background
2005 2006 2007 2008
cable fault
2009
(Different colors correspond to different storeys)
Sin
gle
PM
T r
ate
[kH
z]
Optical background due to 40K decay and bioluminescence
• Typical rates 60-100 kHz per photomultiplier
• Occasional bursts and periods of high rates
Filtered by causality conditions between hits
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QuickTime™ and aGIF decompressor
are needed to see this picture.
Up-going Neutrino Candidate
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Selected Resultsfrom ANTARES
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Atmospheric Muons & Neutrinos
Up-going:ν-induced muons (~1000)
ANTARES (341 days)
Down-going:atm. muons
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 24
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Muon Intensity vs. Depth (90 days, 5 Lines):
2.5km6km Astropart. Phys. 34 (2010) pp. 179-184
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 25
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Upper Limit on Diffuse Flux (334 days)
IceCube 40 Strings
Physics Letters B 696 (2011) 16–22
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 26
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Full-Sky Search for Point Sources (295 days)
Most significant cluster
• Cluster of 8 events:Unbinned likelihood fit: Nsig = 5.16p-value = 0.024 (2.0 σ)
• Also no significant excess for selected sources
Equatorial coordinates
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Flux Limits and Sensitivity
25
preliminarypublication in preparation
Best limits on neutrino fluxes from southern-sky sources
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 28
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• Neutralino (χ) good WIMP candidate
• ANTARES data:No excess
Long term investigation necessary
Dark Matter Searches (WIMPs)
χ
ν
-ν
hard (W+W–)
soft (bb)ANTARES (5-line data, ~70 days)
preliminary
Neutralino mass [GeV]0 100 200 300 400 500 600 700
Φ(ν
μ+
νμ)
(>1
0 G
eV
) fr
om
Su
n [
km
-2 y
r-1]
109
1010
1011
1012
1013
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Alexander Kappes, Forschungsseminar, Humboldt-Universität, 11.02.2011 29
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More Physics
Point sources:
• Gamma-ray bursts
• Flaring sources (e.g. AGNs)
• Use coincidences in neutrino telescopes to trigger optical follow-up
Other topics:
• Neutrino oscillations (atmospheric neutrinos 10 - 100 GeV)
• Exotic physics (Lorentz violation, monopoles, . . .)
• Cosmogenic neutrinos (E 10≳ 17 eV)
• Cosmic-ray anisotropy
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The Future Mediterranean
Neutrino Telescope KM3NeT
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Current Upper Limits on Point Sources
90% C.L. upper flux limits for E-2 spectra (preliminary)
⇒ km3-class detector in Northern Hemisphere needed
Galactic sources with TeV γ-ray emission
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KM3NeT
Artist’s view
• Future cubic-kilometer-class Mediterraneanneutrino telescope(joint effort of ANTARES, NEMO, NESTOR)
• Supported by ESFRI, ASPERA, ASTRONET
• Objectives:
- Exceed Northern-hemisphere telescopes by factor ~50 in sensitivity
- Exceed IceCube sensitivity by substantial factor
- Provide node for earth and marine sciences
- Budget: ~220 MEuro
EU-funded Design Study (2006–09) and Preparatory Phase (2007–11)
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Objective: Support 3D-array of photodetectors andconnect them to shore (data, power, slow control)
• Optical Modules
• Front-end electronics
• Readout, data acquisition, data transport
• Mechanical structures, backbone cable
• General deployment strategy
• Sea-bed network: cables, junction boxes
• Calibration devices
• Shore infrastructure
• Assembly, transport, logistics
• Risk analysis and quality control
Technical Design
Design rationale:cost-effectivereliableproducibleeasy to deploy
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OM with Many Small PMTs
• 31× 3” PMTs in 17-inch glass sphere(total ~140 mW)
• Front-end electronics (B,C)
• Al cooling shield and stem (A)
• Advantages:
- autonomous detection unit with single penetrator
- same photocathode area as 3 large PMTs
- directional information
- reduced afterpulsing
- improved 1-vs-2 photo-electron separation better sensitivity to coincidences⇒
A
B
CC
PMT
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• 20 storeys
• Each storey supports 2 multi-PMTs
• Power and data cables separated from ropes;single backbone cable with breakouts to storeys
• Distance between DU base and first storey = 100m
Flexible Towers with Horizontal Bars
2 km
Footprint “building block”(optimization ongoing)
• 2 “building blocks” required toachieve objectives
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Point Source Sensitivities (1 year)
ANTARES: 1 yr (pred. sensitivity)
Predicted fluxesHalzen, AK, O’Murchadha, PRD (2008)AK, Hinton, Stegmann, Aharonian, ApJ (2006)Kistler, Beacom, PRD (2006)Costantini & Vissani, App (2005) . . .
KM3NeT: 1 yr (pred. sensitivity)KM3NeT
IceCube 80: 1 yr (pred. sensitivity)
ANTARES
IceCube
90% CL sensitivity for E-2 spectra (preliminary)
• Vision of a worldwide neutrino observatory (IceCube + KM3NeT)
• Large overlap region (enhanced sensitivity + cross check)
SNR RX J1713 @ 5σ in 8 years
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Next steps: Prototyping and design decisions
• TDR public since June 2010
• final decisions require site selection
• expected to be achieved by end of 2011
Timeline:
Next Steps and Timeline
nownow
Feb
2006
Feb
2006
Mar
200
8
Mar
200
8
Jun
2010
Jun
2010
Mar
201
2
Mar
201
2
TDRTDRCDRCDR
Design StudyDesign Study
Preparatory phasePreparatory phase
Prototyping and constructionPrototyping and construction
Data takingData taking
2014
2014
2018
2018
Design and site decision
Design and site decision
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Summary
• Neutrino provide complementary information to gamma-rays and protons of the high-energy universe
• ANTARES completed since May 2008
- First results published and further analyses in full swing
- No deviations from background observed
- Detector likely too small to detect cosmic neutrinos
• KM3NeT: km3-class neutrino telescope in Northern Hemisphereneeded to complement IceCube
- In prototyping phase
- Substantially improved sensitivity compared to IceCube
- First data could be available in 2014