km3net - solvay instituteskm3net international solvay institutes 27 29 may 2015, brussels, belgium....
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KM3NeT
International Solvay Institutes
2729 May 2015, Brussels, Belgium.
Maarten de Jong
Astro-particle and Oscillations Research
with Cosmics in the Abyss
(ARCA & ORCA)
1
Introduction
1. Discovery and subsequent observation of high-energy neutrino sources in Universe
2. Measurement of neutrino mass hierarchy
3. Synergy with Earth & Sea sciences
• KM3NeT is a new Research Infrastructure – network of cabled observatories
– located in deep waters of Mediterranean Sea
– hosting multi-km3 Neutrino Telescope
2
Detection principle
muon 1 2 3 4 5
~ km
~ 100 m neutrino
interaction
time resolution 1 ns position resolution 10 cm
angular resolution 0.1 deg
3
KM3NeT
Architecture
shore station
remote access to data
remote operation on off
computer center
4
10100 Mb/s
neutrino telescope
Design ~
60
0 m
Optical module
Launcher vehicle
‒ 31 x 3” PMTs
‒ low-power HV
‒ LED & piezo inside
‒ FPGA readout
‒ White Rabbit
‒ DWDM
‒ rapid deployment
‒ autonomous unfurling
‒ recoverable 5
17”
Building block
6
RX
J17
13
eve
nts
/ y
ear
number of lines number of floors
Smallest detector with optimal efficiency ~ 1/6 total size
labs scaling factor labs scaling factor
ETEL
3-inch PMTs
Key features: – timing ≤ 2 ns (RMS) – QE ≥ 25-30% – collection efficiency ≥ 90% – photon counting purity 100% (by hits, up to 7) – price/cm2 ≤ 10” PMT
ETEL D792 Hamamatsu R12199 HZC XP53B20
7
PDF of muon light
8
50 m
Dt [ns]
Angular resolution 0.1 degrees
1 T
eV m
uo
n PMT
Phased implementation
9
Phase Blocks Primary deliverables
1 0.2 Proof of feasibility and first science results;
2.0
2
ARCA
Measurement of neutrino signal reported by IceCube;
All flavor neutrino astronomy;
1
ORCA Neutrino mass hierarchy;
3 6 (+1) Neutrino astronomy including Galactic sources;
1) Optical module deployed at Antares April 2013 (2500 m)
2) Mini string deployed at Capo Passero May 2014 (3500 m)
Prototyping
10
Eur. Phys. J. C (2014) 74:3056
Rat
e [H
z]
Multiplicity
Rat
e [H
z]
PMT orientation
To be submitted Eur. Phys. J. C
Phase-1
First string assembled end of last year
to be deployed at KM3NeT-France following weeks
• Completion Phase-1 by end 2016 – 24 strings in KM3NeT-Italy
– 6 more strings à la ORCA in KM3NeT-France 11
Phase-1
12
ARCA
13
Measurement of neutrino signal reported by IceCube
~1 km ~1 km
1 building block 1 building block
PDF of shower light (I)
14
wave fro
nt
~ [m] log(E/TeV)
~ 100 m ne
time resolution 1 ns position resolution 10 cm
angular resolution ?
Cascade analysis 1.0 cut & count
1. Online data filter – 5 (or more) coincidences between PMTs in same optical
module (DT = 10 ns)
2. Event filter – number of hits ≥ 2000
3. Vertex cut – veto atmospheric muons
4. Energy cut – total time-over-threshold ≥ 12 ms
5. MRF/MDP cut – 2D cut based on Boosted Decision Tree & energy estimate
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3.) Atmospheric muon veto
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R2 [103 m2]
z [m
]
detector volume vertex cut
cosmic neutrinos atmospheric muons
R2 [103 m2]
80%
5.) Signal to Noise
17
“sweet spot”
5.) Signal to Noise
18 BDT (topology of event)
S e
ven
ts /
yea
r /
blo
ck
atmospheric muons atmospheric neutrinos (tracks) atmospheric neutrinos (showers) cosmic neutrinos (tracks) cosmic neutrinos (showers)
Sensitivity¶
19
observation time [y]
sign
ific
ance
[s
]
muon tracks 𝛉 ≥ 𝟖𝟎°
cascades cut & count
maximum likelihood
¶ Vetoing of atmospheric neutrinos not included.
F = 1.2 10−8 𝐸−2 𝑒−𝐸/(3 𝑃𝑒𝑉) 𝐺𝑒𝑉−1𝑠𝑟−1𝑠−1𝑐𝑚−2
Resolution
20
En [GeV] En [GeV]
Dq
[d
eg]
E R/E
T
Dq ER/ET
ne
KM3NeT/ARCA Preliminary KM3NeT/ARCA Preliminary
1 sigma
90%
Energy Direction
Simulation of 1.5 PeV nt event¶
21 ¶ Passes all cuts.
Diffuse muon analysis
22
sign
ific
ance
[s
]
observation time [y]
ORCA
23
Measurement of
neutrino mass hierarchy
200 m
1 building block
Neutrino mass hierarchy
24
mas
s
nt nm ne
“normal” “inverted”
109 eV
106 eV
103 eV
100 eV
10-3 eV
electron
proton
g
neutrino
1 : 1000,000,000,000
Neutrino mass hierarchy
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oscillations
cross sections
fluxes
matter
L/E [km/GeV]
pro
bab
ility
E [GeV]
s [
10
-36 c
m2]
E [GeV]
EdN
/dE
[cm
-2 s
-1]
E [GeV]
probability
cos(
q)
ORCA
26
observation time [y]
sign
ific
ance
[s
]
¶ Using prior for q23 octant and dCP angle.
Future prospects (I)
27
~1 km
1 building block
~1 km
1 building block
~1 km
1 building block
~1 km
1 building block
~1 km
1 building block
~1 km
1 building block
Future prospects (II)
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RXJ1713¶
Vela X§
observation time [y]
sign
ific
ance
[s
]
RXJ1713-3946
Vela X
¶ S.R. Kelner, et al., Phys. Rev. D 74 (2006) 034018.
§ F.L. Villante and F. Vissani, Phys. Rev. D 78 (2008) 103007.
(binned analysis)
Galactic sources
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sudden Eddy currents
Temperature
Earth & Sea sciences¶
France
observatory food supply
Bioluminescence
short lived (rare) events dominate life in deep-sea
permanent observatory
time profile ¶ Antares
KM3NeT status & outlook
• R&D – developed cost-effective technology – feedback from prototypes confirm key specifications
• Phase-1 – going ahead as planned
• Phase-2 – ARCA
• measurement of IceCube flux with different methodology, complementary field of view and improved resolution
• all flavour neutrino astronomy
– ORCA • measurement of neutrino mass hierarchy
• Future prospects – exploration of our Galaxy
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