recent developments in neutrino telescopy
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Recent Developments in Neutrino Telescopy
Spyros Tzamarias
HEP2012: Recent Developments in High Energy Physics and Cosmology
615 t of C2Cl4
The Nobel Prize in Physics 2002
Masatoshi Koshiba Raymond Davis Jr.
Riccardo Giacconi
These discoveries of low (<100MeV) energy extraterrestrial neutrinos led us to various achievements on basic neutrino properties (oscillations) and stellar evolution.
They also offer important possibilities to progress, e.g., with geoneutrinosand solar (CNO) neutrinos, and even more with supernova neutrinos.
Furthermore, the obtained knowledge and the increased confidence motivate us to continue, widening the scope and field of our investigation.
The current experiments are monitoring a huge range of energies!
Log(
E/eV
)
νμ
μ-W-
d
As proposed by Markov in the late 50s, the neutrino-induced μ's offer the practical way to probe high energy neutrinos, whilst using the whole earth as an absorber of atmospheric muons.
The size of such a detector is dictated by the muon’s range (due to EM interactions)
i.e. the detector size for an efficient TeV-muon detection should be of the order of a km
ln
Extraterrestrial High Energy Neutrino SourcesOr
What do we need these neutrinos for ?
•Cosmic-Hadron accelerators can produce VHE CR’s, γ-rays and neutrinos•Electron acceleration is the main source of the non-thermal EM radiation, up to high energies (up to TeV). Many such e-accelerators have been identified.•There is a connection between the (multi-TeV) γ and neutrino production•Where are these Cosmic-Hadron accelerators?
ρg−CR ≈1eV / cm 3 ≈10−12eρg / cm 3
V ≈1067cm 3 , tesc ≈107 y
P=ρg−CRV / tesc ≈1041eρg / s
ρSN ≈0.03y−1, ESN ≈10
51eρg, e ≈10%
W. Baade and F. Zwicky, Remarks on super-novae and cosmic rays , Phys. Rev. 46 (1934) 76
ρE>1EeV ≈3⋅10−19eρg / cm 3
Pρoduction Rate : R =ρE>1EeV
TH=9⋅1044
eρgMpc3 y
, TH ≈1010 y
thiscan be satuρated by:
R ≈900GRBGpc3 y
⋅1051eρgEM OUTPUT1 24 34 OR R ≈
150AGNGpc3
⋅2⋅1044eρg / sEM OUTPUT
1 244 34 4
Galactic Sources
ExtraGalactic Sources
Neutrinos (for all distances) and gammas point to the source of origin. However…
There many kinds of HE neutrino sources (perhaps as many as the Supersymmetric Scenaria)
n
WIMP(neutralino)
SUN
earth
Indirect Searches for Dark Matter
ICECUBE KM3NeT
Full Sky Coverage
Why neutrinos from Galactic γ-ray (TeV) sources are important ?Observation of PeV (1015 eV) γ-rays will point to hadron accelerators revealing the CR sources. However, a) PeV γ-rays do not survive large distances and b) the γ-ray spectra of the observed galactic sources exhibit energy cut-off
Neutrino observation from RX J1713.7-3946 will prove unambiguously the hadronic production of γ-rays
RX J1713.7-3946
~ e−E/Ec withEc ≈10TeV( )
REMINDER: there are not very reliable phenomenological models to predict precise upper bounds for the extragalactic neutrino fluxes
A more efficient (larger effective area, better resolution) than ICECUBE detector is needed to discover galactic sources
NEMO
21
KM3NeTInternational consortium involving more than 300 scientists from 10 EU countriesOne objective: build the most sensitive high energy neutrino telescopeKM3NeT is one of the 44pan-european researchinfrastructures on the ESFRI EU roadmap
22
An artists impression of KM3NeT (≈ 1/3)
Primary Junction box Secondary Junction boxes
Detection Units
Electro-optical cable
signal hits
background hits pictorial representation of a ν charged current interaction inside the neutrino telescope
Pattern Recognition and Track Reconstruction
Eν<10 TeV
10TeV<Eν<100 TeV
100TeV<Eν<1 PeV
1PeV<Eν
Angle (ψ) between reconstructed muon track and parent neutrino (Degrees)
z
x y
(θm, φm)
ψ
(θtrue, φtrue)
2 22 2 2 2
1 1 1 1 1 12 cos2 22 2 2 2
0
( )2
x y x yw
s s s s
x y
P e e dws s
py yyyp
=
Can we estimate accurately the tracking errors?Median of Ψ (degrees) vs the cosine of the zenith angle
Energy Estimation
HOU Reconstruction & Simulation (HOURS): A complete simulation and reconstruction package for Very Large Volume underwater neutrino Telescopes, A. G. Tsirigotis et al., VLVNT2009
Reconstructed Energy (log of GeV)
0.5<cos(θ)<0.55
R.ADecl.
RX J1713.7-3946
Comparison of the Discovery Potentials
Number of events (N) – Angular profile (S) – Energy (E)
0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 160.50
5.00
T180 NES
T180 NS
T180 N
T180(A)
years
Disc
over
y Po
tenti
al in
uni
ts o
f the
re
fere
nce
flux
RXJ1713
5-σ DISCOVERY POTENTIAL
0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16
T180 T150
T130 S130
S100
years
Disc
over
y Po
tenti
al in
uni
ts o
f the
re
fere
nce
flux
1,00
3 3.5 4 4.5 5 5.5 6 6.5 7 7.5 8 8.5 9 9.5 100.70
T180
Polynomial (T180)
T150
Polynomial (T150)
T130
Polynomial (T130)
S130
Polynomial (S130)
S100
Polynomial (S100)
FOM (years of observation time)5-σ DISCOVERY.
8.4y
7.6y
6.4y
6.0y
5.6y
1,00
KM3NeT with 608 strings at 100m (130m) apart will discover a neutrino source as the RXJ1713 after 5.6 (6) years of observation. The estimation error is less than 0.8y.
PRELIMINARY: An extra 30% improvement ( i.e a discovery after 4 y of observation) can be achieved by taking into account the known source direction. A further improvement is expected by developing a more efficient method to reject low energy atmospheric neutrinos., see A. Tsirigotis talk
KM3NeT-PP general meeting - Catania, february 22 2012
33
KM3NeT and EMSO
E. Migneco
Real Time Environmental Monitoring
Sinergy with the Earth and Sea Science Community
Toulon, Sicily and Hellenic: sites of common interest for KM3NeT
and EMSO
Geophisics (geohazard):Seismic phenomena, low frequency passive acoustics, magnetic field variations,...
Oceanography (water circulation, climate change): Current intensity and direction, Water temperature, Water salinity ,...
Biology (micro-biology, cetaceans,...):Passive acoustics, Biofouling, Bioluminescence, Water samples analysis,...
What after the Preparatory Phase?• Need an organizational structure to manage the post-design
and preparatory phase• A Memorandum of Understanding is in preparation• Goals
– Complete the Physics Studies and the Optimization of the design– Validation of chosen technologies– Complete the final Technical Proposal– Central management– Definition of collaboration rules– Start of construction with engineering arrays in the potential
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