Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Sensitivity of the neutrino Sensitivity of the neutrino telescope Antares to the diffuse telescope Antares to the diffuse
galactic neutrinos fluxgalactic neutrinos flux
Fabrice Jouvenot
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Stable
Neutral
Weak interaction cross section
Neutrino
The neutrino, an astroparticleThe neutrino, an astroparticle
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Radio waves 21,1 cm - Dwingeloo Infrared COBE / DIRBENear infrared COBE / DIRBE Visible Photomosaic - Lausten et al.X-rays 0.25, 0.75, 1.5 keV – ROSAT / PSPC Gamma rays >100 MeV – CGRO / EGRET
Milky WayMilky Way
Neutrinos ANTARES ? The Sky
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
The GalaxyThe Galaxy
Spiral arms
Bulge
Halo
Ring + barGalactic center
8,5 kpc
15 – 20 kpc
Galactic plane~ 1 kpc
Sun
1 pc = 3,3 light years
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Inside the GalaxyInside the Galaxy
• Compact objets
• Interstellar Matter
• Interstellar radiation field
• Magnetic field
• Galatic wind
• Cosmic rays
Atomic Hydrogen
HI
Lyman α, and 21cm absorption
Molecular Hydrogen
H2
2.6 mm emission from the CO rotation
Ionized Hydrogen
HII
MHD models, pulsar
observations
HeliumHe
91 % number71 % mass
9 % number28 % mass
Mean density: 1 proton per cm3
Proton~ 90 %
Alpha~ 9 %
Heavy Nucleus
~ 1 %
Galactoradius [kpc]
Den
sity
[at
oms
cm-3]
R, kpc
En
erg
y d
ens
ity
, eV
cm
-3
CMB
Dust
Stars
In the galactic plane
TOTAL
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Theorical hypothesis
Propagation
Equilibrium between CR, B et ISM.
Cosmic Rays Magnetic Field Interstellar Matter
On Earth
Observables
Electromagnetic Interactions
• Diffusion on magnetic field and galactic winds
• Reacceleration
Nuclear physics
• Nuclear reaction
• Decay
• Energy losses
Propagation of Cosmic-RaysPropagation of Cosmic-Rays
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
GalpropGalpropSimulation of Cosmic-Rays confinmentSimulation of Cosmic-Rays confinment
Reading parameters and data(cross-sections, branching ratio, …)
Creation of the Galaxy(ISM, isrf, …)
Cosmic-Rays and sources
Propagation of the heaviest nucleus to the lightest
Secondary products and decays
Cosmic-rays, electrons/positrons, antiprotons, photons. Neutrinos production
(νμ, νμ, νe, νe from charged pions decays)
)
Cylindrical galactocentric geometry:
– R (0 – 30 kpc)
– z (-4 – 4 kpc)
Sources distributions
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Neutrinos productionNeutrinos production
Process giving a neutrino with energy Eν.(Charged pions decays→ Energy range of the pion (2 body or 3body decay)).
Process creating π in p-p collisions(Δ resonance & multi pion production)
Integral over the CR spectrum and ISM density.
Neutrino Oscillation νe:νμ:ντ
1:2:0 → 1:1:1
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
ModelsModelsObservationsConventional CHard Nucleus HNHard Electron HEMN
Bremsstrahlung
Inverse Compton
Bremsstrahlung
Inverse Compton
Bremsstrahlung
Inverse Compton
E2 x
Int
ensi
ty [
Me
V c
m-2 s
-1 s
r-1 ]
Energy [MeV]
Toward the galactic center
Orion arm
500 pc
500 pc
Towardthe galacticcenter
Sun
Sun
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Energy [MeV]
E2 x
Neu
trin
o f
lux
[par
ticl
es M
eV
s-1 c
m-2]
Energy [MeV]
E2 x
Neu
trin
o f
lux
[par
ticl
es M
eV
s-1 c
m-2]
Galactic Galactic emissionemission
0°-90° 90° 0°-180° 180°
Flu
x di
strib
utio
n (
arb
itrar
y u
nit)
Flu
x di
strib
utio
n (
arb
itrar
y u
nit)
Galactic latitude Galactic longitude
νμ+ νμ on Earth
Energy [MeV]
E2 x
Neu
trin
o f
lux
[par
ticl
es M
eV
s-1 c
m-2]
HEMN model
C model
HE model
HN model
γ = 2,3 à 2,9
EAdE
Ed.
)(
Antares
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Detection PrincipleDetection Principle
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
A bit of geographyA bit of geography
Undersea cable
-2475m Antares
La Seyne-sur-Mer
Michel Pacha Institut
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
The detectorThe detector
60 m – 70 m
• 12 lines of 75 PM
• 5 sectors / line• 5 storeys /
sector • 3 PM / storeys
350 m
100 m
14,5 m
Junction box
Cable 40 km
2475 m
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
BackgroundBackground
Atmospheric
Atmospheric neutrinos
Atmospheric muons
Environmental
Potassium decay
Bioluminescence40K → 40Ca + e- + νe
Time [s]
Co
un
tin
g r
ate
[kH
z]
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
AMANDASouth pole
ANTARES43o North : Galactic centre
observed 2/3 of the time
View of the skyView of the sky
• Instant view : 2 π sr
• Integrated view for a day : 3,5 π sr
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
ReconstructionReconstruction
• Track reconstruction
→ Detector answer
→ Angular resolution
• Energy reconstruction
Angular resolution
Ang
ular
res
olut
ion
[°]
Logarithm of the true energy of the muon [GeV]
Lo
ga
rith
m o
f th
e r
eco
nst
ruct
ed
en
erg
y o
f th
e m
uo
n [
Ge
V]
Antares response function
Num
ber
of
even
ts
Log of the muon energy [GeV]
Spectral indices
2.42.73.7
Effective area for muons
Angle between the neutrino and the reconstructed muon
<1 degreeEff
ect
ive
are
a [
km2
]
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Monte Carlo SimulationMonte Carlo Simulation
5 millions induces muons
(at least 1 PM fired)
Energy: 10 GeV – 107 GeV
Working files
Flux simulation :
1 MeV – 107 GeV
Galactic emission
Earth rotation
Galactic & atmosphericponderation
Atmospheric muons
Isotropic Monte Carlo simulation
Energy: 10 GeV – 107 GeV
95x1010 νμ
110x1010 νμ
Neutrinos
Atmospheric
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Result of the simulationResult of the simulation
Galactic neutrinos : ~ 1 to 40Upgoing muons per year
for the whole sky, E> 10 GeV
Atmospheric neutrinos : ~ 20 000Atmospheric muons : ~ 30 000 000
Upgoing muons per yearfor the whole sky, E> 10 GeV
SignalBackground
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Atmospheric muons
Atmospheric neutrinos
Cut on the qualityL
og
10 (
nu
mb
er o
f ev
ents
per
yea
r)
Energy
Angular cutAtmospheric muons < 10% atm. neutrinos
above 10 TeV
33 millions upgoing reconstructed muons per yearMultiplicity: 4,4
Distance between muons: 15 m
Signal extractionSignal extraction
% o
f th
e n
um
ber
of
even
ts p
er
yea
r
Galactic longitude [°]
Galactic neutrinos
Atmosphericneutrinos
100200 300
0 90-900
0,1
0,2
0
0,01
0,02
0,03
Galactic latitude [°]
Galactic longitude
Ga
lact
ic la
titu
de
Reconstruction quality
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Calculus principle
Detection probabilityDetection probability
Getting probability
Nl Number of events
b
Probability (Nobs > Nl) < 1%
If there’s only background
b+s
Detection probability
bN
eN!
bbNP
estimatedobserved
sbN
eN!
sbsbnNP
lNi
sbniP détection de éProbabilitDetection probability
Detection probability
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
0
0,1
0,2
0,3
0,4
0,5
0,6
0,7
0,8
0,9
1
0 1 2 3 4 5 6 7 8
Logarithme de l'énergie reconstruite, log(E) [GeV]
Pro
bab
ilité
de
dét
ecti
on
1 an
5 ans
10 ans
20 ans
50 ans
100 ans
years
years
years
years
years
years
Det
ecti
on
pro
bab
ilit
y
Cut on log of the reconstructed energy log[GeV]
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Antares sensitivityAntares sensitivity
Detection probability vs observation time (99% CL)
Number of years of running1 10 100 1000
Det
ectio
n pr
obab
ility
0
0,5
1
A kilometric detectoris needed !
Performances
It is not possible to observe the Galaxy in a reasonable time
Limit on the model, γ = 2,3
Antares – 5 years
Antares – 10 years
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Effective area ~ 40 × Antares (2 km²)
Cost ~ 5 × Antares
Kilometric extrapolationKilometric extrapolation
Example of a km3 detector
The HN model is observable.
Sensitivity
HN HE C HEMN
7 1 250 5 000 150 000Homogenous cube
20 x 20 x 20 PM looking downward
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Shape identificationShape identification
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
ConclusionsConclusions
Modelisation
Dark clouds
Galactic doubt
Site choice
Depth
Latitude
Environment
Energie reconstruction
Effective area
Other neutrinos flavours
DetectorGalactic fluxes have been calculated
Answer of neutrino telescopes
Antares: limits on the HN model.
KM3: detection or limits on HN.
Bilan
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Kilometric telescopes
2005 Ice Cube2006 KM3Net
Toward the kilometre cube…Toward the kilometre cube…
1996 – 2000 Tests
2001-2003 Study of feasibility
2005 – 2007 Construction & deployment
Antares
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Shape identification
Shape identificationShape identification
????
????!
Max proba pixel
Scan nearest pixels
Selection max proba
Extension of the sélection
Probability calculation
Decrease the pixel size
0
0,1
0,2
0,3
0,4
0,5
0,6
0,7
0,8
0,9
1
1 77 153 229 305 381 457 533 609 685 761 837 913 989 1065 1141 1217 1293 1369 1445
Série1
Working area
Map
Pixel
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Nuclei
ContraintsContraints
Electrons & positrons
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion
Fabrice Jouvenot University of LiverpoolThe 3rd of February 2006
Stable
Neutral
Weak interaction cross section
NeutrinoE < 1019 eV deviated by magnetic
fields
Short mean free path
E > 1020 eV → GZK effect
Noyaux
AstroparticlesAstroparticles
Short mean free path
1 TeV → 700 Mpc 1 PeV → 15 kpc
Libre parcours moyen dû à l’interaction avec les différents fonds de photons
Photon
Libre parcours moyen due to the interaction with the different photons backgrounds
protons
Introduction The GalaxyThe Galaxy Galactic Neutrinos ANTARESANTARES SensitivitySensitivity Km3Km3 Conclusion