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