Alexander Kappes Erlangen Centre for Astroparticle Physics for the ANTARES collaboration IAU GA, SpS...

Alexander KappesErlangen Centre for Astroparticle Physicsfor the ANTARES collaborationIAU GA, SpS 10, Rio de Janeiro, Aug. 14. 2009

Status of NeutrinoAstronomy

Alexander Kappes, IAU GA, SpS 10, Rio de Janeiro, 14. Aug. 2009 2

Outline

Introduction to neutrino astronomy

Neutrino telescopes: ANTARES and IceCube

Selected results

Outlook


Acceleration at source (cosmic rays, electrons)

Secondary particle production near source(interaction with photons or matter)

• Protons: pion decay

• Electrons: inverse Compton-scattering of photons

e + γ → e + γ (TeV)

Particle production in thenon-thermal universe

p + p(γ) → π± + X μ + νμ

e + νμ + νe

p + p(γ) → π0 + X γ + γ (TeV)

e

active galactic nuclei(artist’s view)

micro-quasars(artist’s view)

supernova remnants(SN1006, optical, radio, X-ray)


Why neutrino astronomy?

• 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


Principle of neutrino detection

muon

νμnuclearreaction

cascade43°

νμ

μTime & position of hits

μ (~ ν) trajectory

Energy

PMT amplitudes


• Flux from above dominated by atmospheric muons

• Neutrino telescopes mainly sensitive to neutrinos from below

Background: atmospheric muonsand neutrinos

p

atmosphere

cosmicrays

μνμ

νμ

cosmic

background

p

μνμ


Neutrino telescope projects

IceCubeIceCube

BaikalBaikalBaikalBaikalANTARESANTARESANTARESANTARES

NESTORNESTORNESTORNESTORNEMONEMONEMONEMO


Neutrino telescopes:

ANTARES and IceCube


Sky coverage

Visibility ANTARES (Mediterranean) > 75% 25% – 75% < 25%

TeV γ-ray sources Galactic extra-Galactic

Visibility IceCube (South Pole) 100% 0%


ANTARES

-1995 m

-2475 m

2 m

• 12 lines (885 PMTs)+1 instrumentation line

• Instrumented volume: ~0.01 km3

• Completed since May 2008


IceCube Observatory

1450 m

2450 m

• IceTopAir shower detector

• InIce80 strings (4800 PMTs)Status now: 58 strings deployedInstrumented volume: 1 km3

• DeepCore6 additional stringsMore densely packedFirst string deployed 2008/09

Low-energy physics, E < 1 TeV (WIMPS, . . . )


Selected results


Atmospheric muons & neutrinos

Up-going:ν-induced muons (~1000)

ANTARES (341 days)

Down-going:atm. muons

Zenith angle (Degrees)


• Skymap for ANTARES 5 lines (140 days, 94 events)

• No significant excess above background

ANTARES: Search for point sources


IceCube: Search for point sources –40 strings (6 months)

PreliminaryBackground: atm. neutrinos(6796 events)

(10981 events)Background: atm. muons

Most-significant spot:all-sky background probability: 61%

Significance


Point source sensitivities

ANTARES: 5 lines 140 days (limits) 12 lines 1 year (pred. sensitivity)

Flux predictionsHalzen, AK, O’Murchadha, PRD (2008)AK, Hinton, Stegmann, Aharonian, ApJ (2006)Kistler, Beacom, PRD (2006)Costantini & Vissani, App (2005). . .

MACRO (6 years)Super-K. (4.5 years)

AMANDA (3.8 years)

IceCube: IceCube 40 Strings 330 days (sensitivity)

IceCube 80 Strings 1 yr (pred. sensitivity)

90% CL sensitivity for E-2 spectra (preliminary)


• 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


`̀

IceCube 86 with Deep CoreSensitivity 1 yr (prel., hard)

IceCube: WIMP searches

Direct detection experiments (CDMS, COUPP, KIMS)

Super-Kamiokande (2004)

AMANDA 7 years soft hard

IceCube 22-strings limits(PRL 102, 201302 (2009)) soft hard

MSSM models}


More physics with neutrino telescopes

• Variable sources (GRBs, AGNs . . . )

• Diffuse neutrino flux

• Cosmic-ray anisotropies (10–100 TeV)

• Supernovae (MeV neutrinos)

• Neutrino oscillations (atmospheric neutrinos 10–100 GeV)

• Exotic physics (Lorentz violation, monopoles, . . .)


Outlook


• km3-scale neutrino telescope in the Mediterranean Sea

(also platform for marine and geological science)

• One of the projects on the roadmap of the European Strategy Forum for Research Infrastructures (ESFRI)

• EU funded Design Study (2006-2009)

• First data in 2012/13 possible

KM3NeT

Artist’s view


Point source sensitivities

ANTARES: 5 lines 140 days (limits) 12 lines 1 year (pred. sensitivity)

MACRO (6 years)Super-K. (4.5 years)

AMANDA (3.8 years)

90% CL sensitivity for E-2 spectra (preliminary)

not final detector

IceCube: IceCube 40 Strings 330 days (sensitivity)

IceCube 80 Strings 1 yr (pred. sensitivity)

KM3NeT: 1 yr (pred. sensitivity)

Flux predictionsHalzen, AK, O’Murchadha, PRD (2008)AK, Hinton, Stegmann, Aharonian, ApJ (2006)Kistler, Beacom, PRD (2006)Costantini & Vissani, App (2005). . .


Summary

• Neutrinos provide complementary information to gamma-rays and protons of the high-energy universe

• ANTARES completed and 70% of IceCube installed

• So far no cosmic high-energy neutrinos identified

- IceCube enters region with realistic discovery potential within the next years

- Significantly more sensitive km3-scale neutrino telescope in theMediterranean needed to further advance into discovery regionand coverage full sky

KM3NeT currently in design phase

Alexander Kappes Erlangen Centre for Astroparticle Physics for the ANTARES collaboration IAU GA, SpS...

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