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Status of neutrino astronomy ( Sources of high-energy neutrinos ) Julia K. Becker Gteborgs Universitet, Sweden see also Physics Reports 458 , ArXiv:0710.1557 (2008) Astrophysical Neutrinos May 31st Neutrino 2008, Christchurch, NZ Julia K

SLIDE 1

Status of neutrino astronomy (Sources of high-energy neutrinos)

Julia K. Becker

Göteborgs Universitet, Sweden

see also Physics Reports 458, ArXiv:0710.1557 (2008)

SLIDE 2

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Astrophysical Neutrinos

SLIDE 3

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Overview

Production of high-energy neutrinos
how?
why?
Potential emitters
Neutrino flux models for extragalactic sources
Active Galactic Nuclei
Gamma Ray Bursts

SLIDE 4

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Neutrino production

pγ ∆+ π+ n/π0 p
π+ µ+ νµ e+ νe νµ νµ
π0 γ γ (Eγ~TeV)
Pions: Correlation TeV Photons – Neutrinos
Optically thick environment: Eγ~keV-GeV
Main assumption:
Lγ ~ Lp ~ Lν
Photon luminosity:

Sources can be identified

Proton luminosity ~ TeV sources
Careful! Other processes (Inverse Compton, proton

synchrotron can contribute, too!)

Animation generated with povray

SLIDE 5

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Neutrino flux from a single source

       − ⋅ ⋅ = Φ

− max

exp E E E A dE d

ν α ν ν ν ν

Spectral index neutrinos ~ spectral behavior protons ~ 2
Maximum neutrino energy ~ proton maximum energy
Normalization Aν: electromagnetic or hadronic emission

... / / / /

p TeV ray X radio

L L L L L

γ ν − −

∝

(dependent on the underlying model)

SLIDE 6

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Diffuse neutrino flux

single source flux source distribution function comoving volume flux decreases with distance d

SLIDE 7

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Why neutrinos, anyway? (I)

Krawczynski et al., ApJ 601 (2004)

(a) Charged Cosmic Rays (b) TeV Photons

1ES1959+650, MWL

SLIDE 8

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Why neutrinos, anyway? (II)

Figure: Wolfgang Wagner, PhD thesis

Cherenkov

SLIDE 9

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Potential HE neutrino sources

SNRs XRBs µquasars Pulsars

Mol. clouds

... AGN GRBs Starbursts GZK νs ...

galactic: extragalactic:

Tycho SNR M87 GRB080319b GRS 1915+105 Crab pulsar M82 GRB080319b M87

SLIDE 10

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

AGN: First discovery

1962: 3C 273 - Quasi-

stellar Object (QSO)

core extremely bright,

not resolvable looks like a star

High Radioemission
1963: ! no star

Active Galaxy (Maarten Schmidt)

www.time.com/time/covers

SLIDE 11

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Ground based

ptical/ radio

HST Image of the Torus and the core

88 000 ly 1.7 arcsec 400 ly 380 arcsec

NGC 4261

SLIDE 12

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker Baikal (2000) Baikal (2000)

Theoretical bounds?

Waxman&Bahcall, PRD 59:23002 (1999) Mannheim et al., PRD 63:23003 (2001) Baikal (2000) Baikal (2000) AMANDA (2008)

IceCube sensitivity

SLIDE 13

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

AGN: Neutrinos & X-rays?

Nellen,Mannheim&Biermann Phys.Rev.D (1993) Stecker&Salamon Space Science Rev. (1996) Alvarez-Muñiz & Mészáros PRD 70 (2004) Fréjus: Rhode&Daum, Astropart. Phys. 4:217 (1996) Baikal: Dzhilkibaev et al., Phys.Atom.Nucl. 63:951 (2000)

Baikal (2000)

SLIDE 14

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

AGN: Neutrinos & X-rays?

Nellen,Mannheim&Biermann Phys.Rev.D (1993) Stecker&Salamon Space Science Rev. (1996) Alvarez-Muñiz & Mészáros PRD 70 (2004) AMANDA (2000-2003) Spectrum: Münich et al., ICRC 2007 Limits: Achterberg et al, PRD 75 (2007)

JKB et al, Astrop. Phys. 28:98 (2007) (1) (2) (3) Data:

SLIDE 15

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Steep or flat spectrum sources?

JKB & P. L. Biermann, ArXiv:0805.1498

SLIDE 16

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Neutrino flux & Cosmic Rays

Normalize to Auger

correlation

Neutrino production

at the foot of the jet Flat spectrum radio q.

Model fits recent
bservations of BL

Lac (Marscher et al,

Nature 2008) and M 87 (Walker et al, ArXiv:0803.1837)

(1) Cuoco & Hannestad, ArXiv:0712.1830 (2) Koers & Tinyakov, ArXiv:0802.2431 (3) Halzen & Ó Murchacha, ArXiv:0802.0887 (4) JKB & Biermann, ArXiv:0805.1498 (5) Kachelrieß et al., ArXiv:0805.2608

SLIDE 17

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Gamma Ray Bursts

SLIDE 18

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Unvoluntary Pioneer - Vela

1967 – 1979
riginal goal:

controling nuclear tests (USA/Soviet Union)

Coincidental

detection of Gamma Ray Bursts

SLIDE 19

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Gamma Ray Burst – time profile

SLIDE 20

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

GRB progenitors

duration > 2 s typically ~ 40 s duration < 2 s ~ms - s

Animated movies: Nasa

Long GRBs Supernova Explosions Short GRBs binary mergers

SLIDE 21

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Prompt GRB ν Spectrum

( )

γ ν γ ν ν ν ν γ γ

ε ε ε ε α β β α F A z t F z E

s s b b

∝ = = + = + = , , , 1 1

Waxman & Bahcall, PRL 78:2292 (1997)

ν

A

b ν

ε

s ν

ε α β

SLIDE 22

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

GRB080319B

http://grb.fuw.edu.pl/pi/index.html

IceCube-9: ~0.1 event IceCube-80: ~1 event

A. Kappes

z = 0.94 t90 = 60s Γ= 285 Fγ = 5.72e-4 erg/cm2 αγ = 0.82 βγ= 3.87 εγ

b= 0.651MeV

SLIDE 23

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

Towards the next generation

IceCube & Km3NeT
North & South view
Acoustic & radio technique

for the highest energies

ANITA, Aura, ARIANNA,

AMADEUS, SalSa, LUNASKA, ...

Together with Glast, CTA,

Hawk,...;Auger South & north, ... create a complete view of the non-thermal Universe

SLIDE 24

May 31st Neutrino 2008, Christchurch, NZ Julia K Becker

High-energy neutrinos

Produced in pγ/pp interactions
Potential sources:
Galactic (only up to 10-100 TeV) – SNR, XRB,

µquasars, pulsars, ...

Extragalactic (up to 1011 GeV) – AGN, GRBs, ...
Experiments
Improvement of limits by 2.5 orders of

magnitude in the past 7 years

First physics conclusions (X-ray emitting AGN, ...)
New generation to come (IceCube, Km3NeT),

Status of neutrino astronomy (Sources of high-energy neutrinos)

Julia K. Becker

Göteborgs Universitet, Sweden

Astrophysical Neutrinos

Overview

Neutrino production

Neutrino flux from a single source

       − ⋅ ⋅ = Φ

− max

exp E E E A dE d

ν α ν ν ν ν

... / / / /

p TeV ray X radio

L L L L L

γ ν − −

∝

(dependent on the underlying model)

Diffuse neutrino flux

single source flux source distribution function comoving volume flux decreases with distance d

Why neutrinos, anyway? (I)

Why neutrinos, anyway? (II)

Potential HE neutrino sources

SNRs XRBs µquasars Pulsars

... AGN GRBs Starbursts GZK νs ...

galactic: extragalactic:

AGN: First discovery

stellar Object (QSO)

not resolvable looks like a star

Active Galaxy (Maarten Schmidt)

NGC 4261

Theoretical bounds?

AGN: Neutrinos & X-rays?

AGN: Neutrinos & X-rays?

Steep or flat spectrum sources?

Neutrino flux & Cosmic Rays

correlation

at the foot of the jet Flat spectrum radio q.

Lac (Marscher et al,

Gamma Ray Bursts

Unvoluntary Pioneer - Vela

controling nuclear tests (USA/Soviet Union)

detection of Gamma Ray Bursts

Gamma Ray Burst – time profile

GRB progenitors

duration > 2 s typically ~ 40 s duration < 2 s ~ms - s

Prompt GRB ν Spectrum

( )

( )

ε ε ε ε α β β α F A z t F z E

∝ = = + = + = , , , 1 1

ν

A

b ν

ε

s ν

ε α β

GRB080319B

IceCube-9: ~0.1 event IceCube-80: ~1 event

z = 0.94 t90 = 60s Γ= 285 Fγ = 5.72e-4 erg/cm2 αγ = 0.82 βγ= 3.87 εγ

Towards the next generation

for the highest energies

Hawk,...;Auger South & north, ... create a complete view of the non-thermal Universe

High-energy neutrinos

µquasars, pulsars, ...

magnitude in the past 7 years

explore optically thin & thick sources