Neutrino Point Sources

(Looking for)

(with Underground Detectors)

THE HIGTEST ENERGY COSMIC RAYS AND

THEIR SOURCES: Moscow

May 21-23, 2004

S.P. Mikheyev

INR RAS

22.05.2004 S. Mikheyev 2

e

Y.Koshio NOON2004

22385 solar events

(14.5 events/day)

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M.Koshiba EPS2003

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origin and acceleration of cosmic rays

understand cosmic cataclysms

find new kind of objects?

Physical motivationPhysical motivation

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Experiment KGFExperiment KGF

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Experiment KGFExperiment KGF

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OutlineOutline

Neutrino production

Perspectives

Search for clusters

Point-like sources (known position)

Detector response function

Detection of neutrino-induced muons

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Opaque matter

Neutrino productionNeutrino production

Proton Accelerator

Target (p,)

p

p p, ± ±

e±

e

0

2

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TeV - sourcesTeV - sourcesM. Mori

Raporter talkICRC 2003

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Supernova remnant Microquasar(SS433 etc.)

Active Galaxy(Markarian 421 etc)

Crab nebula

Black hole with108 x mass of sun

Black hole with mass of sun

1 LJ 106 LJ

extra-galacticgalactic

Neutrino source candidatesNeutrino source candidates

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Neutrino energeticsNeutrino energetics

Neutrino spectra:Neutrino spectra:

Neutrino luminosity yielding 10 events per 10 yielding 10 events per 10 years in 10years in 1033 m m22:Neutrino luminosity yielding 10 events per 10 yielding 10 events per 10 years in 10years in 1033 m m22:

distancedistance LumLum > > exampleexample

4000 Mpc 1049 erg/s agn

100 Mpc 51045 erg/s Markarians 8 Kpc 41037 erg/s pulsars, micro- quasar…

4000 Mpc 1057 erg/100s grb

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Neutrino DetectionNeutrino Detection

+ N - + X

Y(E,E ) = NA E th

E th

E

dE ’ dE ’

d(E,E ) E ’ Reff(E,E ) E ’ E th

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Muon YieldMuon Yield

101 103 105 107

10-11

10-9

10-7

10-5

10-3

Neutrino energy (GeV)

Pro

babili

ty

E =

100 G

eV

th

E =

1 G

eV

th

= 90º

= 150º

=

180º

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Response FunctionResponse Function

Response curves for

various for E- spectra

Y(E,E ) E th

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Atmospheric NeutrinosAtmospheric Neutrinos

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Search windowSearch window

muon – neutrino misalignment

multiple muon scattering in rock

detector properties (possible to measure)

d2

dE dcos

-2/42e dP()d = 22

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Moon Shadow: BaksanMoon Shadow: Baksan

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MA

CR

O C

olla

bora

tion a

stro

-ph/0

302

586

Moon Shadow: MACROMoon Shadow: MACRO

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MA

CR

O C

olla

bora

tion a

stro

-ph/0

302

586

Moon Shadow: MACROMoon Shadow: MACRO

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Super-KamiokandeSuper-Kamiokande

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SKY: Baksan SKY: Baksan

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SKY: MACRO SKY: MACRO

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SKY: Super-Kamiokande SKY: Super-Kamiokande

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Neutrino induced -flux limit (90% C.L.)Neutrino induced -flux limit (90% C.L.)

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Preliminary limits (in units of 10-15 muons cm-2 s-1): Cas A: 0.6 Mk421: 1.4 Mk501: 0.8 Crab: 6.8 SS433: 10.5

1328 events

SKY: AMANDA SKY: AMANDA

Equatorial coordinates: declination vs. right ascension.

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Cluster search: MACROCluster search: MACRO

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Cluster search: Super-KamiokandeCluster search: Super-Kamiokande

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Expected sensitivity AMANDA 97-02 data

4 years Super-Kamiokande

8 ye

ars

MACRO

170 days AMANDA-B10

-90 0-45 9045

10-15

10-14

cm-2 s

-1

declination (degrees)

southern sky

northern sky

SS-433

Mk-421 / ~ 1

25 years Baksan

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Fraction of time sky below horizon

Point sources:

south detector + north detector

PerspectivesPerspectives

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-90 0-45 9045

10-15

10-14

cm-2 s-1

SS-433

Mk-501

/ ~ 1

10-17

10-16

2001

2007

2003

2012

Expected sensitivitiesto steady point sources

GX339-4

„typical“ predictions for AGN, SNR, ... „typical“ predictions for AGN, SNR, ...

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