Neutrino Point Sources (Looking for) (with Underground Detectors) THE HIGTE ST ENERGY COSMIC RAYS...
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Transcript of Neutrino Point Sources (Looking for) (with Underground Detectors) THE HIGTE ST ENERGY COSMIC RAYS...
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)
22.05.2004 S. Mikheyev 3
M.Koshiba EPS2003
22.05.2004 S. Mikheyev 4
origin and acceleration of cosmic rays
understand cosmic cataclysms
find new kind of objects?
Physical motivationPhysical motivation
22.05.2004 S. Mikheyev 5
Experiment KGFExperiment KGF
22.05.2004 S. Mikheyev 6
Experiment KGFExperiment KGF
22.05.2004 S. Mikheyev 7
OutlineOutline
Neutrino production
Perspectives
Search for clusters
Point-like sources (known position)
Detector response function
Detection of neutrino-induced muons
22.05.2004 S. Mikheyev 8
Opaque matter
Neutrino productionNeutrino production
Proton Accelerator
Target (p,)
p
p p, ± ±
e±
e
0
2
22.05.2004 S. Mikheyev 9
TeV - sourcesTeV - sourcesM. Mori
Raporter talkICRC 2003
22.05.2004 S. Mikheyev 10
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
22.05.2004 S. Mikheyev 11
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
22.05.2004 S. Mikheyev 12
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
22.05.2004 S. Mikheyev 13
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
22.05.2004 S. Mikheyev 14
Response FunctionResponse Function
Response curves for
various for E- spectra
Y(E,E ) E th
22.05.2004 S. Mikheyev 15
Atmospheric NeutrinosAtmospheric Neutrinos
22.05.2004 S. Mikheyev 16
Search windowSearch window
muon – neutrino misalignment
multiple muon scattering in rock
detector properties (possible to measure)
d2
dE dcos
-2/42e dP()d = 22
22.05.2004 S. Mikheyev 17
Moon Shadow: BaksanMoon Shadow: Baksan
22.05.2004 S. Mikheyev 18
MA
CR
O C
olla
bora
tion a
stro
-ph/0
302
586
Moon Shadow: MACROMoon Shadow: MACRO
22.05.2004 S. Mikheyev 19
MA
CR
O C
olla
bora
tion a
stro
-ph/0
302
586
Moon Shadow: MACROMoon Shadow: MACRO
22.05.2004 S. Mikheyev 20
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.)
22.05.2004 S. Mikheyev 25
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.
22.05.2004 S. Mikheyev 26
Cluster search: MACROCluster search: MACRO
22.05.2004 S. Mikheyev 27
Cluster search: Super-KamiokandeCluster search: Super-Kamiokande
22.05.2004 S. Mikheyev 28
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
22.05.2004 S. Mikheyev 29
Fraction of time sky below horizon
Point sources:
south detector + north detector
PerspectivesPerspectives
22.05.2004 S. Mikheyev 30
-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, ...
22.05.2004 S. Mikheyev 31