Neutrino Astrophysics - DESYkolanosk/astro0910/skripte/astro05_2… · 50 Mpc. neutrinos....
Transcript of Neutrino Astrophysics - DESYkolanosk/astro0910/skripte/astro05_2… · 50 Mpc. neutrinos....
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 1
Neutrino Astrophysics
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Ring Imaging in Water Tanks
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Energiespektrum
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p beyond ankle
Greisen-Zatsepin-Kuzmin Cut-Off:Energy loss in cosmic microwave
background (CMB)p(100 EeV) + (CMB) p + , n +
p(100 EeV)p
p below ankle isotropized in B-fields
E
eV102010191018
E3
FE
cut-off
reprocessed p
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 6
Neutrino vs. HE gamma and proton astronomy
High energy protons 50 Mpc
neutrinos
Astrophysicalsource
Low energy protons deflected
High energy gammas 10 Mpc
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 7
Neutrino-Productionby proton interaction with matter or with a photon field
0
....
pnp
e
pp
e
or
i.e. e :
:
~ 1:2:0
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 8
Vorhersagen für -Spektren
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 9
Muons cannot travel in rock or water more than
50 km at
any energy
go deep, look only to upward muons or horizontal muons.
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 10
N-Wirkungsquerschnitte
N X
Neutrinos are detected indirectly, following an interaction on a target nucleus N:
1 TeV 1 PeVN0.4
E E 5TeV
E E 5TeV
Gandhi
10-33 cm2
10-35 cm2
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 11
Myon-Reichweite
TeV
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 12
Muon Range
E
(GeV)R
ange
(m)
Muons have long tracks in water
2
24
dE a b Edx
GeVcma 0.2g
cmb 4
1R ln a bEb
10g
R E 300GeV 1 km
Gaisser1 TeV 1 PeV
2·103
2·104
In w
ater
Due to the long muon range the target volume is much bigger than the detector instrumented volume
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 13
-Winkel
1.5
E TeV
X
N
At >TeV energies the muon and the neutrino are co-linear
Reconstruction of the
trajectory allows the identification of the
direction
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Myonspur im Eis/Wasser
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+ N + X high energy
above C-threshold in ice
AMANDA / IceCube
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 16
Amanda
Baikal
Super-K
AntaresNestor
Km3: IceCube
Km3: Nemo
Neutrino Telescopes in Water and Ice
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 17
HE -
astronomy
Point sources
Dark Matter & Exotics
Magneticmonopoles
Atm. neutrinos(charm, oscill.)
GRB coincidencesDiffuse Flux
Q-balls, nuclearites
Neutralinos(WIMPs)
Charged CR(chem. compos)
MeV -
astrophysics(Supernova bursts)
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 18
2000 dataPRELIMINARY
First spectrum > 3 TeV:
- up to 100 TeV
- matches lower-energy Frejus data
2000 data
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AMANDA skyplot 2000-2003
3329 events
1ES 1959+650, an Active Galactic Nucleus already known as a potential hadron
accelerator:
neutrinos are likely to be emitted
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2000-2004: 4282 events 1001 days live-time
On-Source
Off- Source
= 2.25°-3.75°
Search for an excess of events• from candidate sources• anywhere on the northern sky
Atm-
Background from ‘off-source’ data
No detection yet, flux upper limits set
preliminary
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Candidate sourcesSource Events observed/
background(5 years)
Events observed/ background
(4 years)
Flux upper limit Sys. unc. 15% sig, 8% bg
90% (E
>10 GeV) [10-8cm-2s-1](5 years)
Markarian 421 6 / 7.37 6 / 5.58 0.43Markarian 501 8 / 6.39 5 / 4.96 0.851ES1959+650 5 / 4.77 5 / 3.71 0.78M87 6 / 6.08 4 / 4.90 0.503C273 8 / 4.72 0.99SS433 4 / 6.14 2 / 4.50 0.27CI Cam 9 / 6.72 5 / 5.11 1.04Cygnus X-1 8 / 7.01 4 / 5.21 0.76Cygnus X-3 7 / 6.48 6 / 5.04 0.67Crab Nebula 10 / 6.74 10 / 5.36 1.01
No significant excess, no indication for a neutrino sourceNo new events seen from the direction of Crab Nebula
Flux upper limits improved preliminary
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 22
Year2000 2001 2002 2003
May June July
Flux ofTeV photons(arb. units)
0
1
2
3
Gamma-rays
detected
by
a TeV
gamma
telescope
Arrival time of the
neutrinos from
the
direction
of
ES1959+650 detected
by AMANDA
Did we see already
the first signal ?
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Experiment
Atmos.
MCeven
ts/b
in
AMANDA B10,1997 data
AMANDA II (with 3 years data):~ 10 X higher Sensitivity
E2 < 0.8 10-6 GeV-1 cm-2 s-1 sr-1
1. Diffuse flux of muon neutrinos (energy < 1 PeV)
„AGN“ with 10-5 E-2 GeV-1 cm-2 s-1 sr-1
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cascademyon
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Cascades inside detector
Sensitive to all 3 flavorsSensitive to all 3 flavors
CC electron and tau neutrino interaction:
(e,,) + N (e, ) + X
NC neutrino interaction: x + N x + X
Color displays: LE Primary Channels
2370 132501 232631 402762 382893 343023 283154 213285 193415 113546 93677 63807 93938 44069 54199 24330 2
Size displays: ADC Size scaling: Lin
<4 <9 <13 <17 <22 <26 <31 <35
<40 <44 <49 <53 <58 <62 <67 <71
No external geometry file is opened.Detector: amanda-b-10, 19 strings, 680 modulesData file: he_deff.f2kDisplaying data event 1425281 from run 336Recorded yr/dy: 2000/170 59857.5405130 seconds past midnight.Before cuts: 264 hits, 264 OMsAfter cuts : 264 hits, 264 OMs
E2 all
< 0.6 10-6 GeV-1 cm-2 s-1 sr-1
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Experimental all-flavor limits
1: Amanda-B10, muons 3: Baikal all flavor 5: Amanda cascades2: Amanda-II, muons 4: Amanda all flavor UHE Expected: 6: Amanda-II, 4 years 7: IceCube 3 years
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AmandaAt South Pole the Sun sinks maximally 23° below horizon. Thereforeonly Amanda-II with its dramatically improved reconstruction capabilitiesfor horizontial tracks (compared to Amanda-B10) can be used forsolar WIMP search.
Indirect Search for WIMPs
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Limits on the muon flux from neutralino annihilations at the center of the Earth with AMANDA
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Relativistic Magnetic Monopoles
10-16
10-15
10-14
10-18
10-17
= v/c1.000.750.50
uppe
rlim
it(c
m-2
s-1
sr-1
)
Cherenkov-Light n2·(g/e)2
n = 1.33
(g/e) = 137/ 2
8300
KGF
Soudan
MACRO
Orito
Baikal
Amanda
IceCube
electrons
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- 80 Strings- 4800 PMTs Instrumented
Volume: 1 km3
Installation:2005-2010
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• Bartol Research Inst., Delaware• (Univ. of Alabama) • Pennsylvania State University• UC Berkeley• UC Irvine *• Clark-Atlanta University• Univ. of Maryland• IAS, Princeton• University of Wisconsin-Madison• University of Wisconsin-RiverFalls• LBNL, Berkeley• University of Kansas• Southern Univ., Baton Rouge
• Bartol Research Inst., Delaware• (Univ. of Alabama) • Pennsylvania State University• UC Berkeley• UC Irvine *• Clark-Atlanta University• Univ. of Maryland• IAS, Princeton• University of Wisconsin-Madison• University of Wisconsin-RiverFalls• LBNL, Berkeley• University of Kansas• Southern Univ., Baton Rouge
Universität Mainz • Humboldt Univ., Berlin *• DESY, Zeuthen• Universität Dortmund• Universität Wuppertal
Universität Mainz • Humboldt Univ., Berlin *• DESY, Zeuthen• Universität Dortmund• Universität Wuppertal
• Uppsala University• Stockholm University
• Uppsala University• Stockholm University
Chiba University
Chiba University
• Universite Libre de Bruxelles• Vrije Universiteit Brussel• Université de Mons-Hainaut• Universiteit Gent *
• Universite Libre de Bruxelles• Vrije Universiteit Brussel• Université de Mons-Hainaut• Universiteit Gent *
Univ. of Canterbury, ChristchurchUniv. of Canterbury, Christchurch
• Imperial Coll, London• University of Oxford
• Imperial Coll, London• University of Oxford
University UtrechtUniversity Utrecht
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6 Amanda modules
Super-Kamiokande(Japan)
AMANDA-II
IceCube
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Cherenkov tank arrays: IceTop
Southpole, Antarctica1 km²
80 Stations x 2 x 3.14 m² = 503 m²
E > 0.3 PeV
slightly larger than K-GRANDE
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IceCube: DOM
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10” PMTHamatsu- 70
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cos
Aef
f/ km
2
Effective Area of IceCube
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The first muon – IceTop shower coincident event
January 23First runs with the four IceTop stations (8 tanks) taken
January 29 1:31 First IceCube string deployed
February 9First shower/muon coincidence events found
6
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Under construction:Telescopes inMediterranean
4100m
2400m
3400mANTARESNEMO NESTOR
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The ANTARES detector• string based detector • 12 strings• 900 PMTs• 2400 m deep
~70 m
350 m
100 m
14.5 m
Submarine links
JunctionBox
40 km toshore
Anchor/line socket
a storey
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nsec
attenuation length in ice 1-4 km !!10 cm
5-10 m
P
t
50 s
Above
10-100 PeV:
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Sehen und Hören: Nutze alle Sinne Teilchen hören ?!!
Thermoakustisches Modell: Ultrahochenergetische Kaskade
Lokale Erwärmung Expansion
Schallwelle
Akkustische Sensoren
180 MeV Protonen TSL, Uppsala
Akustische Sensoren für den IceCube Detektor
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RICE Radio Ice Cherenkov Experiment
Firn ice (down to 120 m depth)
UHE NEUTRINO
DIRECTION
300 METER DEPTH
E 2 · dN/dE< 10-4 GeV · cm-2 · s-1 · sr-1
20 transmitter + receiver
at 100 PeV
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500 km
60 °
E > 1019 GeV
Area up to106 km2
Masse Up to 10Tera-Tons
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H.Kolanoski -- Astroteilchenphysik -- WS09/10 -- 5.5 HE-Neutrinos 46-90 0-45 9045
10-15
10-14
cm-2 s-1
SS-433
Mk-501 /
~ 1
10-17
10-16
2001
2007
2003
2012
Achieved andexpected sensitivitiesto steady point sources
GX339-4
Super-K,MACRO
AntaresBaikal, Nestor
IceCubeKM3 in Mediterr.
AMANDA
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AMANDA skyplot 2000-2003
3329 events
1ES 1959+650, an Active Galactic Nucleus already known as a potential hadron
accelerator:
neutrinos are likely to be emitted