icecube - astrophysik mit kosmischen neutrinos am südpolkolanosk/talks/dresden06.pdf · 6.juli...
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![Page 1: IceCube - Astrophysik mit kosmischen Neutrinos am Südpolkolanosk/talks/dresden06.pdf · 6.Juli 2006 H.Kolanoski - Seminar TU Dresden 16 E2Φ νμ (E) < 2.6·10 –7 GeV cm-2 s-1](https://reader035.vdocuments.site/reader035/viewer/2022071004/5fc185ada6d5934bef1ecc7d/html5/thumbnails/1.jpg)
6.Juli 2006 H.Kolanoski - Seminar TU Dresden 1
IceCube - Astrophysik mit kosmischen Neutrinos
am Südpol
Hermann Hermann KolanoskiKolanoskiHumboldtHumboldt--UniversitUniversitäätt zuzu BerlinBerlin
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 2
kosmische Neutrinos, die wir kennen:Sonne im Neutrinolicht
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 3
Supernova-Neutrinos
7 Jahre später (Hubble)
Supernova-Alarm auch aus dem Südpoleis
LichtkurveNeutrinos E - t
Supernova SN1987A
kosmische Neutrinos, die wir kennen:
(siehe später)
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 4
Defizit
abwärtsaufwärts
… kosmische Neutrinos, die wir kennen:
Atmosphärische Neutrinos
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 5
Geladene kosmischen Strahlung
PeV ZeVEeV
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 6
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 7
Hillas-DiagrammFragen:
• Wo werden die hohenEnergien erzeugt?
• Wo herrschen die dafürnotwendigen Bedingungen: B·L
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 8
Kosmische Beschleuniger
GRB
Schwarzes LochSupernovarest
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 9
Aktive Galaktische Kerne
The first image is a Hubble Heritage image of M87, whilethe second one is a schematic diagram of an AGN
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 10
/ TeVRadio optical X-ray GeV TeV
IR UV MeV
The electromagneticspectrum of the TeV Gamma-
sources known until now
Synchr. Inv.Compt.
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 11
Warum Neutrinos?
High energy protons 50 Mpc
neutrinos
Astrophysicalsource
Low energy protons deflected
High energy gammas 10 Mpc
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 12
Nachweis hochenergetischer Neutrinos
νN-Wirkungsquerschnitte
Erde als Filter: Methode für νμ und geeignet
νμ (ντ) → μ + X
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AMANDA-IIConstruction: 1995Construction: 1995--2000 2000 -- 19 strings, 677 OMs19 strings, 677 OMs
Prototyp von IceCube (V= 1 km3)V ~ 0.015 km3
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 14
νμ + N → μ + X ⇒ high energy μ above C-threshold in ice
AMANDA / IceCube
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 15
AMANDA-Physik• Atmospheric neutrinos• Point source searches• Gamma-ray bursts• Dark Matter, WIMPs• Galactic plane • Diffuse extra-terrestrial search• Supernovae• Monopoles• Cosmic ray composition• Searches for new physics
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 16
E2Φνμ(E) < 2.6·10–7 GeV cm-2 s-1 sr-1
Includes 33% systematic uncertainty
Limit on diffuse E-2 νμ flux (100-300 TeV):
Atmospheric neutrinos
Measurement extracted Measurement extracted with a with a regularisedregularised
unfolding techniqueunfolding technique
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 17
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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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 18
Year2000 2001 2002 2003
May June July
Flux ofTeV photons(arb. units)
0
1
2
3
νν
Gamma-rays detected by a TeV gamma telescope
Arrival time of the neutrinosfrom the direction ofES1959+650 detected byAMANDA
Did we see already
the first signal ?
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 19
alle 50 Jahre?
SNEWS – SuperNova Early Warning System Reaktionen von MeV-Neutrinos aus einem Supernova-Burstin unserer Galaxis würden die Rauschraten aller Photomultiplier für 5 -10 Sekunden um einige Hertz nach oben treiben.
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Dunkle Materie
sun
⎟
earth
detector
νscatt
capture
annihilation
χ interactions
μχχ υHZ
llqq
→→⎟⎟⎟
⎠
⎞
⎜⎜⎜
⎝
⎛→
±
. . .,,W
0
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 21
Dunkle Materie
Excluded by CDMS
Methode beschrieben in: D. Hubert et al.,ICRC 2005, Pune, astro-ph/0509330Ref. CDMS:
D.S. Akerib et al., Phys. Rev. Lett., 93, 211301 (2004)
ERDE: Sonne:
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 22
RelativisticMagneticMonopoles
10-16
10-15
10-14
10-18
10-17
β = 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
δ electrons
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 23
Cascades inside detectorSensitive to all 3 flavorsSensitive to all 3 flavors
CC electron and tau neutrino interaction: ν(e,τ,) + N → (e, τ) + X
NC neutrino interaction: νx + N → νx + 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 Φall−ν < 0.6 ⋅10-6 GeV-1 cm-2 s-1 sr-1
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 24
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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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 25
Cascade event
Energy = 375 TeV
νe + N --> e- + X
•The length of the actual cascade, ≈ 10 m, is small compared to the spacing of sensors•==> ≈ roughly spherical density distribution of light•1 PeV ≈ 500 m diameter•Local energy deposition = good energy resolution of neutrino energy
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 26
• 80 Strings
• 4800 PMTs
• Instrumented Volume: 1 km3
• Installation: 2005-2011
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 27
• 80 Strings
• 4800 PMTs
• Instrumented Volume: 1 km3
• Installation:2005-2011
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 28
6 Amanda modules
Super-Kamiokande(Japan)
AMANDA-II
IceCube
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 29
Von AMANDA zu IceCube
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 30
The IceCube Collaboration
IceCube and AMANDA collaborations merged, March 2005
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 31
Cherenkov tank arrays: IceTop• Southpole, Antarctica• 1 km²• 80 Stations x 2 x 3.14 m²
= 503 m²• E > 0.3 PeV• slightly larger than K-
GRANDE
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 32
IceCube: DOM
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 33
10” PMTHamatsu-70
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 34
Track Reconstruction in Low Noise Environment
AMANDAIceCube
IceTop
1200 m• Typical event: 30 - 100 PMT fired• Track length: 0.5 - 1.5 km• Flight time: ≈4 µsecs• Accidental noise pulses:
10 p.e. / 5000 PMT / 4 µsec
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 35
Season 2005-06
• Highly successful season!• First string deployed December 25th
• Eighth string deployed January 29th (9 total)
• Dust logger and standard candle• 12 IceTop stations deployed (16 total)• First events already reconstructed
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 36
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 37
Hose reel Drill tower
IceTop tanksHot water generatorThermal power: 5MW
A view from last season
Working time: Nov. - mid-Feb
Plan: deploy 14 strings/season
Completion: 2011
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 38
Hot Water Drilling
IceCube EHWD significant operation – entire drill camp setup, including generators, heater plants, fuel systems, and support workshops. This camp doesn’t move during the season.
2 drill towers connect to central plants and leapfrog over holes.
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 39
Deployment
99% of 604 DOMs survive deployment and freeze-in
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 40
Ice Top
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 41
Dust logger
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 42
Diffusion/Absorption
Diffusion Absorption
Absorptionslänge : ~110 mDiffusionslänge: ~20 m (λ = 400 nm)
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 43
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/muoncoincidence events found
6
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 44
Upgoing neutrino-induced muon in IC-1, number 1
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 45
Upgoing neutrino-induced muon in IC-1, number 2
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 46
Airshower event in IceTop
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 47
ν
μ
Amanda
Baikal
Super-K
AntaresNestor
Km3: IceCube
Km3: Nemo
Neutrino Telescopes in Water and Ice
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 48-90 0-45 9045
10-15
10-14
μ ⋅ cm-2 s-1
SS-433
Mk-501 ν/γ ~ 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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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 49
nsec
attenuation length in ice 1-4 km !!10 cm
5-10 m
P
t
50 μs
Above 10-100 PeV:
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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 50
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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6.Juli 2006 H.Kolanoski - Seminar TU Dresden 51
Sehen und Hören: Nutze alle Sinne Teilchen hören ?!!
Thermoakustisches Modell:Ultrahochenergetische Kaskade
Lokale ErwärmungExpansion
Schallwelle
AkkustischeSensoren
180 MeV Protonen TSL, Uppsala
Akustische Sensoren für den IceCube Detektor
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