Recent Results
Lutz KöpkeUniversity of Mainz, Germany
July 31, 2003
http://amanda.uci.edu
Upgrad
e and
IceCub
e
Neutrin
os
Cosmic
rays
Contributed papers to ICRC Response of AMANDA to cosmic ray muons Cosmic ray flux measurement Cosmic ray composition at the knee with SPASE and AMANDA
Atmospheric neutrino and muon spectra Search for diffuse fluxes of extraterrestrial muon neutrinos AMANDA-B10 limit on UHE-Neutrinos Search for high energy neutrinos of all flavours Search for extraterrestrial point sources of neutrinos Search for muons from WIMP annihilation in center of earth Search for high energy neutrinos from GRBs Online search for neutrino bursts from Supernovae
New capabilities of the AMANDA detector The IceCube high energy neutrino telescope IceTop: the surface component of IceCube Simulation of ice Cherenkov detectors for IceTop
+ 3 individual contributionsblack: parallel talk
Physics motivation
origin and acceleration of cosmic rays understand cosmic cataclysms find new kind of objects?
neutrino properties ( , cross sections ..)
dark matter (neutralino annihilation)
• tests of relativitiy ....• search for big bang relics ...• effects of extra dimension etc. ...
Neutrino source candidatesActive Galaxy(optically dense, e.g. FRII)
Black hole with108 x mass of sun
106 LJ
extra-galactic
Supernova remnant Microquasar(SS433 etc.)
Crab nebula
Black hole with mass of sun
1 LJ
galactic
Importance of all flavor detection
Extended source with e:: =1:2:0 production (e.g. decay) :Expect for Maki-Nakagawa-Sakato mixing matrix with 12=30°, 23=45°, 13=0°:
231231026
81NMSU e:: =1:1:1 on earth
O(10) x less background for e – but you don’t profit from long -range Regeneration of - no absorption in earth even at very high energies !
Detection of e , ,
~ 5 m
Electromagnetic and hadronic cascadesO(km) long muon tracks
direction determination by cherenkov light timing
15 m
Detection of muon neutrinos
atmospheric muons
(e)
cosmicradiation
(e)
earth acts as shield
O(PeV): use horizontal eventsO(10 PeV): use events from above
Above O(PeV): significant absorption:
O(10 PeV)
Complementarity (point sources): E < 100 TeV
South Pole (ice)AMANDA, ICECUBE
Mediterranean (ocean) Antares, Nestor, 1 km3 ...
dots: distribution of gamma ray bursts (GRBs)
galactic center in middle
Northern hemisphere detectors
Nestor
March 29, 20031 of 12 floors deployed4000 m deepcompletion: 2006
Antares
March 17, 20032 strings connected2400 m deepcompletion: start 2006
Baikal NT200
1100 m deepdata taking since 1998new: 3 distant strings
Amundsen-Scott Station South Pole
Optical module
1996-2000
AMANDA II Detector
The AMANDA Collaboration
Venezuela (1)
Europe (10+1)
Antarctica
New Zealand
USA (7+3)Japan
Bartol Research InstituteUC BerkeleyUC IivinePennsylvania StateUW MadisonUW River FallsLBL BerkeleyU. Simón Bolivar, CaracasVUB, BrusselULB-IHEE, BruxellesU. de Mons-HainautImperial College, LondonDESY, ZeuthenMainz UniversitätWuppertal UniversitätStockholm UniversitetUppsala UniversitetKalmar UniversitetSouth Pole Station Antarctica
150 members
+ associated institutes e.g. Chiba University
South Pole
AMANDA
The laboratory
The Dome
The new station operating at least until 2035
Two events ...
200 TeV e candidate
Detector capabilities
muons:directional error: 2.0 - 2.5°energy resolution:¶ 0.3 – 0.4coverage: 2
primary cosmic rays: (+ SPASE)energy resolution:¶ 0.07 – 0.10
„cascades“: (e±, , neutral current)zenith error: 30 - 40° energy resolution:¶ 0.1 – 0.2coverage: 4
effective area (schematic):
E
3 cm2
-interaction in earth, cuts
2 -5m2
100 GeV 100 TeV 100 PeV ¶[log10(E/TeV)]
Atmospheric muons in AMANDA-II
PRELIMINARY threshold energy ~ 40 GeV (zenith averaged)
Atmospheric muons and neutrinos: AMANDA‘s test beams
much improved simulation...but data 30% higher than MC ...
normalize to most vertical bin
Systematic errors:
10% scattering ( 20m @ 400nm) absorption (110m @ 400nm) 20% optical module sensitivity 10% refreezing of ice in hole
poster 1-P-265
Cosmic Ray flux measurement
empirical separation of ice and OM sensitivity effects
PRELIMINARY
In some cases ice and OM-sensitivity effect can be circumvented ...
(E)=0E-
Compatible and competitive () with direct measurements
for QGSJET generator:
(H) = 2.70 ± 0.02 0 (H) = 0.106(7) m-2s-1sr-1TeV-1
talk HE2.1-13
cosmic ray composition studies SPASE-2 (electronic component) - AMANDA B10 (muonic component)
AMANDA II
- unique combination!
talk HE 1.1-25
robust evidence for composition change around knee ...
AM
AN
DA
(cor
rela
te to
#m
uons
)
SPASE-2 (correlated to #electrons)
iron
proton
log(E/GeV)
publication in preparation
Composition change around „knee“
1998 data
1015 eV 1016 eV
talk HE 1.1-25
A=30
A=6
confirms trend seen byother experiments ...
blue band: detector and model uncertaintiesred band: uncertainty due to low
energy normalization
Atmospheric 's in AMANDA-II
neural network energy reconstruction regularized unfolding
measured atmospheric neutrino spectrum
1 sigma energy error
spectrum up to 100 TeV compatible with Frejus data
presently no sensitivity to LSND/Nunokawa prediction of dip structures between 0.4-3 TeV
In future, spectrum will be usedto study excess due to cosmic ‘s
PRELIMINARY
talk HE 2.3-6
Excess of cosmic neutrinos? Not yet ...
cascades (2000 data)
„AGN“ with 10-5 E-2
GeV-1 cm-2 s-1 sr-1
.. for now use number of hit channels as energy variable ...
muon neutrinos (1997 B10-data)accepted by PRL
cuts determined by MC – blind analyses !
talk HE 2.3-4poster HE
2.5 ·106 – 5.6 ·108 GeV:E2 (E) < 7.2 10-7
GeV-1 cm-2 s-1 sr-1
3·103 – 106 GeV:E2 (E) < 8 10-7
GeV-1 cm-2 s-1 sr-1
Expected sensitivity 2000 data:~ 3 10-7 GeV-1 cm-2 s-1 sr-1
AMANDA II (with 3 years data):~ 10 X higher Sensitivity
Diffuse flux muon neutrinosNote that limits depend on assumed energy spectrum ...
prel.
poster 1-P-257poster 1-P-256
Diffuse limit cascades Effective volume
80 TeV – 7 PeV For E2(E) =10-6 GeV cm-2s-1sr-1
flux would expect:
9.3 e , 6.2 , 8.0 events
2 candidate events total observed
E2all (E) < 9·10 - 7 GeV cm-2s-1sr-1
90% CL limit, assuming e:: =1:1:1 :
PRELIMINARY
talk HE 2.3-4
Flux results summary (all flavors)assuming e:: =1:1:1 ratio:
2000 analysis will yield comparable result ...
special analysis for resonant
production (6.3 PeV)
multiplicative factor 3 applied for single e , channels …
eWe ee
...can combine analyses!
talk HE 2.3-4
Theoretical bounds and future
atmospheric
W&B
MPR
DUMAND test string
FREJUS
NT-200
MACRO
NT-200+
AMANDA-II
IceCube
AMANDA-97
AMANDA-00
opaque for neutrons
Mannheim, Protheroe and Rachen (2000) – Waxman, Bahcall (1999) derived from known limits on extragalactic protons + -ray flux
neutrons can escape
sky subdivided into 300 bins (~7°x7°)
below horizon:mostly fake events
above horizon: mostly atmospheric ‘s 697 events observed above horizon 3% non-neutrino background for > 5° cuts optimized in each declination band
PRELIMINARY
Point source search in AMANDA IISearch for excess events in sky bins for up-going tracks
talk HE 2.3-5
no clustering observed - no evidence for extraterrestrial neutrinos ...
Sources declination 1997 ¶ 2000 SS433 5.0o - 0.7
M87 12.4o 17.0 1.0
Crab 22.0o 4.2 2.4
Mkn 421 38.2o 11.2 3.5
Mkn 501 39.8o 9.5 1.8
Cyg. X-3 41.0o 4.9 3.5
Cas. A 58.8o 9.8 1.2
Selected point source flux limitssensitivity flat above horizon - 4 times better than B10 ¶!
declination averaged sensitivity:
lim 0.23•10-7 cm-2s-1 @90%
PRELIMINARY
¶ published Ap. J, 582 (2003)
upper limits @ 90% CL in units of 10-8cm-2s-1
talk HE 2.3-5
-90 0-45 9045
10-15
10-14
muo
ns/c
m2 s
1
10-17
10-16
published data
1 km3 detector, 3 years1 km1 km33
Expected sourcesensitivity
MACRO 8 years
N
AMANDA137 days
declination (degrees)
S
AMANDA+16 (2007)
GX339-4Antares
(2007+)
preliminary 2000 dataSS-433
Mark. 501Crab
GRBsearch in AMANDASearch for candiates correlated with GRBs - background established from data
317 BATSE triggers (1997—2000) effective -area 50000 m2
low background due to space- time coincidence
No excess observed! assuming WB spectrum 4 x 10-8GeV/s/cm2/sr
analysis continues with non-triggered BATSE and IPN3 data …
<20°
PRELIMINARY
talk OG 2.4-7
Outlook... did not mention new improved search for WIMPs (HE 3.3-6)... supernova detection (1-P-258) etc.
combined analysis 1997-2003: 8 x more days !
improved selection and analysis methods ...
new transition waveform based readout installed 02/03improved performance in particular at high energies (1-P-264)
first IceCube strings 2004/05 – combined analysis with AMANDA
increasing energy deposition
no indication of clustering also at higher energies !
Is there a signal at higher energies?
Cygnus-X1
Sun
Cassiopeia. A
Approximate AMANDA horizon
90 000 light years
SMC
LMC
Crab Nebula