Recent Results
Lutz KöpkeUniversity of Mainz, Germany
July 31, 2003
http://amanda.uci.edu
Upgra
de an
d
IceCub
e
Neutri
nos
Cosm
ic ra
ysContributed 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
Electromagnetic and hadronic cascades
~ 5 m
Detection of e , ,
O(km) long muon tracks
direction determination by Cherenkov light timing
15 m
e:: =1:2:0 at source e:: =1:1:1 at Earth ! noscillatio
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):
South Pole (ice)AMANDA, ICECUBE
dots: distribution of gamma ray bursts (GRBs)
galactic center in middle
E < 100 TeV
Mediterranean (ocean) Antares, Nestor, 1 km3 ...
Northern hemisphere detectors
Baikal NT200
1100 m deepdata taking since 1998new: 3 distant strings
Antares Nestor
March 17, 20032 strings connected2400 m deepcompletion: start 2006
March 29, 20031 of 12 floors deployed4000 m deepcompletion: 2006
Optical module (677)
1996-2000
Amundsen-Scott Station South Pole
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-
Spectral index compatible with directmeasurements, error competivie
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
(co
rrel
ate
to #
muo
ns)
SPASE-2 (correlated to #electrons)
iron
proton
log(E/G
eV)
Composition change around „knee“
1015 eV 1016 eV
talk HE 1.1-25
A=30
A=6
(1998 data)publication in preparation
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 optical modules hit as energy variable ...
muon neutrinos (1997 B10-data)accepted by PRL
cuts determined by MC – blind analyses !
talk HE 2.3-4poster HE
AMANDA II (with 3 years data):~ 10 X higher Sensitivity
Diffuse flux muon neutrinos
3·103 – 106 GeV:
E2 (E) < 8 10-7
GeV-1 cm-2 s-1 sr-1
Note that limits depend on assumed energy spectrum ...
2.5 ·106 – 5.6 ·108 GeV:
E2 (E) < 7.2 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
prel.
poster 1-P-257poster 1-P-256
Diffuse limit cascades
effective volume
80 TeV – 7 PeV after acceptance expect:
e : : 1 : 0.67 : 0.41 events
2 candidate events total observed
90% CL upper limit:
E2all (E) < 9·10 - 7 GeV cm-2s-1sr-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
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
sky subdivided into 300 bins (~7°x7°)
below horizon:mostly fake events
talk HE 2.3-5
above horizon: mostly atmospheric ‘s
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 2.3•10-8 cm-2s-1 @90% ¶ published Ap. J, 582 (2003)
PRELIMINARY
upper limits @ 90% CL in units of 10-8cm-2s-1
talk HE 2.3-5
-90 0-45 9045
10-15
10-14
mu o
n s/c
m2 s
1
10-17
10-16
published data
preliminary 2000 data
1 km3 detectors, 3 years1 km1 km33
Expected sourcesensitivity
GX339-4
SS-433
MACRO 8 years
N
AMANDA+16 (2007)
Antares(2007+)
AMANDA137 days
declination (degrees)
S
Mark. 501
Crab
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°10 min
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
..no extraterrestrial neutrinos found yet ...but:
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
Importance of all flavor detection
Extended source with e:: =1:2:0 production (e.g. decay) :E.g.: 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 !
Theoretical bounds and future
atmospheric
W&B W&B
MPRMPR
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
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 , 3.8 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