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