Carlos de los HerosDivision of High Energy Physics

Uppsala University

PartikeldagarnaKarlstad, March 31st-April 1st 2004

STATUS OF AMANDAAMANDA AND ICECUBEICECUBE

The AMANDA/ICECUBE CollaborationsThe AMANDA/ICECUBE Collaborations

Bartol Research InstituteUC Berkeley

UC IrvinePennsylvania State

UW MadisonUW River FallsLBNL Berkeley

U. Simón Bolivar, CaracasVUB-IIHE, Brussel

ULB-IIHE, BruxellesUniversité de Mons-Hainaut

Imperial College, LondonDESY, Zeuthen

Mainz Universität

Wuppertal UniversitätStockholm Universitet

Uppsala UniversitetKalmar UniversitetSouth Pole Station

+ University of Maryland, US Clark-Atlanta University, US Southern University, US IAS, Princeton, US University of Alabama, US University of Oxford, UK University of Utrecht, NL Chiba University, Japan U. of Canterbury, Christchutch, NZ

as ICECUBE members

150 members

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THE SWEDISH GROUPS

• Stockholm: Finance– P. O. Hulth SU– K. Hultqvist SU/VR– C. Walck SU/VR– S. Hundertmark SU– C. Bohm SU

Grad students:– Y. Minaeva– T. Burgess– C. Wiedemann– P. Ekström

Technicians:– L. Thollander (100%)

Grants:– Travel VR 650kSEK 02-04

• Uppsala: Finance– O. Botner UU/VR– A. Hallgren UU/VR– C. de los Heros VR– A. Bouchta VR

Grad students:– A. Davour– J. Lundberg– A. Pohl

Technicians:– B. Hagberg (35%)

Grants:– Travel VR 325kSEK 02-04– C.d.l.H. VR 135kSEK/yr (02-

05)

36 MSEK (VR+Wallenberg) for IceCube instrumentation (managed by SU+UU)

NEUTRINO ASTRONOMYNEUTRINO ASTRONOMY

• Cosmic rays @ >>TeV exist

acceleration sites must sit somewhere

• SNe remnants• Active Galactic Nuclei• Gamma Ray Burst• Exotics (decays of topological defects...)

proton acceleration

Neutrinos : not absorbed, not deflected:

difficult to detect

Protons : deflected in magnetic fields, GZK -rays : propagate straight, however:

– reprocessed in sources– absorbed in IR (100 TeV) and 3K (10 PeV)

?

explained explained by SNby SN

unexplainedunexplained

Guaranteed sources:

• atmospheric neutrinos (from & K mesons decay)

• galactic plane: – CR interacting with ISM, concentrated on the disk

• cosmological neutrinos:– extragalactic origin of UHECR: p + n + (p 0)

THE AMANDA DETECTORTHE AMANDA DETECTOR

19 strings677 PMTstrigger rate: 80 Hznoise rate: 1 kHz

O(km) long muon tracks

15 m5.0

)TeV/(5.1

E

• up/down 10-5 background froma) misreconstructed atmospheric muonsb) coincident muons

• muon range scales with log(E)• CC/E cte up to 10 TeV

determination of the trajectory by Cherenkov light timing

constant

detectability

for E-2 source

geographic South Pole

AMANDA

THE SITETHE SITE

2km deep

DAILY WORK COMMUTE. NO TRAFFIC JAMS

drill studiesatmospheric muonsin-situ light sources

• Bubbles vs. depth• Dust layers• Drill-hole bubbles

DETECTOR MEDIUM: ICE PROPERTIESDETECTOR MEDIUM: ICE PROPERTIES

ice optical parameters:

abs ~ 110 m @ 400 nmscatt ~ 20 m @ 400 nm

Electromagnetic and hadronic cascades

~ 5 m

• : oscillation + regeneration at PeV important

• no EM / hadronic cascade differentiation (even if slightly different shape and lowerlight output for hadronic cascades)

ALL FLAVOUR DETECTIONALL FLAVOUR DETECTION

DETECTOR CAPABILITIESDETECTOR CAPABILITIES

muons:directional error: 2.0° - 2.5°energy resolution: 0.3 – 0.4coverage: 2

primary cosmic rays: (+ SPASE2)energy resolution: 0.07 – 0.10

„cascades“: (e±, , neutral current)zenith error: 30° - 40° energy resolution: 0.1 – 0.2

(5TeV < E < 5 PeV)coverage: 4

3 cm2

5m2

effective area (schematic):

E

-interaction in earth, detector response

100 GeV 100 TeV 100 PeV

AMANDA PHYSICS TOPICSAMANDA PHYSICS TOPICS

Cosmology / Particle Physics / Astrophysics

• Dark matter / exotic particles: neutralinos, magnetic monopoles, extra dim.

solar WIMP’s signature: Excess from the Sun direction

heavy and slow particles

• primary CR spectrum / charm production

atmospheric muons / neutrinos (also calibration of Amanda)

CR composition (with surface detector SPASE-2)

• cosmogenic flux: top-down scenario from topological decays

extra-terrestrial diffuse flux

• CR origin / acceleration sites (AGN, GRBs)

extra-terrestrial flux (diffuse / punctual / transient)

• SN monitor of the milky way

low energy EM cascades (global noise increase throughout Amanda)

SWEDISH ACTIVITIESSWEDISH ACTIVITIES• Physics analyses:

– Dark matter searches (WIMP, K-K, Simpzillas). AD, YM, CPH, TB, PE– UHE neutrinos. SH, CW– Point source searches. JL– Monopole searches. AP

• Software– AMANDA simulation. SH, CW– IceCube simulation/reconstruction. SH, AB, TB, CW

• Management– IceCube collaboration board. PO, OB– PO Icecube spokesperson– KH IceCube simulation coordinator– AH AMANDA analysis coordinator– CdlH AMANDA software coordinator

• Hardware– AMANDA trigger (AH, Pawel Marcinewski)– AMANDA amplifiers (PO, LT)

TeV-PeV DIFFUSE FLUXTeV-PeV DIFFUSE FLUX

• data sample ’97

• hit channels multiplicity as energy indicator

• cuts optimized for best sensitivity

atm.

Exp.

„AGN“ with 10-5 E-2

GeV-1 cm-2 s-1 sr-1

cut

E2 (E) < 8.4 10-7 GeV cm-2 s-1 sr-1

PRL 90 (2003), 251101

NO EXCESS OBSERVED

assuming a E-2 flux (6 TeV < E < 1 PeV) :

DIFFUSE FLUX (cascades)DIFFUSE FLUX (cascades)

PRELIMINARY

no earth propagation effects

e

•2000 data sample, 197 days lifetime

• sim. BG:atm. muons atm. neutrinos

DIFFUSE FLUX (cascades)DIFFUSE FLUX (cascades)PRELIMINARY

MPR

SDSSUHE analysis

• sensitivity to all three flavors

• some AGN core models discarded

• assuming a E-2 flux (50 TeV < E < 5 PeV):

E2all (E) < 8.6·10 – 7 GeV cm-2 s-1 sr-1

( e:: =1:1:1)

paper internally refereed

E2all (E) < 9.8·10– 6 GeV cm-2 s-1 sr-1

( e:: =1:1:1)

E2e(E) < 6.5·10– 6 GeV cm-2 s-1 sr-1

Phys. Rev. D67, 2003

From data sample ’97, 130 days lifetime (5 TeV < E < 300 TeV):

UHE UHE neutrinosneutrinos

Simulated UHE event

R > 10 km

10-6 E-2

Neural Net Parameter „NN2“ for neutrino vs.atm muon separation

downward muons and muons close to horizon

data sample ’97 (131 days acquisition)

uncertainties on • neutrino cross section

• muon propagation• primary flux normalization& elemental composition

NO EXCESS OBSERVED

E2 all (E) < 1.510-6 GeV cm-2 s-1 sr-1

( e:: =1:1:1)

assuming a E-2 flux (1 PeV < E < 3 EeV) :

paper in progress

PRELIMINARYExperimentCORSIKA MC

POINT SOURCE SEARCHESPOINT SOURCE SEARCHES

•cuts optimized in each declination band•sensitivity flat up to horizon, (in average 4 times better than 1997 analysis,

declination averaged sensitivity (integrated above 10 GeV) :

Search for an event excess in the northern sky

699 neutrino events observed from below the horizon (2000 data)<10% non-neutrino background for >5°

no clustering observed: no evidence for point sources

grid: sky subdivided into 300 bins ~7°x7°

Astrophys. J. 583, 2003 )

lim 2.3·10-8 cm-2s-1

Phys. Rev. Lett. 92, 2004

above horizon:mostly fake events

below horizon: mostly atmospheric ‘s(this means northern sky)

upper limits in units of 10-7cm-2s-1

integrated above E=10 GeV, for an assumed E-2 spectral shape

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

FLUX LIMITS ON SELECTED SOURCESFLUX LIMITS ON SELECTED SOURCES

upper limits in units of 10-8cm-2s-1 for an assumed E-2 spectral shape integrated above E=10 GeV

Sensitivity at the level of TeV -ray flux (’97 active state)

AMANDA-II achieved the sensitivity to search for neutrinos from TeV -ray sources (~1)

SEARCH FOR SEARCH FOR CORRELATED WITH CORRELATED WITH GRBsGRBs

Year #GRB bkg observed

1997 78 0.06 0

1998 94 0.20 0

1999 96 0.20 0

2000 44 0.83 0

Total 312 1.29 0

• analysis is blind: finalized off-source (±5 min) with MC signal

• <20° + other event quality parameters

• BG stability required within ±1 hour from burst

Low background due to space and time coincidence

PRELIMINARY

effective -area 50000 m2

4.8 x 10-8 GeV s-1 cm-2 sr-1

NO EXCESS OBSERVED

assuming Waxmann-Bahcall spectrum (EB at 100 TeV and = 300) :

10 min

Best sensitivity of existing indirect searches

WIMPS FROM THE SUNWIMPS FROM THE SUN

Exclusion sensitivity from analyzing the off-source bins

Sensitivity on the muon flux coming from neutralino annihilations in the center of the Sun:

• (soft channel)• (hard channel)

analysis possible thanks to improved reconstruction capability for horizontal tracks, compared to Amanda B-10

HZ,W,,ll,qq -xx

bbxx -WWxx

ATMOSPHERIC NEUTRINOS WITH AMANDA

• Neural network energy reconstruction

• regularized unfolding spectrum up to 100 TeV

• results compatible with Frejus data

PRELIMINARY

Possible to use the energy spectrum to study excess due to

cosmic ‘s

Atmospheric muons and neutrinos: AMANDA‘s test beams

AMANDA Publications/yrAMANDA Publications/yr

0

2

4

6

8

10

12

14

16

18

20

1993

1995

1997

1999

2001

2003

Conference

Refereed

ICECUBEICECUBE

ICETOP: COINCIDENT EVENTSICETOP: COINCIDENT EVENTS

• Two functions– veto and calibration– cosmic-ray physics

• Energy range:– ~3 x 1014 -- 1018 eV– few to thousands of muons per event

• Large solid angle– One IceTop station per hole– ~ 0.5 sr for C-R physics with “contained”

trajectories– Larger aperture as veto

60 optical sensors

Main Cable

SensorBase with HV generatorElectrical

feedthrough for power + data

Glass pressure sphere. Rated to 10000 psi. Outer diameter: 13"

Photomultiplier

Gel

String

ICECUBE STRING AND DOM

HV Base

Flasher Board

Main Board

10” PMT

13” Glass sphere

OM spacing 17m

– 3 Production and testing Facilities• UW-Madison (PSL)• DESY (Germany)• Stockholm/Uppsala (Sweden)

PRODUCTION SCHEDULEPRODUCTION SCHEDULE

Project Year 3 4 5 6 7 8 TotalDeployment Year 04/05 05/06 06/07 07/08 08/09 09/10Drill/deploy strings 4 12 16 18 18 12 80Strings in ice 4 16 32 50 68 80 80DOMs needed 400 834 1064 1242 1182 778 5500Calendar year of prod. 2004 2005 2006 2007 2008 2009Cable systems to build 5 14 24 24 15 0 82Total DOMs: build and test 400 834 1064 0 5500DOMs: DESY 60 210 280 0 1330DOMs: Sweden 50 140 180 0 880DOMs: PSL 290 484 604 0 3290

3202

1912

780510

We start now!

TRACK RECONSTRUCTION IN A LOW TRACK RECONSTRUCTION IN A LOW NOISE ENVIRONMENTNOISE ENVIRONMENT

• 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/4µsec

Important Detector Parameters

(astro/ph:0305196 ):• Angular resolution: 0.7 degrees• Effective muon detector area:

1 km (after background

suppression)

AMANDA-II

1 km

10 TeV

Eµ=6 PeV ≈ 1000 hits

ENERGY RECONSTRUCTIONENERGY RECONSTRUCTIONSmall detectors: Muon energy is difficult to measure because of fluctuations in dE/dx IceCube: Integration over large sampling and scattering of light reduces the fluctuations in energy loss. --> Require large dynamic range in amplitude.

Eµ=10 TeV ≈ 90 hits

RECENT RESULTSRECENT RESULTS

• Four Digital Optical Modules (DOM) plus a DOM Hub are collecting IceTop data using test software– Successfully synchronized with GPS time– Data compared with SPASE

• Successfully transferring data from the DOM to DOM Hub to Data Collection program @ PSL– Remotely setting DOM parameters– Recording DOM Monitor, Configuration, and PMT hit data for analysis

by DOM Test software– Involves software developed at LBNL, UW and PSU

OUTLOOKOUTLOOK

•First results from AMANDA-II published

•papers from analysis of 97-2000+ data in progress

•combined analysis ’00-’03 on their way

•Amanda-II detector shows greatly improved capabilities

•digitized readout since 2003: waveform resolution

•ice description mature

•first IceCube strings in 2004/05

PROJECT COSTPROJECT COST

$296MTotal Project Cost

~$30.2MNon-U.S. contribution

$266.7MU.S. contribution

Feb 2004

SPASE/AMANDA: CR composition

SPASE-2

AMANDA

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Iron

log(E/PeV)

Proton

SPASE-2 electronAMANDA B10 muon

SPASE-2 (number of electrons)

composition change around the kneepaper in preparation

Amanda-B10 / Spase-2 calibration: accepted