carlos de los heros division of high energy physics uppsala university partikeldagarna
DESCRIPTION
STATUS OF AMANDA AND ICECUBE. Carlos de los Heros Division of High Energy Physics Uppsala University Partikeldagarna Karlstad, March 31st-April 1st 2004. The AMANDA/ICECUBE Collaborations. Bartol Research Institute UC Berkeley UC Irvine Pennsylvania State UW Madison - PowerPoint PPT PresentationTRANSCRIPT
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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uryNumber of institutions
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
AM
AN
DA
(n
um
be
r o
f m
uo
ns)
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