IceCube:Exploring the Universe from the South Polewith high energy neutrinosKirill Filimonov for Kurt WoschnaggUniversity of California Berkeley

and the IceCube CollaborationSCAR Open Science Conference - 2010

Victor Hess Nobel 1936Balloon flights1911-1913Equiv. LHC energy1 event km -2 yr -1 Power law over many decadesCosmic rays: a 100 year-old mystery

NeutrinosCosmic ray g-ray Neutrino connection

109PhotonsNeutrinosC.R.1012101510181021NeutrinoCosmic rayEnergy (eV)neutrinos neutral - good not absorbed - good and bad!Neutrinos as Astronomical Messengers

m tracks (nm)Cascades (ne,t CC, ne,m,t NC)Neutrino interaction with matter

Antarctic Ice is the most transparent natural solid knownAverage optical ice parameters:

labs ~ 110 m @ 400 nmlsca ~ 20 m @ 400 nmWhy the South Pole?

Cosmic rays interacting in the atmosphere: high energy muonsUse Earth as a filter to look for neutrinos: throw out down-going tracksProblem: Background rejection

arXiv:0902.0021NeutrinosMuons106All-sky muon flux (IC22, 2008)

Where are we ?South PolerunwayAMANDA-IIAmundsen-Scott South Pole Station

University of AlabamaUniversity of Alaska,AnchorageUniversity of California, BerkeleyUniversity of California, IrvineClark-Atlanta UniversityBartolResearch Institute, University of DelawareGeorgia Institute of TechnologyUniversity of KansasLawrence Berkeley Natl. LaboratoryUniversity of MarylandOhio State UniversityPennsylvania State UniversitySouthern University and A&M CollegeUniversity of Wisconsin, MadisonUniversity of Wisconsin, River FallsRWTH AachenRuhr-Universitt BochumUniversitt BonnDESY, ZeuthenUniversitt DortmundMPIfK HeidelbergHumboldt Universitt, BerlinUniversitt MainzBUGH Wuppertal Stockholms UniversitetUppsala UniversitetVrije Universiteit BrusselUniversit Libre de BruxellesUniversiteit GentUniversit de MonsUniversity of AlbertaChiba UniversityUniversity of CanterburyEPF LausanneOxford UniversityUniversity of the West IndiesThe IceCube Collaboration

AMANDA2450 m1450 m324 mIceTop: Surface Air Shower ArrayDigital Optical ModuleDeep Core:(Low energy extension)IceCube: (Main Instrument)80 Strings / 60 DOMs each1 km3 instrumentedIceCube Detector

Digital Optical Module (DOM) each DOM, independently collects light signals

time stamps them with 2 nanoseconds precision and sends them to an event builder

IceCube Current Status: 79-Strings Taking Data

IceCube Selected Results: IC22, IC40

zenith angle number of PMTIceCube measures the atmospheric neutrino flux predicted:

IceCube 22 string analysis4492 neutrino events at high purity (>95%)

Atmospheric muon neutrino spectrum

Cosmic rays blocked by the moon lead to a point-like deficit in the distribution of down-going muons in the detector.

Moon Shadow

Cosmic rays blocked by the moon lead to a point-like deficit in the distribution of down-going muons in the detector.

Moon Shadow Need high statistics and good angular resolution!

Pointing accuracy is confirmed!Moon Shadow

J. Dumm ICRC 2009J. Aguilar Vulcano 2010Full-sky point source search (IC40)Preliminary results from 375.5 days exposure36,900 events: 14,121 upgoing and 22,779 downgoingMaximum p-value 5.2 x 10-6, seen in 18% of randomized sky mapsNorthern sky: atmospheric neutrino backgroundSouthern sky: atmospheric muon background demand high energy events

Point Source List

Includes preliminary limits on 39 pre-selected point sources, largest p-value 62%compilation J. Dumm/T. MontaruliSensitivity to Neutrino Point Sources

Phys. Rev. Lett. 103, 221102 (2009)Ultra-high energy neutrino search (IC22)Look for neutrinos from entire sky by demanding high energies (~PeV)Reduces data to 1,877 events; max p-value 37.4% not significant

Also search for correlations withAuger, HiRes UHE events within 3 radiusObserve 60 events, 43.7 expectedp-value 0.98%, 2.33 (preliminary)

Diffuse All-Flavor Neutrino Flux Limits

Sensitivity to muon flux from neutralino annihilations in the Sun or the center of the Earth

Indirect Dark Matter Search: the Sun

Indirect Dark Matter Search: the Sun

No observed excess in IC22 (275 days of data)

arXiv0912.5183Indirect Dark Matter Search: Galactic Halo

IceCube construction is nearly complete79 of a planned 86 strings now operatingIceCube is detecting neutrinos: ~ 20 000 neutrinos already observed in two seasons of partially built detector (consistent with expected rate of atmospheric neutrinos) Results from 22-string and 40-string configurations consistent with atmospheric flux, but several interestingly low p-valuesRich physics is aheadcosmic ray (CR) spectrum, CR composition CR anisotropies atmospheric neutrinos (oscillations,effects of quantum gravity, ) neutrino point sources gamma ray bursts multimessenger approaches diffuse fluxes dark matter magnetic monopoles supernova bursts shadow of the moon atmosphere physics glaciology new technologies for highest energies (radio, acoustics) Summary

*1) Motivation for neutrino astronomy2) Selected AMANDA results3) Plans and Status for IceCube*****These graphs come from studying in situ light sources. Point out the bubbly ice scattering part and that theres a ton of climate information here.

Absorption tells you the string spacing, the cost, and the threshold. Scattering tells you how easy it is to do reconstruction. You can take the product of the two to get the propagation length. Mention the other natural Cerenkov medium, water, and ANTARES, NEMO, etc.**********Soft vs. hard limit?