The IceCube Neutrino Telescope

1. The IceCube Neutrino Telescope Kyler Kuehn Center for Cosmology and AstroParticle Physics The Ohio State University Novel Searches for Dark Matter CCAPP November 17, 2008

2. The IceCube Collaboration Sweden: Uppsala Universitet Stockholm Universitet Germany: Universität Mainz DESY-Zeuthen Universität Dortmund Universität Wuppertal Humboldt Universität MPI Heidelberg RWTH Aachen USA: Bartol Research Institute, Delaware Pennsylvania State University UC Berkeley UC Irvine Clark-Atlanta University University of Alabama University of Maryland University of Wisconsin-Madison University of Wisconsin-River Falls Lawrence Berkeley National Lab University of Kansas Georgia Institute of Technology Southern University and A&M College, Baton Rouge University of Alaska, Anchorage The Ohio State University UK: Oxford University Netherlands: Utrecht University Japan: Chiba University Belgium: Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut Switzerland: EPFL New Zealand: University of Canterbury >30 institutions, ~250 members http://icecube.wisc.edu

3. South Pole Amundsen-Scott Station Skiway Counting House IceCube AMANDA Drill Camp

5. IceCube IceTop

6. The Enhanced Hot Water Drill (EHWD) Drill camp (5 MW hot water heater) Hose Reel Hot water hoses (2) IceTop Tanks (w/ sun shield) Drill head Solar heated Facilities • Drill speeds ~ 2 m/minute • ~40 hours to drill a hole • ~12 hours to deploy a string • Deploy: DOMs, pressure sensors, Std. Candle, dust logger, …

7. EHWD in Action

8. A New Astronomical Messenger Cutoff determined by μG galactic B field Cutoff determined by e+e- threshold for stellar IR photons diffuse, GRB AGN, TD Neutrinos open a new window onto astrophysical processes in ways which no other particle can

9. Neutrino Detection • Neutrino interacts with a nucleon and produces a lepton • Lepton emits Cherenkov light as it travels through ice (in 41° cone) • Light is detected by Digital Optical Module (DOM)   • 35 cm pressure vessel surrounding a 25 cm Photomultiplier • 400 ns recording time • 3 channels gives a 14 bit dynamic range • 1 - 2% of DOMs fail during freeze-in • 15 year survival probability 96%

10. Muon from IC40 Data Neutrino Event Identification Cascades Tracks IceCube Angular Resolution < 1°

11. A Wealth of Science AGNs, GRBs: cosmic accelerators?   Diffuse Sources  ? Point Sources  GZK/UHE  Supernovae DM: Solar WIMPs (see subsequent talks) CRs

12. AMANDA Datasets Most published physics results are from AMANDA completed 1997 completed 2000 In 2006 AMANDA was merged into IceCube. * Not including AMANDA B-10 (1997-1999)

13. IceCube Datasets IC1 + IC9 + IC22 + IC40

14. Cosmic Ray Flux Measurement • IceCube can measure the “background” cosmic ray μ flux • Allows evaluation of detector simulation as well as • Cosmic ray flux and composition around the knee • Prompt contribution to muon flux from charm production Atm.  Atm.  Cosmic Ray Astrophysical 

15. IC9 Diffuse Analysis • Search for excess of unresolved neutrinos from astrophysical sources • Use energy based variables (NCh) to separate astrophysical  from atmospheric  • Preliminary sensitivity: E-2 dN/dE < 1.4 x 10-7 GeV/cm2/s/sr • Roughly comparable to limit from AMANDA combined 4-year limit E-2 E-3.7 Most stringent AMANDA limits: ≤ 106 GeV - E-2 dN/dE < 9 x 10-8 [Ap.J 675, 1014, (2008)] > 106 GeV - E-2 dN/dE < 7.4 x 10-8 [Phys. Rev. D 76, 042008 (2007)]

16. Point Source Search • Search for excess of astrophysical neutrinos from a common direction over the background of atmospheric neutrinos from the Northern hemisphere Atm.  Atm.  * Livetime varies for specific scenarios

17. IceCube Point Source Searches IC9 • 26 a priori source locations • 60% of random datasets had a sigma higher than 3.35 - no excess seen C. Finley et al. arXiv:0711.0353 [astro-ph] p.107-110 •  Unbinned likelihood + energy information •  Hottest spot at r.a.153º, dec.11º •  p‐value (pre-trials): 7×10‐7 (4.8σ) •  p‐value (post-trials) 1.34% (2.2σ) •  Consistent with background fluctuation IC22

18. AMANDA ν IceCube CGRO IPN Satellites (Fermi, Swift, HETE, ...) γ, ν GRB timing/localization information from correlations among satellites A Distant GRB

19. Cascade(Rolling) Cascade(Trig & Roll) R03b  search MN06 WB03 R03a GRBs in AMANDA & IceCube • AMANDA •  search • Over 400 GRBs in Northern Hemisphere • Cascade search • Triggered search for 73 GRBs in both hemispheres • Rolling search for 2001-2003 • IceCube • 93 SWIFT bursts during IC22 • GRB080319B: brightest (optical) burst ever • ~0.1  events predicted in IC22 using fireball model • ~1  event predicted for equivalent burst in IC80 R03b: Supranova model WB03: Waxman-Bahcall model R03a: Choked Burst model MN06: Murase Nagataki model

20. Future Plans • Deep Core (see subsequent talks) • Greatly enhances IceCube sensitivity to lower energy ’s • Lower mass solar WIMPs • Atmospheric neutrinos • Six new strings • 60 high QE DOMs in clear ice • First string deployed 08/09, • Remaining strings deployed 09/10 • Multi-messenger astronomy • Correlations with ROTSE, AGILE, MAGIC, and LIGO • New Technologies • 3 Prototype digital radio strings deployed with IceCube strings • 4 Hydrophones deployed above IceCube Dust concentration Very clear ice D. Cowen, Neutrino 2008

21. Optional Slides

22. IceTop Counting Rate (Hz) Solar Physics Dec. 13, 2006 Solar outburst seen by international monitoring network • IceTop is sensitive to ~GeV particles emitted by the Sun during outburst • Monitor IceTop tanks rates • Can extract energy spectrum in 1 - 10 GeV region • Paper in preparation

23. Real Moon Dummy Moons Obs. Exp. (°) (°) (°) CR Moon Shadow • Select well reconstructed tracks and look in angular bins • See a 4  deficit in the direction of the moon in 3 mos. of IC40 data • Independent method of calibrating IceCube’s angular resolution

24. Flux Limits for Point Sources