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

The IceCube Collaboration 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 Sweden: Uppsala Universitet Stockholm Universitet UK: Oxford University Belgium: Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut Germany: Universität Mainz DESY-Zeuthen Universität Dortmund Universität Wuppertal Humboldt Universität MPI Heidelberg RWTH Aachen New Zealand: University of Canterbury Netherlands: Utrecht University Switzerland: EPFL Japan: Chiba University >30 institutions, ~250 members

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

5 IceTop

6 The Enhanced Hot Water Drill (EHWD) Drill camp (5 MW hot water heater) Hot water hoses (2) Hose Reel Drill head Solar heated Facilities IceTop Tanks (w/ sun shield) 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, …

EHWD in Action

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

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 Neutrino Event Identification Muon from IC40 Data Tracks Cascades Track-LikeIceCubeAMANDA Time Resolution (nsec) 25-7 Energy Resolution (log 10 E) 0.3 – 0.4 Field of View2π Cascade-LikeIceCubeAMANDA Time Resolution (nsec) 25-7 Energy Resolution (log 10 E) 0.18 Field of View4π IceCube Angular Resolution < 1°

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

12 In 2006 AMANDA was merged into IceCube. AMANDA Datasets YearLivetime d d d d d d d Total*3.8 years Most published physics results are from AMANDA completed 2000 completed 1997 * Not including AMANDA B-10 ( )

13 IceCube Datasets #StringsYearRun Length CR  Rate  rate IC days5 Hz~0.01/day IC days80 Hz~ 1.5/day IC days550 Hz~ 20/day IC402008~ 1year1400 Hz IC years1650 Hz ~ 200/day IC1 IC9 IC22 IC

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 14 Cosmic Ray Flux Measurement Atm.  Atm. Astrophysical Cosmic Ray

15 IC9 Diffuse Analysis Preliminary sensitivity: E - 2 dN/dE < 1.4 x GeV/cm 2 /s/sr Roughly comparable to limit from AMANDA combined 4-year limit Most stringent AMANDA limits: ≤ 10 6 GeV - E -2 dN/dE < 9 x [Ap.J 675, 1014, (2008)] > 10 6 GeV - E -2 dN/dE < 7.4 x [Phys. Rev. D 76, (2007)] E -3.7 E -2 Search for excess of unresolved neutrinos from astrophysical sources Use energy based variables (NCh) to separate astrophysical  from atmospheric 

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.  Detector (Years) Energy (TeV) Live Time (days) AMANDA B-10 ( ) AMANDA-II ( ) AMANDA-II ( ) IceCube 22 (2007) IceCube 22 + AMANDA * * Livetime varies for specific scenarios

17 26 a priori source locations 60% of random datasets had a sigma higher than 3.35  - no excess seen IceCube Point Source Searches C. Finley et al. arXiv: [astro-ph] p 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 IC9

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

19 Cascade (Trig & Roll) Cascade (Rolling)  search WB03 MN06 R03b R03a R03b: Supranova model WB03: Waxman-Bahcall model R03a: Choked Burst model MN06: Murase Nagataki model 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 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

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 Very clear ice Dust concentration D. Cowen, Neutrino 2008

Optional Slides

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

Real MoonDummy Moons Obs. Exp.  (°) 23 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

Flux Limits for Point Sources