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

>30 institutions, ~250 members 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 Switzerland: EPFL Belgium: Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut Largely US, international collaboration with a significant contribution from Europe. New Zealand: University of Canterbury >30 institutions, ~250 members http://icecube.wisc.edu

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

IceCube IceTop

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, …

EHWD in Action

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

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%

Neutrino Event Identification Tracks Cascades Muon from IC40 Data IceCube Angular Resolution < 1° Track-Like IceCube AMANDA Time Resolution (nsec) 2 5-7 Energy Resolution (log10E) 0.3 – 0.4 Field of View 2π Cascade-Like IceCube AMANDA Time Resolution (nsec) 2 5-7 Energy Resolution (log10E) 0.18 Field of View 4π

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

AMANDA Datasets Year Livetime 2000 197 d 2001 193 d 2002 204 d 2003 Most published physics results are from AMANDA Year Livetime 2000 197 d 2001 193 d 2002 204 d 2003 213 d 2004 194 d 2005 199 d 2006 187d Total* 3.8 years completed 2000 completed 1997 In 2006 AMANDA was merged into IceCube. * Not including AMANDA B-10 (1997-1999)

IceCube Datasets + + + #Strings Year Run Length CR  Rate  rate IC1 2005 164 days 5 Hz ~0.01/day IC9 2006 137 days 80 Hz ~ 1.5/day IC22 2007 319 days 550 Hz ~ 20/day IC40 2008 ~ 1year 1400 Hz IC80 2011 10 years 1650 Hz ~ 200/day IC1 + IC9 + IC22 + IC40

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 

IC9 Diffuse Analysis Search for excess of unresolved neutrinos from astrophysical sources Use energy based variables (NCh) to separate astrophysical  from atmospheric  E-2 E-3.7 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 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)]

Point Source Search Search for excess of astrophysical neutrinos from a common direction over the background of atmospheric neutrinos from the Northern hemisphere Detector (Years) Energy (TeV) Live Time (days) AMANDA B-10 (1997-1999) 1 - 1000 623 AMANDA-II (2000-2004) 1.6 - 2600 1001 (2000-2006) 1.6 -2600 1387 IceCube 22 (2007) 5 - 5000 270 IceCube 22 + AMANDA 0.1 - 10 1657* Atm.  Atm.  * Livetime varies for specific scenarios

IceCube Point Source Searches 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

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

GRBs in AMANDA & IceCube Cascade (Trig & Roll) Cascade (Rolling)  search WB03 MN06 R03b R03a 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

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

Optional Slides

Solar Physics Dec. 13, 2006 Solar outburst seen by international monitoring network IceTop Counting Rate (Hz) 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

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 Real Moon Dummy Moons Obs. Exp. (°)

Flux Limits for Point Sources