Ice Cube Christian Spiering for the Ice Cube

Ice. Cube Christian Spiering for the Ice. Cube Collaboration EPSC, Cracow July 2009 1

The Ice. Cube Collaboration Germany: Sweden: USA: Bartol Research Institute, Delaware University of California, Berkeley University of California, Irvine Pennsylvania State University Clark-Atlanta University Ohio State University Georgia Tech University of Maryland University of Alabama, Tuscaloosa University of Wisconsin-Madison University of Wisconsin-River Falls Lawrence Berkeley National Lab. University of Kansas Southern University and A&M College, Baton Rouge University of Alaska, Anchorage Uppsala Universitet Stockholm Universitet UK: Oxford University Netherlands: Utrecht University Switzerland: DESY-Zeuthen Universität Mainz Universität Dortmund Universität Wuppertal Humboldt Universität MPI Heidelberg RWTH Aachen Belgium: Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut EPFL Japan: Chiba University New Zealand: University of Canterbury 33 institutions, ~250 members 2

The Amundsen-Scott Station South Pole Station Building Astronomy Sector Ice. Cube AMANDA skiway 3

Ice. Cube Observatory 07/08: 18 06/07: 13 05/06: 8 04/05: 1 08/09: 19 strings Remaining: 22 Ice. Cube Strings 5 Deep. Core Strings complete in January 2011 4 Ice. Cube

Ice. Cube/Amanda Selected results cosmic ray (CR) spectrum, CR composition CR anisotropies shadow of the moon atmospheric neutrinos (oscillations, effects of quantum gravity, … ) neutrino point sources gamma ray bursts multimessenger approaches diffuse fluxes dark matter magnetic monopoles supernova bursts atmosphere physics glaciology new technologies for highest energies (radio, acoustics) Ice. Cube high energy extension plans 5

Shadow of the Moon § Absolute pointing 1° § Angular resolution 1° Downward muons, max. 28° above horizon, median energy of primary parent ~ 30 Te. V Cosmic Rays 0. 5° 8 months Ice. Cube 40 strings 6

90 Large-scale anisotropy of downgoing muons 0 24 h 12 Te. V Ice. Cube -90 90 (40 strings 2008) anisotropies on the per-mille scale 24 h 0 126 Te. V (skymap in equatorial coordinates) -90 7

Compare to Northern hemisphere Tibet air shower array • Compton-Getting effect ? • Heliosphere effect ? • Nearby pulsars ? • Interstellar magnetic field ? Simulation (Lallement et al. Science 2005) • First observation on Southern hemisphere adds important piece of information. 8 MILAGRO

Search for neutrino point sources Amanda 2000 -2006 9 6595 Events

Amanda 2000 -2006 significance map δ=90º Max Significance δ=54º, α=11. 4 h 3. 38σ 0 h 24 h 0 2. 5 95 of 100 background maps (data randomized in RA) have a point with significance ≥ 3. 38 10 5

First look above horizon (Ice. Cube 2007, 22 strings) Pe. V-Ee. V range Northern hemisphere Southern hemisphere Sensitivity of ¼ Ice. Cube, 1 year ~ 2 x sensitivity of Amanda 7 years enter new territory ! 11

All-sky map (6 months Ice. Cube 2008, 40 strings) Preliminary Northern hemisphere Te. V - Pe. V Background: atmospheric neutrinos Southern hemisphere Pe. V - Ee. V Background: atmospheric muons Reduced by 10 -5 using energy cut 175. 5 days livetime, 6796 up-going events, 10981 down-going events 12

All-sky map (6 months Ice. Cube 2008, 40 strings) Preliminary Hottest location at r. a. =114. 95°, dec. =15. 35° Pre-trial -log 10(p-value) = 4. 43 all-sky p-value is 61% not significant 13

Point Sources limits/sensitivities 40 string results preliminary MACRO SK ANTARES 40 -string Discovery Potential: 5σ in 50% of trials AMANDA 7 yr 40 -string Sensitivity: IC 22 Flux excluded at 90%cl 80 -string Sensitivity: Based on 40 -string analysis 14

Diffuse Neutrino Fluxes Ic Integral limits (E-2 flux) from Baikal, Amanda Ice. Cube e. C ub e at m Ice. Cube EHE analysis Auger . WB bound GZK 15

Neutrinos from GRB Razzaque et al. , PRD 68 (2003) t ~ -100 s 16 Waxman & Bahcall, PRL 78: 2292 (1997) t ~ 0 t 90 Waxman & Bahcall, Ap. J 541: 707 (2000) t ~ t 90 ?

E 2 flux (Ge. V cm-2 s-1 sr-1) Neutrinos from GRB 10 -7 AMANDA limit from 408 bursts 1997 -2003 10 -8 Waxman-Bahcall GRB prediction 10 -9 10 -10 104 105 106 107 neutrino energy E (Ge. V) t ~ -100 s 17 108 t ~ 0 t 90 Waxman & Bahcall, Ap. J 541: 707 (2000) t ~ t 90 ?

Neutrinos from naked-eye GRB 080319 B § Duration: 70 s, z=0. 94 § Brightest GRB (optical) ever § Large number of g-ray, x-ray, UV and optical, observations Full-Ice. Cube expectation ~ 1 event § Detector was in maintenance mode 9 out of 22 strings. § Signal expectation: 0. 1 events (G = 300) § No events at GRB position/time after cut Limit 18 Pi of the Sky

Indirect Dark Matter Search Sun Earth Detector Amanda skymap around Sun 19

Indirect Dark Matter Search 20

Indirect Dark Matter Search …. . apply to spin-dependent cross section • Models with strong spin-dependent coupling are the least constrained by direct DM searches. • W. r. t. spin-dependent coupling, Amanda & Ice. Cube are ~100 times more sensitive than direct search experiments (Sun is mostly hydrogen) Effect of Deep. Core 21

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