News from the South Pole: Recent Results from the IceCube and AMANDA Neutrino Telescopes Alexander Kappes UW-Madison PANIC ‘08 November 2008, Eilat (Israel)

Outline High-energy cosmic neutrino sources The IceCube and AMANDA neutrino telescopes Physics topics (recent results) – Moon shadow – Steady point-like sources – Gamma ray bursts – Dark Matter (WIMPs) ➞ Talk by Catherine De Clercq – Exotic physics ➞ Talk by John Kelley Alexander KappesPANIC'08, Eilat2

Alexander KappesPANIC'08, Eilat3 Target: photon field molecular cloud interstellar medium Cosmic ray accelerator p + p(  ) →  ± + X   +   e + e +  cosmic ray + neutrinos p + p(  ) →  0 + X cosmic ray + photons Supernova remnants (Cas A) Gamma-ray bursts (GRB B, Swift) ?

Principle of neutrino detection Alexander KappesPANIC'08, Eilat4 nuclear reaction muon infrequently, a cosmic neutrino crashes into an atom in the ice and produces a nuclear reaction muon travels kilometers in the ice blue (Cherenkov) light produced optical sensors capture (and map) the light 

IceTop InIce Air shower detector 160 ice-tanks in surface array Threshold ~ 300 TeV 80 Strings each with 60 Optical Modules 17 m between Modules 125 m between Strings : 1 String : 8 Strings AMANDA ( ) 19 Strings 677 Modules Currently deployed: 40 Strings 80 IceTop tanks 3 more seasons planned :13 Strings : 18 Strings 1450m 2450m The IceCube and AMANDA neutrino telescopes Alexander Kappes5PANIC'08, Eilat

Backgrounds: Atmospheric muons & neutrinos Alexander KappesPANIC'08, Eilat6 Backgrounds: - Downgoing μ - Atmospheric ν Data-MC comparison Down-going atm. muons Up-going -induced muons Significantly higher sensitivity for up-going High-purity (atmospheric) up-going neutrino sample after cuts Cosmic neutrinos typically have harder spectra (E -2 )

Pointing accuracy: the Moon shadow in IceCube 40-strings Moon shadow observed in first 3 months of IC40 data Validates pointing capabilities: Angular resolution: – IceCube 22 < 1.5° – IceCube 80 < 1° Alexander KappesPANIC'08, Eilat7 Preliminary true moonmean from fake moons difference

AMANDA point source search Unbinned likelihood method using energy information Final 7 year AMANDA (3.8 yr livetime) analysis 95% of RA-randomized skymaps have maximum significance > 3.38 σ → Not significant Alexander KappesPANIC'08, Eilat8 Significance Max Significance  =54 o,  =11.4h 3.38 

AMANDA point source search Unbinned likelihood method using energy information Final 7 year AMANDA (3.8 yr livetime) analysis 95% of RA-randomized skymaps have maximum significance > 3.38 σ → Not significant Alexander KappesPANIC'08, Eilat9 Significance Max Significance  =54 o,  =11.4h 3.38  3yr max significance: 3.73   1.5  5yr max significance: 3.74   2.8 

Search for point sources with IceCube 22-strings Unbinned likelihood method using energy information Hottest spot found at r.a. 153º, dec. 11º pre-trial p-value: 7×10 -7 (4.8 sigma) Accounting for all trials, p-value for analysis is 1.34% (2.2 sigma). At this significance level, consistent with fluctuation of background. Alexander Kappes10PANIC'08, Eilat preliminary

Current neutrino flux limits / sensitivities Alexander KappesPANIC'08, Eilat11 IceCube 22 AMANDA 3.8 years IceCube 80

Analysis of “naked eye” GRB B  March 19, 06:12:49 UTC (duration ~70 s)  Position: RA = º, Dec = º  Brightest (optical) GRB ever observed: z = 0.94 (D A = 1.6 Gpc, light travel time 7.5 Gyr)  Expect ~0.1 events in IceCube 9-strings (Fireball model,  = 300) Alexander KappesPANIC'08, Eilat12 Pi-of-the-Sky (optical)

Analysis of “naked eye” GRB B  March 19, 06:12:49 UTC (duration ~70 s)  Position: RA = º, Dec = º  Brightest (optical) GRB ever observed: z = 0.94 (D A = 1.6 Gpc, light travel time 7.5 Gyr)  Expect ~0.1 events in IceCube 9-strings (Fireball model,  = 300)  Unbinned likelihood method yields 0 signal events  Expect O (1) event in IceCube 80 from similar burst! Alexander KappesPANIC'08, Eilat13 Pi-of-the-Sky (optical)

Gamma-ray bursts with IceCube 22-strings Currently analyzing data from 41 bursts (Swift, AGILE + others) Individual modeling of bursts according to GRB fireball model Expected events: – average Waxman-Bahcall ~0.7 – individual GRB spectra ~0.5 Outlook: IceCube 80 will be able to see WB GRB flux within few years Alexander KappesPANIC'08, Eilat14 Discovery potential for average WB bursts ~30% chance preliminary

Conclusions and Outlook IceCube halfway completed (40 strings), completion planned for 2011 Verification of pointing accuracy via observation of Moon shadow Search for point-like sources over the whole sky – Final AMANDA 7 year (3.8 years livetime) analysis – IceCube 22-string analysis ➞ no significant access above background observed Search for neutrinos from gamma-ray bursts – Individual analysis of “naked eye” GRB B ➞ no signal events found – Analysis results for 41 bursts with IceCube 22-strings coming soon With the nearing completion of the first km 3 -scale detector, IceCube, neutrino astronomy enters into a new era Alexander KappesPANIC'08, Eilat15 Exciting times lie ahead !

The IceCube collaboration Alexander KappesPANIC'08, Eilat16 Univ Alabama, Tuscaloosa Univ Alaska, Anchorage UC Berkeley UC Irvine Clark-Atlanta University U Delaware / Bartol Research Inst Georgia Tech University of Kansas Lawrence Berkeley National Lab University of Maryland The Ohio State University Pennsylvania State University University of Wisconsin-Madison University of Wisconsin-RiverFalls Southern University, Baton Rouge  Universität Mainz Humboldt Univ., Berlin DESY, Zeuthen Universität Dortmund Universität Wuppertal MPI Heidelberg RWTH Aachen Uppsala University Stockholm University Chiba University Universite Libre de Bruxelles Vrije Universiteit Brussel Université de Mons-Hainaut Universiteit Gent EPFL, Lausanne Univ. of Canterbury, Christchurch University of Oxford University Utrecht 32 Institutions, ~250 members

Backup Alexander KappesPANIC'08, Eilat17

Effective muon neutrino area Alexander KappesPANIC'08, Eilat18

Separation of atmospheric and cosmic neutrinos Alexander KappesPANIC'08, Eilat19 Atmospheric neutrinos irreducible background (~60,000 per year in IceCube with 80 strings) Cosmic neutrinos typically have harder spectra (E -2 ) (detected events peak at higher energies)

A Priori Source List for IC22 Obj. Name ra(deg) dec(deg) p-value (pre-trial) MGRO_J ( , ) : MGRO_J ( , 6.280) : Cyg_OB2 ( , ) : SS_433 ( , 4.983) : Cyg_X-1 ( , ) : LS_I_+61_303 ( , ) : GRS_ ( , ) : XTE_J ( , ) : GRO_J ( , ) : Geminga ( , ) : Crab_Nebula ( , ) : Cas_A ( , ) : Mrk_421 ( , ) : Mrk_501 ( , ) : ES_ ( , ) : ES_ ( , ) : H_ ( , ) : ES_ ( , ) : BL_Lac ( , ) : S5_ ( , ) : C66A ( , ) : C_454.3 ( , ) : C_38.41 ( , ) : PKS_ ( , ) : C_273 ( , 2.052) : M87 ( , ) : NGC_1275 ( , ) : Cyg_A ( , ) : (only excesses reported, otherwise given as “---”) Lowest p-value (0.07) is for 1ES Not significant after trial factor of 28 sources in list.

All Flavor GRB Limits from AMANDA II Limits from triggered searches assume ~700 bursts per year ~420 GBs investigated AMANDA starts to exclude flux models! Cascade search in IceCube much more competitive (factor 70 in instrumented vol.) Eff. volume (cascades) grows faster than eff. area (muon)! Muon searches (only trig) Cascade searches (trig + roll) only rolling