neutrino astronomy francis halzen University of Wisconsin

neutrino astronomy francis halzen University of Wisconsin http://icecube.wisc.edu

menu neutrino astronomy cosmic ray accelerators and neutrinos: km 3 neutrino detectors Amanda and Antares: first generation detectors ~ 0.015 km 3 IceCube results: neutrino astronomy muon astronomy (?) dark matter search

M. Markov 1960 B. Pontecorvo M.Markov : we propose to install detectors deep in a lake or in the sea and to determine the direction of charged particles with the help of Cherenkov radiation.

shielded and optically transparent medium muon interaction lattice of photomultipliers neutrino

Cherenkov light

cherenkov radiation: particle s speed exceeds the speed of light

photomultiplier tube

2008 ANTARES

2000 AMANDA South Pole Dome 1500 m 2000 m [not to scale] Amundsen-Scott South Pole station

AMANDA proof of concept neutrino interaction muon track ν μ + N μ+ X

atmospheric neutrinos high energy cosmic ray π μ ν μ 15 Km

detector measures the atmospheric neutrino flux predicted: method validated ~ 100 TeV zenith angle number of PMT

energy estimation muon track π γ bremsstrahlung e + e - photo-nuclear pair-creation convert light emitted to estimate of the muon energy ( number of optical modules, number of photons, de/dx, Sean Grullon

drilling and deployment to 2500 m in less than 2 days 3.5 cm/second 18

photomultiplier starts its journey to 2500 m the IceCube project transforms a billion tons of ice into a particle physics detector

start 05-06 1 million pounds of cargo C-130 planes: > 50 flights IceCube

IceCube Site 5 megawatt power plant

one of 21 drill modules arrive in antarctica

Hose winch Drill tower Hot water generator IceTop Tanks 5 megawatt hot water drilling system

125 m 26

IceCube deployments Counting house: commissioned in January 2007 Completion 2011 : 80 strings 60 modules each 17m between modules 125m between strings 1 km³ ; ~1GTon 78 72 46 56 74 73 67 66 65 58 57 48 47 39 38 49 59 2006-2007: 13 strings 2005-2006: 8 strings 40 50 2004-2005 : 1 string 29 30 21 1997optical modules in ice: AMANDA 677 IceCube 1320

since jan 09 59 out of 86 2007-2008: 18 Strings 2006-2007: 13 Strings 2008-2009: 18+1 Strings 2004-2005 : 1 String 2005-2006: 8 Strings 1450 m 2450 m

IceCube neutrinos (40 out of 80 strings) operated for 276 days collected 10,000 neutrinos

one in 10 6 muon tracks is produced by a neutrino

challenge : p separate neutrinos (filtered by the Earth) from down- going cosmic ray muons at a level of much less than one per million ν μ

challenge : separate neutrinos filtered by the Earth from down- going cosmic ray muons at a level of much less than one per million

IceCube background: downgoing cosmic ray muons ~ 2000 per second signal: upgoing muons initiated by neutrinos ~ 10 per hour

within trigger time window down down down up

upcoming neutrinos downgoing muons

IceCube then and now PeV: x2 EeV: x3 IceCube neutrino area predicted performance (blue) Astroparticle Physics 20, 507 (2004)

atmospheric neutrinos: ultimate background ν μ,(e,τ) HE Cosmic Particle (~PeV) μ ν μ Angular Resolution ν μ < 1

AMANDA II 2000 directions of ~ 600 neutrinos

IceCube supersedes AMANDA by superior angular resolution IceCube 22 strings: 5114 neutrinos in 276 days

the hottest spot location is: Ra 153.5, Dec 11.5 events: 11 background: 3.3 -log 10 (p-value) : 6.14 (4.8 sigma) happens in 63 out of 10 4 scrambled maps, or the probability is ~ 0.01

intermezzo on point source search

looking up background of atmospheric muons instead of neutrinos reduced by 10-5

looking up

40 strings for ½ year ~ ¼ km 3 yr of data 7 events with probability 10-4.43 pre-trial not significant

diffuse flux excess of extra-terrestrial neutrinos (E -2 ) over atmospheric neutrinos (E -3.7 ) at the high-energy tail of an energy distribution

neutrinos associated with extragalactic cosmic rays IceCube AMANDA IceCube 22 strings

grb 070925 (3.84 sigma, 2.81 sigma post trial) Parameter Value Parameter Value GRB zenith 67.98 GRB azimuth 78.90 zenith 69.45 azimuth 73.28 angle difference to GRB 5.44 paraboloid sigma 1.70 rlogl 7.20 log10(hits) 2.93 log10(charge) 3.46 nchannel 143 svm classifier -0.947 Time of event 75.56 GRB T100-3 to 33 next 40 strings : 1.5 events from 86 bursts

with unbiased surveys expect the unexpected the cosmic ray sky!

first view of the Southern hemisphere in TeV muons 90 0 24h -90 significance for each bin value from the average bin value for each declination

is this real? is the background more interesting? Tibet array: northern hemisphere

expect the unexpected with unbiased surveys IceCube & Tibet Array IceCube & Milagro

significance maps for two energy bins 90 0 24h -90 significance map for median energy significance map for median energy 12.6 TeV 126 TeV not the sun! sturcture of galactic magnetic field (large scale)? nearby sources (small scale)?

vela? geminga?

particle physics with one million atmospheric neutrinos (10 GeV ~ 1 PeV) deep core ( < 10 GeV, oscillations, hierarchy ) measurement of the high-energy neutrino cross section neutrino hierarchy with DeepCore quantum decoherence test special and general relativity with new precision search for magnetic monopoles search for dark matter search for topological defects and cosmological remnants search for non-standard model neutrino interactions Planck scale physics with GRBs particle physics with MeV neutrinos from supernova explosion in the galaxy ( 2 megaton )

to 10 GeV with DeepCore tau electron muon

bigger and better detector LED flasher board main board HV board

digital optical module R7081-02 25 cm OB-LED Delay Trigger (2) x 2.6 x 9 x16 x2 x0.25 MUX Pulser ATWD ATWD fadc 10b 10b 10b 40 MHz FPGA DP Ram CPU 10b 8b ADC DAC +/-5V, 3.3V, 2.5V, 1.8V Configuration Device 32b LPF SDRAM 1 megabaud DOR DC-DC 8Mbit 16Mb (n+1) (n 1) LC 20 MHz SDRAM 16Mb Oscillator Corning Frequency Ctl (was Toyocom) Monitor & Control DACs & ADCs 8b, 10b, 12b CPLD PMT Power 8b 16b Flash Flasher Board Flash 4Mb 4Mb 64 Bytes

The Digital Optical Module (DOM) Onboard capture of PMT waveforms 300 MHz for ~400 ns with custom chip 40 MHz for 6.4 µsec with comm. fast ADC Digitized Waveform Absolute timing resolution < 2 ns (RMS) Dynamic range ~1000 p.e./10 ns Deadtime < 1% Noise rate ~700 Hz (260 Hz w / artif. deadtime) Failure rate < 1%

AMANDA/IceCube as MeV ν detector PMT noise low (~ 300 Hz) ice uniformly illuminated detect correlated rate increase on top of PMT noise

hierarchy with galactic supernova explosion

WIMPs captured in the sun χ annihilate into neutrinos ν μ n DETECT χ + χ W + W ν +... b + b ν +...

atmospheric neutrino events the sun

sensitivity to wimp dark matter : spin-dependent interactions ) 2 Neutralino-proton SD cross-section (cm 10 10 10 10-36 -37-38 -39 2 0.05 < Ω χ h < 0.20-32 10 σ < σlim CDMS(2008)+XENON10(2007) SI SI σ < 0.001xσlim CDMS(2008)+XENON10(2007) -33 SI SI 10 CDMS (2008) COUPP (2008) IceCube-80+DeepCore 1800d sens. (hard) KIMS (2007) -34 10 SUPER-K 1996-2001 IceCube-22 2007 (soft) IceCube-22 2007 (hard) -35 10 AMANDA 7y (hard) AMANDA 7y (soft) 10-40 10-41 10 10 2 10 3 10 Neutralino mass (GeV) 4

conclusions IceCube is taking data with a ¾ km 3 instrumented volume integrated exposure reaches 1 km 2 year this year Antares TDR for KM3NeT this year