• we built a km3 neutrino detector 3 challenges: • drilling • optics of ice • atmospheric muons • atmospheric neutrino spectrum • atmospheric.
Download ReportTranscript • we built a km3 neutrino detector 3 challenges: • drilling • optics of ice • atmospheric muons • atmospheric neutrino spectrum • atmospheric.
• we built a km3 neutrino detector 3 challenges: • drilling • optics of ice • atmospheric muons • atmospheric neutrino spectrum • atmospheric muon spectrum: first surprise • search for the sources of the Galactic cosmic rays • search for the extragalactic cosmic rays • gamma ray bursts • GZK neutrinos • a multi-wavelength story • search for dark matter IceCube.wisc.edu WIMP search strategies • Direct detection • Indirect detection: – neutrinos from the Earth/Sun – antiprotons from the galactic halo – positrons from the galactic halo – gamma rays from the galactic halo – gamma rays from external galaxies/halos – synchrotron radiation from the galactic center / galaxy clusters – ... direct detection - general principles c c • WIMP + nucleus WIMP + nucleus • Measure the nuclear recoil energy • Suppress backgrounds c December c c June • Search for an annual modulation due to the Earth’s motion around the Sun present limits DAMA result (> 8 sigma) neutralino capture and annihilation rc c sun velocity distribution n interactions sscatt nm n int. m int. Gcapture m Gannihilation cc qq ll nm W , Z,H Silk, Olive and Srednicki, ’85 Gaisser, Steigman & Tilav, ’86 cc ,bb ,tt , ,W , Z , H H 0 0 Freese, ’86; Krauss, Srednicki & Wilczek, ’86 Gaisser, Steigman & Tilav, ’86 supersymmetry on the back of an envelope arXiv 9404252 WIMP Capture and Annihilation c nm n DETECT c+cW+Wn+n indirect detection for cyclists e.g. n-telescope searches for 500 GeV WIMP 1. c - flux 300 km/s > LHC limit 500GeV c r c v 2.4 10 [ ] cm2 s 1 mc 500GeV 0.4 GeV cm3 8 104 [ ] cm3 mc 4 2. solar cross section sun n s c p M sun sc p mp [1.2 1057 ][10 41 cm2 ] ( GF m ) 2 p G ~ M 2 F 2 Z 2 2 MZ mH4 Nsun = capture rate = annihilation rate c c W W mnm 500 GeV 250 GeV 3. Capture rate by the sun Nsun c sun 3 x 10 s 20 4. Number of muon-neutrinos Nn 2 x 0.1 Nsun 1 Nn 8 2 1 n 2 x 10 cm s 2 4 d # events A E 250GeV n runningtime 10 cm 2 2 # events = 60 per year update: focus region neutrino rate versus WIMP mass white line: 100 events km-2 yr-1 IC22 solar neutrino rate vs wimp mass 0—1 TeV 100 events km-2 yr-1 • capture • equilibrium dN 2 Ccap Cann N dt 1 1 2 Gann Cann N Ccap 2 2 neutrino flux indirect detection of dark matter wimp-nucleon cross section the sun atmospheric neutrino events sensitivity to wimps with spin-independent interactions <103 SI limit >103 SI limit arXiv:0906.1615 arXiv:0906.1615 neutrinos from the center of the Galaxy conclusions • supersymmetry comes in 2 flavors: spin-independent ( favors direct detection because of A2 ) and spin-dependent • IceCube is competitive for spin-dependent • can probe most of the interesting parameter space of the MSSM • [astrophysics is known ( no toothfairies )] IceCube: multiwavelength analysis • • • • • IceCube supernova explosions (millisecond alert) a story from AMANDA days TeV gamma ray observations GRB IceCube takes data continuously and records and archives them supernova burst: light fromn e PMT noise low (280 Hz) detect correlated rate increase on top of PMT noise when supernova neutrinos pass through the detector p ne Kitaura, Janka, Hillebrandt (Astron. Astrophys. 450 (2006) 345) Garching first 20 msec e p n n e Simulation Data deleptonization Luminosities starting points of neutrino showers • equivalent detection volume of a 2.5 megaton SuperK-style detector • 1 million events from 10 kpc • time of neutronization to a few milliseconds 106 eventswith1.7m sec sampling start : 3m sat 95% CL signal depends on • properties of the supernova collapse • unknown neutrino physics Kamioka II 1987A Participation in SNEWS …several hours advanced notice to astronomers … Super-K SNO coincidence server @ BNL alert LVD AMANDA (IceCube) IceCube will follow this year http://snews.bnl.gov astro-ph/0406214