Neutrinos as astronomical messengers
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1 I Taboada / Georgia Tech Aug 10, 2010
2 Neutrinos as astronomical messengers Photon B Neutrino Cosmic ray
3 High- energy neutrino detec5on: tradi5onal way Astrophysical neutrino Cosmic Ray Atmospheric muon Atmospheric Neutrino Cosmic Ray Build a BIG detector (~1 km 3 of water) Build underground Use Earth as a filter Cherenkov Detec5on
4 High- energy neutrino detec5on: tradi5onal way Astrophysical neutrino Cosmic Ray Atmospheric muon Atmospheric Neutrino IceCube is in fact a 4π sr detector Cosmic Ray Build a BIG detector (~1 km 3 of water) Build underground Use Earth as a filter Cherenkov Detec5on
5 The IceCube collabora5on. Approximately 250 people Canada: U Alberta USA: U Alabama, Tuscaloosa U Alaska, Anchorage UC Berkeley UC Irvine U Delaware Georgia Tech U Kansas LBNL U Maryland Ohio State U Pennsylvania State U U Wisconsin-Madison U Wisconsin-River Falls Clark Atlanta U Southern U, Baton Rouge Barbados: U West Indies Sweden: Uppsala U Stockholm U UK: Oxford Belgium: U Libre de Bruxelles Vrije U Brussel U de Mons U Gent Switzerland: EPFL, Lausanne Germany: U Mainz Humboldt U, Berlin DESY, Zeuthen U Dortmund U Wuppertal MPI Heidelberg RWTH Aachen Bonn Bochum Japan: Chiba U New Zealand: U Canterbury Antarctica: South Pole Station
6
7 IceCube performance Low noise rates: ~300Hz (SPE/sec) Rate with correlated pulses ~500Hz Supernova MeV ν detecuon! High duty cycle: >97% 32 / 4790 DOMs dead (0.7%) Event rates (79 strings) Muons: ~1.8 khz Neutrinos: ~220/day
8 Observa5on of the Moon shadow (14 Moon cycles IC40) Cosmic Rays Preliminary
9 Atmospheric muon neutrinos Preliminary
10 Preliminary All Sky Point Source Search. IC40 10! pre- trial
11 Preliminary All Sky Point Source Search. IC40 Northern hemisphere Background: atmospheric neutrinos upgoing events 11! Southern hemisphere Background: atmospheric muons Reduced by 10-5 using energy cut downgoing (high energy) muon events pre- trial Livetime = days
12 Preliminary All Sky Point Source Search. IC40 12! Hottest location in the all-sky search is: Ra=113.75, Dec=15.15 All- sky p- value = 18% not significant, no evidence for neutrino source pre- trial
13 Catalog # Sources Milagro 17 E -2 Stacked Source Search Model p-value N s γ ν µ + ν τ upper limit uniform Milagro 6 (SNR) Halzen et al (2008) Starburst Galaxies Clusters of Galaxies 127 E -2 prop to FIR flux Φ 90 = (*) SF = Φ 90 = Model A SF = 2.6 Model B SF = 4.0 Isobaric 0.0 SF = 4.4 Central AGN Likelihood method provides signal normalizauon and spectral index consistent with the data 0.0 SF = 2.0 (*) A posteriori source selecuon Φ 90 in units of TeV - 1.cm - 2.s - 1 SF: model scaling factor
14 Cosmic Ray Anisotropy Preliminary
15 Neutrinos from GRBs Preliminary IceCube in coincidence with Fermi/GBM has a 95% of detecuon potenual of Waxman- Bahcall model at 5 σ in one year. Within 5 years, IceCube will extensively sample the allowed parameter space of the Waxman- Bahcall model. 117 Northern hemisphere GRBs, reported mostly by Fermi.
16 DeepCore Science Poten5al Indirect dark mafer search (Sun, Center of galaxy) 4π sr neutrino astronomy (>10 GeV) Neutrino oscillauons
17 Conclusions and outlook IceCube construcuon almost completed IceCube meeung or exceeding its design requirements IceCube is a 4π sr detector IceCube already producing scienufic results. Point sources, diffuse, GRBs, Atmospheric neutrinos, cosmic rays, Target of opportunity programs, indirect Dark Mafer search, etc
18 IC22+AMANDA, op5mized for soz spectra sources Galac5c Plane Scan Preliminary GalacUc LaUtude (deg) GalacUc Longitude (deg)
19 IC22+AMANDA, op5mized for soz spectra sources Cygnus Region (selected a- priori) Preliminary GalacUc LaUtude (deg) GalacUc Longitude (deg)
20 IC22+AMANDA, op5mized for soz spectra sources Cygnus region Preliminary GalacUc LaUtude (deg) Preliminary 2.3 σ, 1% p- value GalacUc Longitude (deg)
21 I Taboada / Georgia Tech Aug 10, 2010
22 Iridium satellites SN/GRB IceCube I Taboada / Georgia Tech Northern hemisphere IceCube CPU ROTSE III Aug 10, 2010
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