icecube & limits on neutrino emission from gamma-ray bursts icecube collaboration journal club...
TRANSCRIPT
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ICECUBE &Limits on neutrino emission from gamma-ray
bursts
IceCube collaboration
Journal Club talk 4.15.2011 Alex Fry
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Outline
• Neutrinos: The little neutral particles which are just right for exploring the universe.
• IceCube: A detector for neutrinos.• Gamma-Ray Burst model constraints from
IceCube• Conclusions
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Neutrinos
• Neutrinos are leptons like electrons, but neutrinos interact only via the weak force
• Neutrinos come in three flavors: electron, muon, and tau
• Neutrinos have a small, but nonzero mass• Neutrinos are created prodigiously by the Sun
(70 billion per second per square cm on Earth) and other nuclear reactions in the Universe.
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Neutrinos are specialParts of the universe are inaccessible for study using other types of cosmic rays: • protons do not carry directional information
because they are deflected by magnetic fields• neutrons decay before reaching the earth and
high-energy photons are absorbed• high-energy photons are absorbed
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Neutrino mixing
• Neutrinos change ‘flavors’ and so can be any of the three types
• For example, the T2K experiment being worked on by some people here at UW will measure the mixing from νμ to νe by leveraging the mixing as a function of distance
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Neutrino sources
• Supernovae• AGN• Cosmic Ray collisions in Earth’s atmosphere• Cosmic Neutrino Background from Big Bang• Dark Matter annihilations• Gamma-Ray Bursts
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IceCube
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IceCube is at the Amundson-Scott South Pole Station.
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Each photomultiplier is enclosed in a transparent pressure sphere, a Digital Optical Module (DOM). The DOM also contains a digitally controlled high voltage supply to power the photomultiplier, an analog transient waveform digitizer and LED flashers.
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DOMs measure the arrival time of every photon to an accuracy of better than 5 nanoseconds.
They cost about $350 each for a total cost of 1.7 million for the DOMs alone.
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Detecting Neutrinos in Ice
electron neutrino creates an electron, the muon neutrino a muon, and the tau neutrino a tau lepton.
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Detecting Neutrinos in Ice
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Cherenkov light
electromagnetic radiation is emitted when a charged particle passes through a dielectric medium at a speed greater than the phase velocity of light in the medium
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Muon events are most easily detected because the muon travels for a long time (much further than the Cherenkov light in the ice)
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IceCubeIcecube also uses surface detector modules to help reject cosmic ray showers from above.In this paper 160 million events detected and 99.9% were rejected.
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IceCube Neutrino Science
• Ice properties• Gamma-Ray Bursts• Diffuse neutrino backgrounds• Extremely high energy astrophysics• Dark matter, WIMPS• Supernova monitor• Relativistic magnetic monopoles
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Gamma-Ray Burst Constraints
• Gamma-ray bursts are one of the few plausible candidates for ultra-high energy cosmic rays.
• Long duration GRBs (>2 s) are thought be collapse of massive stars into BH and short duration GRB (<2 s) are thought be merger compact objects
• Both events are consistent with the fireball model and producing lots of high energy cosmic rays and neutrinos.
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Gamma-Ray Burst Constraints
The fireball model:• Mass rapidly accretes onto the newly formed
black hole. • A highly relativistic outflow/fireball dissipates
energy via synchrotron or IC (electrons)• Radiation emitted in Kev-Mev range is seen as
the gamma-ray signal (energy 1051 to 1054 erg)
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Gamma-Ray Burst Constraints
The fireball model continued:• Protons are also accelerated via the Fermi
mechanism with an energy spectrum E-2 and energy=1020 eV (Waxman 1995).
• The protons interact with the Mev photons and create other particles (Δ+ to pions) and ultimately neutrinos in the ratio (1:2:0 for νe:νμ:ντ).
• Thus high energy cosmic rays and neutrinos (which arrive at earth in the ratio 1:1:1) are plausibly explained by GRBs.
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Gamma-Ray Burst Constraints
So IceCube should be able to detect GRB’s
Sensitivity of the IceCube detector to astrophysical sources of high energy muon neutrinos. Ahrens et al. 2004
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Gamma-Ray Burst Constraints
Thin lines - 41 selected neutrino spectra for 41 bursts.Thick dotted line - standard Waxman spectra for single burst.Thick solid line – sum of allThick dashed lined – sum of 41 Waxman like spectra.
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Gamma-Ray Burst Constraints
IceCube has found no evidence for neutrino emission excluding prevailing models at 90% confidence.
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Conclusions
• In the coming years data will improve and better constraints will be had. Stay tuned.
• But where are the missing neutrinos?
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Emperor Penguins
• Emperor Penguins are endemic to Antartic costal regions.
• An Emperor Penguin can hold its breath for 20 minutes, and dive to depths of over 550 m (1/5 the depth of IceCube).
• Emperor Penguins are awesome.
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ref
• Search for muon neutrinos from Gamma-Ray Bursts with the IceCube neutrino telescope IceCube Collaboration: R. U. Abbasi, et al
• Sensitivity of the IceCube detector to astrophysical sources of high energy muon neutrinos. Ahrens et al. 2004
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