Swift and IceCube: Linking the E-m and Neutrino Skies

Details Swift and IceCube: Linking the E-m and Neutrino Skies Swift and IceCube: Linking the E-m and Neutrino Skies

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.3210n&link_type=abstract

American Astronomical Society, HEAD meeting #11, #32.10; Bulletin of the American Astronomical Society, Vol. 41, p.705

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Over the past five years, NASA's Swift Observatory has greatly enhanced our understanding of violent astrophysical events, including gamma-ray bursts, supernovae, and active galactic nuclei. While Swift studies the electromagnetic radiation from these events, other observatories are searching for corresponding cosmic rays, gravity waves, and neutrinos. We are currently working to use the rapid response of Swift to follow up triggers from these multi-messenger observatories. This talk will address the new capabilities required of Swift and introduces the collaborative effort between the Swift and IceCube teams. The IceCube telescope, located at the South Pole, is searching for astrophysical neutrinos through their interactions in the polar ice. To reduce background events, IceCube searches for a multiplicity of neutrinos with high temporal and spatial coincidence. Two or more neutrinos that reconstruct nearby in the sky can be used to trigger follow up searches for electromagnetic counterparts. In response, Swift will slew to observe the IceCube trigger region in X-ray and UV, tiling as necessary to cover the IceCube error circle. By accumulating data over a number of orbits, Swift will distinguish between steady sources and the afterglow typical of a burst event. This and similar efforts are exploration-driven. In particular, we will be sensitive to burst events that do not produce prompt gamma rays, which are conjectured to be significantly more numerous than gamma-emitting bursts. The sensitivity for discovering these events will be presented.

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