Event Reconstruction at the Sudbury Neutrino Observatory

Details Event Reconstruction at the Sudbury Neutrino Observatory Event Reconstruction at the Sudbury Neutrino Observatory

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..apr.x7003b&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

The Sudbury Neutrino Observatory is sensitive to solar neutrinos through three reactions: charged current, neutral current, and elastic scattering. Each neutrino interaction in SNO leads to either one or more γ-rays or an electron in the detector giving rise to Čerenkov radiation, which is detected by approximately 9600 photomultiplier tubes. The relative time-of-flight, spatial distribution, and number of these photons detected are used to reconstruct the position in the detector and momentum of the events. The backgrounds in SNO (mostly low energy backgrounds from daughters of ^232Th and ^238U in detector materials) have characteristic distributions in position and momentum that are well separated from the neutrino events so that momentum and position cuts can be applied to reduce those backgrounds to a negligible fraction of the neutrino signal. The position and momentum distributions of neutrino events are also used as characteristic distributions for separating the three signal classes. An overview of the methods used to reconstruct events in SNO will be presented, along with the method of evaluating reconstruction performance and systematic uncertainties with calibration data.

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