| Names |
R. Abbasi, Y. Abdou, T. Abu-Zayyad, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. M. Allen, D. Altmann, K. Andeen, J. Auffenberg, X. Bai, M. Baker, S. W. Barwick, R. Bay, J. L. Bazo Alba, K. Beattie, J. J. Beatty, S. Bechet, J. K. Becker, K.-H |
| Abstract |
The IceCube neutrino observatory in operation at the South Pole,
Antarctica, comprises three distinct components: a large buried array
for ultrahigh energy neutrino detection, a surface air shower array, and
a new buried component called DeepCore. DeepCore was designed to lower
the IceCube neutrino energy threshold by over an order of magnitude, to
energies as low as about 10 GeV. DeepCore is situated primarily 2100 m
below the surface of the icecap at the South Pole, at the bottom center
of the existing IceCube array, and began taking physics data in May
2010. Its location takes advantage of the exceptionally clear ice at
those depths and allows it to use the surrounding IceCube detector as a
highly efficient active veto against the principal background of
downward-going muons produced in cosmic-ray air showers. DeepCore has a
module density roughly five times higher than that of the standard
IceCube array, and uses photomultiplier tubes with a new photocathode
featuring a quantum efficiency about 35% higher than standard IceCube
PMTs. Taken together, these features of DeepCore will increase IceCube's
sensitivity to neutrinos from WIMP dark matter annihilations,
atmospheric neutrino oscillations, galactic supernova neutrinos, and
point sources of neutrinos in the northern and southern skies. In this
paper we describe the design and initial performance of DeepCore. |