Optical properties of deep glacial ice at the South Pole

By M. Ackermann, J. Ahrens, X. Bai, M. Bartelt, S. Barwick, R. Bay, T. Becka, J. Becker, K. Becker, P. Berghaus and 107 more. 2006

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OBSERVATION AND CHARACTERIZATION OF A COSMIC MUON NEUTRINO FLUX FROM THE NORTHERN HEMISPHERE USING SIX YEARS OF ICECUBE DATA (2016, methodology): “The Cherenkov light from charged particles is tracked through the ice to the DOMs (Lundberg et al. 2007; Chirkin 2013c, and from work by C. Kopper in 201155) taking into account the Antarctic ice properties (Ackermann et al. 2006; Aartsen et al. 2013b; Chirkin 2013a).”
Methods for point source analysis in high energy neutrino telescopes (2008, background): “Photons are propagated with an effective scattering length of 21 m and an absorption length of 120 m, which are typical values for South Pole ice [21].”
Measurement of South Pole ice transparency with the IceCube LED calibration system (2013, methodology): “d absorption coeﬃcients of each ice layer are best interpreted as the average of their true values over the thickness of the ice layer. The chosen thickness of 10 m is the same as the value chosen in [4] but smaller than the vertical DOM spacing of 17 m. Due to small depth oﬀsets between the DOMs on”
IceCube sensitivity for low-energy neutrinos from nearby supernovae (2011, methodology): “The optical scattering and absorption in glacial ice at the South Pole has been studied extensively (Ackermann et al., 2006) by the AMANDA and IceCube Collaboration with pulsed Table 1.”