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• Other Authors: The Pennsylvania State University CiteSeerX Archives
• Format: Text
• Language: English
• Subjects: Antarctic; Nestor; South Pole; The Antarctic; Antarc*; South pole
• Online Access: http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.522.5355; http://icecube.berkeley.edu/~bprice/publications/Ocean.lake.ice.pdf

it such as active galactic nuclei.1 All agree that such the water in the hole refreezes after the string is in observatories will require a huge volume of transpar-ent, deep material such as lake or ocean water or ice, which acts as both the target and the medium for detecting the charged particles produced in interac-tions of such neutrinos. Estimates of the fluxes and detection rates of ultrahigh-energy astrophysical neutrinos lead to the requirement of an effective vol-ume.1 km3 so as to see at least a few events per day. Two instruments consisting of three-dimensional ar-rays of phototubes have made encouraging starts. The first is an array of five strings with a total of 23 working pairs of phototubes at a depth of;1 km in Lake Baikal.2 The second is the Antarctic muon and neutrino detecting array ~AMANDA! South Pole ar-ray, consisting of four strings with 73 working pho-totubes frozen into ice at depths of 0.8–1 km ~Ref. 3!, below which are five new strings with 79 working phototubes at depths of 1.6–2 km ~Ref. 4!. Both of place.! For deep ocean sites, such as have been pro-posed for the deep underwater muon and neutrino detector ~DUMAND!5 and NESTOR,6 the problems of deploying strings from shipboard have not been solved, but the basic concept is the same: The pho-totubes of an array accurately record arrival times and intensities of the photons in the moving cone of Cherenkov light produced by muons or electrons cre-ated in interactions of muon or electron neutrinos, respectively. The optical properties of the medium become of crucial importance when one takes into account the cost of expanding from the small-scale instruments now under construction to km3 scale volumes. The region of interest for detection of Cherenkov light is 320 # l # 620 nm. At wavelengths shorter than;320 nm, light is absorbed by the glass pressure vessel that houses a phototube; at wavelengths longer than;620 nm, the quantum efficiency of the phototube becomes too low. The quantities relevant to the media are the ...