S. Barwick, James Beatty, David Besson, John Clem, Stephane Coutu, Michael DuVernois, Paul Evenson, Peter Gorham, Francis Halzen, Abram Jacobson, David Kieda, John Learned, Kurt Liewer, Stephen Lowe, Charles Naudet, Allen Odian, David Saltzberg, David Seckel
The ANITA project is designed to investigate ultra-high energy (>1017 eV) cosmic ray interactions throughout the universe by detecting the neutrinos created in those interactions. These high energy neutrinos are detectable through their interactions within the Antarctic ice sheet, which ANITA will use as a detector target that effectively converts the neutrino interactions to radio pulses. This paper will give an overview of the project including scientific objectives, detection description and mission design.
James Beatty, H. Ahn, P. Allison, M. J. Choi, N. Conklin, Stephane Coutu, Michael DuVernois, O. Ganel, S. Jaminion, K. Kim, M. Lee, L. Lutz, Pier Marrocchesi, S. Minnick, S. Mognet, Kyung-wook Min, S. Nutter, H. Park, I. Park, K. Petska, E. Schindhelm, Eun-Suk Seo, Simon Swordy, J. Wu, J. Yang
The cosmic ray all-particle spectrum has a small steepening of its spectral slope, or 'knee', near 1015 eV. Changes in the nuclear composition of cosmic rays may be associated with the knee and provide clues concerning the origin of the spectral change. An ultra-long duration balloon experiment, Cosmic Ray Energetics and Mass (CREAM), is being constructed to measure cosmic ray elemental spectra at energies just below the knee to look for evidence of changes in composition. CREAM employs a thin calorimeter and transition radiation detector to provide multiple measures of the particle energy. A novel technique, the timing charge detector, is used to identify the charge of the incident primary cosmic ray in the presence of the albedo particles generated by interactions in the calorimeter.
We will report on the details of the ANITA instrument. This instrument is fundamentally a broadband antenna, which is arrayed and constructed in such a way as to be optimized for the detection and characterization of high-energy neutrino cascades. The requirement to maximize the detector view of the Antarctic ice fields implies low gain antennas yet the need for maximum sensitivity dictates using the highest gain possible. Since the Cherenkov signal increases quadratically at higher frequencies suggesting that the optimal selection is an antenna with constant gain as a function of frequency. The baseline design will be a linearly polarized log-periodic zigzag (LPZZ) antenna.
The Auger Observatory southern site's surface detector will consist of 1600 water Cerenkov detectors spaced 1.5 km apart on a 3000 km2 site in Mendoza, Argentina. A discussion of the design and results from deployment of an engineering array are presented.
Stephane Coutu, S. Barwick, A. Bhattacharyya, James Beatty, C. Bower, C. Chaput, G. De Nolfo, Don Ellithorpe, D. Ficenec, J. Knapp, D. Lowder, Steven McKee, Dietrich Mueller, J. Musser, S. Nutter, E. Schneider, Simon Swordy, K. Tang, Gregory Tarle, Andrew Tomasch, E. Torbet
The high-energy antimatter telescope (HEAT) instrument has been flown successfully by high-altitude balloon in 1994 and 1995, in a configuration optimized for the detection and identification of cosmic-ray electrons and positrons at energies from about 1 GeV up to 50 GeV and beyond. It consists of a two-coil superconducting magnet and a precision drift-tube tracking hodoscope, complemented with a time-of-flight system, a transition radiation detector and an electromagnetic shower counter. We review the design criteria for optimal e+/- detection and identification, and assess the instruments' performance and background rejection during its first two flights. We also review the adaptation of HEAT for measurements of high-energy cosmic- ray antiprotons and for isotopic composition studies.
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