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Address correspondence to R. D. Jackson, U.S. Water Conservation Lab., 4431 E. Broadway Rd., Phoenix, AZ 85040. Received 16 March 1990; revised 26 June 1990. and gypsum sand. Results are presented in terms of relative bidirectional reflectance factors (BRFs) as a function of view angle at a number of solar zenith angles, nadir BRFs as a function of solar zenith angles, and, for wheat, vegetatio...

One major problem of phase-referencing VLBI observations are phase errors due to the unknown tropospheric zenith delay at each antenna. These errors degrade the quality of the phase-referenced image and limit the achievable astrometric accuracy. We will present and compare two independent methods to estimate the zenith delay offset at each antenna. The zenith delay offsets can then be used to c...

An experimental investigation of ir sky radiance and radiance fluctuations in the 8-13-micro atmospheric window is reported. Measurements were made with ground-based, filtered bolometer detector radiometers under clear sky and cirrus overcast conditions. Sky radiance was measured very close to the limb of the sun to permit detection of the solar aureole caused by forward scattering by cirrus ic...

TeV gamma rays from the blazar Markarian 501 have been detected with the University of Durham Mark 6 atmospherič Cerenkov telescope using the imaging technique at large zenith angles. Observations were made at zenith angles in the range 70 • − 73 • during 1997 July and August when Markarian 501 was undergoing a prolonged and strong flare.

March 197-i ABSTR.ACT The flux of atmospheric muons as a function of momentum and zenith angle is measured for p > 0.3 TeV and 60" < 8 C 87.. Special attention is given the angular distribution above. 1 TeV. In 1967, Bergeson et al. [i] published data from an underground cosmic ray experiment, suggesting that a new process is occurring in nucleon-nudleon interactions at energies of several TeV....

The analytical expression for integral energy spectra and zenith angle distributions of atmospheric muons at large depths is derived. Fluctuations of muon energy losses are described using the parametrized correction factor. The fitting formula for the sea level muon spectrum at different zenith angles for spherical atmosphere is proposed. The concrete calculations for pure water are presented.