Several angular diameter-redshift tests are provided with models of evolution to confirm the galaxy results. Galaxy counts and redshift distributions are found to be in agreement with the later up to 0.25z, where the existence of a local hole has been recently proposed at optical and near infrared wavelengths. These precise luminosity functions are applied to determine the necessary evolution for LCDM and universe with global gravitational potential. Local morphological luminosity functions are derived from several surveys and transformed to the BRIHK-bands through color-magnitude relations. Substantial evidence of a global gravitational potential is discussed including galaxy counts, angular size-redshift relations, SNIa and large-scale B-mode polarization within the cosmic background radiation. We compare the resulting stellar radius with empirically derived estimates from temperature and brightness measurements, confirming the latter can be biased for stars with ambiguous stellar classifications. This is a resolution never achieved before with optical measurements and represents an order of magnitude improvement over the equivalent lunar occultation method. Here we report two occultations of stars observed by the VERITAS Cherenkov telescopes with millisecond sampling, from which we are able to provide a direct measurement of the occulted stars' angular diameter at the $\leq0.1$ milliarcsecond scale. However, their large mirror area makes them well suited for such high-time-resolution precision photometry measurements. Atmospheric Cherenkov telescopes used for particle astrophysics observations have not generally been exploited for optical astronomy due to the modest optical quality of the mirror surface. This fundamental limitation can be overcome by studying the diffraction pattern in the shadow cast when an asteroid occults a star, but only when the photometric uncertainty is smaller than the noise added by atmospheric scintillation. Direct measurement of stellar angular diameters is difficult: at interstellar distances stars are generally too small to resolve by any individual imaging telescope. The angular size of a star is a critical factor in determining its basic properties.
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