Imaging hot stars at very high angular resolution with intensity interferometry There has been a recent interest to revive Stellar Intensity Interferometry (SII) with future air Cherenkov telescope arrays. These large arrays with nearly 100 telescopes, and baselines ranging between a few tens of meters, to a kilometer, will probe stars at the sub-milliarcsecond scale at short visible wavelengths (~ 400 nm). Only the magnitude of the Fourier transform of the radiance distribution of the star is accessible in SII. However, recent developments in phase recovery will allow for model independent images to be recovered. Hot stars are of particular interest in SII due to their high spectral density and therefore high signal-to-noise ratio. The capabilities and limitations of air Cherenkov telescope arrays used to image hot stars are discussed.