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Intensity interferometry, based on the Hanbury Brown-Twiss effect, is asimple and inexpensive method for optical interferometry at microarcsecondangular resolutions; its use in astronomy was abandoned in the 1970s because oflow sensitivity. Motivated by recent technical developments, we argue that thesensitivity of large modern intensity interferometers can be improved byfactors up to approximately 25,000, corresponding to 11 photometric magnitudes,compared to the pioneering Narrabri Stellar Interferometer. This is madepossible by (i) using avalanche photodiodes (APD) as light detectors, (ii)distributing the light received from the source over multiple independentspectral channels, and (iii) use of arrays composed of multiple large lightcollectors. Our approach permits the construction of large (with baselinesranging from few kilometers to intercontinental distances) opticalinterferometers at the cost of (very) long-baseline radio interferometers.Realistic intensity interferometer designs are able to achieve limiting R-bandmagnitudes as good as ~14, sufficient for spatially resolved observations ofmain-sequence O-type stars in the Magellanic Clouds. Multi-channel intensityinterferometers can address a wide variety of science cases: (i) linear radii,effective temperatures, and luminosities of stars; (ii) mass-radiusrelationships of compact stellar remnants; (iii) stellar rotation; (iv) stellarconvection and the interaction of stellar photospheres and magnetic fields; (v)the structure and evolution of multiple stars; (vi) direct measurements ofinterstellar distances; (vii) the physics of gas accretion onto supermassiveblack holes; and (viii) calibration of amplitude interferometers by providing asample of calibrator stars.

Optical Multi-Channel Intensity Interferometry - or: How To Resolve O-Stars in the Magellanic Clouds