Characterization of microdot apodizers for imaging exoplanets with next-generation space telescopes

A major science goal of future, large-aperture, optical spacetelescopes is to directly image and spectroscopically analyze reflected light from potentially habitable exoplanets. To accomplish this, the optical system must suppress diffracted light from the star to reveal point sources approximately ten orders of magnitude fainter than the host star at small angular separation. Coronagraphswith microdot apodizersachieve the theoretical performance needed to image Earth-like planets with a range of possible telescope designs, including those with obscured and segmented pupils. A test microdot apodizerwith various bulk patterns ( step functions, gradients, and sinusoids) and 4 different dot sizes (3, 5, 7, and 10 $\mu$m) made of small chrome squares on anti-reflective glass was characterized with microscopy, optical laser interferometry, as well as transmission and reflectance measurements at wavelengths of 600 and 800 nm. Microscopy revealed the microdotswere fabricated to high precision. Results from laser interferometry showed that the phase shifts observed in reflection vary with the local microdot fill factor. Transmission measurements showed that microdot fill factorand transmission were linearly related for dot sizes >5 $\mu$m. However, anomalously high transmittance was measured when the dot size is <5x the wavelength and the fill factoris approximately 50%, where the microdotpattern becomes periodic. The transmission excess is not as prominent in the case of larger dot sizes suggesting that it is likely to be caused by the interaction between the incident field and electronic resonances in the surface of the metallic microdots. We used our empirical models of the microdot apodizersto optimize a second generation of reflective apodizerdesigns and confirmed that the amplitude and phase of the reflected beam closely matches the ideal wavefront.