Direct detection of earth-like planets using an internal coronagraph will require telescope wavefront stability on the order of ~ 10 picometers over a time scale of ~ 10 minutes. Passive wavefront stability of a space telescope at this level has never been demonstrated, yet active sensing and control is feasible. However, the sensing must be done during the science observation, and with a minimum of non-common path errors. The sensing and control must be done where it matters most – at the location of the focal plane mask. We have architected such a device, that will enable both of these capabilities. There are three key components of this optical element: 1) the coronagraphic field stop 2) the Zernike phase dimple and 3) the dielectric coating/antireflection surface. We will discuss the design and engineering of these key components, with an emphasis on the first iteration of the actual devices. We will also provide characterization of these devices in our metrology setup. Status of the testing and characterization of these devices in the vacuum, high-contrast optical testbed will also be discussed.
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