The design of x-ray telescopes is roughly classified into two types based on the mirror configuration, focusing on high spatial resolution and large effective area. High spatial resolution mirrors are fabricated by polishing thick quartz or zero-Dewar glass substrates to form Wolter-I optics with a high precision. These optics are mounted on x-ray observatories, such as Einstein,1 ROSAT,2 and Chandra.3 These telescopes have high angular resolution of several or sub arc seconds, but they require a large diameter to have a large effective area because the thick substrate causes a dead area in the mirror. On the other hand, mirrors with large effective areas are formed by nested thin substrates made of aluminum foil and are mounted on Japanese x-ray observatories, such as ASCA,4 Suzaku,5 and ASTRO-H.6,7 These telescopes have higher collecting area to weight ratios than other x-ray telescope designs, but the angular resolution of the telescopes is limited to . This limitation is caused, in part, by the approximate conical shape of the Wolter-I optics (paraboloid and hyperboloid), the positional error between the two stage mirrors, and deformation of the substrate itself. The approximation and the separation occurs because the aluminum foil cannot be formed to the original Wolter-I monolithic geometry.