$a$ and $b$.

![image](fig05.eps)

![\[fig:PIAACMC\_Subaru\_PSFs\] Simulated Subaru PIAACMC images of 5 point sources of equal brightness. The point sources are at coordinates (0;0), (1;0), (0;2), (-4;0) and (0;-8) in $/lambda/D$ units. A non-coronagraphic images (left) shows all five point sources. The partially transmissive central focal plane mask is visible in the intermediate focal plane image (center), where off-axis PSFs are distorted by the PIAA remapping. In the output focal plane image (right), the central source is fully canceled and the off-axis PSFs images are sharp thanks to the inverse PIAA optics. ](fig06.eps)

PIAACMC design examples
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### Centrally obscured pupils: Subaru Telescope pupil

The Subaru telescope pupil is representative of current large aperture astronomical telescopes, with a large central obstruction and thick spiders. Both features must be taken into account for the design of a high performance coronagraph.

Figure \[fig:PIAACMC\_Subaru\] shows two PIAACMC designs for the Subaru Telescope pupil. The small IWA design (left) was computed from the $b/2=0.6 \lambda/D$ beam remapping, and uses a small sub-$\lambda/D$ radius focal plane mask with high transmission. The large IWA design was computed from $b/2=1.2 \lambda/D$, adopts a larger mostly opaque focal plane mask, and relies on a stronger PIAA remapping. Both designs 