Grazing-incidence X-ray optics redirect X-rays by shallow specular reflections along mirror surfaces. Riccardo Giacconi's lecture describes coaxial paraboloidal and hyperboloidal mirrors using two reflections, and the later Einstein observatory's imaging capability. Focusing separates collecting area from detector area: the collected source signal can remain large while the detector background is drawn from a smaller region.[ref]
An ideal lossless geometrical optics calculation explains the shallow angle. Take vacuum refractive index one and a material with real refractive index , where . Let be the grazing angle measured from the surface. Snell's law written for angles from the normal requires . A propagating transmitted ray exists only if . Thus the ideal threshold isThe last step uses the Taylor series . For a chosen , radians, or . Absorption makes the refractive index complex and softens this ideal threshold; surface roughness and alignment errors also reduce throughput or worsen the point spread function. These are reasons to calibrate X-ray effective area and angular resolution, rather than assume that reflection is perfect.
The benefit can be quantified without specifying a historical telescope. Suppose a source retains fraction of its counts inside an extraction region, while a uniform detector background contributes counts over detector area . In the background-dominated limit of the same independent on-off model,Reducing by a factor of 100 at fixed and X-ray effective area improves this ideal ratio tenfold. A collimator restricts admitted directions; focusing optics bring selected rays together. An image also separates nearby sources and identifies clean background regions, connecting optical design directly to a better constrained inverse problem.
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