Performance predictions of a Schwarzschild imaging microscope for soft x‐ray applications

Harvey, James E.; Lewotsky, Kristin; Kotha, Anita

doi:10.1117/1.601011

Cited by 10 publications

(2 citation statements)

References 23 publications

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“…The rms radius of the resulting image is just the root-sum-square ͑rss͒ of the geometrical rms radius and the rms radius of the diffraction-limited PSF. 21 Figure 3 thus plots the reduction in rms image radius as a function of field angle for geometrical design errors only, and when including diffraction effects for two different wavelengths when going from an f /4 classical Cassegrain design to the aplanatic Ritchey-Chretien design. Even with diffraction effects included, the optical performance of the aplanatic Ritchey-Chretien telescope is far superior to that of the classical Cassegrain telescope.…”

Section: The Aplanatic Cassegrain Telescopementioning

confidence: 98%

Systems engineering analysis of aplanatic Wolter type I x-ray telescopes

Thompson

Harvey

2000

Opt. Eng

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It is well known that normal-incidence aplanatic telescope designs perform better at small field angles than ones corrected only for spherical aberration. This is why most large astronomical telescopes fabricated in the past fifty years have been of the Ritchey-Chretien (aplanatic) design rather than of the classical Cassegrain design. For the relatively new field of x-ray astronomy, the Wolter type I grazing incidence design has been extensively utilized. It consists of a paraboloidal primary mirror coaxial with a confocal hyperboloidal secondary mirror. Aplanatic versions of the Wolter type I grazing incidence x-ray telescope have been discussed in detail in the literature, and are widely touted as being superior designs. However, scattering effects from residual optical fabrication errors and other practical engineering error sources prevent these grazing-incidence telescopes from being near diffraction-limited (even on axis) at the very short operational x-ray wavelengths. A systems engineering analysis of these error sources indicates that they will dominate coma at the small field angles, and of course astigmatism, field curvature, and higher-order aberrations dominate coma at the large field angles. Hence, there is little improvement in performance when going to an aplanatic design. Comparison of performance predictions for the classical versus aplanatic Wolter type I x-ray telescope are presented for the special case of the Solar X-Ray Imager (SXI) baseline design. SXI is expected to become a standard subsystem aboard the next generation of NOAA/GOES weather satellites. © 2000 Society of Photo-Optical Instrumentation Engineers. [S0091-3286(00)

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Section: The Aplanatic Cassegrain Telescopementioning

confidence: 98%

Systems engineering analysis of aplanatic Wolter type I x-ray telescopes

Thompson

Harvey

2000

Opt. Eng

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“…A number of X-ray space missions (Aschenbach 1988;Citterio et al 1988;Gondoin et al 1994;Weisskopf et al 2000;Gehrels et al 2004;Pareschi & Ferrando 2005;Bookbinder et al 2008;Friedrich et al 2008) have stimulated both theoretical and experimental research (Spiller 1994;Church & Takacs 1995, 1993Harvey 1995a;Harvey et al 1996;Stearns et al 1998;Harvey 1995b;Christensen et al 1988;Karabacak et al 2000;Zhao & Spreybroeck 2003) to understand and characterize in a more robust way the scattering of electromagnetic waves from rough surfaces. The typical resolution requirement at the focal plane of an X-ray telescope is sharper than 20 half energy width at X-ray photon energy between 0.1 keV and 80 keV, depending on the mission (Gondoin et al 1994;Pareschi & Ferrando 2005;Friedrich et al 2008), and at a grazing-incidence angle in the range between about 0.1…”

Section: Introductionmentioning

confidence: 99%

Roughness scattering in X-ray grazing-incidence telescopes

Zocchi¹

2009

A&A

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In the framework of the scalar theory of diffraction, we determine the rms width of the angle spread function degraded by surface roughness in reflective grazing-incidence optics of cylindrical symmetry for X-ray astronomy. Our derivation does not rely on the small roughness approximation, is thus valid for arbitrary roughness values, and takes into full consideration the cylindrical symmetry of the mirrors. The dependence of the rms beam width on both the grazing-incidence angles and the radiation wavelength is studied for both single and double reflection optics, the latter being more relevant to X-ray telescopes. When the small roughness approximation is applicable, we also derive an expression for the angle spread function of the optical system in the presence of roughness scattering that provides the correct expression for the rms beam width.

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Nonspecular scattering from extreme ultraviolet multilayer coatings

Stearns¹,

Gullikson

2000

Physica B: Condensed Matter

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Performance predictions of a Schwarzschild imaging microscope for soft x‐ray applications

Cited by 10 publications

References 23 publications

Systems engineering analysis of aplanatic Wolter type I x-ray telescopes

Systems engineering analysis of aplanatic Wolter type I x-ray telescopes

Roughness scattering in X-ray grazing-incidence telescopes

Nonspecular scattering from extreme ultraviolet multilayer coatings

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