John F. Meekins, Herbert Gursky, and Raymond G. Cruddace, "Optimization of the Rowland circle grating for high-resolution astrophysical spectrometers working at soft x-ray and EUV wavelengths," Appl. Opt. 24, 2987-2995 (1985)
The continued maturation of x-ray and EUV astronomy has created a requirement for high-resolution spectroscopy to resolve spectral features and measure line profiles and Doppler shifts. We consider in this paper the familiar fixed-grating spectrometer (Rowland configuration) operating at grazing incidence behind the focus of a grazing-incidence telescope. By optimizing the grating shape and grating-detector geometry, we find that a peak resolving power near 104 and greater should be achievable in the 50–500-Å band. An important innovation to the standard configuration is the addition of an elliptical mirror. The optimization technique used is adaptable to other geometries as well as other applications in which a fixed grating is desired.
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Line density varies in accord with Eq. 7.
The optimization was performed under the constraint that λ0 = 145 Å to force the peak in the resolving power distribution to shorter wavelengths.
Image loci are formed on right circular cylinders (to within a rms value of 200 μm). The x and z positions of the axis of the cylinder are in the coordinate system of Fig. 1.
Table IV
Constraints on the Source Diameter Sap and Detector Spatial Resolution Sdet for the Spectrometer to Achieve the Resolving Power P of the Optimized Grating
Line density varies in accord with Eq. 7.
The optimization was performed under the constraint that λ0 = 145 Å to force the peak in the resolving power distribution to shorter wavelengths.
Image loci are formed on right circular cylinders (to within a rms value of 200 μm). The x and z positions of the axis of the cylinder are in the coordinate system of Fig. 1.
Table IV
Constraints on the Source Diameter Sap and Detector Spatial Resolution Sdet for the Spectrometer to Achieve the Resolving Power P of the Optimized Grating