Systems engineering analysis of five 'as-manufactured' SXI telescopes

Harvey, James E.; Atanassova, Martina; Krywonos, Andrey

doi:10.1117/12.622376

Cited by 5 publications

(4 citation statements)

References 10 publications

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“…For completeness, the table includes (in the shaded rows) information on orbiting high-resolution x-ray telescopes for solar-physics research (Yohkoh SXT 56,57,58 and Hinode XRT 59,60 ) and for space-weather monitoring (GOES SXI 61,62,63 ). However, such solar x-ray telescopes are much smaller and less complex than those needed for x-ray astronomy.…”

Section: Past and Current Missionsmentioning

confidence: 99%

High-resolution x-ray telescopes

O’Dell¹,

Brissenden

Davis

et al. 2010

SPIE Proceedings

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High-energy astrophysics is a relatively young scientific field, made possible by space-borne telescopes. During the half-century history of x-ray astronomy, the sensitivity of focusing x-ray telescopes-through finer angular resolution and increased effective area-has improved by a factor of a 100 million. This technological advance has enabled numerous exciting discoveries and increasingly detailed study of the high-energy universe-including accreting (stellar-mass and super-massive) black holes, accreting and isolated neutron stars, pulsar-wind nebulae, shocked plasma in supernova remnants, and hot thermal plasma in clusters of galaxies. As the largest structures in the universe, galaxy clusters constitute a unique laboratory for measuring the gravitational effects of dark matter and of dark energy. Here, we review the history of high-resolution x-ray telescopes and highlight some of the scientific results enabled by these telescopes. Next, we describe the planned next-generation x-ray-astronomy facility-the International X-ray Observatory (IXO). We conclude with an overview of a concept for the next next-generation facility-Generation X. The scientific objectives of such a mission will require very large areas (about 10000 m2) of highly-nested lightweight grazing-incidence mirrors with exceptional (about 0.1-arcsecond) angular resolution. Achieving this angular resolution with lightweight mirrors will likely require on-orbit adjustment of alignment and figure.Comment: 19 pages, 11 figures, SPIE Conference 7803 "Adaptive X-ray Optics", part of SPIE Optics+Photonics 2010, San Diego CA, 2010 August 2-

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Section: Past and Current Missionsmentioning

confidence: 99%

High-resolution x-ray telescopes

O’Dell¹,

Brissenden

Davis

et al. 2010

SPIE Proceedings

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“…This yields a systems engineering analysis of the quality of the aerial image produced in the telescope focal plane. 10,17 However, as indicated by Fig. 3, we have yet to accurately model the detector effects.…”

Section: Systems Engineering Analysis Of Image Qualitymentioning

confidence: 99%

“…However, the image quality criterion for a wide-field imaging application should be expressed in terms of some field-weighted-average "resolution" over a predetermined OFOV. [11][12][13][14][15][16][17][18][19][20] This is certainly the case for the SXI telescope operating in a staring mode, recording and transmitting full solar disk-images of solar flare activity for study by NOAA scientists and solar physicists. Specifically, we will choose the field-weighted-average half power radius ͑HPR fwa ͒ of the DPSFs discussed in the previous section.…”

Section: Image Quality Criteria For Wide-field Imaging Systemsmentioning

confidence: 99%

Balancing detector effects with aberrations in the design of wide-field grazing incidence x-ray telescopes

2006

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Most imaging systems today include a mosaic detector array in the focal plane. Optical designers of astronomical telescopes typically produce a design that yields a superb on-axis aerial image in the focal plane, and detector effects are included only in the analysis of the final system performance. Aplanatic optical designs ͑corrected for spherical aberration and coma͒ are widely considered to be superior to nonaplanatic designs. However, there is little merit in an aplanatic design for wide-field applications because one needs to optimize some fieldweighted-average measure of resolution over the desired operational field of view ͑OFOV͒. Furthermore, when used with a mosaic detector array in the focal plane, detector effects eliminate the advantage of the aplanatic design even at small field angles. For wide fields of view, the focal plane is frequently despaced to balance field curvature with defocus thus obtaining better overall performance. We will demonstrate that including detector effects in the optical design process results in a different optimal ͑nonaplanatic͒ design for each OFOV that is even superior to an optimally despaced aplanatic design.

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“…Goodman [4] has shown that a similar linear systems approach to image analysis as degraded by diffraction and geometrical aberrations is not strictly true, and Harvey and Krywonos [5] have quantitatively evaluated the assumption for different amounts of defocus. They then proceed to successfully apply the linear system formulation of image quality to the case of an x-ray telescope [6,7]. This paper confirms that the explicit expression for the system PSF is not rigorously true; however, it discusses the assumptions and approximations made in the mathematical formulation, explains why the explicit expression should be sufficiently accurate for most optical engineering applications, then goes on to numerically validate it for the specific application of a two-mirror extreme ultraviolet (EUV) telescope.…”

Section: Introductionmentioning

confidence: 99%

Image degradation due to surface scatter in the presence of aberrations

Choi

Harvey

2012

Appl. Opt.

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Image analysis in the presence of surface scatter due to residual optical fabrication errors is often perceived to be complicated, nonintuitive, and achieved only by computationally intensive nonsequential ray tracing with commercial optical analysis codes such as ASAP, Zemax, Code V, TracePro, or FRED. However, we show that surface scatter can be treated very similarly to conventional wavefront aberrations. For multielement imaging systems degraded by both surface scatter and aberrations, the composite point spread function is obtained in explicit analytic form in terms of convolutions of the geometrical point spread function and scaled bidirectional scattering distribution functions of the individual surfaces of the imaging system. The approximations and assumptions in this formulation are discussed, and the result is compared to the irradiance distribution obtained using commercial software for the case of a two-mirror telescope operating at an extreme ultraviolet wavelength. The two results are virtually identical.

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Systems engineering analysis of five 'as-manufactured' SXI telescopes

Cited by 5 publications

References 10 publications

High-resolution x-ray telescopes

High-resolution x-ray telescopes

Balancing detector effects with aberrations in the design of wide-field grazing incidence x-ray telescopes

Image degradation due to surface scatter in the presence of aberrations

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