Grazing incidence wavefront sensing and verification of x-ray optics performance

Saha, Timo T.; Rohrbach, Scott; Zhang, William W.; Evans, Tyler; Hong, M.

doi:10.1117/12.893404

Cited by 6 publications

(3 citation statements)

References 5 publications

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“…The results were very encouraging in that the mirror pair not only came in under the 15 arc-second boundary, but also under the 10 arc-second milestone. 8 • This improved the alignment iteration threshold from two arc-seconds, to one arc-second. In the bonding lab, the ceiling light above the VAF was removed to help stabilize temperature, and the lights were kept off as much as possible.…”

Section: Glass 30 Degree Mhs January Permanent Bonding and X-ray Testmentioning

confidence: 99%

Alignment and integration of lightweight mirror segments

et al. 2011

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The optics for the International X-Ray Observatory (lXO) require alignment and integration of about fourteen thousand thin mirror segments to achieve the mission goal of 3.0 square meters of effective area at 1.25 keY with an angUlar resolution of five arc-seconds. These mirror segments are 0.4 mm thick, and 200 to 400 mm in size, which makes it difficult not to impart distortion at the sub-arc-second level. This paper outlines the precise alignment, permanent bonding, and verification testing techniques developed at NASA's Goddard Space Flight Center (GSFC). Improvements in alignment include new hardware and automation software. Improvements in bonding include two module new simulators to bond mirrors into, a glass housing for proving single pair bonding, and a Kovar module for bonding multiple pairs of mirrors. Three separate bonding trials were x-ray tested producing results meeting the requirement of sub ten arc-second alignment . This paper will highlight these recent advances in alignment, testing, and bonding techniques and the exciting developments in thin x-ray optic technology development.

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Section: Glass 30 Degree Mhs January Permanent Bonding and X-ray Testmentioning

confidence: 99%

Alignment and integration of lightweight mirror segments

et al. 2011

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“…It copies the figure of conventionally fabricated mandrels to cOlllIJlercially procured (Schott D263) thin (-0.4 mm) float glass sheets while preserving their excellent micro-roughness (-4A rms measured over a 300 /lm span). As shown in Figure 2 (right panel), it has been able to make mirror substrates consistently at -6.5 are-seconds (HPD); Each entry in the histogram represents a substrate pair which has been precisely measured with optical metrology [19,20,21,22,23,24] and whose x-ray imaging performance calculated with standard performance prediction techniques. The glass slumping process is capable of making substrates the meet the requirements of a sub-l0 arc-second mirror assembly: It has been used to making the more than 10,000 substrates for the NuST AR mission [7].…”

Section: Technical Approaches and Statusmentioning

confidence: 99%

Next generation astronomical x-ray optics: high angular resolution, light weight, and low production cost

et al. 2012

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X-ray astronomy depends on the availability of telescopes with high resolution and large photon collecting areas. Since x-ray observation can only be carried out above the atmosphere, these telescopes must be necessarily lightweight. Compounding the lightweight requirement is that an x-ray telescope consists of many nested concentric shells, which further require that x-ray mirrors must also be geometrically thin to achieve high packing efficiency. This double lightweight and geometrically thin requirement poses significant technical challenges in fabricating the mirrors and in integrating them into mirror assemblies. This paper reports on the approach, strategy and status of our x-ray optics development program whose objective is to meet these technical challenges at modest cost to enable future x -ray missions, including small Explorer missions in the near term, probe class missions in the medium term, and large flagship missions in the long term.

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“…Ray tracing software implemented in the optical analysis of the deformed mirror models use approximate ray trace equations described by Saha et.al [5]. This ray trace analysis introduces several assumptions in the analysis process.…”

Section: Modeling Assumptionsmentioning

confidence: 99%

Size optimization for mirror segments for X-ray optics

et al. 2011

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The flight mirror assemblies (FMA) for X-ray telescopes similar to that of the International X-ray Observatory (IXO) concept consist of several thousands of individual mirror segments. The size, shape, and location of these mirrors affect many characteristics of the telescope design. Mission requirements among other factors in turn restrict mirror segment parameters such as thickness, axial-length, azimuthal span, and mass density. This paper provides an overview of the critical relationships relating to mirror segment size and configuration throughout the design and analysis of an X-ray mirror assembly. A computational analysis is presented in the form of ray tracing pairs of thin X-ray mirror segments of varying sizes aligned in gravity and supported using kinematic constraints with corresponding self weight distortions calculated using finite element analysis (FEA). The work in this paper may be used as a starting point for determining mirror segment sizes for X-ray missions like that ofIXO and beyond.

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Grazing incidence wavefront sensing and verification of x-ray optics performance

Cited by 6 publications

References 5 publications

Alignment and integration of lightweight mirror segments

Alignment and integration of lightweight mirror segments

Next generation astronomical x-ray optics: high angular resolution, light weight, and low production cost

Size optimization for mirror segments for X-ray optics

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