&lt;title&gt;Newly modified cryogenic optical test facility at Marshall Space Flight Center&lt;/title&gt;

Eng, Ron; Kegley, Jeffrey R.; Keidel, John W.

doi:10.1117/12.406547

Cited by 6 publications

(3 citation statements)

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“…The test optics may remain in the horizontal orientation, with the optical axis vertical, which greatly reduces the gravity distortions of the test optics. Due to the collimation, the X-ray source appears to be at infinity, avoiding the problems of partial illumination due to vignetting vignetting and focus shift due to a divergent beam, as encountered in conventional facilities like XRCF [43] or PANTER.…”

Section: Next Stepsmentioning

confidence: 99%

ATHENA optics technology development

Bavdaz¹,

Wille²,

Ayre³

et al. 2022

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray

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The next generation X-ray observatory ATHENA (Advanced Telescope for High ENergy Astrophysics) requires an optics with unprecedented performance. It is the combination of low mass, large effective area and good angular resolution that is the challenge of the X-ray optics of such a mission. ATHENA is the second Large Class mission in the Science Programme of ESA, and is currently in a reformulation process, following a design-to-cost approach to meet the cost limit of an ESA L-class mission.The Silicon Pore Optics (SPO) is the mission enabler being specifically developed for ATHENA, in a joint effort by industry, research institutions and ESA. All aspects of the optics are being addressed, from the mirror plates and their coatings, over the mirror modules and their assembly into the ATHENA telescope, to the facilities required to build and test the flight optics, demonstrating performance, robustness, and programmatic compliance.The SPO technology is currently being matured to the level required for the adoption of the ATHENA mission, i.e., the start of the mission implementation phase. The monocrystalline Silicon material and pore structure of the SPO provide this optics with excellent thermal and mechanical properties. Benefiting from technology spin-in from the semiconductor industry, the equipment, processes, and materials used to produce the SPO are highly sophisticated and optimised.

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Section: Next Stepsmentioning

confidence: 99%

ATHENA optics technology development

Bavdaz¹,

Wille²,

Ayre³

et al. 2022

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray

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“…This measurement is similar, though not precisely identical, to measuring the surface normal piston motion of each PMSA fitting. 14 . The SPS-DSPI was used to collect the critical measurement data.…”

Section: Backplane Stability Test Article (Bsta)mentioning

confidence: 99%

Development of electronic speckle pattern interferometry for testing JWST composite structures

et al. 2007

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The stability requirements for the James Webb Space Telescope (JWST) optical metering structure are driven by the science objectives of the mission. This structure, JWST Optical Telescope Element (OTE) primary mirror backplane, has to be stable over time at cryogenic temperatures. Successful development of the large, lightweight, deployable, cryogenic metering structure requires verification of structural deformations to nanometer level accuracy in representative test articles at cryogenic temperature. An instantaneous acquisition phase shifting speckle interferometer was designed and built to support the development of JWST Optical Telescope Element (OTE) primary mirror backplane. This paper discusses characterization of the Electronic Speckle Pattern Interferometer (SPS-DSPI) developed for JWST to verify its capabilities to measure structural deformations in large composite structures at cryogenic temperature. Interferometer performance during the Backplane Stability Test Article (BSTA) test that completed the TRL-6 (Technology Readiness Level-6) demonstration of Large Precision Cryogenic Structures will also be discussed.

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“…Modifications after Chandra added the ability to optically evaluate structures and direct-incidence optics in relevant thermal environments from 300 to 20 Kelvin; these additional capabilities were utilized by James Webb Space Telescope from 2005 to 2015. Details of the facility's existing x-ray and cryogenic testing capabilities can be found in [1] and [2].…”

Section: Introductionmentioning

confidence: 99%

Capability improvements at the Marshall Space Flight Center's x-ray and cryogenic facility

Kegley,

Abbot,

Baumgartner

et al. 2023

Optics for EUV, X-Ray, and Gamma-Ray Astronomy XI

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The X-Ray and Cryogenic Facility (XRCF) at Marshall Space Flight Center is the world’s largest x-ray optic calibration facility and NASA’s premier cryogenic optical test facility. Built specifically to calibrate the Chandra telescope, the facility contributed to several other x-ray missions until 2005 when it became dedicated to normal incidence optical testing at cryogenic temperatures. Recently the facility’s x-ray test capability has been returned to service and updated. New beam monitors, focal plane detectors, and test article and instrument positioning systems have been added. The x-ray data acquisition system has been updated. A real-time position monitoring metrology system is being developed that will enable calibration of large diameter optics via partial illumination in a diverging beam. The newly expanded x-ray test capabilities of the facility will be discussed.

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<title>Newly modified cryogenic optical test facility at Marshall Space Flight Center</title>

Cited by 6 publications

References 0 publications

ATHENA optics technology development

ATHENA optics technology development

Development of electronic speckle pattern interferometry for testing JWST composite structures

Capability improvements at the Marshall Space Flight Center's x-ray and cryogenic facility

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