Translator Disclaimer
1 October 1991 X-ray interferometric observatory
Author Affiliations +
X-ray interferometry has the potential for observations of unprecedented angular resolution and far-reaching astrophysical consequences. A new concept for an x-ray interferometric observatory that obtains an angular resolution 105 times better than AXAF is presented. Using a grazing incidence fringe spectrum design, the x-ray interferometer operates over a broad band (0.2 - 8 keV), with on the order of magnitude 18 concentric Wolter-Schwarzschild mirror shells of diameter 0.6 - 2.4 m. A fringe-sensitive detector measures the closely spaced Fizeau fringes in the focal plane. Fringe phasing is maintained using an optical metrology system and two optical Michelson stellar interferometers to provide absolute inertial reference for the phase tracking center. Mirror phasing is maintained with active control of low spatial frequency figure errors. The interferometer is capable of obtaining detailed images of nearby stellar coronae, imaging the broad-line regions and jets of many AGNs, and resolving the accretion disks of a selection of bright AGNs and QSOs.
© (1991) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Christopher Martin "X-ray interferometric observatory", Proc. SPIE 1549, EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy II, (1 October 1991);


X-ray interferometry: ultra-high-resolution astronomy
Proceedings of SPIE (December 20 2001)
Maxim: micro-arcsecond x-ray imaging mission
Proceedings of SPIE (February 26 2003)
MAXIM Pathfinder: a practical configuration
Proceedings of SPIE (January 29 2004)
The status of the Constellation-X mission
Proceedings of SPIE (September 18 2007)
The optical demonstration of an x-ray interferometer
Proceedings of SPIE (October 07 2005)
Formation-flying interferometry
Proceedings of SPIE (February 26 2003)

Back to Top