X-ray interferometric observatory

Details X-ray interferometric observatory X-ray interferometric observatory

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991spie.1549..203m&link_type=abstract

Proc. SPIE Vol. 1549, p. 203-220, EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy II, Oswald H. Siegmund; Richard E. Rot

Astronomy and Astrophysics

Astronomy

Scientific paper

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 10(superscript 5) 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.

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