On-orbit performance of the fine guidance sensor FGS-1R

Chisholm, Kevin P.; Ftaclas, C.; Abramowicz-Reed, Linda

doi:10.1117/12.317119

Cited by 1 publication

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“…The modification required the replacement of a stationary fold flat mirror with one mounted on an articulating mechanism. This, now referred to as the Articulating Mirror Assembly (AMA) replaced the fold flat #3 (FF3) mirror in the original design 10 . By adjusting the tip/tilt of the AMA, it became possible to re-align the wavefront's tilt axis with the Koesters prism's dielectric surface, thereby mitigating the deleterious effects of the spherical aberration.…”

Section: Fgs1rmentioning

confidence: 99%

“…Provided that the axis of rotation of the wavefront at the face of the Koesters prism is perfectly aligned (in the same plane) with the dielectric surface within the prism (point "b" in figure 4), the interferometric response would be unaffected by spherical aberration. 1,10 However, small deviations In orbit tests of the FGSs were made to evaluate the impact of the OTA's spherical aberration upon the instruments' performance. Four facts soon became clear.…”

Section: Spherical Aberration and The Effect On The Fgsmentioning

confidence: 99%

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Fine guidance sensors aboard the Hubble Space Telescope: the scientific capabilities of these interferometers

et al. 1998

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The Fine Guidance Sensors (FGS) aboard the Hubble Space Telescope (HST) are optical white light shearing interferometers that offer a unique capability to astronomers. The FGSs's photometric dynamic range, fringe visibility, and fringe tracking ability allow the instrument to exploit the benefits of performing interferometry from a spacebased platform. The FGSs routinely provide HST with 2 milli-seconds of arc pointing stability. The FGS designated as the Astrometer, FGS3, has also been used to (1) perform 2 mas relative astrometry over the central 4 arc minutes of its field of view, (2) determine the true relative orbits of close (20mas) faint (m v =15) binary systems, (3) measure the angular diameter of a giant star, (4) search for extra-solar planets, (5) observe occultations of stars by solar system objects, as well as (6) photometrically monitor stellar flares on a low mass M dwarf. In this paper we discuss this unique instrument, its design, performance, and the areas of science for which it is the only device able to successfully observe objects of interest.

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Section: Fgs1rmentioning

confidence: 99%

Section: Spherical Aberration and The Effect On The Fgsmentioning

confidence: 99%