Non-redundant Masking (NRM) on JWST FGS-TFI

Details Non-redundant Masking (NRM) on JWST FGS-TFI Non-redundant Masking (NRM) on JWST FGS-TFI

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21335003s&link_type=abstract

American Astronomical Society, AAS Meeting #213, #350.03; Bulletin of the American Astronomical Society, Vol. 41, p.486

Physics

Optics

Scientific paper

The 7-hole non-redundant mask in FGS-TFI will deliver at least 10 magnitudes of dynamic range between 0.1 and 0.4 arcsec at 3.8 um and longer wavelengths, using routine target acquisition, observing sequences, and pipeline data calibraton. This places protoplanets in Taurus within JWST's purview, opening up a search space inaccessible to JWST coronagraphs and future 30-m extremely large telescopes, especially in the mid-IR. NRM will also enable milliarcsecond astrometry on JWST.
On the ground NRM mitigates speckle noise. On JWST it will deliver unsurpassed contrast while reducing JWST mission risk induced by the telescope's segmented, deployable primary mirror and wavefront sensing schemes. NRM will image the vicinity of an M=7 star in 10ks, meshing with next-generation extreme adaptive optics coronagraphs. Targets as bright as M=3 will also be observable with NRM on JWST.

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