AO4ELT5 Proceedings

Phasing the GMT with a next generation e-APD dispersed fringe sensor: design and on-sky prototyping

Kopon, Derek (Harvard-Smithsonian Center for Astrophysics), McLeod, Brian (Harvard-Smithsonian Center for Astrophysics), Bouchez, Antonin (GMTO Corporation), Catropa, Daniel (Harvard-Smithsonian Center for Astrophysics), van Dam, Marcos A. (Flat Wavefront), McCracken, Ken (Harvard-Smithsonian Center for Astrophysics), McMuldroch, Stuart (Harvard-Smithsonian Center for Astrophysics), Podgorski, William (Harvard-Smithsonian Center for Astrophysics), D’Arco, Joseph (Harvard-Smithsonian Center for Astrophysics), Close, Laird (Steward Observatory, University of Arizona), Males, Jared (Steward Observatory, University of Arizona), Morzinski, Katie (Steward Observatory, University of Arizona)

The GMT will be a 25.4-meter telescope consisting of 7 primary and secondary mirror segments that must be phased to within a fraction of an imaging wavelength in order to achieve diffraction limited performance. The need to use off-axis guide stars, coupled with the large (350 mm) segment gaps, makes the task of phasing the GMT uniquely challenging. To meet these requirements, the Acquisition, Guiding, and Wavefront Sensing system (AGWS) will use four J-band dispersed fringe sensors (DFS) to measure segment piston at each segment boundary. This DFS will use a novel array of doublet prisms, instead of grisms, to disperse segment boundary fringes with maximal throughput, minimal stray light, and no spurious diffractive orders. The DFS will also use a low noise SAPHIRA e-APD array reading out at ~100 Hz in order to freeze atmospheric turbulence in the segment boundary fringe images. We will test a prototype of this DFS on the Magellan Clay 6.5 meter telescope using an adaptive optics corrected beam from the MagAO system. We present the design of the next generation phasing prototype.

DOI: 10.26698/AO4ELT5.0101- Proceeding PDF

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