This work presents the conceptual design of a wavefront sensor utilizing the double-roof pyramid prism proposed for the On-Instrument Wavefront Sensor (OIWFS) within the Giant Magellan Telescope Multi-Object Astronomical and Cosmological Spectrograph (GMACS). It details the design process, presents simulation methods and results to verify the sensor’s performance, and investigates the sensor’s precision and limits by the telescope primary segments tilt to be estimated. The results of the simulations show that the pyramidal sensor has sufficient sensitivity to measure misalignment between the primary segments of up to 3μrad with an error of less than 5% and proved to be effective in estimating the wavefront slope for these limits. The optical model generated images of the exit pupil on the detector in compliance with the precautions demonstrated regarding field rotation, lateral color distortions, differential distortions, and pupil misalignments. The mechanical model resulted in an instrument that allows a complete scan over the external field intended for the search for a guide star and a detailed mechanical design for the manufacture of the pyramidal prisms. Opto-mechanical COTS elements were presented to exemplify the system. This contribution adds to the ongoing development of adaptive optics technology for GMACS on the Giant Magellan Telescope (GMT).
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