Advances in optical and near-infrared (NIR) instrumentation for astronomy, from modest early telescopes to today’s cryogenically cooled instruments on 10-meter-class observatories, have continually expanded our understanding of the universe. Modern systems now combine large primary mirrors, adaptive optics (AO) to correct for atmospheric distortion, and integral field spectrographs (IFS) that provide spatially resolved spectra. Together, these technologies enable transformative capabilities across a wide range of science cases.
This thesis presents the design and development of Liger, a second-generation AO-fed IFS for the W. M. Keck Observatory. Liger builds on the design of the InfraRed Imaging Spectrograph (IRIS), the first-light instrument for the Thirty Meter Telescope (TMT), and adapts it for Keck using new re-imaging optics and a custom-designed imager. I detail the mechanical design of the imager subsystem, including the characterization chamber, baffling, kinematic mounting system, pupil-viewing camera, and detector mount. The design is validated through structural analysis using SolidWorks Simulation, and I report on fabrication progress and plans for future characterization.
A key innovation of the Liger imager is a mounting system that positions pick-off mirrors directly above the detector to redirect light from the imager focal plane to the spectrograph. This enables simultaneous imaging and integral field spectroscopy, allowing for advanced techniques such as using imager-derived point spread function (PSF) data to improve IFS data reduction.
In addition to hardware, I developed end-to-end data simulation software to predict Liger’s sensitivity to both point and extended sources, benchmarking performance against other world-class observatories. I present sensitivity estimates for the imager and all IFS modes using point sources, and validate results by comparing simulated outputs to real observations of resolved sources. I also discuss how variations in PSF parameters affect measurements of galaxy properties such as the Sérsic index.
This work advances the design and scientific capabilities of AO-fed IFS instruments. Liger lays a foundation for future innovations on current 8–10 meter-class telescopes and the next generation of 30-meter-class observatories. My contributions to instrument design and modeling support more precise, efficient, and far-reaching high-resolution astrophysics.