In this investigation, a polarization multiplexing technique is applied to optical testing, especially shearing interferometers, low coherence interferometers and a clocking motion interpreter. Polarization multiplexing techniques possess the snapshot capability in interferometers and polarization imaging devices, and can enhance the measurement speed compared to the conventional optical techniques, which needs a timely-mannered procedure. Experimental results show the various application of the polarization multiplexing technique and give some insight to be used in optical testing area.
The search for artificial and natural objects in both cis-lunar and trans-lunar space has grown increasingly important. To accurately detect and track small objects, stray light mitigation is a necessity. Observations conducted in 2022 from a ground-based telescope intended to track such objects have been hampered by excess lunar stray light. In this paper, we present work done to resolve this problem by applying black pigments to the optical tube and thus suppressing its surface scattering. A non-sequential ray tracing model was created to analyze the telescope’s final focal plane irradiance. This model was used to identify critical and illuminated surfaces to determine the stray light paths that have affected observations. We conducted experimental tests to measure the Bidirectional Reflectance Distribution Function (BRDF) of various practical, readily available, and robust black coatings, including paints such as Black 3.0 and Musou. After application on the actual telescope tube, the new surface coating reduced the photon count on the detector from a variable-angle off-axis point source by 76% over all angles measured.
OASIS (Orbiting Astronomical Satellite for Investigating Stellar Systems) is a space-based, MIDEX mission concept that employs a 14 meter inflatable aperture and cryogenic heterodyne receivers to perform high resolution (R<106) observations at terahertz frequencies. OASIS targets far-infrared transitions of H2O and its isotopologues, as well as HD and other molecular species from 660 to 63 μm that are otherwise obscured by the Earth’s atmosphere. OASIS will have <10x the collecting area and <4x the angular resolution of Herschel and complements the short wavelength capabilities of JWST. With its large collecting area and suite of terahertz heterodyne receivers, OASIS will have the sensitivity to follow the water trail from galaxies to oceans. OASIS represents a paradigm shift in the realization of large space apertures. Our paper will focus on how the development work for OASIS can be leveraged to realize a new generation of space telescopes.
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