Hartmann mask

Abstract: In lateral shearing interferometry, interferograms with a good contrast can be obtained at any distance without self-imaging limitations based on a modified Hartmann mask (MHM) and a randomly encoded hybrid grating (REHG). The present study analyzes and compares the diffraction orders, the contrast of carrier fringes, the available spectral bandwidth, and the wavefront measurement accuracy of the lateral shearing interferometer using MHM and REHG. Numerical simulations show that the performance of the REHG is superior to that of the MHM with respect to fringe contrast, available spectral bandwidth, and wavefront measurement accuracy. For the REGH, if the phase step of the phase chessboard is within the range of (2n+1±0.2)π, the contrast of the carrier fringes is almost invariant along the propagation axis, and the wavefront reconstruction error generated from higher diffraction orders is small enough to be neglected. Optimal quantization of the REHG is also studied. When M is equal to 2 and N is not less than 5, the quantization result can meet the requirement of the measurement accuracy.

Abstract: The wavefront measurement is an important part both in adaptive optics and in optical shop testing. A number of wavefront sensors based on interferometric or on Hartmann principle is known; this thesis investigates particular technologies that can help to increase the accuracy and/or speed of existing wavefront sensors either by optimising the wavefront reconstruction algorithm or by optimising the hardware. The topics discussed are interferogram analysis, optimising of the Hartmann mask geometry, and design of a 2D heterodyne phase detector.

Abstract: Shack–Hartmann wavefront sensing in general requires careful registration of the reimaged telescope primary mirror to the Shack–Hartmann mask or lenslet array. The registration requirements are particularly demanding for applications in which segmented mirrors are phased using a physical optics generalization of the Shack–Hartmann test. In such cases the registration tolerances are less than 0.1% of the diameter of the primary mirror. We present a pupil registration algorithm suitable for such high accuracy applications that is based on the one used successfully for phasing the segments of the Keck telescopes. The pupil is aligned in four degrees of freedom (translations, rotation, and magnification) by balancing the intensities of subimages formed by small subapertures that straddle the periphery of the mirror. We describe the algorithm in general terms and then in the specific context of two very different geometries: the 492 segment Thirty Meter Telescope, and the seven “segment” Giant Magellan Telescope. Through detailed simulations we explore the accuracy of the algorithm and its sensitivity to such effects as cross talk, noise/counting statistics, atmospheric scintillation, and segment reflectivity variations.

Abstract: The James Webb Space Telescope is a large, deployable telescope that will operate at cryogenic temperatures at the Earth-Sun Lagrange 2 point. The Webb Optical Telescope Element (OTE) consists of 18 actively controlled Primary Mirror Segment Assemblies (PMSAs), an actively controlled Secondary Mirror Assembly (SMA), and an Aft-Optics Subsystem (AOS) that contains a fixed Tertiary Mirror and a Fine Steering Mirror. The OTE is combined with the Integrated Science Instrument Module (ISIM) to create the full optical train called OTIS (OTE and ISIM). OTIS has recently undergone cryogenic vacuum testing in Chamber A at Johnson Space Center in Houston, TX. A key outcome of this test was to verify there is adequate range of motion in PMSA and SMA actuators to align them to AOS/ISIM under flight-like conditions. The alignment state of the PMSAs and SMA was measured using photogrammetry and cross-checked optically using a variation of a classical Hartmann test. In the “Pass-and-a-Half” (PAAH) configuration, fiber sources near the Cassegrain focus propagate light through the full optical train and small tilts on the PMSAs create an array of spots on the science instrument detectors, mimicking the effect of a Hartmann mask. Comparison of measured and modeled spot arrays provides the alignment state of the SMA and the global tilt of the primary mirror. This paper will discuss the methodology, testing, and analysis performed to measure the alignment state of OTIS using the Hartmann method and verify the primary and secondary mirrors can be successfully aligned on orbit to meet performance requirements.