Cryogenic focus measurement system for a wide-field infrared space telescope.

We describe a technique for measuring focus errors in a cryogenic, wide-field, near-infrared space telescope. The measurements are made with a collimator looking through a large vacuum window, with a reflective cold filter to reduce the background thermal infrared loading on the detectors and optics. The vacuum window and cold filter introduce a wavefront error that we characterize using an autocollimating microscope. For the 200 mm diameter aperture f/3 space telescope SPHEREx, we achieve a focus position measurement with a ∼15µm systematic and a ∼5µm statistical error.

Sidelobe modeling and mitigation for a three mirror anastigmat cosmic microwave background telescope.

Telescopes measuring cosmic microwave background (CMB) polarization on large angular scales require exquisite control of systematic errors to ensure the fidelity of the cosmological results. In particular, far-sidelobe contamination from wide angle scattering is a potentially prominent source of systematic error for large aperture microwave telescopes. Here we describe and demonstrate a ray-tracing-based modeling technique to predict far sidelobes for a three mirror anastigmat telescope designed to observe the CMB from the South Pole. Those sidelobes are produced by light scattered in the receiver optics subsequently interacting with the walls of the surrounding telescope enclosure. After comparing simulated sidelobe maps and angular power spectra for different enclosure wall treatments, we propose a highly scattering surface that would provide more than an order of magnitude reduction in the degree-scale far-sidelobe contrast compared to a typical reflective surface. We conclude by discussing the fabrication of a prototype scattering wall panel and presenting measurements of its angular scattering profile.

Millimeter-wave center of curvature test for a fast paraboloid.

We describe a technique for measuring the surface profile of a radio telescope with a fast paraboloidal primary. The technique uses a sensor, at the center of curvature of the primary, consisting of a millimeter-wave source and an array of receivers to measure the field in the caustic. The sensor is mounted on the telescope enclosure and it moves with the telescope, so the measurements can be used for continuous, slow, closed-loop control of the surface. Sensor decenter and despace errors, due to wind buffeting and thermal deformation of the sensor support, do not compromise the surface measurements because they result in profile errors that are mainly translation, which has no effect on astronomical observations, or tilt and defocus, which can be measured using astronomical sources. If the position of the sensor is known to 20 µm rms, the surface can be measured to ~1 µm rms at λ=3 mm.

Mapping speed for an array of corrugated horns.

I address the choice of horn diameter for millimeter-wave array receivers with corrugated horns. For maximum point-source mapping speed, in both total power and polarization with typical receiver noise contributions and a close-packed horn array that fills the field of view, the optimum horn diameter is 1.6-1.7Flambda, where F is the focal ratio. A +/-25% change in horn diameter gives <10% degradation in mapping speed. Correlated noise from the cold stop, atmosphere, and cosmic microwave background has little effect on the mapping speed and optimum horn diameter.

Location of the elevation axis in a large optical telescope.

Proposed designs for the next generation of large optical telescopes favor a tripod or quadrupod secondary support, and a primary supported from the back, but it is not yet clear whether the elevation axis should be in front of the primary or behind it. A study is described of the effect of elevation-axis location on key performance parameters (fundamental frequency, blockage, and wind-induced secondary decenter) for a 30-m Cassegrain telescope with amount configuration that is typical of the new designs. For a fast (e.g., f/1) primary, the best location for the elevation axis is behind the primary. The penalty for moving the elevation axis in front of the primary is roughly a 40% decrease in fundamental frequency and a corresponding reduction in the control bandwidth for pointing and optical alignment.

Wind-induced deformations in a segmented mirror.

A Zernike expansion of wind-induced deformations in a segmented mirror is described. The wind model is a frozen turbulent field with a Kolmogorov spectrum for scales smaller than the outer scale and a flat spectrum for scales larger than the outer scale. The approach allows a mode-by-mode comparison of the wave-front error contributions from atmospheric phase distortions, wind-induced deformations, and the mirror control system noise. This is used to design a controller that minimizes the mirror surface errors by application of corrections based on edge sensor measurements and wave-front measurements on a guide star.

Design considerations for a highly segmented mirror.

Design issues for a 30-m highly segmented mirror are explored, with emphasis on parametric models of simple, inexpensive segments. A mirror with many small segments offers cost savings through quantity production and permits high-order active and adaptive wave-front corrections. For a 30-m f/1.5 paraboloidal mirror made of spherical, hexagonal glass segments, with simple warping harnesses and three-point supports, the maximum segment diameter is approximately 100 mm, and the minimum segment thickness is approximately 5 mm. Large-amplitude, low-order gravitational deformations in the mirror cell can be compensated if the segments are mounted on a plate floating on astatic supports. Because gravitational deformations in the plate are small, the segment actuators require a stroke of only a few tens of micrometers, and the segment positions can be measured by a wave-front sensor.

Spatial spectrum analysis of wave-front correction with a segmented mirror.

An expression is derived for the spatial power spectrum of wave-front errors after correction with a segmented mirror. This includes estimates of the spectral contributions of segment piston and tilt corrections and spatial aliasing by a regular array of segments. The approach allows rapid computation of wave-front error spectra in systems with highly segmented mirrors.

Mirrors with regular hexagonal segments.

The point-spread function and emissivity are calculated for a mirror made from regular hexagonal segments of just a few different sizes. A mirror of this type has many similar segments, which is an advantage for manufacturing, and for an approximately f/1 mirror with > or = 1000 segments and > or = 4 sizes of regular hexagons the increase in intersegment gap area is negligible. This result raises the possibility of making a mirror from very large numbers of identical small segments that are warped to the required figure.

Model of image degradation due to wind buffeting on an extremely large telescope.

A parametric model of wind buffeting on an extremely large telescope with a multipod secondary support is described. The model estimates wave-front errors that are due to wind buffeting on a segmented primary, wind-induced secondary figure and position errors, and primary-mirror deformations caused by wind forces on the secondary support. The approach is based on a Zernike expansion of pressure fluctuations, with simple models of stiffness, resonance, and control. The model shows that wind buffeting on a multipod attached to the primary mirror cell significantly degrades the image quality in a large telescope with a slow primary.