In this paper we describe the optical modelling of astronomical telescopes that exploit bolometric detectors fed by multimoded horn antennas. In cases where the horn shape is profiled rather than being a simple cone, we determine the beam at the horn aperture using an electromagnetic mode-matching technique. Bolometers, usually placed in an integrating cavity, can excite many hybrid modes in a corrugated horn; we usually assume they excite all modes equally. If the waveguide section feeding the horn is oversized these modes can propagate independently, thereby increasing the throughput of the system. We use an SVD analysis on the matrix that describes the scattering between waveguide (TE/TM) modes to recover the independent orthogonal fields (hybrid modes) and then propagate these to the sky independently where they are added in quadrature. Beam patterns at many frequencies across the band are then added with a weighting appropriate to the source spectrum. Here we describe simulations carried out on the highest-frequency (857-GHz) channel of the Planck HFI instrument. We concentrate in particular on the use of multimode feedhorns and consider the effects of possible manufacturing tolerances on the beam on the sky. We also investigate the feasibility of modelling far-out sidelobes across a wide band for electrically large structures and bolometers fed by multi-mode feedhorns. Our optical simulations are carried out using the industry-standard GRASP software package.
The advanced camera for surveys, designed to be installed in 1999 during the third servicing mission of the Hubble Space Telescope, is a high performance axial bay camera.
This paper describes the process used to verify that the mounts designed for the STIS and COSTAR program would perform as designed. The optics on these two programs were all fabricated to (lambda) /100 rms surface figure. Some of the optics were bonded into mounts and others were mechanically mounted. All the mounts were designed to impart less than 0.005 (lambda) rms additional distortion with a goal of 0.003 (lambda) rms. A series of tests showed that the mounts performed as designed. Stability, thermal performance, contamination, and survivability were also tested.
The purposes of the Phase II alignment are to coalign mirror pairs for the FOC and FOS channels and to set the compensation mechanisms of each channel to the optimum positions to allow the overall system performance to be determined and verified through use of the RAS/HOMS equipment without requiring adjustment of the mechanism compensators during testing. This alignment process is performed with the COSTAR instrument installed in the COSTAR Alignment System (CAS), using a well characterized interferometer system as the optical source. The interferometer uses a custom designed reference sphere with built-in spherical aberration to enable the highly aberrated two-mirror systems to be observed in double-pass.
The Refractive Aberration Simulator (RAS) produces an image field which matches the as- built Hubble Space Telescope (HST) image field to a very high degree at 632.8 nm. The instrument is used to provide HST-like aberrated image plane illumination to the COSTAR and FOC-STM instruments during the final performance verification operations. It is capable of providing up to 15 simultaneous inputs to the instruments or metrology equipment located at its image plane. It consists of 6 anti-reflection coated glass lenses, each requiring lateral positioning accuracy as fine as +/- 10 microns, axial positioning accuracy of +/- 140 microns, and angular positioning of +/- 12.7 arcseconds, a fiber coupled laser source system, removable aperture stops for providing obscured or unobscured wavefronts, and a three-axis positionable source plate with removable fiber couplers for measurement or alignment operations.
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