Nov/Dec, 2022


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result is that starlight is greatly dimmed while faintly glowing objects (that were previously invisible) will appear relatively undimmed.


Testing Critical Components The High-Contrast Imaging


Testbed (HCIT) facility at NASA’s JPL is a large optical laboratory that hosts three optical testbeds inside vacuum chambers designed to advance coronagraph technolo- gies for space. The Roman testbed is a 6 foot


diameter vacuum chamber with a 7.5-foot cylindrical section, and can accommodate tables up to 8 feet in length when accounting for the outward bulge of the end cap doors. Power cables, data cables, water lines, and optical fibers are fed through ports in the side- walls. Two ports are occupied by camera umbilicals to connect bench-mounted camera enclo- sures to the lab air, which permit the use of Andor Neos CMOS cameras as science detectors in the chamber, despite their lack of vacuum compatibility. The bench itself is a 6.5 by 4


foot invar optical table placed on three vacuum customized Minus K Technology Negative-Stiffness 500CM-1CV isolator legs to pas- sively isolate the bench from vibrations. These legs have a manual adjustment range that allows them to be returned to account for changes in weight distribution on the table follow- ing hardware modifications. The testbed is heavily


instrumented with temperature sensors, as well as a few accelerometers, with contamina- tion monitors planned for the future. The chamber wall tem- perature is maintained to within ±0.1 K using a simple control system. More sophisticated con- trol is used to stabilize the Deformable Mirror (DM) temper- ature to milli-K levels. Within Roman, the bench


and optical telescope assembly (OTA) sub-bench are on inde- pendent PI thermal control loops which stabilize the mean bench temperature to 30 mK P-V under normal conditions. The chamber itself is con-


trolled to a set point above labo- ratory ambient by a PID loop implemented with heater tape under an insulation layer, and can be stabilized to 50 mK P-V. All


optical mounts were


machined from invar with optics bonds within flexure mounts, to minimize the effect of residual thermal fluctuations on the sys- tem. The primary heat sources on the table are the two cameras and the DM electronics, and all are cooled by a pair of external water-cooling loops. A telescope simulator on a sub-bench is kinematically


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mounted to the northwest corner of the bench, and simulates the


front end of the telescope. This includes a jitter mirror (JM) to


Page 59


Space Telescope Vibration Isolation Optimizes Image Clarity Continued from page 57


inject tip/tilt errors into the coro- nagraph in a controlled manner, and a simulator for the optical telescope assembly which defines the upstream pupil and provides light that isn’t collimated as well. The Decadal Survey Testbed


(DST) is a new, advanced testbed aimed to demonstrate the coron- agraph technologies required for a mission following Roman that will directly image and charac- terize Earth-like exoplanets, that consists of a stellar source simu- lator, two deformable mirrors (DMs) for wavefront control,


Continued on next page


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