The Direct Detection Spectrometer Instrument (DDSI) is one of two instruments designed for the Far-IR Spectroscopy Space Telescope (FIRSST) recently proposed to NASA in response to the Astrophysics Probe Explorer call. The DDSI consists of two modules: HR delivering spectra at R~20,000 to 100,000 in three select bands (HR1-3) across 56-184μm, and LR providing broadband spectral coverage at R~100 in four bands (LR1-4) across 35-260 µm. The dispersive element of the HR bands is a compact optical resonator known as a virtually imaged phase array. All DDSI bands use microwave kinetic inductance detector (MKID) arrays cooled to 120mK. The total DDSI MKID pixel count is 2612 pixels.
Commissioning the Webb telescope to realize the observatory’s full capability necessitated the development of robust wavefront sensing and control processes. These processes rely on techniques that were adapted or newly innovated for the mission, and further adaptation of these techniques may be expected for future segmented telescopes. Over the course of mission development, these techniques were refined to form a baseline wavefront commissioning plan that assumes several conditions and performance requirements are met. Herein we present efforts carried out to define and develop contingency concepts of operation for Webb telescope commissioning, and the mission-level approach to managing the response to deviations from the baseline plan in the event of significant off-nominal or anomaly scenarios encountered by the wavefront team. An overview of selected contingencies is presented along with more detailed example model cases and instances of interest encountered in flight.
The James Webb Space Telescope (JWST) is a segmented deployable telescope, currently operating at L2. The telescope utilizes 6 degrees of freedom for adjustment of the Secondary Mirror (SM) and 7 degrees of freedom for adjustment of each of its 18 segments in the Primary Mirror (PM). After deployment, the PM segments and the SM arrived in their correct optical positions to within a ~1 mm, with accordingly large wavefront errors. A Wavefront Sensing and Controls (WFSC) process was executed to adjust each of these optical elements in order to correct the deployment errors and produce diffraction-limited images across the entire science field. This paper summarizes the application of the WFSC process.
In 2014, the Optical Ground Support Equipment was integrated into the large cryo vacuum chamber at Johnson Space Center (JSC) and an initial Chamber Commissioning Test was completed. This insured that the support equipment was ready for the three Pathfinder telescope cryo tests. The Pathfinder telescope which consists of two primary mirror segment assemblies and the secondary mirror was delivered to JSC in February 2015 in support of this critical risk reduction test program prior to the flight hardware. This paper will detail the Chamber Commissioning and first optical test of the JWST Pathfinder telescope.
The gas cloud imager (GCI) is a passive uncooled multispectral camera capable of unprecedented sensitivity for
analyzing hydrocarbon gas mixtures in a scene. The GCI is currently finishing its final stages of development,
and promises to obtain a 220×220 image of gas concentrations at 30 frames/sec, allowing for real-time display in
a compact instrument without moving parts. We summarize measurement approach and discuss the advantages
of the GCI instrument design against conventional instruments.
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