NASA’s Habitable Worlds Observatory will consist of a segmented telescope and high contrast coronagraph to characterize exoplanets for habitability. Achieving this objective requires an ultra-stable telescope with wavefront stability of picometers in certain critical modes. The NASA funded Ultra-Stable Large Telescope Research and Analysis – Technology Maturation program has matured key component-level technologies in 10 areas spanning an “ultra-stable” architecture, including active components like segment edge sensors, actuators and thermal hardware, passive components like low distortion mirrors and stable structures, and supporting capabilities like precision metrology. This paper will summarize the final results from the four-year ULTRA-TM program, including advancements in performance and/or path-to-flight readiness, TRL/MRL maturation, and recommendations for future work.
KEYWORDS: Telescopes, Mirrors, James Webb Space Telescope, Space telescopes, Coronagraphy, Observatories, Engineering, Design, Thermal stability, Off axis mirrors
The Astro2020 Decadal Survey recommends an ambitious mission named Habitable Worlds Observatory (HWO) to explore the universe and search for life on exoplanets. HWO builds upon NASA investments, including the James Webb Space Telescope segmented optical system, Roman Space Telescope coronagraph, large mission concept studies, and technology development. Studies continue to drive our understanding of the HWO mission trade space and increase the readiness of relevant technologies. NASA’s Great Observatory Maturation Program (GOMAP) will explain how mission architecture decisions impact science yields and improve understanding of the boundaries and opportunities within the mission trade spaces.
NASA’s Habitable Worlds Observatory will consist of a segmented telescope and high contrast coronagraph to characterize exoplanets for habitability. Achieving this objective requires an ultra-stable telescope with wavefront stability of picometers in certain critical modes. The NASA funded Ultra-Stable Large Telescope Research and Analysis – Technology Maturation program continues to mature key component-level technologies for this new regime of “ultra-stable optical systems,” including active components like segment edge sensors, actuators and thermal hardware, passive components like low distortion mirrors and stable structures, and supporting capabilities like precision metrology. This paper will present an update to the latest results from hardware testbeds and simulations in the areas listed above. It will also contain a correction to previously published results of Ball’s Integrated Demo, which consists of a capacitive sensor and three actuators operating in closed loop.
We present a segment-level wavefront stability error budget for space telescopes essential for exoplanet detection. We use a detailed finite element model to relate the temperature gradient at the location of the primary mirror to wavefront variations on each of the segment. We apply the PASTIS sensitivity model forward approach to allocate static tolerances in physical units for each segment, and transfer these tolerances to the temporal domain via a model of the WFS&C architecture in combination with a Zernike phase sensor and science camera. We finally estimate the close-loop variance and limiting contrast for the segments’ thermo-mechanical modes.
The recently released Astro2020 Decadal Survey recommends a large IR/O/UV space telescope that can observe potentially habitable exoplanets. Achieving this goal requires a telescope with wavefront stability on the order of picometers in some modes. The Ultra-Stable Large Telescope Research and Analysis – Technology Maturation (ULTRATM) program has matured key component-level technologies for this new regime of “ultra-stable optical systems,” including active components like segment edge sensors, actuators and thermal sensing and control hardware, as well as passive components like low distortion mirror mounts and stable composites for structures. Hardware testbeds have demonstrated component performance in the desired regime and with path-to-flight properties and simulations have applied those results to the flight system. These component level demonstrations are a critical step to enable subsequent subsystem and system level demonstrations of an ultra-stable telescope.
Design To Unit Production Cost (DTUPC) is of crucial importance to the viability and implementation of constellations which require tens to hundreds of small to moderate sized spaceborne telescopes (10-cm to 50-cm aperture). Emerging technologies enable cost-effective alternatives to the traditional design and build of such telescopes. This is especially true for the structure of Optical Telescope Assemblies (OTAs) addressing environments where orbital phase modulated thermal gradients and transients dominate design. The implementation of a dimensionally stable structure is crucial to the performance of a telescope, and typically, compensation with focus mechanisms is not a cost-effective option in this size. ALLVAR Alloys, a family of emerging aerospace materials exhibiting Negative Thermal Expansion (NTE), can offer novel and cost-effective approaches to OTA metering. These Titanium-based alloys’ NTE can be used to dial in a specific thermal expansion or zero expansion profile by compensating for the natural expansion of other telescope components. For the first time, a telescope designer can passively control thermal stability of a telescope’s metering/support structures. This is true both for designs based on materials with low or high Coefficients of Thermal Expansion (CTE) and low or high thermal diffusivity (for example ULE®, ZERODUR® or ClearCeram metered with CFRP and Invar vs. all Aluminum or all SiC approaches). NTE ALLVAR Alloys offer a brand-new solution for athermalizing telescope structures and offer several benefits over Invar and CFRP including lower cost, faster lead time, and greater thermal stability control in modulated orbital thermal environments.
To achieve the ambitious science goal of performing direct imaging of earth-like exoplanets with a high contrast coronagraph, future space-based astronomical telescopes will require wavefront stability several orders of magnitude beyond state-of-the-art. The Ultra-Stable Large Telescope Research and Analysis – Technology Maturation (ULTRA-TM) program is maturing key component-level technologies for this new regime of “ultra-stable optical systems” through hardware testbeds that demonstrate component performance in the desired picometer regime and with path-to-flight properties. This paper describes the initial results from these testbeds – which address key capabilities across the ultrastable architecture and include active components like segment edge sensors, actuators and thermal sensing and control hardware, as well as passive components like low distortion mirror mounts and stable composites for structures. These promising experimental results are the first steps in our team’s technical maturation plan to credibly enable a large, ultrastable telescope in space. The resulting component, sub-system and system roadmaps are meant to support planning for technology development efforts for future NASA missions.
We present a segment-level wavefront stability error budget for the LUVOIR A architecture essential for exoplanet detection. We start with a detailed finite element model to relate the temperature and gravity gradients at the location of the primary mirror to wavefront variations for each segment, and propagate the elements through a diffractive model of the observatory and coronagraphic instrument. Segment level errors are measured via a model of the WFS&C architecture in combination with a Zernike phase sensor and science camera. These sensitivities are used to relate semi-analytically the open and closed loop variance of the segments’ thermo-mechanical modes.
KEYWORDS: Space telescopes, Telescopes, James Webb Space Telescope, Mirrors, Optical instrument design, Astronomy, Space operations, Cryogenics, Aerospace engineering, Cryocoolers
The Origins Space Telescope will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did galaxies evolve from the earliest galactic systems to those found in the universe today? How do habitable planets form? How common are life-bearing worlds? We describe how Origins was designed to answer these alluring questions. We discuss the key decisions taken by the Origins mission concept study team, the rationale for those choices, and how they led through an exploratory design process to the Origins baseline mission concept. To understand the concept solution space, we studied two distinct mission concepts and descoped the second concept, aiming to maximize science per dollar and hit a self-imposed cost target. We report on the study approach and describe the concept evolution. The resulting baseline design includes a 5.9-m diameter telescope cryocooled to 4.5 K and equipped with three scientific instruments. The chosen architecture is similar to that of the Spitzer Space Telescope and requires very few deployments after launch. The cryo-thermal system design leverages James Webb Space Telescope technology and experience.
The Origins Space Telescope (Origins) study team prepared and submitted a Mission Concept Study Report for the 2020 Decadal Survey in Astrophysics. During the study, a Materials Working Group was formed to evaluate materials for Origins. The Materials Working Group identified material candidates and evaluated the candidates using driving requirements and key material considerations. The evaluation resulted in several options to aid the study team in making a materials selection for the mission concept. Our paper details the approach to the materials evaluation and the results.
The Origins Space Telescope will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did galaxies evolve from the earliest galactic systems to those found in the Universe today? How do habitable planets form? How common are life-bearing worlds? To answer these alluring questions, Origins will operate at mid- and far-infrared (IR) wavelengths and offer powerful spectroscopic instruments and sensitivity three orders of magnitude better than that of the Herschel Space Observatory, the largest telescope flown in space to date. We describe the baseline concept for Origins recommended to the 2020 US Decadal Survey in Astronomy and Astrophysics. The baseline design includes a 5.9-m diameter telescope cryocooled to 4.5 K and equipped with three scientific instruments. A mid-infrared instrument (Mid-Infrared Spectrometer and Camera Transit spectrometer) will measure the spectra of transiting exoplanets in the 2.8 to 20 μm wavelength range and offer unprecedented spectrophotometric precision, enabling definitive exoplanet biosignature detections. The far-IR imager polarimeter will be able to survey thousands of square degrees with broadband imaging at 50 and 250 μm. The Origins Survey Spectrometer will cover wavelengths from 25 to 588 μm, making wide-area and deep spectroscopic surveys with spectral resolving power R ∼ 300, and pointed observations at R ∼ 40,000 and 300,000 with selectable instrument modes. Origins was designed to minimize complexity. The architecture is similar to that of the Spitzer Space Telescope and requires very few deployments after launch, while the cryothermal system design leverages James Webb Space Telescope technology and experience. A combination of current-state-of-the-art cryocoolers and next-generation detector technology will enable Origins’ natural background-limited sensitivity.
To achieve the ambitious goal of directly imaging exo-Earths with a coronagraph, future space-based astronomical telescopes will require wavefront stability several orders of magnitude beyond state-of-the-art. The Ultra-Stable Large Telescope Research and Analysis – Technology Maturation (ULTRA-TM) program will mature critical technologies for this new regime of “ultra-stable optical systems” through component-level hardware demonstrations.
This paper describes the progress towards demonstrating performance of these technologies in the picometer regime and with flight-like properties – including active systems like segment sensing and actuation and thermal sensing and control, as well as passive systems like low distortion mirror mounts and composite structures. Raising the TRL of these technologies will address the most difficult parts of the stability problem with the longest lead times and provide significant risk reduction for their inclusion in future mission concepts.
A novel seldom used, thermal analysis approach for system-level thermal design is developed that leverages frequencybased techniques and metrics common in structural dynamics modeling. The ULTRA study, which is assessing technological capabilities for a 15-meter telescope requiring sub nanometer optical stability was the foundation for the initial thermal math model and requirements design space discussed in this paper. For such a large, space-based system under tight tolerances, a typical thermal analysis approach will not generate a meaningful understanding of which effects drive the thermal management design. To address this issue, a perturbance-based thermal modeling approach, which is more suited to generating an understanding of the bulk system-level sensitivities, was used instead. The model developed begins by running discrete sensitivities over a range of input perturbance frequencies. The output quantifies the system response to the various sources of thermal energy input. Results are gathered and combined to from Bode plots to quantify the effect of the system perturbances. These plots can quickly characterize the impact of certain thermal designs in relation to a frequency-based wave front error budget. Resulting sensitivities at the system / sub-system scale and the process for producing such results for the LUVOIR thermal math model utilized in the Ultra study are presented. Thermal stability is key to achieving coronographic missions with 10 E-10 contrast.
The Origins Space Telescope will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did galaxies evolve from the earliest galactic systems to those found in the universe today? How do habitable planets form? How common are life-bearing worlds? To answer these alluring questions, Origins will operate at mid- and far-infrared wavelengths and offer powerful spectroscopic instruments and sensitivity three orders of magnitude better than that of Herschel, the largest telescope flown in space to date. After a 3 ½ year study, the Origins Science and Technology Definition Team will recommend to the Decadal Survey a concept for Origins with a 5.9-m diameter telescope cryocooled to 4.5 K and equipped with three scientific instruments. A mid-infrared instrument (MISC-T) will measure the spectra of transiting exoplanets in the 2.8 – 20 μm wavelength range and offer unprecedented sensitivity, enabling definitive biosignature detections. The Far-IR Imager Polarimeter (FIP) will be able to survey thousands of square degrees with broadband imaging at 50 and 250 μm. The Origins Survey Spectrometer (OSS) will cover wavelengths from 25 – 588 μm, make wide-area and deep spectroscopic surveys with spectral resolving power R ~ 300, and pointed observations at R ~ 40,000 and 300,000 with selectable instrument modes. Origins was designed to minimize complexity. The telescope has a Spitzer-like architecture and requires very few deployments after launch. The cryo-thermal system design leverages JWST technology and experience. A combination of current-state-of-the-art cryocoolers and next-generation detector technology will enable Origins’ natural backgroundlimited sensitivity.
Direct imaging of exoearths with high-contrast internal coronagraphs depends on ultra-stable opto-mechanical systems. Ultra-stable mirror assemblies enable decadal survey missions like LUVOIR and HabEx. To precisely define the necessary level of stability, the essential first step is to budget the maximum allowable disturbances for each optic in the system. Ideally, allocations are budgeted with respect to spatial- and time-domain frequencies. If allocations do not span these domains, the optic assembly designer cannot take advantage of frequency bands where requirements are looser because of assumptions about telescope control systems and internal coronagraph filtering. This paper explores how mirror assembly technologies and designs are predicted to impact stability, especially within the frequency bands that drive coronagraph contrast performance.
Coronographic missions require ultra-stable mirror systems to achieve 10 E-10 contrast. The LUVOIR ULTRA study is assessing technological capabilities for a 15-meter telescope requiring sub nanometer optical stability. For ULTRA individual mirror stabilities at the picometer level are required. Thermal sensitivities for a proposed mirror design have been incorporated into a stability budget that indicates the level of stability required is attainable. Key factors to meeting stability allocations are an athermal design, acceptable mirror CTE homogeneity and mirror mount pad design. This paper will present the sensitivities and error budget used to predict the on-orbit mirror stability.
The author requests that a paper given by Matt East from Harris come before this presentation if both are presented.
KEYWORDS: Wavefronts, Coronagraphy, Mirrors, Control systems, Telescopes, Error analysis, Aerospace engineering, James Webb Space Telescope, Active remote sensing, Optics manufacturing
To meet the ambitious science goal of characterizing exo-Earths via direct imaging and spectroscopy, future space-based astronomical telescopes will have requirements for optical stability at least several orders of magnitude beyond the current state of the art. Mission concepts requiring stability on the order of picometers include the Large UV/Optical/Infrared (LUVOIR) Surveyor and the Habitable Exoplanet (HabEx) Observatory, which use large primary mirrors and internal coronagraphs to perform high contrast imaging. The Ultra-stable Large Telescope Research and Analysis (ULTRA) Program is a system study performed by an industry consortium led by Ball Aerospace to evaluate potential architectures, perform trade studies, and identify technology gaps that must be addressed to enable picometerlevel optical stability in space. This paper will describe the results of the study, including identification and prioritization of technology gaps and a development roadmap to raise the technology readiness level (TRL) of key enhancing/enabling technologies.
The HabEx mission concept is intended to directly image planetary systems around nearby stars, and to perform a wide range of general astrophysics and solar system observations. The baseline HabEx design would use both a coronagraph and a starshade for exoplanet discovery and characterization. We describe a lower-cost alternative HabEx mission design, which would only use a starshade for exoplanet science. The starshade would provide excellent exoplanet science performance, but for a smaller number of detected exoplanets of all types, including exoEarth candidates, and a smaller fraction of exoplanets with measured orbits. The full suite of HabEx general astrophysics and solar-system science would be supported.
The Origins Space Telescope (OST) will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did the universe evolve in response to its changing ingredients? How common are life-bearing planets? To accomplish its scientific objectives, OST will operate at mid- and far-infrared wavelengths and offer superlative sensitivity and new spectroscopic capabilities. The OST study team will present a scientifically compelling, executable mission concept to the 2020 Decadal Survey in Astrophysics. To understand the concept solution space, our team studied two alternative mission concepts. We report on the study approach and describe both of these concepts, give the rationale for major design decisions, and briefly describe the mission-enabling technology.
NASA is exploring telescope and mirror technology options to meet the demanding science goals of the proposed HabEx space telescope. A key priority for the HabEx mission concept would be to leverage affordable telescope solutions that can meet challenging telescope performance requirements with a demanding program timeline. The baseline approach for HabEx is to use an unobscured, monolithic primary mirror with a coronagraph to optimize system performance. NASA is performing an initial study to investigate the feasibility of a HabEx Lite concept which would not leverage a coronagraph and would therefore, have lower exoEarth yield as a consequence, but could provide system mass, cost, and schedule advantages. The HabEx Lite concept leverages replicated, ULE® mirror segments to provide an attractive, alternative telescope architecture to meet the HabEx threshold mission needs. We present the initial mirror design and performance assessment for the HabEx Lite concept.
The HabEx mission concept is intended to directly image planetary systems around nearby stars, and to perform a wide range of general astrophysics and solar system observations. Its main goal is the discovery and characterization of Earthlike exoplanets through high-contrast imaging and spectroscopy. The baseline HabEx concept would use both a coronagraph and a starshade for exoplanet science. We describe an alternative, “HabEx Lite” concept, which would use a starshade (only) for exoplanet science. The benefit is lower cost: by deleting the complex coronagraph instrument; by lowering observatory mass; by relaxing tolerances and stability requirements; by permitting use of a compact on-axis telescope design; by use of a smaller launch vehicle. The scientific penalty of this lower cost option is a smaller number of detected exoplanets of all types, including exoEarth candidates, and a smaller fraction of exoplanets with measured orbits. Our approach uses a non-deployed segmented primary mirror, whose manufacture is within current capabilities.
Large visible telescopes present challenging requirements for manufactured surface figure and stability. By comparison, far infrared (IR) telescopes relax many of these requirements by ~100x. These relaxed requirements may translate into reduced cost, schedule, mass, and system complexity. This paper explores how different mirror substrate materials might take advantage of these requirements while operating in a cryogenic environment. Primary mirror materials are evaluated for an Origins Space Telescope (OST) concept, using a 9.1 m segmented aperture in a 30 μm diffraction limited system.
KEYWORDS: Mirrors, Adhesives, Wavefronts, 3D modeling, Control systems, Systems modeling, Thermal modeling, Temperature metrology, Coronagraphy, Metrology
For internal coronagraph options on the LUVOIR or HabEx mission concepts, the stated challenge of 10 picometers RMS wavefront stability over 10 minutes will govern the performance of every structure that connects the focal plane assembly to each optical surface. This paper interrogates wavefront stability of a mounted mirror assembly for a primary mirror segment assembly, and stability of the optical surface. Analysis describes stability of each element in a primary mirror segment assembly (PMSA) to understand the impact of each component of the PMSA on surface figure error (SFE) over short time periods.
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