We propose an approach for coarse alignment of a segmented space telescope using science instrument images. The recommended steps go from large post launch rigid body misalignments to within the capture range of coarse phasing where segment piston error is the predominant residual wavefront error. These steps include five data collection and analysis methods comprising of metrology capture, segment capture and identification, segment translation, segment stacking, and fine alignment. Using a proposed architecture for the NASA Habitable Worlds Observatory (HWO) we describe the details of our recommended approach for each telescope alignment step. We then compare this recommended sequence to alternative alignment progressions used in existing segmented testbeds and telescopes in terms of number of data collections required. This model-based demonstration establishes that the recommended coarse and fine alignment sequence performs more efficiently in time and resource cost, handing off to coarse and fine phasing activities further along the telescope commissioning process.
Object-Oriented Matlab Adaptive Optics (OOMAO) is a Matlab toolbox dedicated to Adaptive Optics (AO) systems. It is based on a small set of classes representing the source, atmosphere, telescope, wavefront sensor, Deformable Mirror (DM) and an imager of an AO system. The original OOMAO toolbox was developed for modeling the performance of adaptive optics systems utilizing plane-waves. We have extended the capabilities of the OOMAO toolbox by adding a new method, a Gaussian-beam source, to an existing class, source. This new source method is needed to use OOMAO for modeling laser communications uplinks that are currently under development by many institutions. In this paper, we describe the method that we newly added, namely, Gaussian-beam source uplink, and present several numerical examples. These include results from the simulation for uplink pre-compensation of lasers. We will also show how well uplink works in and outside of the isoplanatic patch.
The HabEx (Habitable Exoplanet) space telescope mission concept carries two complementary optical systems as part of its baseline design, a coronagraph and a starshade, that are designed to detect and characterize planetary systems around nearby stars. The starshade is an external occulter which would be 72 m in diameter and fly some 124,000 km ahead of the telescope. A starshade instrument on board the telescope enables formation flying to maintain the starshade within 1 m of the line of sight to the star. The starshade instrument has various modes, including imaging from the near UV through to the near infrared and integral field spectroscopy in the visible band. The coronagraph would provide imaging and integral field spectroscopy in the visible band and would reach out to 1800 nm for low resolution spectroscopy in the near infrared. To provide the necessary stability for the coronagraph, the telescope would be equipped with a laser metrology system allowing measurement and control of the relative positions of the principal mirrors. In addition, a fine guidance sensor is needed for precision attitude control. The requirements for telescope stability for coronagraphy are discussed. The design and requirements on the starshade will also be discussed.
End-to-end numerical optical modeling of the WFIRST coronagraph incorporating wavefront sensing and control is used to determine the performance of the coronagraph with realistic errors, including pointing jitter and polarization. We present the performance estimates of the current flight designs as predicted by modeling. We also describe the release of a new version of the PROPER optical propagation library, our primary modeling tool, which is now available for Python and Matlab in addition to IDL.
Starshades have been designed to work with large and small telescopes alike. With smaller telescopes, the targets tend to be brighter and closer to the Solar System, and their putative planetary systems span angles that require starshades with radii of 10-30 m at distances of 10s of Mm. With larger apertures, the light-collecting power enables studies of more numerous, fainter systems, requiring larger, more distant starshades with radii >50 m at distances of 100s of Mm. Characterization using infrared wavelengths requires even larger starshades. A mitigating approach is to observe planets between the petals, where one can observe regions closer to the star but with reduced throughput and increased instrument scatter. We compare the starshade shape requirements, including petal shape, petal positioning, and other key terms, for the WFIRST 26m starshade and the HABEX 72 m starshade concepts, over a range of working angles and telescope sizes. We also compare starshades having rippled and smooth edges and show that their performance is nearly identical.
Exo-S is a probe-class mission study that includes the Dedicated mission, a 30 m starshade co-launched with a 1.1 m commercial telescope in an Earth-leading deep-space orbit, and the Rendezvous mission, a 34 m starshade intended to work with a 2.4 m telescope in an Earth-Sun L2 orbit. A third design, referred to as the Rendezvous Earth Finder mission, is based on a 40 m starshade and is currently under study. This paper presents error budgets for the detection of Earth-like planets with each of these missions. The budgets include manufacture and deployment tolerances, the allowed thermal fluctuations and dynamic motions, formation flying alignment requirements, surface and edge reflectivity requirements, and the allowed transmission due to micrometeoroid damage.
KEYWORDS: Coronagraphy, Error analysis, Performance modeling, Statistical analysis, James Webb Space Telescope, Mirrors, Systems modeling, Wavefronts, Space telescopes, Diffraction
We have combined our Excel-based coronagraph dynamics error budget spreadsheets with DAKOTA scripts to perform statistical analyses of the predicted dark-hole contrast. Whereas in the past we have reported the expected contrast level for an input set of allocated parameters, we now generate confidence intervals for the predicted contrast. Further, we explore the sensitivity to individual or groups of parameters and model uncertainty factors through aleatory-epistemic simulations based on a surrogate model fitted to the error budget. We show example results for a generic high-contrast coronagraph.
The Astrophysics Focused Telescope Assets (AFTA) study in 2012-2013 included a high-contrast stellar coronagraph to complement the wide-field infrared survey (WFIRST) instrument. The idea of flying a coronagraph on this telescope was met with some skepticism because the AFTA pupil has a large central obscuration with six secondary mirror struts that impact the coronagraph sensitivity. However, several promising coronagraph concepts have emerged, and a corresponding initial instrument design has been completed. Requirements on the design include observations centered 0.6 deg off-axis, on-orbit robotic serviceability, operation in a geosynchronous orbit, and room-temperature operation (driven by the coronagraph’s deformable mirrors). We describe the instrument performance requirements, the optical design, an observational scenario, and integration times for typical detection and characterization observations.
It is likely that the coming decade will see the development of a large visible light telescope with enabling
technology for imaging exosolar Earthlike planets in the habitable zone of nearby stars. One such technology utilizes an external occulter, a satellite flying far from the telescope and employing a large screen, or
starshade, to suppress the incoming starlight suffciently for detecting and characterizing exoplanets. This
trades the added complexity of building the precisely shaped starshade and flying it in formation against
simplifications in the telescope since extremely precise wavefront control is no longer necessary. In this paper we present the results of our project to design, manufacture, and measure a prototype occulter petal as
part of NASA's first Technology Development for Exoplanet Missions program. We describe the mechanical design of the starshade and petal, the precision manufacturing tolerances, and the metrology approach.
We demonstrate that the prototype petal meets the requirements and is consistent with a full-size occulter
achieving better than 10-10 contrast.
We evaluate in detail the stability requirements for a band-limited coronagraph with an inner working angle as small as 2
λ/D coupled to an off-axis, 3.8-m diameter telescope. We have updated our methodologies since presenting a stability
error budget for the Terrestrial Planet Finder Coronagraph mission that worked at 4 λ/D and employed an 8th-order
mask to reduce aberration sensitivities. In the previous work, we determined the tolerances relative to the total light
leaking through the coronagraph. Now, we separate the light into a radial component, which is readily separable from a
planet signal, and an azimuthal component, which is easily confused with a planet signal. In the current study,
throughput considerations require a 4th-order coronagraph. This, combined with the more aggressive working angle,
places extraordinarily tight requirements on wavefront stability and opto-mechanical stability. We find that the
requirements are driven mainly by coma that leaks around the coronagraph mask and mimics the localized signal of a
planet, and pointing errors that scatter light into the background, decreasing SNR. We also show how the requirements
would be relaxed if a low-order aberration detection system could be employed.
The NASA Exoplanet program and the Cosmic Origins program are exploring technical options to combine the visible
to NIR performance requirements of a space coronagraph with the general astrophysics requirements of a space
telescope covering the deep UV spectrum. Are there compatible options in terms of mirror coatings and telescope
architecture to satisfy both goals? In this paper, we address some of the main concerns, particularly relating to
polarization in the visible and throughput in the UV. Telescope architectures employing different coating options
compatible with current technology are considered in this trade study.
External occulters provide the starlight suppression needed for detecting and characterizing exoplanets with
a much simpler telescope and instrument than is required for the equivalent performing coronagraph. In
this paper we describe progress on our Technology Development for Exoplanet Missions project to design,
manufacture, and measure a prototype occulter petal. We focus on the key requirement of manufacturing a
precision petal while controlling its shape within precise tolerances. The required tolerances are established
by modeling the effect that various mechanical and thermal errors have on scatter in the telescope image
plane and by suballocating the allowable contrast degradation between these error sources. We discuss the
deployable starshade design, representative error budget, thermal analysis, and prototype manufacturing.
We also present our metrology system and methodology for verifying that the petal shape meets the contrast
requirement. Finally, we summarize the progress to date building the prototype petal.
We present a starshade error budget with engineering requirements that are well within the current manufacturing and
metrology capabilities. The error budget is based on an observational scenario in which the starshade spins about its axis
on timescales short relative to the zodi-limited integration time, typically several hours. The scatter from localized petal
errors is smoothed into annuli around the center of the image plane, resulting in a large reduction in the background flux
variation while reducing thermal gradients caused by structural shadowing. Having identified the performance
sensitivity to petal shape errors with spatial periods of 3-4 cycles/petal as the most challenging aspect of the design, we
have adopted and modeled a manufacturing approach that mitigates these perturbations with 1-m long precision edge
segments positioned using commercial metrology that readily meets assembly requirements. We have performed
detailed thermal modeling and show that the expected thermal deformations are well within the requirements as well.
We compare the requirements for four cases: a 32 m diameter starshade with a 1.5 m telescope, analyzed at 75 and 90
mas, and a 40 m diameter starshade with a 4 m telescope, analyzed at 60 and 75 mas.
This paper describes a general purpose Coronagraph Performance Error Budget (CPEB) tool that we have developed
under the NASA Exoplanet Exploration Program. The CPEB automates many of the key steps required to evaluate
the scattered starlight contrast in the dark hole of a space-based coronagraph. It operates in 3 steps: first, a CodeV or
Zemax prescription is converted into a MACOS optical prescription. Second, a Matlab program calls ray-trace code
that generates linear beam-walk and aberration sensitivity matrices for motions of the optical elements and line-ofsight
pointing, with and without controlled coarse and fine-steering mirrors. Third, the sensitivity matrices are
imported by macros into Excel 2007 where the error budget is created. Once created, the user specifies the quality
of each optic from a predefined set of PSDs. The spreadsheet creates a nominal set of thermal and jitter motions and
combines them with the sensitivity matrices to generate an error budget for the system. The user can easily modify
the motion allocations to perform trade studies.
The Terrestrial Planet Finder Coronagraph (TPF-C) demands extreme wave front control and stability to achieve its goal of detecting earth-like planets around nearby stars. We describe the performance models and error budget used to evaluate image plane contrast and derive engineering requirements for this challenging optical system. We show that when the coronagraph is coupled to an 8th-order band-limited mask, the performance is limited by shearing of the starlight beam across imperfect optics (a.k.a. beam walk), and that this in turn demands tight rigid body pointing, sub-milliarcsecond fine guiding, high-quality optics, and sub-micron positional stability of the optics including the secondary mirror. Additionally we show that the stability of low-order aberrations (focus, astigmatism, coma, and trefoil) is required to be ~ 2-4 Angstroms, while higher-order modes must remain stable to a few picometers.
The Terrestrial Planet Finder Coronagraph (TPF-C) for observing and characterizing exo-solar planets requiring star light suppression to 10-10 level demands optical aberrations and instrument stability to sub-nm levels. Additionally, wavefront polarization has to be tightly controlled over the 8m x 3.5m primary mirror aperture and 500nm - 800nm minimum bandwidth because the Deformable Mirror (DM) employed to control the wavefront can not correct simultaneously for the different wavefronts presented by two orthogonal uncorrected polarization fields. Further, leakage of cross polarization fields introduced by the various optical surfaces can degrade the image contrast. The study reported here shows mirror coating designs that reduce the phase difference between orthogonal polarizations reflected by a mirror surface to less than 0.6 deg over the bandwidth and aperture which may encounter a maximum angle of incidence of about 12 deg at a curved mirror. Such designs mitigate the contrast degradation due to cross polarization leakage. Simulations show that required contrast levels can be achieved with such coatings.
The Terrestrial Planet Finder (TPF) employs an aggressive coronagraph designed to obtain better than 1e-10 contrast inside the third Airy ring. Minute changes in low-order aberration content scatter significant light at this position. One implication is the requirement to control low-order aberrations induced by motion of the secondary mirror relative to the primary mirror; sub-nanometer relative positional stability is required. We propose a 6-beam laser truss to monitor the relative positions of the two mirrors. The truss is based on laser metrology developed for the Space Interferometry Mission.
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