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.
The James Webb Space Telescope features a powerful complement of focal-plane instruments: the Mid-Infrared Instrument (MIRI), the Near-Infrared Camera (NIRCam), the Near-Infrared Imager and Slitless Spectrograph (NIRISS), the Near-Infrared Spectrograph (NIRSpec), and the Fine Guidance Sensor (FGS). These instruments offer an exciting suite of scientific capabilities for imaging, high-contrast imaging, and spectroscopy. To bring these capabilities on-line after launch, a carefully scoped and sequenced set of commissioning activities has been developed. These activities will confirm the functionality of the instruments, characterize their performance (optimizing where possible), obtain initial calibrations at a level required to properly plan observations, and demonstrate essential operational sequences such as target acquisition. We present a high-level overview of these activities and the planned commissioning timeline to execute them.
The WFIRST Astrometry Working Group, Robyn Sanderson, Andrea Bellini, Stefano Casertano, Jessica Lu, Peter Melchior, Mattia Libralato, David Bennett, Michael Shao, Jason Rhodes, Sangmo Tony Sohn, Sangeeta Malhotra, Scott Gaudi, S. Michael Fall, Edmund Nelan, Puragra Guhathakurta, Jay Anderson, Shirley Ho
The Wide-Field Infrared Space Telescope (WFIRST) will be capable of delivering precise astrometry for faint sources over the enormous field of view of its main camera, the Wide-Field Imager (WFI). This unprecedented combination will be transformative for the many scientific questions that require precise positions, distances, and velocities of stars. We describe the expectations for the astrometric precision of the WFIRST WFI in different scenarios, illustrate how a broad range of science cases will see significant advances with such data, and identify aspects of WFIRST’s design where small adjustments could greatly improve its power as an astrometric instrument.
KEYWORDS: James Webb Space Telescope, Point spread functions, Stars, Target acquisition, Space telescopes, Coronagraphy, Mirrors, Detection and tracking algorithms, Optimization (mathematics), Image processing
We discuss new results of coronagraphic simulations demonstrating a novel mode for JWST that utilizes sub-pixel
dithered reference images, called Small-Grid Dithers, to optimize coronagraphic PSF subtraction. These sub-pixel
dithers are executed with the Fine Steering Mirror under fine guidance, are accurate to ~2-3 milliarcseconds (1-σ/axis),
and provide ample speckle diversity to reconstruct an optimized synthetic reference PSF using LOCI or KLIP. We also
discuss the performance gains of Small-Grid Dithers compared to the standard undithered scenario, and show potential
contrast gain factors for the NIRCam and MIRI coronagraphs ranging from 2 to more than 10, respectively.
KEYWORDS: James Webb Space Telescope, Wavefront sensors, Space telescopes, Observatories, Image segmentation, Stars, Point spread functions, Wavefronts, Space operations, Mirrors
The James Webb Space Telescopes segmented primary and deployable secondary mirrors will be actively con- trolled to achieve optical alignment through a complex series of steps that will extend across several months during the observatory's commissioning. This process will require an intricate interplay between individual wavefront sensing and control tasks, instrument-level checkout and commissioning, and observatory-level calibrations, which involves many subsystems across both the observatory and the ground system. Furthermore, commissioning will often exercise observatory capabilities under atypical circumstances, such as fine guiding with unstacked or defocused images, or planning targeted observations in the presence of substantial time-variable offsets to the telescope line of sight. Coordination for this process across the JWST partnership has been conducted through the Wavefront Sensing and Control Operations Working Group. We describe at a high level the activities of this group and the resulting detailed commissioning operations plans, supporting software tools development, and ongoing preparations activities at the Science and Operations Center. For each major step in JWST's wavefront sensing and control, we also explain the changes and additions that were needed to turn an initial operations concept into a flight-ready plan with proven tools. These efforts are leading to a robust and well-tested process and preparing the team for an efficient and successful commissioning of JWSTs active telescope.
KEYWORDS: Image segmentation, James Webb Space Telescope, Point spread functions, Wavefront sensors, Space telescopes, Telescopes, Mirrors, Sensors, Cameras, Wavefronts
We present several engineering and algorithmic aspects of non-redundant masking (NRM) as they pertain to the James Webb Space Telescope (JWST). NRM's fundamental data structures have multiple uses in wavefront sensing as well in as high resolution imaging. Kernel phases are a full aperture generalization of NRM applicable to moderate and high Strehl ratio images. Eigenphases, the complement to kernel phases, provide wavefront sensing with single in-focus images. Thus this set of phases is relevant to wavefront sensing with routine science images on any Nyquist-sampled science camera on JWST. We attempt to organize these apparently diverse aspects of such Fizeau interferometry into an inter-related picture in order to facilitate their development and potential use on JWST and future space telescopes.
KEYWORDS: Coronagraphy, Stars, James Webb Space Telescope, Point spread functions, Target acquisition, Detection and tracking algorithms, Space telescopes, Planets, Telescopes, Observatories
Coronagraphic Target Acquisition (TA) is an important factor that contributes to the contrast performance and typically depends on the coronagraph design. In the case of JWST, coronagraphic TAs rely on measuring the centroid of the star's point spread function away from the focal plane mask, and performing a small angle ma- neuver (SAM), to place the star behind the coronagraphic mask. Therefore, the accuracy of the TA is directly limited by the SAM accuracy. Typically JWST coronagraphic observations will include the subtraction of a reference (either a reference star, or a self-reference after a telescope roll). With such differential measurement, the reproducibility of the TA is a very important factor. We propose a novel coronagraphic observation concept whereby the reference PSF is first acquired using a standard TA, followed by coronagraphic observations of a reference star on a small grid of dithered positions. Sub-pixel dithers (5-10 mas each) provide a small reference PSF library that samples the variations in the PSF as a function of position relative to the mask, thus compen- sating for errors in the TA process. This library can be used for PSF subtraction with a variety of algorithms (e.g; LOCI or KLIP algorithms, Lafrenière et al. 2007; Soummer, Pueyo and Larkin 2012). These sub-pixel dithers are executed under closed-loop fine guidance, unlike a standard SAM that executes the maneuver in coarse point mode, which can result in a temporary target offset of 1 arcsecond and would bring the star out from behind the coronagraphic mask. We discuss and evaluate the performance gains from this observation scenario compared to the standard TA both for MIRI coronagraphs.
KEYWORDS: Stars, James Webb Space Telescope, Solar system, Observatories, Sensors, Target acquisition, Space operations, Space telescopes, Planets, Comets
The James Webb Space Telescope will provide a unique capability to observe Solar System objects such as Kuiper Belt
Objects, comets, asteroids, and the outer planets and their moons in the near and mid-infrared. A recent study developed
the conceptual design for a capability to track and observe these objects. In this paper, we describe how the requirements
and operations concept were derived from the scientific goals and were distributed among the Observatory and Ground
Segment components in order to remain consistent with the current event-driven operations concept of JWST. In the
event-driven operations concept, the Ground Segment produces a high-level Observation Plan that is interpreted by on-board
scripts to generate commands and monitor telemetry responses. This approach allows efficient and flexible
execution of planned observations; precise or conservative timing models are not required, and observations may be
skipped if guide star or target acquisition fails. The efficiency of this approach depends upon most observations having
large time intervals in which they can execute. Solar System objects require a specification of how to track the object
with the Observatory, and a guide star that remains within the field of view of the guider during the observation. We
describe how tracking and guiding will be handled with JWST to retain the efficient and flexible execution
characteristics of event-driven operations. We also describe how the implementation is distributed between the
Spacecraft, Fine Guidance Sensor, On-board Scripts, and Proposal Planning Subsystem, preserving the JWST operations
concept.
KEYWORDS: Stars, Sensors, Calibration, Binary data, Signal to noise ratio, Optical interferometry, Target detection, Solids, Space telescopes, Hubble Space Telescope
The Hubble Space Telescope's Fine Guidance Sensor FGS1r has been used to observe cool white dwarf stars with apparent magnitudes that are near the FGS's faint limit. We had expected to discover that about 10% of these stars are actually binary white dwarf systems. Furthermore, we expected the binaries to have angular separations much larger than the size of the FGS white light fringes, making them easy to resolve. Although we did find 10% of the stars to be binaries, most have angular separations less than 25 milli-arcseconds, well below the HST diffraction limit. Instead of two widely separated fringes, we observed fringes that displayed subtle differences, in amplitude and morphology, from those of point sources. A major complication for our program was the need to address and remove the effects of the detector's dark current, which for the faintest targets contributed up to 40% of the counts. This paper outlines the process we employed to extract the science from the data. Our scientific motivation is briefly discussed
With a white-light interferometer (Fine Guidance Sensor 3) on the Hubble Space Telescope (HST) we have secured fringe scanning and fringe tracking observations to measure distances, orbits, and, hence, masses, for several nearby low-mass stars. We have made progress towards a more precise Mass-Luminosity Relation (MLR) for the lower Main Sequence. However, the MLR is a map whose low mass region is complicated by relative and absolute age and whose high-mass end is very poorly determined. To begin to disentangle these effects, and to obtain high-precision mass determinations throughout the Main Sequence, we will participate in the Space Interferometry Mission (SIM) to observe binary stars of all masses in five star clusters with a large range of well-known ages and chemical compositions. We will also observe a sample of stars throughout the Main Sequence. The unparalleled angular resolution and limiting magnitude of SIM will allow us to obtain masses precise to 1%.
The fine guidance sensors (FGS) aboard the Hubble Space Telescope (HST) are optical white light shearing interferometers that offer a unique capability to astronomers. The FGS's photometric dynamic range, fringe visibility, and fringe tracking ability allow the instrument to exploit the benefits of performing interferometry form a space-based platform. The FGSs routinely provide HST with 2 milli-seconds of arc pointing stability. The FGS designated as the Astronomer, FGS3, has also been used to (1) perform 2 mas relative astrometry over the central 4 arc minutes of its field of view, (2) determine the true relative orbits of close faint binary systems, (3) measure the angular diameter of a giant star, (4) search for extra-solar planets, (5) observe occultations of stars by solar system objects, as well as (6) photometrically monitor stellar flares on a low mas M dwarf. In this paper we discuss this unique instrument, its design, performance, and the areas of science for which it is the only device able to successfully observe objects of interest.
G. Benedict, Barbara McArthur, Edmund Nelan, William Jefferys, Otto Franz, Larry Wasserman, Darrell Story, Peter Shelus, A. Whipple, Arthur Bradley, R. Duncombe, Q. Wang, Paul Hemenway, William van Altena, Laurence Fredrick
Space-based interferometry already exists. We describe our experiences with on-orbit calibration and scientific observations with Fine Guidance Sensor 3 (FGS 3), a white- light interferometer aboard Hubble Space Telescope. Our goal, 1 millisecond of arc precision small-field astrometry, has been achieved, but not without significant challenges. These included a mechanically noisy on-orbit environment, the self-calibration of FGS 3, and significant temporal changes in our instrument. Solutions included a denser set of drift check stars for each science observation, fine- tuning exposure times, overlapping field observations and analyses for calibration, and a continuing series of trend- monitoring observations. HST FGS 3 will remain a competitive astrometric tool for faint targets in crowded fields and for faint small-separation binaries until the advent of large- aperture, ground-based and longer-baseline space-based interferometers.
KEYWORDS: Stars, Control systems, Prisms, Servomechanisms, Calibration, Monochromatic aberrations, Signal attenuation, Space operations, Mirrors, Interferometers
The three fine guidance sensors on-board the Hubble Space Telescope are the first white-light amplitude shearing interferometers to be used for space platform guidance, control, and astrometry. Two fine guidance sensors (FGS) under fine lock control now maintain spacecraft pointing precision to within 7 milliseconds of arc rms over the majority of each orbit. Fine guidance sensor control optimization techniques have yielded significant improvement in tracking stability, integrated performance with the pointing control system, loss-of-lock statistics and astrometric accuracy. We describe the optical interferometer, based on the Koester's prism design. We include a discussion of the instrument calibration status, the FGS fine lock performance design enhancements, pointing control system design enhancements, and ground software techniques appropriate to jitter removal in astrometric data. The combination results in marc sec precision astrometry.
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