Enabling tilt and imaging-while-slewing for ground-based liquid mirror telescopes would allow for very large-scale, lowcost mirror solutions. To explore how to accomplish this, our team has taken a systems approach leveraging optical, manufacturing, material, and modeling expertise to address the key technical challenges of creating a stable liquid surface. These technical challenges include maintaining optical quality surface figures while slewing and tilting, creating high optical reflectance concomitantly with controllable liquids, characterizing large-scale deformable optics, and manufacturing and scalability of proposed designs to greater than 50 m configurations. In this paper, we present both a solution framework as well as preliminary modeling results to demonstrate mirror feasibility for a ferrofluid, magnetically-actuated approach.
In parallel with the overall telescope liquid mirror design effort, we discuss nanomaterial synthesis techniques for reflective ferrofluid as well as manufacturing development of a magnetically permeable metallic paraboloid shell with surface wicking structure and electromagnetic control coil arrays. The forces from the coils and capillarity from the wick establish the requisite control and stability to deliver required wavefront performance and maintain fluid stability. We share our initial model and small-scale coupon test results for baseline ferrofluid, wicking structure, and actuation inputs to demonstrate feasibility. We also outline next steps for our optical and ferrofluid modeling and material synthesis for a prototype 50 cm mirror we anticipate building in the near future.
For the Large Ultraviolet/Optical/Infrared Surveyor (LUVOIR) to perform high-contrast direct imaging of habitable exoplanets using a coronagraph instrument, the system must maintain extremely low system dynamic wavefront error (on the order of 10 picometers RMS over the spatial frequencies corresponding to the dark-hole region of the coronagraph) over a long time wavefront control sampling interval (typically 10 or more minutes). Meeting this level of performance requires a telescope vibration isolation system that delivers a high degree of dynamic isolation over a broad frequency range. A non-contact pointing and isolation system called the Vibration Isolation and Precision Pointing System (VIPPS) has been baselined for the LUVOIR architecture. Lockheed Martin has partnered with NASA to predict the dynamic wavefront error (WFE) performance of such a system, and mature the technology through integrated modeling, subsystem test and subscale hardware demonstration. Previous published results on LUVOIR dynamic WFE stability performance have relied on preliminary models that do not explicitly include the effects of a segmented Primary Mirror. This paper presents a study of predicted dynamic WFE performance of the LUVOIR-A architecture during steady-state operation of the coronagraph instrument, using an integrated model consisting of a segmented primary mirror, optical sensitivities, steering mirror and non-contact isolation, and control systems. The design assumptions and stability properties of the control system are summarized. Principal observatory disturbance sources included are control moment gyroscope and steering mirror exported loads. Finally, observatory architecture trades are discussed that explore tradeoffs between system performance, concept of operation and technology readiness.
The telescope form known as the Three Mirror Anastigmat (TMA), has gained in popularity as optical manufacturing and optical test techniques have improved. TMAs are now widely used throughout the optical industry, and are described in numerous publications. These telescopes may be designed to produce output beams that are afocal (collimated) or focal. In this paper, the optimal surface shapes will be examined for both types of TMA telescopes. Optimal is defined to be the surface shapes that minimize the wavefront error (WFE). The following design constraints are applied: the entrance pupil is on the primary mirror (PM) and the system WFE is largely free of primary spherical aberration, coma, astigmatism, and field curvature. Variable design parameters include: the radius of curvature of the PM, the distance to the secondary mirror (SM) the effective focal length, and the system magnification. Additionally, many first order optical parameters are derived from this selection of inputs. In particular, the differences in wavefront error aberrations associated with focal and afocal TMAs are characterized, and it is shown that the conic constant of the PM is ideally -1, resulting in a parabolic surface shape, to achieve the lowest design residual WFE for afocal TMAs. In contrast, focal TMAs are shown to require a PM surface that is an ellipsoid, with conic constant k in the range -1 < k < 0. Example telescope designs are illustrated.
MTF is one of the most common metrics used to quantify the resolving power of an optical component. Extensive literature is dedicated to describing methods to calculate the Modulation Transfer Function (MTF) for stand-alone optical components such as a camera lens or telescope, and some literature addresses approaches to determine an MTF for combination of an optic with a detector. The formulations pertaining to a combined electro-optical system MTF are mostly based on theory, and assumptions that detector MTF is described only by the pixel pitch which does not account for wavelength dependencies. When working with real hardware, detectors are often characterized by testing MTF at discrete wavelengths. This paper presents a method to simplify the calculation of a polychromatic system MTF when it is permissible to consider the detector MTF to be independent of wavelength.
Mathematical models are used to establish the exact path of a beam reflected by a plane mirror in terms of the mirror geometry descriptors. In particular, the mirror geometry descriptors (tilt angles) are determined as functions of the beam path in image space. This is also useful for determining scan patterns when the mirror is used as a scanning device. These formulations are readily adaptable to commercially available ray tracing programs.
KEYWORDS: Sapphire, Reflection, James Webb Space Telescope, Optical testing, Optical alignment, Refractive index, Space telescopes, Near infrared, Cameras, Cryogenics
The Near Infrared Camera (NIRCam) instrument used to align and obtain science data for NASA’s James Webb Space Telescope (JWST) was tested at the module level at flight-like cryogenic temperature. This paper explains the innovative techniques used to measure the precise location and orientation of the modules. A laser tracker was used to precision locate the instrument, using a flat reference mirror/reticle surface on the modules inside a chamber through its port windows. This technique established 6 degrees of freedom of position and orientation. The accuracy achieved was on the order of 20 microns in position and 5 arc-seconds in angular orientation.
KEYWORDS: Reticles, James Webb Space Telescope, Mirrors, Cameras, Environmental sensing, Cryogenics, Near infrared, Autocollimation, Space telescopes, Optical alignment
The Near Infrared Camera (NIRCam) instrument used to align and obtain science data for NASA’s James Webb Space Telescope (JWST) was tested at the module level at flight-like cryogenic temperature. This paper explains the background that created the innovative techniques used to measure NIRCam’s modules alignments in 6 degrees of freedom (DOF) inside a thermal vacuum chamber. All 6 DOF were measured remotely, through a single chamber window port, using only a flat reference mirror/reticle surface mounted on each module. This measured orientation was then used to determine the optical input axis and entrance pupil for each module. The accuracy achieved was on the order of 20 microns in position and 5 arc seconds in angular orientation.
The NIRCam instrument on the James Webb Space Telescope (JWST) will provide a coronagraphic
imaging capability to search for extrasolar planets in the 2 - 5 microns wavelength range. This capability is
realized by a set of Lyot pupil stops with patterns matching the occulting mask located in the JWST
intermediate focal plane in the NIRCam optical system. The complex patterns with transparent apertures
are made by photolithographic process using a metal coating in the opaque region. The optical density
needs to be high for the opaque region, and transmission needs to be high at the aperture. In addition, the
Lyot stop needs to operate under cryogenic conditions. We will report on the Lyot stop design, fabrication
and testing in this paper.
KEYWORDS: Monte Carlo methods, Tolerancing, Staring arrays, James Webb Space Telescope, Optical components, Optical alignment, Cameras, Content addressable memory, Systems modeling, Cryogenics
The requirements for the Near Infrared Camera (NIRCam) instrument for NASA's James Webb Space Telescope (JWST) specify that the instrument be aligned and operate at cryogenic temperatures. The error budget for the integration of the optical components was analyzed using a multi-parameter Monte Carlo simulation with compensators. Results from these simulations were used to revise the alignment process and error budget. This paper presents an overview of this analysis.
The requirements for the Near Infrared Camera (NIRCam) instrument for NASA's James Webb Space Telescope (JWST) designate that the instrument be aligned to within specified wavefront tolerance limits. A sensitivity analysis was performed to determine the best selection of field point locations and wavelengths at which to take measurements to meet the wavefront requirements. This paper presents an overview of this analysis.
The aspheric reflecting surface types studied by L. Mertz for correcting certain aberrations of a spherical primary telescope mirror are examined and some properties of these surfaces are presented. For the one-surface aspheric that corrects spherical aberration of all orders, a sixth-order equation for the surface shape is derived. For the set of two aspheric surfaces correcting spherical aberration and coma of all orders, a set of differential equations has been developed to describe the surface shapes. The off-axis imaging performance is derived from the on-axis imaging properties and compared with ray-trace results.
The aspheric reflecting surface types studied by L. Mertz for correcting certain aberrations of a spherical primary
telescope mirror are examined and some properties of these surfaces are presented. For the one-surface aspheric that
corrects spherical aberration of all orders, a 6th order equation for the surface shape is derived. For the set of two
aspheric surfaces correcting spherical aberration and coma of all orders, a set of differential equations have been
developed to describe the surface shapes. The off-axis imaging performance is derived from the on-axis imaging
properties and compared with ray trace results.
Optical systems, which operate over a wide range of Fresnel numbers, are often times performance-limited by diffraction effects. In order to characterize such effects at the 40-100 picometer level, a diffraction testbed has been built which has the capability of measuring diffraction effects at this level. Concurrently, mathematical diffraction modeling tools have been developed that propagate an input wavefront through an optical train, while retaining amplitude and phase information at a grid resolution sufficient for yielding picometer-resolution diffraction test data. This paper contains a description of this diffraction hardware testbed, the diffraction modeling approach, and a comparison of the modeled and hardware test results, which then serves as validation of the diffraction modeling methodology.
Using the Lockheed in-house computer program OPTIMA for optical design and analysis, a facility has been implemented which enables the optical designer to target any performance parameter at any temperature in the range of interest. A database with thermal properties of the optical materials was added to the program along with routines facilitating the evaluation of an optical system at arbitrary temperatures. In the optimization section of the program, alternate lens configurations are used to represent the lens at different temperatures. During the optimization the program automatically changes temperature and computes the requested performance parameters at the desired temperatures. Applications for this method include the design of high-performance camera objectives optimized for a large temperature range.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.