The sole instrument on NASA’s ICESat-2 spacecraft shown in Figure 1 will be the Advanced Topographic Laser Altimeter System (ATLAS)1. The ATLAS is a Light Detection and Ranging (LIDAR) instrument; it measures the time of flight of the six transmitted laser beams to the Earth and back to determine altitude for geospatial mapping of global ice. The ATLAS laser beam is split into 6 main beams by a Diffractive Optical Element (DOE) that are reflected off of the earth and imaged by an 800 mm diameter Receiver Telescope Assembly (RTA). The RTA is composed of a 2-mirror telescope and Aft Optics Assembly (AOA) that collects and focuses the light from the 6 probe beams into 6 science fibers. Each fiber optic has a field of view on the earth that subtends 83 micro Radians. The light collected by each fiber is detected by a photomultiplier and timing related to a master clock to determine time of flight and therefore distance. The collection of the light from the 6 laser spots projected to the ground allows for dense cross track sampling to provide for slope measurements of ice fields. NASA LIDAR instruments typically utilize telescopes that are not diffraction limited since they function as a light collector rather than imaging function. The more challenging requirements of the ATLAS instrument require better performance of the telescope at the ¼ wave level to provide for improved sampling and signal to noise. NASA Goddard Space Flight Center (GSFC) contracted the build of the telescope to General Dynamics (GD). GD fabricated and tested the flight and flight spare telescope and then integrated the government supplied AOA for testing of the RTA before and after vibration qualification. The RTA was then delivered to GSFC for independent verification and testing over expected thermal vacuum conditions. The testing at GSFC included a measurement of the RTA wavefront error and encircled energy in several orientations to determine the expected zero gravity figure, encircled energy, back focal length and plate scale. In addition, the science fibers had to be aligned to within 10 micro Radians of the projected laser spots to provide adequate margin for operations on-orbit. This paper summarizes the independent testing and alignment of the fibers performed at the GSFC.
KEYWORDS: Mirrors, Telescopes, Optical design, Space telescopes, Staring arrays, Sensors, James Webb Space Telescope, Infrared telescopes, Observatories, Ray tracing
The WFIRST-AFTA Wide-Field Infrared Survey Telescope TMA optical design provides 0.28-sq°FOV Wide Field Channel at 0.11” pixel scale, operating at wavelengths between 0.76-2.0μm, including a spectrograph mode (1.35-1.95μm.) An Integral Field Channel provides a discrete 3”x3.15” field at 0.15” sampling.
We present the Wide Field Infra-Red Survey Telescope (WFIRST) wide field instrument concept based on the reuse of a
2.4m telescope recently made available to NASA. Two instrument channels are described, a wide field channel
(~0.8x0.4degrees, 300Mpix, imaging and spectroscopy over 0.76-2.0um), and an integral field unit (3x3 arcsec, 1Mpix,
R{2pixel} ~100 over 0.6-2.0um). For this mission concept, the telescope, instruments, and spacecraft are in a
geosynchronous orbit and are designed for serviceability. This instrument can accomplish not only the baseline exoplanet
microlensing, dark energy, and infrared surveys for WFIRST, but can perform at higher angular resolution and with
deeper observations. This enables significant opportunities for more capable general observer programs. The emphasis
on achieving very good imaging stability is maintained from the previous work.
For the purpose of this paper, actual field curvature is the field dependent departure of the location of best image quality from a nominal surface along the direction of the optical axis. Usually this nominal surface is a plane where an image is formed and acquired. To the extent that location of best focus is displaced from it, the image is degraded due to defocus. Because the departure follows a curve in general, image quality over the field of view is compromised. Various image quality metrics can be used to calculate actual field curvature. These can also be used to generate contours of equivalent image quality, or isoquals, which are orthogonal to actual field curvature. This yields a solid method for evaluating how good the image quality of an optical system must be. It also yields a method for gaging geometric image quality versus diffraction and spawns new definitions for diffraction limited image quality.
Filters are employed in optical systems to reduce stray light and block unwanted spectra. However, common filter materials are susceptible to solarization, a bulk degradation wherein the material properties change when exposed to UV radiation. A new decay model is developed to describe this behavior. Solarization effects for various kinds of filters are measured and recommendations for mitigation are made.
The Rapid Confocal Sensor delivers sub-micron depth and five-micron lateral resolutions over a 300-mm format. With some a priori knowledge of a sample, an analysis over the 300-mm field is completed in approximately 7 minutes. An overview of the optical system (sensor) is given. Application of this technology is made to rapid 3D process inspection of semiconductor samples, particularly die contact bumps. Results demonstrating performance from a commercially available system are presented.
The concept and design for a novel four-quadrant position and focus error sensor are presented. Expected performance and theory of operation of the astigmatic focus sensor are presented. Features include wide field of view, broad wavelength coverage, high efficiency, integral field and pupil stops, and alignment and assembly benefits. A new method for sectioning the field is utilized, an internal mirrorlette array (IMA). The advantages of the IMA are given. This error sensor is implemented in the WIYN Tip-Tilt Module, an add-on imaging instrument for the 3.5 m WIYN telescope at Kitt Peak National Observatory.
The Kitt Peak Mayall 4-m telescope required a new prime focus corrector having a flat focal plane covering 36 arcmin on a side (51 arcmin diagonal) to accommodate the Mosaic 8K X 8K CCD system. The scientific requirements for the new corrector included atmospheric dispersion compensation (ADC), excellent near-UV efficiency, excellent image quality, and extremely low scattered light and ghosting. The optical system designed to meet these demands exhibits excellent and stable performance through its first year of operation. This paper describes the innovative design and engineering aspects of the corrector. Science verification data are presented to demonstrate some of the attributes of the new corrector.
A number of common building materials and finishes are found to be phosphorescent. To avoid this as a source of stray light, it is suggested that with sensitive low-light level systems, material selection be done judiciously and with cognizance of this phenomenon. Luminous radiance and decay properties for various materials are presented. The common causative ingredient of phosphorescent materials is identified as titanium di-oxide (TiO2), an increasingly popular and widespread white pigment. Techniques used to discover and check questionable articles are presented.
Grazing incidence reflections as a source of stray light are a problem which continues to beleaguer optical systems and instrumentation. These reflections tend to be specular and are a primary cause of ghosting. Traditional means of blackening (absorption) fail miserably. Techniques of scattering the undesirable/problem light into a larger (and more benign) solid angle, while successful, are often impractical. Furthermore, while these techniques excel at reducing ghosting, they typically redirect significant light into the diffuse background, reducing the SNR. Black flocking combines the advantages of absorption and scattering. Historical disadvantages of flocking are its poor durability and the difficulty of applying flock to irregular surfaces. Presented here, is the technique of electrostatic application, which overcomes these shortfalls. BRDF (bi-directional reflectance distribution function) measurements of black flocking are presented and comparisons made with other blackening techniques. An example of this technique is shown where it is used to improve a low-light spectrographic instrument. Finally, proposed specifications for the application of (black) flocking are made for use in optics.
Fiber-fed spectrographs have now been employed in astronomy for several years. They offer the principle advantages of increasing the number of objects with which simultaneous spectra may be recorded, better stability, an improvement in versatility, and factors associated with the mode-scrambling properties of fibers. However, the nature of these spectrographs pose new questions of certain design parameters. A traditional figure of merit for spectrographs is the throughput-resolution product (A(Omega) R). It is shown that A(Omega) R is no longer a constant as the entrance `slit' is varied. Here, `slit' has a new meaning. In both the first and higher order optics sense, A(Omega) R is investigated and compared with a better figure of merit. This new figure of merit maximizes the potential information content at the spectrograph focal plane. At a minimum, it incorporates the oft neglected instrument response and transmission/efficiency parameters (such as with a grating). Other refinements are made as well. Comparisons may be made both across spectrometer types and as a design guide within a family, where options must be evaluated.
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