The Plankton, Aerosol, Cloud, ocean Ecosystem (PACE) satellite is a strategic climate continuity mission that will answer new and emerging advanced science questions related to Earth’s changing climate. These science goals are accomplished via PACE’s main optical instrument, a sophisticated spectrograph, the Ocean Color Instrument (OCI) consisting of UV/VIS and VIS/NIR channels each complete with a dichroic, grating, and detector. We will overview the characterization methods used for each component, with respect to its metrology targets, and further discuss how baseline characterization served as a proxy when lines of sight to the optical components’ boresights were lost in later integration steps.
The NASA Goddard Space Flight Center (GSFC) and its partners have broad experience in the alignment of flight optical instruments and spacecraft structures. Over decades, GSFC developed alignment capabilities and techniques for a variety of optical and aerospace applications. In this paper, we provide an overview of a subset of the capabilities and techniques used on several recent projects in a “toolbox” format. We discuss a range of applications, from small-scale optical alignment of sensors to mirror and bench examples that make use of various large-volume metrology techniques. We also discuss instruments and analytical tools.
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.
The optical alignment of the star trackers on the Global Precipitation Measurement (GPM) core spacecraft at NASA
Goddard Space Flight Center (GSFC) was challenging due to the layout and structural design of the GPM Lower Bus
Structure (LBS) in which the star trackers are mounted as well as the presence of the star tracker shades that blocked
line-of-sight to the primary star tracker optical references. The initial solution was to negotiate minor changes in the
original LBS design to allow for the installation of a removable item of ground support equipment (GSE) that could be
installed whenever measurements of the star tracker optical references were needed. However, this GSE could only be
used to measure secondary optical reference cube faces not used by the star tracker vendor to obtain the relationship
information and matrix transformations necessary to determine star tracker alignment. Unfortunately, due to
unexpectedly large orthogonality errors between the measured secondary adjacent cube faces and the lack of cube
calibration data, we required a method that could be used to measure the same reference cube faces as originally
measured by the vendor. We describe an alternative technique to theodolite autocollimation for measurement of an
optical reference mirror pointing direction when normal incidence measurements are not possible. This technique was
used to successfully align the GPM star trackers and has been used on a number of other NASA flight projects. We also
discuss alignment theory as well as a GSFC-developed theodolite data analysis package used to analyze angular
metrology data.
The Solar Terrestrial Relations Observatory (STEREO) is a pair of identical satellites that will orbit the Sun so as to drift ahead of and behind Earth respectively, to give a stereo view of the Sun. STEREO is currently scheduled for launch in November 2005. One of the instrument packages that will be flown on each of the STEREO spacecrafts is the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI), which consists of an extreme ultraviolet imager, two coronagraphs, and two side-viewing heliospheric imagers to observe solar coronal mass ejections all the way from the Sun to Earth. We report here on the inner coronagraph, labeled COR1. COR1 is a classic Lyot internally occulting refractive coronagraph, adapted for the first time to be used in space. The field of view is from 1.3 to 4 solar radii. A linear polarizer is used to suppress scattered light, and to extract the polarized brightness signal from the solar corona. The optical scattering performance of the coronagraph was first modeled using both the ASAP and APART numerical modeling codes, and then tested at the Vacuum Tunnel Facility at the National Center for Atmospheric Research in Boulder, Colorado. In this report, we will focus on the COR1 optical design, the predicted optical performance, and the observed performance in the lab. We will also discuss the mechanical and thermal design, and the cleanliness requirements needed to achieve the optical performance.
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