National Aeronautics and Space Administration
Small Business Innovation Research 2001 Program Solicitation

TOPIC S3 Astronomical Search for Origins

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S3.01 Ultralight Adaptive Large Telescope Systems
S3.02 Precision Constellations for Interferometry
S3.03 Astronomical Instrumentation
S3.04 Astrobiology
S3.05 High Contrast Astrophysical Imaging

NASA's Origin's Program seeks the answers to two broad questions related to life on Earth as we know it. How did we get here and are we alone? The answers lie in an understanding of how galaxies, stars, and planetary systems were formed in the early universe. We must determine whether planetary systems and Earth-like planets are typical companions of average stars and if life beyond Earth is a rare, possibly nonexistent, occurrence or if it is robust and has spread throughout the galaxy. Origin's primary mission goals are to study the early universe, find planets around other stars, and search for life beyond Earth. The technologies and discoveries needed to achieve these goals fall into the categories of very large space observatory systems, precision spacecraft constellations, advanced astronomical instrumentation, and new techniques for laboratory astrobiology.

S3.01 Ultralight Adaptive Large Telescope Systems
Lead Center: MSFC
Participating Center(s): GSFC, JPL, LaRC

The long-range goal of the Astronomical Search for Origins and Planetary Systems (ASO) theme in the Space Science Enterprise is to detect, characterize, and ultimately image extra-solar planets in orbit around nearby stars. Results from these efforts may provide clues as to the existence of life on these planets and the nature of life within our own solar system. The level of image resolution needed to accomplish these observations requires the development of telescopes with light gathering apertures that are many times the size of NASA's 8-meter Next Generation Space Telescope (NGST). Such large aperture requirements have recently stimulated the development of new and unconventional telescope design concepts, ranging from single light collection stations employing a myriad of distributed reflective mirrors to constellations of large telescopes flying in formation and operating as interferometers.

In addition to a large aggregate aperture requirement, these new observatories must maintain a low areal density (including the optics, reaction structure, actuators, and wiring). 100 kg/m² is typical for conventional telescopes, and NGST is striving to achieve between 10 and 15 kg/m². However, for ASO missions and other future telescope programs, areal densities of " kg/m² or less are required to enable affordable and launchable system architectures. Other system design considerations include the ability to deploy components from a stowed launch configuration to a final on-orbit configuration without degrading the system's optical quality, the need for precise structural and system control mechanisms used to maintain diffraction-limited imaging capabilities, and the ability to successfully endure and perform within the harsh space environment.

Specifically, this subtopic is soliciting concepts and enabling technologies for large space-based telescope systems designed to accomplish either near-term objectives (i.e., ~10m apertures and 1-10kg/m² areal densities) and/or far-term objectives (i.e., 20-40m apertures and < 1kg/m² areal densities). Specific areas of interest include:

• Novel concepts for space telescope system design and implementation
• Active/adaptive wavefront sensing and control at ambient and cryogenic temperatures
• Large, lightweight, cryogenic, optical materials
• Large, transmissive optics and optical materials
• Large, reflective optics and optical materials
• Low cost, in situ metrology techniques for space-deployed optics
• Low areal density precision structures
• Pliable structures with shape memory
• Low weight, low cost actuators for optical surfaces
• Deformable, controllable optics
• Membrane mirrors
• Non-contacting, shape control actuation for membrane mirrors
• Integral membrane mirror and shape control actuation subsystem
• Membrane mirror packaging and deployment
• Large, aperture telescope structures, materials, and deployment

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S3.02 Precision Constellations for Interferometry
Lead Center: JPL
Participating Center(s): None

This subtopic includes hardware and software technologies necessary to establish, maintain and operate hyper-precision spacecraft constellations at a level that enables separated spacecraft optical interferometry. Also included are technologies for analysis, modeling and visualization of such constellations.

In a constellation for large effective telescope apertures, multiple, collaborative spacecraft in a precision formation collectively form a variable-baseline interferometer. These formations require the capability for autonomous precision alignment and synchronized maneuvers, reconfigurations, and collision avoidance. It is important that, in order to enable precision spacecraft formation keeping from coarse requirements (relative position control of any two spacecraft to less than one cm, and relative bearing of 1 arcmin over target range of separations from a few meters to tens of kilometers) to fine requirements (micron relative position control and relative bearing control of 0.1 arcsec), the interferometer payload would still need to provide at least 1 to 3 orders of magnitudes improvement on top of the S/C control requirements. The spacecraft also require onboard capability for optimal path planning, and time optimal maneuver design and execution.

Innovations that address the above precision requirements are solicited for distributed constellation systems in the following areas:

• Integrated optical/formation/control simulation tools
• Distributed, multi-timing, high fidelity simulations
• Formation modeling techniques
• Precision guidance, control architectures and design methodologies
• Centralized/decentralized formation estimation
• Distributed sensor fusion
• RF/optical precision metrology systems
• Formation sensors
• Precision micro-thrusters/actuators
• Autonomous re-configurable formation techniques
• Optimal, synchronized, maneuver design methodologies
• Collision avoidance mechanisms
• Formation management and station keeping
• Six degrees of freedom precision formation testbeds

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S3.03 Astronomical Instrumentation
Lead Center: JPL
Participating Center(s): ARC

Much of the scientific instrumentation used in future NASA observatories for the Origins Program theme will be similar in character to instruments used for present day space astrophysical observations. However, the performance and observing efficiency of these instruments must be greatly enhanced. The instrument components are expected to offer much higher optical throughput, larger fields of view, and better detector performance. The wavelengths of primary interest extend from the near-infrared to past 100 microns. Measurement techniques include imaging, photometry, spectroscopy, coronography, and polarimetry. Of particular interest are technologies supporting the following:

Advanced Detectors
These efforts should propose breakthrough capabilities in spectral coverage, large array size with uniform high quantum efficiency, ultra-low dark current, elevated operating temperatures, spectroscopic capabilities, or their ability to operate effectively and reproducibly over long periods (ex. 5-10 years of space observations at low power, extreme temperatures, etc.).

High Performance Filters
There is a critical need for filters with good in-band transmission and very low out-of-band transmission at all wave-lengths of interest but particularly at wavelengths > 5 microns. Desirable passbands range from 50 percent to less than 1 percent with in-band transmissions > 70 percent.

Other Optical and Opto-mechanical Instrument Components
Given the call for multiple capability instruments, there is a growing need for breakthrough concepts in instrument optics which minimize the volume requirements while adding capabilities (spectral, or otherwise) to the instrument. These elements may include gratings, prisms, dichroics, or other novel components.

Mechanical Coolers
The best detectors for wavelengths > 5 microns usually need to be cooled to < 10 K. There are a number of proposed Origins missions which have cooling requirements from 50 mK to 20 K; highly stable (both mechanical and temperature stability), long life coolers are needed for these. Efforts may address the component level such as materials for magnetic refrigerants or novel heat switches, or they may address entire systems such as pulse tube, J-T, sorption, or sub-kelvin coolers.

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S3.04 Astrobiology
Lead Center: ARC
Participating Center(s): None

Astrobiology includes the study of the origin, evolution and distribution of life in the universe. New technologies are required to enable the search for extant or extinct life elsewhere in the solar system, to obtain an organic history of planetary bodies, to discover and explore water sources elsewhere in the solar system and to distinguish microorganisms and biologically important molecular structures within complex chemical mixtures. For example, gaseous biomarkers, produced by microbial communities, are among our targets in current search strategies for life in the atmospheres of extrasolar planets. Both gaseous and mineral biomarkers produced by these communities are profoundly affected by internal biogeochemical cycling. The small spatial scales at which these biogeochemical processes operate necessitate measurements made using microsensors. Microbial ecology research at NASA could benefit enormously from collaboration of sensor technologists and microbial ecologists. The search for life on other planetary bodies will also require systems capable of moving and deploying instruments across and through varied terrain to access biologically important environments.

A second element of Astrobiology is the understanding of the evolutionary development of biological processes leading from single cell organisms to multi-cell specimens and to complex ecological systems over multiple generations. Understanding the effects of gravity on the evolution of living systems is a fundamental question of substantial, inherent scientific value in our quest to understand life. In addition, radiation of varying levels is assumed to have varying effects on the development and evolution of life. Knowledge of the effects of radiation and gravity on lower organisms, plants, humans and other animals (as well as elucidation of the basic mechanisms by which these effects occur) will be of direct benefit to the quality of life on Earth. These benefits will occur through applications in medicine, agriculture, industrial biotechnology, environmental management and other activities dependent on understanding biological processes over multiple generations.

A third component of Astrobiology includes the study of evolution on ecological processes. Astrobiology intersects with NASA Earth science studies through the highly accelerated rate of change in the biosphere being brought about by human actions. One particular area of study with direct links to Earth science is microbe-environment interactions. These interactions can be seen in carbon cycles and nitrogen cycles. Some examples of rapid changes that affect these microbial processes are increases in UV, increases in average and seasonal temperatures, and changes in the length of the growing season, all which are key issues in both Earth Science and Astrobiology. Additional areas include Controlled Environment Sustainability Research (CESR), growth chambers and monitoring capabilities. This research requires unique instrumentation and information science technologies that are not covered in the Earth science program.

NASA seeks innovations in the following technology areas:

Mobility/Sampling/Subsurface Water Detection Systems

• Innovative techniques that meet these needs are required, e.g., for Mars exploration, technologies that would enable the aseptic acquisition of deep subsurface samples, the detection of aquifers, or the enhancement at the performance of long distance ground roving, tunneling, or flight vehicles are required. For Europa exploration, technologies which enable the penetration of deep ice are required. Desirable features for both Mars and Europa exploration include the ability to carry an array of instruments and imaging systems, to provide aseptic operation mode, and to maintain a pristine research environment.
• Low cost lightweight systems to assist in the selection and acquisition of the most scientifically interesting samples are also of significant interest.

Analytical Tools

• High sensitivity (femtomole or better), high resolution methods applicable to all biologically relevant classes of compounds for separation of complex mixtures into individual components.
• Advanced in situ and laboratory based, microbial sensing/monitoring system capable of providing quantitative spatial and temporal visualization of material and functions in selected specimens. Advanced miniaturized biological in situ sample acquisition and handling systems optimized for extreme environment applications.
• High sensitivity (femtomole or better) characterization of molecular structure, chirality, and isotopic composition of biogenic elements (H, C, N, O, S) embodies individual compounds and structures.
• High spatial resolution (5 angstrom level) electron microscopy techniques to establish details of external morphology, internal structure, elemental composition and mineralogical composition of potential biogenic structures.
• Innovative software to support studies of the origin and evolution of life. The areas of special interest are (1) biomolecular and cellular simulations; (2) evolutionary and phylogenetic algorithms and interfaces; (3) DNA computation; and (4) image reconstruction and enhancement for remote sensing.
• In order to address the imperative to understand gaseous biomarker production, we desire technologies capable of measuring a range of volatile compounds at small spatial scales, possibly through the coupling of gas diffusion sensors to portable mass spectrometers. Improved sensor designs for a wide range of analytes, including oxygen, pH, sulfide, carbon dioxide, hydrogen, and small molecular weight organic acids both on and near surfaces that could serve as habitats for microbes.
• Nondestructive structural characterization of micro-areas of microsamples of rocks and minerals by diffraction (1-100 micron scale). Tools to Support Gravity and Radiation Studies of Biological Systems over Multiple Generations These technologies must be miniaturized to minimize weight, volume and power requirements and must operate autonomously for extended periods of time to accommodate monitoring multiple generations of organisms. Thus, instrumentation must be self-calibrating, require no or minimal consumables and be remotely controlled.
• Biotechnology - determining mutation rates and genetic stability in a variety of organisms as well as accurately determining protein regulation changes in microgravity and radiation environments.
• Automated chemical analytical instrumentation for determining gross metabolic characteristics of individual organisms and ecologies as well as chemical composition of environments.
• Spectral/imaging technology with high resolution and low power requirements.
• Habitat support - technologies for supporting miniature ecosystems isolated from their support environments, data collection and transmission technologies in concert with the automated chemical instrumentation described above. Candidate technologies include sensor and telemetry systems as well as variable-spectrum, low power light sources for simulating conditions on the early Earth.

Algorithms for processing and analyzing recovered data. Instrumentation and information technologies to support the study of evolution of ecological processes and CESR are:

• Miniature to microscopic, high resolution, field worthy, smart sensors or instrumentation for the accurate and unattended monitoring of environmental parameters that include, but are not limited to, solar radiation (190-800 nm at < 1nm resolution), ions and gases of the various oxidation states of carbon and nitrogen (at the nanomolar level for ions in solution and at the femtomolar or better level for gases), in a variety of habitats (e.g., marine, freshwater, acid/alkaline hot springs, Antarctic climates or boreholes into the Earth).
• High resolution, high sensitivity (femtomole or better) methods for the isolation and characterization of nucleic acids (DNA/RNA) from a variety of organic and inorganic matrices.
• Mathematical models capable of predicting the combined effects of elevated pCO2 (change in CO2 over the eons) and solar UV radiation on carbon sequestration and N2O emissions from experimental data obtained from field and laboratory studies of C-cycling rates, N-cycling rates, as well as diurnal and seasonal changes in solar UV.
• Microscopic techniques and technologies to study soil cores, microbial communities, pollen samples, etc. in a laboratory environment for the detailed spectroscopic analysis relevant to evolution as a function of climate changes.
• Robotic system designed to provided access to terrestrial and extraterrestrial environments such as deep ocean, hydrothermal vents.

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S3.05 High Contrast Astrophysical Imaging
Lead Center: JPL
Participating Center(s): None

This subtopic addresses the unique problem of imaging faint astrophysical objects that are located within the obscuring glare of much brighter sources. Some examples include planetary systems beyond our own and the detailed, inner structure of galaxies with very bright nuclei. Contrast ratios of one million to one billion over an angular spatial scale of less than one arcsecond are typical of these objects.

The innovative research focuses on advances in coronagraphic and star light cancellation instruments that operate at visible and infrared wavelengths. Typically, these instruments would be intended for operation in space as part of a future observatory mission. Some examples of areas of interest include:

• Ultra-low scatter optics and coatings
• Advanced aperture apodization techniques
• High precision, wavefront, error sensing techniques
• Small stroke, high precision deformable mirrors and controllers
• Advanced starlight coronagraphic instrument concepts
• Interferometric starlight cancellation techniques

For infrared applications, operating at cryogenic temperatures is a typical requirement.

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