Lessons learned from the implementation, operation, and science processing from a number of successful NASA LaRC remote sensing experiments will be presented. Despite good flight heritage, well-known designs, and known data retrieval algorithms these experiments remain challenging. The authors will summarize common lessons learned from different project phases and discuss these lessons in the context of planned and future missions with emphasis on improving Level 1 data quality.
The Stratospheric Aerosol and Gas Experiment III/Meteor Instrument was launched from Baikonur, Kazakhstan on December 10, 2001. After initial commissioning phase activities, it began routine solar occultation measurements by March 2002. During the first year of operation, additional measurement capabilities such as lunar occultation and limb scattering were successfully implemented with the SAGE III instrument. This paper will present a summary of the various data sets gathered from the SAGE III instrument during the first year of operation. Measurements of ozone, aerosol, and nitrogen dioxide from solar occultation, lunar occultation, and limb scattering techniques will be presented and discussed.
This paper presents a comparison of the three forward model computational schemes, namely, Emissivity Growth Approximation (EGA), Curtis-Godson Approximation (CGA), and line-by-line (LBL) approach developed for SAGE III water vapor retrieval. For all three schemes, we have incorporated the most recent laboratory measurements of spectral line parameters to avoid the bias which is known to exist in HITRAN-96 database. Discussions are focused on the strength and weakness of each scheme with respect to accuracy and computational efficiency. The computer time for the LBL has been reduced significantly. The advantage of the LBL is manifest when the dependence of EGA and CGA on a huge pre-calculated lookup table and the breakdown of assumptions for these two schemes at lower altitudes are taken into account.
Under a joint agreement between the National Aeronautics and Space Agency (NASA) and the Russian Aviation and Space Agency (RASA), the Stratospheric Aerosol Gas Experiment III (SAGE III) instrument
was launched in low earth orbit on December 10, 2001 aboard the Russian Meteor-3M(1) satellite from the Baikonur Cosmodrome. SAGE III is a spectrometer that measures attenuated radiation in the 282 nm to
1550 nm wavelength range to obtain the vertical profiles of ozone, aerosols, and other chemical species that are critical in studying the trends for the global climate change phenomena. This instrument version is more advanced than any of the previous versions and has more spectral bands, elaborate data gathering and storage, and intelligent terrestrial software. There are a number of Russian scientific instruments aboard the Meteor satellite in addition to the SAGE III instrument. These instruments deal with land imaging and
biomass changes, hydro-meteorological monitoring, and helio-geophysical research. This mission was under development for over a period of six years and offered a number of unique technical and program management challenges for both Agencies. SAGE III has a long space heritage, and four earlier versions of this instrument have flown in space for nearly two decades now. In fact, SAGE II, the fourth instrument, is still flying in space on NASA's Earth Radiation Budget Satellite (ERBS), and has been providing important atmospheric data over the last 18 years. It has provided vital ozone and aerosol data in the mid latitudes and has contributed vastly in ozone depletion research. Ball Aerospace built the instrument under Langley
Research Center's (LaRC) management. This paper presents the process and approach deployed by the SAGE III and the Meteor teams in performing the initial on-orbit checkout. It further documents a number of early science results obtained by deploying low risk, carefully coordinated procedures in resolving the serious operational issues of this satellite.
SAGE III is a NASA EOS instrument designed to provide long term measurements of ozone, aerosol, water vapor, and other gases in the atmosphere. The instrument was launched on a Russian Spacecraft Meteor 3M on December 10, 2001. This paper will provide a brief discussion of the SAGE III data that will be made available to the science community to perform study on problem related to global climate change issues. The SAGE III measurement strategy, data retreival technique, and the expected quality of the data products will be discussed. Preliminary data obtained from the instrument will be presented.
The Stratospheric Aerosol and Gas Experiment III (SAGE III) Meteor mission was originally scheduled for launch in the early summer of 2001. This paper will discuss the overall SAGE III/Meteor mission and provide a description of the instrument performance based on different pre-launch tests that have been performed over the last two years. Pre- launch tests include instrument radiometric throughput and calibration; wavelength calibration; polarization response; and in-atmospheric testing including sun and moon viewing. The resulting data demonstrate the capability of the instrument to provide high spectral resolution atmospheric spectral measurement in the visible to the near IR wavelength region with a high SNR. The instrument has been integrated onto the Meteor spacecraft at the NIIEM facility in Russia. Since the launch of the Meteor SAGE III has been delayed until the end of 2001, this paper will only provide a description of the planned initial operation of the SAGE III instrument after launch.
Five functional UV-VIS-NIR spectrometer/telescopes were built for the Stratospheric Aerosol and Gas Experiment III (SAGE III) satellite instrument project. Three will be on satellite platforms in the early part of the decade, and a fourth, the SAGE III Test Model (TM) is functioning as a ground-based instrument. The fifth is used as a software test-bed to support Mission Operations for the space instruments. The SAGE III instrument is spatially scanning UV-VIS-NIR holographic grating spectrometer using a cooled CCD detector. This paper presents performance results from the TM instrument. The TM instrument has been used in cross calibration studies during which one of the SAGE III flight instruments directly sampled the Sun, Moon, and twilight sky from the ground. Comparisons of SNRs, and relative responsivities are presented. TM zenith twilight spectra and measurement sensitivities are presented including a comparison of its twilight radiance measurements with the MODTRAN 3.7 atmospheric radiance/transmittance model. In addition the TM results of sampling planetary and stellar spectra are presented.
This paper presents an overview of the SAGE III water vapor retrieval algorithm. Results of simulated retrieval are shown to demonstrate the advantages of the non-linear optimization algorithm in reducing the influence of the contributions due to interfering species. Diagnostic analyses of the retrieval are conducted to examine the characteristics of the matrices of contribution functions and the averaging kernels. The results indicate that high vertical resolution profiles of water vapor can be retrieved form the SAGE III measurements and the total random errors are less than 10% for altitudes below 42 km.
This study shows that the temperature information in the upper stratosphere can be derived from the SAGE II 385-nm observations. The preliminary results indicate that the zonal mean temperature increases with altitude below 50 km and decreases above 50 km. At 50 km, a regional maximum of 263 K is located in the tropics, and a minimum of 261 K occurs in the subtropics in both hemispheres. The derived long-term temperature changes from 1985 to 1997 reveal a statistically significant negative trend of -2 to -2.5 K/decade in the tropical upper stratosphere and about -2 K/decade in the subtropics near the stratopause. At latitudes poleward of 50 degrees, the results show a statistically significant positive trend of about 1 K/decade in the upper stratosphere. The preliminary results also show large annual temperature oscillations in the extratropics with a maximum amplitude of approximately 8 K located at about 44 km near 50 degrees in both hemispheres during local summer. In addition, the semiannual oscillation is found to be a maximum in the tropics with a peak amplitude of approximately 3.3 K located at about 42 km during the equinox.
The Stratospheric Aerosol and gas Experiment III (SAGE III) is part of the NASA EOS program designed for long term monitoring of atmospheric ozone and aerosol, together with other atmospheric species important to the study of global change. SAGE III is an advanced version of the previous occultation instruments such as SAM II, SAGE I, and SAGE II which have provided long term data on aerosol and ozone for the last twenty years. SAGE III will continue these long term measurements well into the first decade of the 21st century. SAGE III will measure profiles of aerosols, ozone, water vapor, nitrogen dioxide, temperature, pressure, chlorine dioxide, and nitrogen trioxide using the solar and lunar occultation techniques. Currently two SAGE III instruments will be launched between 1999 and 2003. The First SAGE III will be on a Russian Meteor 3M spacecraft to be launched in the Fall of 1999. The second SAGE III will be on the Space Station in 2003.
An overview of joint Russian-American mission operations for the Meteor-3M/SAGE III mission is presented. The Russian Space Agency is responsible for the operation and sustaining engineering of the Meteor-3M spacecraft. The SAGE III mission operations center located at the NASA Langley Research Center is responsible for instrument operation, sustaining engineering, Level 0 data processing, and orbit determination. SAGE III science data is received at ground stations located at the NASA Wallops Flight Facility and in Russia using redundant, twice daily, data playbacks. The highly autonomous mission design requires a high degree of payload autonomy. A combination of navigation data provided by the spacecraft's GPS/GLONASS receiver and novel on-board event scheduling software is used to schedule routine occultation measurements without the need for ground commanding.
This paper presents the SAGE III mission for the International Space Station. SAGE III is fifth in a series of instruments developed to monitor aerosols and gaseous constituents in the stratosphere and troposphere. Three instruments are being developed by the National Aeronautics and Space Administration (NASA) Langley Research Center for the Earth Science Enterprise: one for a high-inclined orbit aboard the Russian Meteor-3M (M3M) spacecraft; one for a mid-inclined (51.6 deg) orbit on the International Space Station, the subject of this paper; and a third for a potential flight of opportunity (FOO) mission. The SAGE III/ISS payload is comprised of international components: a pointing platform called the Hexapod, provided by the European Space Agency and the Expedite the Processing of Experiments to International Space Station (ISS) (EXPRESS) pallet adapter, (part of a carrier system to be built by Brazil for NASA. The SAGE III/ISS mission is manifested for a launch on the ISS Utilization Flight (UF) 3, currently scheduled to launch February 2003.
The SAGE III is the fourth generation of solar occultation instruments designed to measure aerosols and trace gas species in the stratosphere and upper troposphere. It will be launched aboard a Meteor-3M platform in the summer of 1999 and the International Space Station Alpha in 2001. SAGE III preserves the robust characteristics of the SAGE series, including self-calibration and high vertical resolution, and adds new capabilities including a lunar occultation mode. This paper will describe the SAGE III instrument and outline its potential contribution to global change research.
Degradation of sensitive satellite surface scan adversely effect the accuracy, lifetime and mission effectiveness of a spacecraft or payload. More sophisticated and complex space systems have increased the concern about contamination. Thus, it has become necessary to develop better prediction tools and testing techniques for use in contamination prevention and control. This paper discusses the effect of the induced contamination environment on the long-term degradation of two remote sensing instruments. Both instruments were the subject of contamination control programs. The Stratospheric Aerosol Gas Experiment (SAGE II) was launched by the shuttle on the Earth Resources Budget Satellite in 1984. The result of a throughput degradation contamination assessment performed prior to launched compares actual results acquired through March, 1998. The SAGE II instrument still continues to produce data within the limits predicted. A Total Ozone Mapping Spectrometer was launched in 1991 on a Russian Meteor-3 spacecraft. Degradation of the solar calibration diffuser plates have been observed and reported earlier. A new instrument, SAGE II, will be launched in 1999 on another METEOR-3 spacecraft from the Baikonur Cosmodrome in Kazakhstan. The METEOR- 3M/SAGE III is currently undergoing an intense contamination control program in order that data of the same quality as the SAGE II instrument will be realized.
SAGE III is part of the Mission to Planet Earth's Earth Observatory System with a first launch in the summer of 1998. SAGE III will provide long term monitoring of atmospheric species such as ozone and aerosols which play an important role in global environmental and climatic changes. This paper will briefly describe the goal of the SAGE III experiment, the instrument design, and the development of the processing algorithm for routine data processing to produce scientifically important data products for the science community.
The results of the NRL program focuses on high resolution, high aspect ratio, patterning of W are summarized. The work investigates three parallel approaches: reactive ion etching (RIE), electron cyclotron resonance (ECR) etching, and chemically assisted ion beam etching (CAIBE). Key issues that are analyzed for each process are the etch mask, anisotropy, selectivity, etch stop, compatibility with high resolution (sub-250 nm) lithographic patterning of W, and applicability to membranes. In the first two methods, prevention of sidewall undercutting was the key issue. Here the effort focuses on sidewall passivation and substrate cooling. RIE is a commonly utilized fabrication tool and the process has been developed to etch 100 nm lines. ECR is a relatively new process and there are more degrees of freedom than RIE. Both SF6 chemistry and CBrF3 chemistry have been investigated. Methods to minimize the mask erosion are described and a comparison of Cl2 chemistry to SF6 chemistry is made. The results on the three dry etching techniques are described and contrasted.
Loretta Shirey, Kelly Foster, William Chu, John Kosakowski, Kee Rhee, Elizabeth Dobisz, Charles Eddy, D. Park, I. Peter Isaacson, Daniel McCarthy, Christie Marrian, Martin Peckerar
A process for etching fine features in tungsten (100 nm linewidth or less) to produce patterned absorbers has been developed. The pattern is first defined in a chrome etch mask on the tungsten absorber layer using e-beam lithography and s then transferred into the tungsten by reactive-ion-etching. H2 is mixed with SF6 to passivate the sidewalls of the tungsten features because SF6 alone causes severe undercutting of the features. Control of undercutting is the key challenge in reactive ion etching of tungsten. With an optimum mixture of 20% H2 and 80% SF6, plus substrate cooling to -25 degree(s)C, undercutting can be controlled for 250 nm geometries. Increased undercutting has been observed at the endpoint of the etching process, the chromium etch stop layer. This is demonstrated through a computer model. The endpoint can be controlled through laser endpoint detection. For sub 250 nm geometries, additional sidewall passivation is accomplished with an intermittent etch process, thereby allowing the etching of high aspect ratio 100 nm features in 650 nm thick tungsten layers.
SAGE III has been selected as part of the earth observing system for flight on the aerosol and chemistry satellites missions beginning in the year 2000. During lunar and solar occultation, SAGE III will measure vertical profiles of O3, NO2, H2O, NO3, OClO, temperature, and aerosols from cloud tops through the stratosphere, and of O3 through the mesosphere. This paper describes the lineage of SAGE III, its science objectives, current instrument design, details of phase B testing and analysis, expected performance, and its contributions to monitoring global change and to meeting other EOS objectives.
The SAGE III instrument, the latest in a series of satellite-based instruments employing the self-calibrating solar occultation technique to monitor aerosols and trace gases in the atmosphere, and potential contributions to monitoring global change and other EOS objectives are described. Uses of these data are illustrated with SAGE I and II long-term ozone, aerosol, and water vapor data. The SAGE III instrument will improve the SAM II and SAGE data products with greater overall accuracy, and will provide the ability to extend these measurements over a greater height range. SAGE III will provide long-term self-calibrating global data sets from the midtroposphere to mesosphere, which will contribute greatly to the quantification and understanding of global change.
The calibration plan for the SAGE III instruments for maintaining instrument performance during the Earth Observing System (EOS) mission lifetime is described. The SAGE III calibration plan consists of detailed preflight and inflight calibration on the instrument performance together with the correlative measurement program to validate the data products from the inverted satellite measurements. Since the measurement technique is primarily solar/lunar occultation, the instrument will be self-calibrating by using the sun as the calibration source during the routine operation of the instrument in flight. The instrument is designed to perform radiometric calibration of throughput, spectral, and spatial response in flight during routine operation. Spectral calibration can be performed in-flight from observation of the solar Fraunhofer lines within the spectral region from 290 to 1030 nm wavelength.
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