The detection and quantification of greenhouse gas (GHG) emissions, in particular carbon dioxide (CO2) and methane (CH4), is presently one of the main goals of remote sensing of atmospheric gasses on a global scale, for the strong impact these molecules have on climate change. Of particular urgency is the quantification of emissions from anthropogenic sources, a high-priority task addressed by the ESA Copernicus mission CO2M, which will provide global coverage detection of CO2 and CH4. The observation of CO2M, capable of quantifying emissions from the major sources, can be complemented by other observation systems addressing the smaller, and more numerous, sources. In this domain, static interferometers can offer several advantages. This paper reports on the main results of two activities completed within the ESA Future Missions activities in the Earth Observation Program, for the development of small instruments based on static interferometer designs, for the detection of CO2. The two studies, named Carbon-HIGS and Carbon-CGI, investigated two instruments operating in the SWIR and NIR bands, with a targeted precision of 2 ppm and an accuracy of 1 ppm for CO2 atmospheric concentration, covering a relatively small swath of 50 km at a spatial sampling better than 300 m. We summarize the general detection principles, the result of the design activities, and the estimated instrument performances. Both concepts are suitable candidates to work in conjunction with the Copernicus mission offering a zoom-mode observation, for quantification of medium-sized GHG sources and improved localization and understanding of anthropogenic emissions. Additional presentation content can be accessed on the supplemental content page.
CarbonHIGS is a 2D imager designed to measure the enhancement of CO2 concentration in emission plumes from power plants. The origin of HIGS, and the physics of the working principle will be explained. Two possible implementations of HIGS will be presented, i.e. one that uses power splitting while the other one uses polarization splitting. The characteristics of these implementations will be discussed. In the final part of this paper the preliminary design of the CarbonHIGS system will be shown.
The first diffraction gratings on curved substrates were manufactured by employing ruling engines by H. A. Rowland. Due to the ruling principle, these gratings are characterized by equidistant parallel lines if the line pattern is projected along the optical axis onto a tangential plane in the vertex of the grating substrate. The Offner spectrometer is based on such a classical grating on a convex spherical substrate. This spectrometer type shows very good field correction properties. Therefore, it is among the most promising spectrometer types to meet the demands of hyper-spectral imaging. A further improvement of the optical performance is based on the modification of the surface figure of the substrate to an aspherical shape while keeping the mentioned constant grating line distribution. There are many reasons to employ interference lithography/holography - and in particular the direct blazing approach - even for the generation of the specific Offner grating line distribution on the convex substrate. A main benefit of this method is the attainable nearly perfect angular orientation of the blaze facets for the whole grating aperture. Here the achievable well defined blaze structure leads to best diffraction efficiencies close to the theoretical optimum - independent from the local curvature of the substrate. To manage the more complex recording setups of direct blazed Offner gratings, reliable methods for testing the wave front quality are a necessary pre-condition. A corresponding test method based on holographic principles will be introduced in the following text. The aspherical Offner grating was designed for the application in the UV-1 spectrometer within the Sentinel 5 mission, which is part of the European Earth Observation Program Copernicus". The spectrometer is a passive grating imaging spectrometer with a swath width of 2.670km and a spatial resolution of 50x50km2.
Optical communications will complement radio frequency (RF) communications in the coming decades to enhance throughput, power efficiency and link security of satellite communication links. To enable optical communications technology for intersatellite links and (bi-directional) ground to satellite links, TNO develops a suite of technologies in collaboration with industry, which comprises of terminals with different aperture sizes, coarse pointing assemblies and fast steering mirrors. This paper presents the current state of the development of TNO technology for optical space communications. It mainly focuses on the development of an optical head with an entrance aperture of 70 mm, an optical bench for CubeSats and coarse pointing assemblies (CPAs). By continuing these steps, world wide web based on satellite communications will come closer.
Optical communications will complement radio frequency (RF) communications in the coming decades to enhance throughput, power efficiency and link security of satellite communication links. To enable optical communications technology for intersatellite links and (bi-directional) ground to satellite links, TNO develops a suite of technologies in collaboration with industry. Throughout these developments there is a particular aim for high levels of system integration, compactness and low recurring cost in order to meet the overall requirements related to market viability. TNO develops terminals with aperture sizes of 70 and 17 mm, coarse pointing assemblies and fast steering mirrors. This paper discusses the state of development of these different technologies and provides and outlook towards the future.
The impact of NO2 and other atmospheric trace gases on health and the environment is now acknowledged by governments around the world. The sources, both natural and anthropogenic, have been shown to affect the quality of life due to low air quality in densely populated areas. Consequently, the need for accurate global NO2 measurements with high spatial- and temporal resolution to monitor NO2 is becoming ever more important. Through an ESA study, TNO and KNMI have been evaluating measurement requirements and an instrument design for a ‘Compact NO2 Spectrometer’, based on a hyperspectral imaging instrument operating in the VIS (405-490nm] spectral range and aimed at combining the performance of state-of-the-art instruments with fine spatial sampling (0.5x0.5 km2). By use of a novel free-form optics a very compact low volume and low mass design has been achieved. Combining this with other small satellite design approaches for components the aim is to create a low cost instrument capable of being flown on a wide variety of space platforms. Global daily coverage can then be achieved with a relatively small constellation of instruments. The key design features are described for a ‘Compact NO2 Spectrometer’, such as the optical design approach, the use of free-form optics, an ‘athermal’ all aluminium approach. An overview of the development and airborne results from a breadboard of a small prototype system (Spectrolite) developed by TNO which uses many of the design features envisaged for this new instrument is given.
TROPOMI, the Tropospheric Monitoring Instrument, is a passive UV-VIS-NIR-SWIR trace gas spectrograph in the line of SCIAMACHY (2002) and OMI (2004), instruments with the Netherlands in a leading role. Both instruments are very successful and remained operational long after their nominal life time.
TROPOMI is the next step, scheduled for launch in 2015. It combines the broad wavelength range from SCIAMACHY from UV to SWIR and the broad viewing angle push-broom concept from OMI, which makes daily global coverage in combination with good spatial resolution possible. Using spectral bands from 270-500nm (UV-VIS) 675-775nm (NIR) and 2305-2385nm (SWIR) at moderate resolution (0.25 to 0.6nm) TROPOMI will measure O3, NO2, SO2, BrO, HCHO and H2O tropospheric columns from the UV-VIS-NIR wavelength range and CO and CH4 tropospheric columns from the SWIR wavelength range. Cloud information will be derived primarily from the O2A band in the NIR. This will help, together with the aerosol information, in constraining the light path of backscattered solar radiation. Methane (CH4), CO2 and Carbon monoxide (CO) are the key gases of the global carbon cycle. Of these, Methane is by far the least understood in terms of its sources and is most difficult to predict its future trend. Global space observations are needed to inform atmospheric models. The SWIR channel of TROPOMI is designed to achieve the spectral, spatial and SNR resolution required for this task.
TROPOMI will yield an improved accuracy of the tropospheric products compared to the instruments currently in orbit. TROPOMI will take a major step forward in spatial resolution and sensitivity. The nominal observations are at 7 x 7 km2 at nadir and the signal-to-noises are sufficient for trace gas retrieval even at very low albedos (down to 2%). This spatial resolution allows observation of air quality at sub-city level and the high signal-to-noises means that the instrument can perform useful measurements in the darkest conditions.
TROPOMI is currently in its detailed design phase. This paper gives an overview of the challenges and current performances. From unit level engineering models first results are becoming available. Early results are promising and this paper discusses some of these early H/W results.
TROPOMI is the single payload on the Sentinel-5 precursor mission which is a joint initiative of the European Community (EC) and of the European Space Agency (ESA). The 2015 launch intends to bridge the data stream from OMI / SCIAMACHY and the upcoming Sentinel 5 mission. The instrument is funded jointly by the Netherlands Space Office and by ESA. Dutch Space is the instrument prime contractor. SSTL in the UK is developing the SWIR module with a significant contribution from SRON. Dutch Space and TNO are working as an integrated team for the UVN module. KNMI and SRON are responsible for ensuring the scientific capabilities of the instrument.
KEYWORDS: Sensors, Short wave infrared radiation, Spectroscopy, Space telescopes, Telescopes, Astronomical imaging, Calibration, Electronics, Near infrared, Space operations
The Tropospheric Monitoring Instrument TROPOMI is ready for system level verification. All sub-units have been integrated and tested and final integration at Dutch Space in Leiden has been completed. The instrument will be subjected to a testing and calibration program and is expected to be ready for delivery to the spacecraft early 2015. Using TROPOMI measurements, scientists will be able to improve and continue the study of the Earth’s atmosphere and to monitor air quality, on both global and local scale.
Optical components such as diffraction gratings are widely used in Space-flight satellites to analyse light properties from soft-X rays to Infra-Red. The diffraction gratings are one of the key optical components of space-flight instruments and have to exhibit very high optical performances.
Earth observation measurements at wavelengths below 320nm are challenging due to the steep decrease of the earth irradiance towards shorter wavelengths. Stray light and ghosting of longer wave light can easily overwhelm the signals at short wavelengths. In the UV channel (270-320nm) of the TROPOMI instrument this challenge has been addressed using a number of coatings. Three black UV mirror coatings absorb light with a wavelength above 370nm. Together, these achieve more than four orders suppression of long wave out-of-band light. A lowpass transmission filter with a position dependent cut-off wavelength is deposited on the last lens surface, directly in front of the detector. At the position where short wavelength light passes the filter, longer wavelength in-band stray light and ghosts are blocked. A simulation predicts that this graded filter reduces ghosting by a factor 20 and scatter related stray light by factor 30.
The Tropospheric Monitoring Instrument, TROPOMI, is a passive UV-VIS-NIR-SWIR spectrograph, which uses sun
backscattered radiation to study the Earth's atmosphere and to monitor air quality, on both global and local scale. It
follows in the line of SCIAMACHY (2002) and OMI (2004), both of which have been very successful. OMI is still
operational. TROPOMI is scheduled for launch in 2015. Compared with its predecessors, TROPOMI will take a major
step forward in spatial resolution and sensitivity. The nominal observations are at 7 x 7 km2 at nadir and the signal-tonoises
are sufficient for trace gas retrieval even at very low albedos (2 to 5%). This allows observations of air quality at
sub-city level. TROPOMI has reached CDR status and production of flight model units has started. Flight detectors have
been produced and detector electronics is expected to be finished by mid-2013. The instrument control unit is undergoing
extensive tests, to ensure full instrument functionality. Early results are promising and this paper discusses these H/W
results, as well as some challenges encountered during the development of the instrument.
The Tropospheric Monitoring Instrument (TROPOMI) is being developed for launch in 2014 on ESAs Sentinel 5
Precursor satellite. TROPOMI is a passive sun backscatter spectrograph using the ultraviolet-to-SWIR wavelengths to
have good sensitivity down to the surface. Together with its spatial resolution of 7 x 7 km2 it allows good observations
of sources and sinks of air quality and climate related gases and aerosols. This spatial resolution results in a high
fraction of cloud-free observations and is combined with a wide cross-flight swath to allow daily coverage of the
complete Earth.
The instrument has as predecessors the OMI instrument (Ozone Monitoring Instrument) on NASAs AURA satellite and
the SCIAMACHY instrument on ESAs ENVISAT, where the push broom concept is derived from OMI and the SWIR
observations from SCIAMACHY.
The wavelength bands of TROPOMI are a UV band (270 - 320 nm) for the ozone profile and SO2 products, a UVIS
band (320 - 500 nm) for O3, NO2, BrO, HCHO and OClO total columns, a NIR band (675 - 775 nm) for clouds and H2O
columns and a SWIR band (2305 - 2385 nm) for CH4 and CO columns and the HDO/H2O ratio.
The paper will give an overview of the challenges and current performances.
The TROPOMI UVN module is funded by the Netherlands and the SWIR module and platform is provided via ESA.
The instrument development is now a truly European programme with contributions from several countries.
The Tropospheric Monitoring Instrument (TROPOMI) is currently planned for launch on ESA's Sentinel 5 precursor
satellite in the time frame of 2014. TROPOMI is an ultraviolet-to-SWIR wavelengths imaging spectrograph that uses
two-dimensional detectors to register both the spectrum and the swath perpendicular to the flight direction. The swath is
about 110 degrees wide to allow daily global coverage from the polar orbit of the Sentinel 5 precursor satellite. The
instrument follows the heritage of SCIAMACHY (ENVISAT, launch 2002) and OMI (AURA, launch 2004), but it has
been improved in several ways: the ground resolution is down to 7 x 7 km2, the instrument is fit for low albedo scenes
and the wavelength bands are optimized using the SCIAMACHY and OMI heritages to have the best trace gas products.
The first two improvements basically mean that the instrument aperture is much larger for TROPOMI and, related to
this, the reading of the detectors much faster. The selected wavelength bands for TROPOMI are UV1 (270-310 nm),
UV2 (310 - 370 nm), VIS (370 - 500 nm), NIR (675 - 775 nm) and SWIR (2305 - 2385 nm). The first three bands are
very similar to the OMI bands, the NIR has been added to improve on clouds and air mass corrections and the SWIR
allows measuring CH4 and CO. The paper discusses the development status on several topics, such as detector selection
and polarization scrambler performance simulations using the TIDE grid based level 2 scene simulator.
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